Sample records for observed band positions

  1. Absence of paired crossing in the positive parity bands of 124Cs

    NASA Astrophysics Data System (ADS)

    Singh, A. K.; Basu, A.; Nag, Somnath; Hübel, H.; Domscheit, J.; Ragnarsson, I.; Al-Khatib, A.; Hagemann, G. B.; Herskind, B.; Elema, D. R.; Wilson, J. N.; Clark, R. M.; Cromaz, M.; Fallon, P.; Görgen, A.; Lee, I.-Y.; Ward, D.; Ma, W. C.

    2018-02-01

    High-spin states in 124Cs were populated in the 64Ni(64Ni,p 3 n ) reaction and the Gammasphere detector array was used to measure γ -ray coincidences. Both positive- and negative-parity bands, including bands with chiral configurations, have been extended to higher spin, where a shape change has been observed. The configurations of the bands before and after the alignment are discussed within the framework of the cranked Nilsson-Strutinsky model. The calculations suggest that the nucleus undergoes a shape transition from triaxial to prolate around spin I ≃22 of the positive-parity states. The alignment gain of 8 ℏ , observed in the positive-parity bands, is due to partial alignment of several valence nucleons. This indicates the absence of band crossing due to paired nucleons in the bands.

  2. Improved Band-to-Band Registration Characterization for VIIRS Reflective Solar Bands Based on Lunar Observations

    NASA Technical Reports Server (NTRS)

    Wang, Zhipeng; Xiong, Xiaoxiong; Li, Yonghong

    2015-01-01

    Spectral bands of the Visible Infrared Imaging Radiometer Suite (VIIRS) instrumentaboard the Suomi National Polar-orbiting Partnership (S-NPP) satellite are spatially co-registered.The accuracy of the band-to-band registration (BBR) is one of the key spatial parameters that must becharacterized. Unlike its predecessor, the Moderate Resolution Imaging Spectroradiometer (MODIS), VIIRS has no on-board calibrator specifically designed to perform on-orbit BBR characterization.To circumvent this problem, a BBR characterization method for VIIRS reflective solar bands (RSB) based on regularly-acquired lunar images has been developed. While its results can satisfactorily demonstrate that the long-term stability of the BBR is well within +/- 0.1 moderate resolution bandpixels, undesired seasonal oscillations have been observed in the trending. The oscillations are most obvious between the visiblenear-infrared bands and short-middle wave infrared bands. This paper investigates the oscillations and identifies their cause as the band spectral dependence of the centroid position and the seasonal rotation of the lunar images over calibration events. Accordingly, an improved algorithm is proposed to quantify the rotation and compensate for its impact. After the correction, the seasonal oscillation in the resulting BBR is reduced from up to 0.05 moderate resolution band pixels to around 0.01 moderate resolution band pixels. After removing this spurious seasonal oscillation, the BBR, as well as its long-term drift are well determined.

  3. Projected Shell Model Description of Positive Parity Band of 130Pr Nucleus

    NASA Astrophysics Data System (ADS)

    Singh, Suram; Kumar, Amit; Singh, Dhanvir; Sharma, Chetan; Bharti, Arun; Bhat, G. H.; Sheikh, J. A.

    2018-02-01

    Theoretical investigation of positive parity yrast band of odd-odd 130Pr nucleus is performed by applying the projected shell model. The present study is undertaken to investigate and verify the very recently observed side band in 130Pr theoretically in terms of quasi-particle (qp) configuration. From the analysis of band diagram, the yrast as well as side band are found to arise from two-qp configuration πh 11/2 ⊗ νh 11/2. The present calculations are viewed to have qualitatively reproduced the known experimental data for yrast states, transition energies, and B( M1) / B( E2) ratios of this nucleus. The recently observed positive parity side band is also reproduced by the present calculations. The energy states of the side band are predicted up to spin 25+, which is far above the known experimental spin of 18+ and this could serve as a motivational factor for future experiments. In addition, the reduced transition probability B( E2) for interband transitions has also been calculated for the first time in projected shell model, which would serve as an encouragement for other research groups in the future.

  4. Structure of positive parity bands and observation of magnetic rotation in 108Ag

    NASA Astrophysics Data System (ADS)

    Sethi, Jasmine; Palit, R.

    2015-10-01

    The interplay of nuclear forces among the neutron particles (holes) and proton holes (particles) in the odd-odd nuclei gives rise to a variety of shapes and hence novel modes of excitations. The odd-odd nuclei in the A ~ 110 region have proton holes in the g9/2 orbital and the neutron particles in the h11/2 orbitals. A systematic study of shears mechanism in A ~ 110 region indicates the presence of magnetic rotation (MR) phenomenon in Ag and In isotopes. Therefore, the structure of doubly odd 108Ag nucleus was probed in two different reactions, i.e, 100Mo(11B, 4n)108Ag at 39 MeV and 94Zr(18O, p3n)108Ag at 72 MeV beam energies. The emitted γ-rays were detected using the Indian National Gamma Array (INGA) at TIFR, Mumbai. A significant number of new transitions and energy levels were identified. Lifetime measurements, using the Doppler shift attenuation method, have been carried out for a positive parity dipole band. Tilted Axis Cranking (TAC) calculations have been performed for two positive parity dipole bands.

  5. Band positions of Rutile surfaces and the possibility of water splitting

    NASA Astrophysics Data System (ADS)

    Esch, Tobit R.; Bredow, Thomas

    2017-11-01

    It is well known that both the band gap and the band edge positions of oxide semiconductors are important for the photocatalytic water splitting. In this study, we show that different surface terminations of the same crystalline solid lead to considerable variations of the band gaps and band edges. As an example, we investigate the low-index surfaces of rutile TiO2. A series of hybrid methods based on the PBE exchange-correlation functional, PBE0, HSE06 and HISS, are employed to study the effect of long-range exchange on the electronic properties. In aqueous solution, the oxide particles employed in photocatalysis are fully covered with water molecules. We therefore study the influence of molecularly and dissociatively adsorbed water on the band positions. It is found that water adsorption leads to significant shifts of the band edge positions due to changes of the electrostatic potential at the surface atom positions.

  6. Determination of Precise Satellite Orbital Position Using Multi-Band GNSS Signals

    DTIC Science & Technology

    2017-10-16

    AFRL-AFOSR-JP-TR-2018-0002 Determination of Precise Satellite Orbital Position Using Multi -Band GNSS Signals Erry Gunawan NANYANG TECHNOLOGICAL...Position Using Multi -Band GNSS Signals 5a.  CONTRACT NUMBER 5b.  GRANT NUMBER FA2386-15-1-4041 5c.  PROGRAM ELEMENT NUMBER 61102F 6. AUTHOR(S) Erry...Grant FA2386-15-1-4041 “Determination of Precise orbital position using multi -band GNSS signals” October 13, 2017 Name of Principal Investigators

  7. Standard Observing Bands: Is Now the Time to Replace S/X with X/Ka?

    NASA Technical Reports Server (NTRS)

    Jacobs, C. S.; Lanyi, G. E.; Naudet, C. J.

    2004-01-01

    In this paper we will argue that the VLBI community should be developing a road map to transition from S/X to simultaneous X and Ka-band (32 GHz) observations. There are both negative and positive reasons for planning such a transition. On the negative side, we will outline concerns that S-band observations may be headed toward obsolescence. On the positive side, we will refer to evidence that X/Ka has potential for providing a more stable reference frame than S/X. We will propose timetables for a transition to X/Ka observing starting from the current status of X/Ka and plans that are now taking shape. First X/Ka fringes were obtained in 2001 with the Deep Space Network. Future plans will be discussed including a proposed X/Ka-band upgrade to the VLBA. Lastly, we will consider the need for a period of overlap between S/X and X/Ka so that the long and rich history of astrometric and geodetic VLBI is not compromised.

  8. Observation and Uses of Position-Space Bloch Oscillations in an Ultracold Gas.

    PubMed

    Geiger, Zachary A; Fujiwara, Kurt M; Singh, Kevin; Senaratne, Ruwan; Rajagopal, Shankari V; Lipatov, Mikhail; Shimasaki, Toshihiko; Driben, Rodislav; Konotop, Vladimir V; Meier, Torsten; Weld, David M

    2018-05-25

    We report the observation and characterization of position-space Bloch oscillations using cold atoms in a tilted optical lattice. While momentum-space Bloch oscillations are a common feature of optical lattice experiments, the real-space center-of-mass dynamics are typically unresolvable. In a regime of rapid tunneling and low force, we observe real-space Bloch oscillation amplitudes of hundreds of lattice sites, in both ground and excited bands. We demonstrate two unique capabilities enabled by tracking of Bloch dynamics in position space: measurement of the full position-momentum phase-space evolution during a Bloch cycle, and direct imaging of the lattice band structure. These techniques, along with the ability to exert long-distance coherent control of quantum gases without modulation, may open up new possibilities for quantum control and metrology.

  9. Observation and Uses of Position-Space Bloch Oscillations in an Ultracold Gas

    NASA Astrophysics Data System (ADS)

    Geiger, Zachary A.; Fujiwara, Kurt M.; Singh, Kevin; Senaratne, Ruwan; Rajagopal, Shankari V.; Lipatov, Mikhail; Shimasaki, Toshihiko; Driben, Rodislav; Konotop, Vladimir V.; Meier, Torsten; Weld, David M.

    2018-05-01

    We report the observation and characterization of position-space Bloch oscillations using cold atoms in a tilted optical lattice. While momentum-space Bloch oscillations are a common feature of optical lattice experiments, the real-space center-of-mass dynamics are typically unresolvable. In a regime of rapid tunneling and low force, we observe real-space Bloch oscillation amplitudes of hundreds of lattice sites, in both ground and excited bands. We demonstrate two unique capabilities enabled by tracking of Bloch dynamics in position space: measurement of the full position-momentum phase-space evolution during a Bloch cycle, and direct imaging of the lattice band structure. These techniques, along with the ability to exert long-distance coherent control of quantum gases without modulation, may open up new possibilities for quantum control and metrology.

  10. Observations of banding in first-year Arctic sea ice

    NASA Astrophysics Data System (ADS)

    Cole, David M.; Eicken, Hajo; Frey, Karoline; Shapiro, Lewis H.

    2004-08-01

    Horizontal banding features, alternating dark and bright horizontal bands apparent in ice cores and stratigraphic cross sections have long been observed in first-year sea ice and are frequently associated with bands of high and low brine or gas porosity. Observations on the land-fast ice near Barrow, Alaska, in recent years have revealed particularly striking banding patterns and prompted a study of their macroscopic and microscopic characteristics. The banding patterns are quantified from photographs of full-depth sections of the ice, and examples are presented from the Chukchi Sea and Elson Lagoon. Statistics on band spacing are presented, and the growth records for three seasons are employed to estimate their time of formation. These data provide insight into the periodicity of the underlying phenomena. Micrographs are used to examine the microstructural variations associated with various banding features and to quantify the geometry of the constituent brine inclusions associated with high- and low-porosity bands. The micrography revealed that the area fraction of brine inclusions varied by a factor of nearly 3 through the more pronounced high- and low-porosity bands. Vertical micrographs obtained shortly after the materials' removal from the ice sheet showed that significantly larger inclusions form abruptly at the start of the high-porosity bands and frequently terminate abruptly at the end of the band. Crystallographic observations indicated that the high-porosity bands supported the nucleation and growth of crystals having substantially different orientations from the very well aligned columnar structure that characterized the bulk of the sheet.

  11. Banded whistlers observed on OGO-4

    NASA Technical Reports Server (NTRS)

    Paymar, E. M.

    1972-01-01

    Inspection of broadband VLF records from OGO-4 shows that some whistlers exhibit a banded structure in which one or more bands of frequencies are missing from the whistler's spectrum. The phenomenon is commonly observed by satellites on midlatitude field lines at all local times and at various longitudes around the world. The dispersion of banded whistlers (BW) is of several tens of sec to the 1/2 power, indicating that they originated in the opposite hemisphere and are propagating downward at the satellite. BW are generally spread in time (tenths of seconds) rather than sharply defined and tend to occur at random. The frequency spacing of the bands may be either uniform or irregular, and may vary radically between successive events. Several possible explanations for BW are considered. In particular, an analysis of the interaction of plane electromagnetic waves traveling in an anisotropic plasma with a field aligned slab of enhanced ionization is presented with promising results.

  12. Line Assignments and Position Measurements in Several Weak CO2 Bands Between 4590/cm and 7930/cm

    NASA Technical Reports Server (NTRS)

    Giver, L. P.; Kshirsagar, R. J.; Freedman, R. C.; Chackerian, C., Jr.; Wattson, R. B.; Gore, Warren J. (Technical Monitor)

    1998-01-01

    A substantial set of CO2 spectra from 4500 to 12000/cm has been obtained at Ames with 1500 m path length using a Bomem DA8 FTS. The signal/noise was improved compared to prior spectra obtained in this laboratory by including a filter wheel limiting the band-pass of each spectrum to several hundred per cm. We have measured positions of lines in several weak bands not previously resolved in laboratory spectra. Using our positions and assignments of lines of the Qbranch of the 31103-00001 vibrational band at 4591/cm, we have redetermined the rotational constants for the 31103f levels. Q-branch lines of this band were previously observed, but misassigned, in Venus spectra by Mandin. The current HITRAN values of the rotational constants for this level are incorrect due to the Q-branch misassignments. Our prior measurements of the 21122-00001 vibrational band at 7901/cm were limited to Q-and R-branch lines; with the improved signal/noise of these new spectra we have now measured lines in the weaker P branch. The 21122 (Gv = 790148/cm) levels are known to be perturbed by the 32211 (G(sub v) = 789757/cm) levels; new DND calculations predict that high-J lines of the forbidden 32211-00001 vibrational band 'borrow' intensity from the corresponding transitions of the 21122-00001 band. We have identified such Q- and R-branch transitions of the 32211-00001 band from 26 < J" < 44, based on our position measurements of lines in the 32211-02201 band at 6562/cm.

  13. The Mars Observer Ka-band link experiment

    NASA Technical Reports Server (NTRS)

    Rebold, T. A.; Kwok, A.; Wood, G. E.; Butman, S.

    1994-01-01

    The Ka-Band Link Experiment was the first demonstration of a deep-space communications link in the 32- to 35-GHz band (Ka-band). It was carried out using the Mars Observer spacecraft while the spacecraft was in the cruise phase of its mission and using a 34-meter beam-waveguide research and development antenna at the Goldstone complex of the DSN. The DSN has been investigating the performance benefits of a shift from X-band (8.4 GHz) to Ka-band (32 GHz) for deep-space communications. The fourfold increase in frequency is expected to offer a factor of 3 to 10 improvement (5 to 10 dB) in signal strength for a given spacecraft transmitter power and antenna size. Until recently, the expected benefits were based on performance studies, with an eye to implementing such a link, but theory was transformed to reality when a 33.7-GHz Ka-band signal was received from the spacecraft by DSS 13. This article describes the design and implementation of the Ka-Band Link Experiment from the spacecraft to the DSS-13 system, as well as results from the Ka-band telemetry demonstration, ranging demonstration, and long-term tracking experiment. Finally, a preliminary analysis of comparative X- and Ka-band tracking results is included. These results show a 4- to 7-dB advantage for Ka-band using the system at DSS 13, assuming such obstacles as antenna pointing loss and power conversion loss are overcome.

  14. Line Assignments and Position Measurements in Several Weak CO2 Bands between 4590 /cm and 7930/ cm

    NASA Technical Reports Server (NTRS)

    Giver, L. P.; Kshirsagar, R. J.; Freedman, R. C.; Chackerian, C.; Wattson, R. B.

    1998-01-01

    A substantial set of CO2 spectra from 4500 to 12000 /cm has been obtained at Ames with 1500 m path length using a Bomem DA8 FTS. The signal/noise was improved compared to prior spectra obtained in this laboratory by including a filter wheel limiting the band-pass of each spectrum to several hundred/cm. We have measured positions of lines in several weak bands not previously resolved in laboratory spectra. Using our positions and assignments of lines of the Q branch of the 31103-00001 vibrational band at 4591/cm, we have re-determined the rotational constants for the 31103f levels. Q-branch lines of this band were previously observed, but misassigned, in Venus spectra by Mandin. The current HITRAN values of the rotational constants for this level are incorrect due to the Q-branch misassignments. Our prior measurements of the 21122-00001 vibrational band at 7901/cm were limited to Q- and R-branch lines; with the improved signal/noise of these new spectra we have now measured lines in the weaker P branch.

  15. On the role of covariance information for GRACE K-band observations in the Celestial Mechanics Approach

    NASA Astrophysics Data System (ADS)

    Bentel, Katrin; Meyer, Ulrich; Arnold, Daniel; Jean, Yoomin; Jäggi, Adrian

    2017-04-01

    The Astronomical Institute at the University of Bern (AIUB) derives static and time-variable gravity fields by means of the Celestial Mechanics Approach (CMA) from GRACE (level 1B) data. This approach makes use of the close link between orbit and gravity field determination. GPS-derived kinematic GRACE orbit positions, inter-satellite K-band observations, which are the core observations of GRACE, and accelerometer data are combined to rigorously estimate orbit and spherical harmonic gravity field coefficients in one adjustment step. Pseudo-stochastic orbit parameters are set up to absorb unmodeled noise. The K-band range measurements in along-track direction lead to a much higher correlation of the observations in this direction compared to the other directions and thus, to north-south stripes in the unconstrained gravity field solutions, so-called correlated errors. By using a full covariance matrix for the K-band observations the correlation can be taken into account. One possibility is to derive correlation information from post-processing K-band residuals. This is then used in a second iteration step to derive an improved gravity field solution. We study the effects of pre-defined covariance matrices and residual-derived covariance matrices on the final gravity field product with the CMA.

  16. Tuning colloidal quantum dot band edge positions through solution-phase surface chemistry modification

    PubMed Central

    Kroupa, Daniel M.; Vörös, Márton; Brawand, Nicholas P.; McNichols, Brett W.; Miller, Elisa M.; Gu, Jing; Nozik, Arthur J.; Sellinger, Alan; Galli, Giulia; Beard, Matthew C.

    2017-01-01

    Band edge positions of semiconductors determine their functionality in many optoelectronic applications such as photovoltaics, photoelectrochemical cells and light emitting diodes. Here we show that band edge positions of lead sulfide (PbS) colloidal semiconductor nanocrystals, specifically quantum dots (QDs), can be tuned over 2.0 eV through surface chemistry modification. We achieved this remarkable control through the development of simple, robust and scalable solution-phase ligand exchange methods, which completely replace native ligands with functionalized cinnamate ligands, allowing for well-defined, highly tunable chemical systems. By combining experiments and ab initio simulations, we establish clear relationships between QD surface chemistry and the band edge positions of ligand/QD hybrid systems. We find that in addition to ligand dipole, inter-QD ligand shell inter-digitization contributes to the band edge shifts. We expect that our established relationships and principles can help guide future optimization of functional organic/inorganic hybrid nanostructures for diverse optoelectronic applications. PMID:28508866

  17. Tuning colloidal quantum dot band edge positions through solution-phase surface chemistry modification

    NASA Astrophysics Data System (ADS)

    Kroupa, Daniel M.; Vörös, Márton; Brawand, Nicholas P.; McNichols, Brett W.; Miller, Elisa M.; Gu, Jing; Nozik, Arthur J.; Sellinger, Alan; Galli, Giulia; Beard, Matthew C.

    2017-05-01

    Band edge positions of semiconductors determine their functionality in many optoelectronic applications such as photovoltaics, photoelectrochemical cells and light emitting diodes. Here we show that band edge positions of lead sulfide (PbS) colloidal semiconductor nanocrystals, specifically quantum dots (QDs), can be tuned over 2.0 eV through surface chemistry modification. We achieved this remarkable control through the development of simple, robust and scalable solution-phase ligand exchange methods, which completely replace native ligands with functionalized cinnamate ligands, allowing for well-defined, highly tunable chemical systems. By combining experiments and ab initio simulations, we establish clear relationships between QD surface chemistry and the band edge positions of ligand/QD hybrid systems. We find that in addition to ligand dipole, inter-QD ligand shell inter-digitization contributes to the band edge shifts. We expect that our established relationships and principles can help guide future optimization of functional organic/inorganic hybrid nanostructures for diverse optoelectronic applications.

  18. Extragalactic radio sources - Accurate positions from very-long-baseline interferometry observations

    NASA Technical Reports Server (NTRS)

    Rogers, A. E. E.; Counselman, C. C., III; Hinteregger, H. F.; Knight, C. A.; Robertson, D. S.; Shapiro, I. I.; Whitney, A. R.; Clark, T. A.

    1973-01-01

    Relative positions for 12 extragalactic radio sources have been determined via wide-band very-long-baseline interferometry (wavelength of about 3.8 cm). The standard error, based on consistency between results from widely separated periods of observation, appears to be no more than 0.1 sec for each coordinate of the seven sources that were well observed during two or more periods. The uncertainties in the coordinates determined for the other five sources are larger, but in no case exceed 0.5 sec.

  19. Band-edge positions in G W : Effects of starting point and self-consistency

    NASA Astrophysics Data System (ADS)

    Chen, Wei; Pasquarello, Alfredo

    2014-10-01

    We study the effect of starting point and self-consistency within G W on the band-edge positions of semiconductors and insulators. Compared to calculations based on a semilocal starting point, the use of a hybrid-functional starting point shows a larger quasiparticle correction for both band-edge states. When the self-consistent treatment is employed, the band-gap opening is found to result mostly from a shift of the valence-band edge. Within the non-self-consistent methods, we analyse the performance of empirical and nonempirical schemes in which the starting point is optimally tuned. We further assess the accuracy of the band-edge positions through the calculation of ionization potentials of surfaces. The ionization potentials for most systems are reasonably well described by one-shot calculations. However, in the case of TiO2, we find that the use of self-consistency is critical to obtain a good agreement with experiment.

  20. Probing the gamma-ray variability in 3C 279 using broad-band observations

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Rani, B.; Krichbaum, T. P.; Lee, S. -S.

    2016-09-27

    In this study, we present the results of a broad-band radio-to-GeV observing campaign organized to get a better understanding of the radiation processes responsible for the γ-ray flares observed in 3C 279. The total intensity and polarization observations of the source were carried out between 2013 December 28 and 2014 January 03 using the Fermi-Large Area Telescope, Swift-XRT, Swift-UVOT, and Korean VLBI Network telescopes. A prominent flare observed in the optical/near-UV passbands was found to be correlated with a concurrent γ-ray flare at a confidence level >95 percent, which suggests a co-spatial origin of the two. Moreover, the flaring activitymore » in the two regimes was accompanied by no significant spectral variations. A peak in the X-ray light curve coincides with the peaks of the fractional polarization curves at 43 and 86 GHz radio bands. No prominent variation was noticed for the total intensity and the electric vector position angle observations at radio bands during this period. We noticed a possible hint of steepening of the radio spectrum with an increase in percentage polarization, which suggests that the radio polarization variations could be simply due to a spectral change. In a simple scenario, the correlated optical/γ-ray flares could be caused by the same population of emitting particles. The coincidence of the increase in radio polarization with the X-ray flux supports the picture that X-rays are produced via inverse-Compton scattering of radio photons. Finally, the observed fractional variability for the γ-ray flare ~0.23 does not exceed that in the optical regime, which is inconsistent with what we usually observe for 3C 279; it could be due to different dependencies of the magnetic field and the external radiation field energy density profiles along the jet.« less

  1. UNITED STATES DEPARTMENT OF TRANSPORTATION GLOBAL POSITIONING SYSTEM (GPS) ADJACENT BAND COMPATIBILITY ASSESSMENT

    DOT National Transportation Integrated Search

    2018-04-01

    The goal of the U.S. Department of Transportation (DOT) Global Positioning System (GPS) Adjacent Band Compatibility Assessment is to evaluate the maximum transmitted power levels of adjacent band radiofrequency (RF) systems that can be tolerated by G...

  2. Observation of symmetry-protected topological band with ultracold fermions

    PubMed Central

    Song, Bo; Zhang, Long; He, Chengdong; Poon, Ting Fung Jeffrey; Hajiyev, Elnur; Zhang, Shanchao; Liu, Xiong-Jun; Jo, Gyu-Boong

    2018-01-01

    Symmetry plays a fundamental role in understanding complex quantum matter, particularly in classifying topological quantum phases, which have attracted great interests in the recent decade. An outstanding example is the time-reversal invariant topological insulator, a symmetry-protected topological (SPT) phase in the symplectic class of the Altland-Zirnbauer classification. We report the observation for ultracold atoms of a noninteracting SPT band in a one-dimensional optical lattice and study quench dynamics between topologically distinct regimes. The observed SPT band can be protected by a magnetic group and a nonlocal chiral symmetry, with the band topology being measured via Bloch states at symmetric momenta. The topology also resides in far-from-equilibrium spin dynamics, which are predicted and observed in experiment to exhibit qualitatively distinct behaviors in quenching to trivial and nontrivial regimes, revealing two fundamental types of spin-relaxation dynamics related to bulk topology. This work opens the way to expanding the scope of SPT physics with ultracold atoms and studying nonequilibrium quantum dynamics in these exotic systems. PMID:29492457

  3. Fireball Observations in Visible and Sodium Bands

    NASA Astrophysics Data System (ADS)

    Fletcher, Sandra

    On November 17th at 1:32am MST, a large Leonid fireball was simultaneously imaged by two experiments, a visible band CCD camera and a 590nm filtered band equi-angle fisheye and telecentric lens assembly. The visible band camera, ROTSE (Robotic Optical Transient Search Experiment) is a two by two f/1.9 telephoto lens array with 2k x2k Thompson CCD and is located at 35.87 N, 106.25 W at an altitude of 2115m. One-minute exposures along the radiant were taken of the event for 30 minutes after the initial explosion. The sodium band experiment was located at 35.29 N,106.46 W at an altitude of 1860m. It took ninety second exposures and captured several events throughout the night. Triangulation from two New Mexico sites resulted in an altitude of 83km over Wagon Mound, NM. Two observers present at the ROTSE site saw a green flash and a persistent glow up to seven minutes after the explosion. Cataloging of all sodium trails for comparison with lidar and infrasonic measurements is in progress. The raw data from both experiments and the atmospheric chemistry interpretation of them will be presented.

  4. Tuning colloidal quantum dot band edge positions through solution-phase surface chemistry modification

    DOE PAGES

    Kroupa, Daniel M.; Vörös, Márton; Brawand, Nicholas P.; ...

    2017-05-16

    Band edge positions of semiconductors determine their functionality in many optoelectronic applications such as photovoltaics, photoelectrochemical cells and light emitting diodes. Here we show that band edge positions of lead sulfide (PbS) colloidal semiconductor nanocrystals, specifically quantum dots (QDs), can be tuned over 2.0 eV through surface chemistry modification. We achieved this remarkable control through the development of simple, robust and scalable solution-phase ligand exchange methods, which completely replace native ligands with functionalized cinnamate ligands, allowing for well-defined, highly tunable chemical systems. By combining experiments and ab initio simulations, we establish clear relationships between QD surface chemistry and the bandmore » edge positions of ligand/QD hybrid systems. We find that in addition to ligand dipole, inter-QD ligand shell inter-digitization contributes to the band edge shifts. As a result, we expect that our established relationships and principles can help guide future optimization of functional organic/inorganic hybrid nanostructures for diverse optoelectronic applications.« less

  5. Tuning colloidal quantum dot band edge positions through solution-phase surface chemistry modification

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Kroupa, Daniel M.; Vörös, Márton; Brawand, Nicholas P.

    Band edge positions of semiconductors determine their functionality in many optoelectronic applications such as photovoltaics, photoelectrochemical cells and light emitting diodes. Here we show that band edge positions of lead sulfide (PbS) colloidal semiconductor nanocrystals, specifically quantum dots (QDs), can be tuned over 2.0 eV through surface chemistry modification. We achieved this remarkable control through the development of simple, robust and scalable solution-phase ligand exchange methods, which completely replace native ligands with functionalized cinnamate ligands, allowing for well-defined, highly tunable chemical systems. By combining experiments and ab initio simulations, we establish clear relationships between QD surface chemistry and the bandmore » edge positions of ligand/QD hybrid systems. We find that in addition to ligand dipole, inter-QD ligand shell inter-digitization contributes to the band edge shifts. As a result, we expect that our established relationships and principles can help guide future optimization of functional organic/inorganic hybrid nanostructures for diverse optoelectronic applications.« less

  6. Development and Observation of the Phase Array Radar at X band

    NASA Astrophysics Data System (ADS)

    Ushio, T.; Shimamura, S.; Wu, T.; Kikuchi, H.; Yoshida, S.; Kawasaki, Z.; Mizutani, F.; Wada, M.; Satoh, S.; Iguchi, T.

    2013-12-01

    A new Phased Array Radar (PAR) system for thunderstorm observation has been developed by Toshiba Corporation and Osaka University under a grant of NICT, and installed in Osaka University, Japan last year. It is now well known that rapidly evolving severe weather phenomena (e.g., microbursts, severe thunderstorms, tornadoes) are a threat to our lives particularly in a densely populated area and is closely related to the production of lightning discharges. Over the past decade, mechanically rotating radar systems at the C-band or S-band have been proved to be effective for weather surveillance especially in a wide area more than 100 km in range. However, severe thunderstorm sometimes develops rapidly on the temporal and spatial scales comparable to the resolution limit (-10 min. and -500m) of typical S-band or C-band radar systems, and cannot be fully resolved with these radar systems. In order to understand the fundamental process and dynamics of such fast changing weather phenomena like lightning and tornado producing thunderstorm, volumetric observations with both high temporal and spatial resolution are required. The phased array radar system developed has the unique capability of scanning the whole sky with 100m and 10 to 30 second resolution up to 60 km. The system adopts the digital beam forming technique for elevation scanning and mechanically rotates the array antenna in azimuth direction within 10 to 30 seconds. The radar transmits a broad beam of several degrees with 24 antenna elements and receives the back scattered signal with 128 elements digitizing at each elements. Then by digitally forming the beam in the signal processor, the fast scanning is realized. After the installation of the PAR system in Osaka University, the initial observation campaign was conducted in Osaka urban area with Ku-band Broad Band Radar (BBR) network, C-band weather radar, and lightning location system. The initial comparison with C band radar system shows that the developed

  7. Operational Observation of Australian Bioregions with Bands 8-19 of Modis

    NASA Astrophysics Data System (ADS)

    McAtee, B. K.; Gray, M.; Broomhall, M.; Lynch, M.; Fearns, P.

    2012-07-01

    Data from bands 1-7 are the most common bands of the MODIS instrument used for near-real time terrestrial earth observation operations in Australia. However, many of Australia's bioregions present unique scenarios which constitute a challenge for quantitative environmental remote sensing. We believe that data from MODIS bands 8-19 may provide significant benefit to Earth observation over particular bioregions of the Australian continent. Examples here include the use of band 8 in characterising aerosol optical depth over typically bright land surfaces and accounting for anomalous retrievals of atmospheric water vapour obtained using MOD05 based on the abundance of Australia's 'red dirt', which exhibits absorption features in the near infrared bands 17-19 of MODIS. Bioregion-focused applications such as those mentioned above have driven the development of automated processing, infrastructure for the atmospheric and BRDF correction of the first 19 bands of MODIS rather than only the first 7, which is more often the case. This work has been facilitated by the AusCover project which is the remote sensing component of the Terrestrial Ecosystem Research Network (TERN), itself a program designed to create a new generation of infrastructure for ecological study of the Australian landscape.

  8. A Ka-band (32 GHz) beacon link experiment (KABLE) with Mars Observer

    NASA Technical Reports Server (NTRS)

    Riley, A. L.; Hansen, D. M.; Mileant, A.; Hartop, R. W.

    1987-01-01

    A proposal for a Ka-Band (32 GHz) Link Experiment (KABLE) with the Mars Observer mission was submitted to NASA. The experiment will rely on the fourth harmonic of the spacecraft X-band transmitter to generate a 33.6 GHz signal. The experiment will rely also on the Deep Space Network (DSN) receiving station equipped to simultaneously receive X- and Ka-band signals. The experiment will accurately measure the spacecraft-to-Earth telecommunication link performance at Ka-band and X-band (8.4 GHz).

  9. Observation of band gaps in the gigahertz range and deaf bands in a hypersonic aluminum nitride phononic crystal slab

    NASA Astrophysics Data System (ADS)

    Gorisse, M.; Benchabane, S.; Teissier, G.; Billard, C.; Reinhardt, A.; Laude, V.; Defaÿ, E.; Aïd, M.

    2011-06-01

    We report on the observation of elastic waves propagating in a two-dimensional phononic crystal composed of air holes drilled in an aluminum nitride membrane. The theoretical band structure indicates the existence of an acoustic band gap centered around 800 MHz with a relative bandwidth of 6.5% that is confirmed by gigahertz optical images of the surface displacement. Further electrical measurements and computation of the transmission reveal a much wider attenuation band that is explained by the deaf character of certain bands resulting from the orthogonality of their polarization with that of the source.

  10. An 'X-banded' Tidbinbilla interferometer

    NASA Technical Reports Server (NTRS)

    Batty, Michael J.; Gardyne, R. G.; Gay, G. J.; Jauncy, David L.; Gulkis, S.; Kirk, A.

    1986-01-01

    The recent upgrading of the Tidbinbilla two-element interferometer to simultaneous S-band (2.3 GHz) and X-band (8.4 GHz) operation has provided a powerful new astronomical facility for weak radio source measurement in the Southern Hemisphere. The new X-band system has a minimum fringe spacing of 38 arcsec, and about the same positional measurement capability (approximately 2 arcsec) and sensitivity (1 s rms noise of 10 mJy) as the previous S-band system. However, the far lower confusion limit will allow detection and accurate positional measurements for sources as weak as a few millijanskys. This capability will be invaluable for observations of radio stars, X-ray sources and other weak, compact radio sources.

  11. Development of an S-band cavity Beam Position Monitor for ATF2

    NASA Astrophysics Data System (ADS)

    Heo, A.; Kim, E.-S.; Kim, H.; Son, D.; Honda, Y.; Tauchi, T.

    2013-04-01

    We have developed an S-band cavity Beam Position Monitor (BPM) in order to measure the position of an electron beam in the final focus area at ATF2, which is the test facility for the final focus design for the International Linear Collider (ILC). The lattice of the ILC Beam Delivery System (BDS) has been modified, requiring a larger physical aperture of 40 mm in the final focus area. The beam orbit measurement in this area is now covered with high resolution S-Band cavity BPMs. In this paper we summarize the design of the cavity BPM and the first experimental results. The calibration slopes were measured as 0.87 counts/μm in the x-coordinate direction and 1.16 counts/μm in the y-coordinate direction.

  12. Strong RFI observed in protected 21 cm band at Zurich observatory, Switzerland

    NASA Astrophysics Data System (ADS)

    Monstein, C.

    2014-03-01

    While testing a new antenna control software tool, the telescope was moved to the most western azimuth position pointing to our own building. While de-accelerating the telescope, the spectrometer showed strong broadband radio frequency interference (RFI) and two single-frequency carriers around 1412 and 1425 MHz, both of which are in the internationally protected band. After lengthy analysis it was found out, that the Webcam AXIS2000 was the source for both the broadband and single-frequency interference. Switching off the Webcam solved the problem immediately. So, for future observations of 21 cm radiation, all nearby electronics has to be switched off. Not only the Webcam but also all unused PCs, printers, networks, monitors etc.

  13. Estimating Coastal Turbidity using MODIS 250 m Band Observations

    NASA Technical Reports Server (NTRS)

    Davies, James E.; Moeller, Christopher C.; Gunshor, Mathew M.; Menzel, W. Paul; Walker, Nan D.

    2004-01-01

    Terra MODIS 250 m observations are being applied to a Suspended Sediment Concentration (SSC) algorithm that is under development for coastal case 2 waters where reflectance is dominated by sediment entrained in major fluvial outflows. An atmospheric correction based on MODIS observations in the 500 m resolution 1.6 and 2.1 micron bands is used to isolate the remote sensing reflectance in the MODIS 25Om resolution 650 and 865 nanometer bands. SSC estimates from remote sensing reflectance are based on accepted inherent optical properties of sediment types known to be prevalent in the U.S. Gulf of Mexico coastal zone. We present our findings for the Atchafalaya Bay region of the Louisiana Coast, in the form of processed imagery over the annual cycle. We also apply our algorithm to selected sites worldwide with a goal of extending the utility of our approach to the global direct broadcast community.

  14. Ka-band and X-band observations of the solar corona acquired during the Cassini 2001 superior conjunction

    NASA Technical Reports Server (NTRS)

    Morabito, D. D.

    2002-01-01

    Simultaneous dual-frequency Ka-band (32 GHz) and X-band (8.4 GHz) carrier signal data have been acquired during the superior conjunction of the Cassini spacecraft June 2001, using the NASA Deep Space Network's facilities located in Goldstone, California. The solar elongation angle of the observations varied from -4.1 degrees (-16 solar radii) to -0.6 degrees (-2.3 solar radii). The observed coronal and solar effects on the signals include spectral broadening, amplitude scintillation, phase scintillation, and increased noise. The measurements were generally consistent with existing solar models, except during solar transient events when the signatures of the measurements were observed to increase significantly above the quiet background levels. This is the second solar conjunction of Cassini for which simultaneous X/Ka data were acquired. Both solar conjunctions, conducted in May 2000 and June 2001, occurred near the peak of the current 11 year solar cycle.

  15. Challenges for continuity of L-Band observations over land

    USDA-ARS?s Scientific Manuscript database

    Over land, L-band observations are primarily used for the detection of soil freeze/thaw events and the quantification of surface soil moisture content. Both products have important science, climate and decision support applications and would benefit from longer historical data records derived from s...

  16. Excitation of O+ Band EMIC Waves Through H+ Ring Velocity Distributions: Van Allen Probe Observations

    NASA Astrophysics Data System (ADS)

    Yu, Xiongdong; Yuan, Zhigang; Huang, Shiyong; Yao, Fei; Wang, Dedong; Funsten, Herbert O.; Wygant, John R.

    2018-02-01

    A typical case of electromagnetic ion cyclotron (EMIC) emissions with both He+ band and O+ band waves was observed by Van Allen Probe A on 14 July 2014. These emissions occurred in the morning sector on the equator inside the plasmasphere, in which region O+ band EMIC waves prefer to appear. Through property analysis of these emissions, it is found that the He+ band EMIC waves are linearly polarized and propagating quasi-parallelly along the background magnetic field, while the O+ band ones are of linear and left-hand polarization and propagating obliquely with respect to the background magnetic field. Using the in situ observations of plasma environment and particle data, excitation of these O+ band EMIC waves has been investigated with the linear growth theory. The calculated linear growth rate shows that these O+ band EMIC waves can be locally excited by ring current protons with ring velocity distributions. The comparison of the observed wave spectral intensity and the calculated growth rate suggests that the density of H+ rings providing the free energy for the instability has decreased after the wave grows. Therefore, this paper provides a direct observational evidence to the excitation mechanism of O+ band EMIC waves: ring current protons with ring distributions provide the free energy supporting the instability in the presence of rich O+ in the plasmasphere.

  17. Near-midnight observations of nitric oxide delta- and gamma-band chemiluminescence

    NASA Technical Reports Server (NTRS)

    Tennyson, P. D.; Feldman, P. D.; Hartig, G. F.; Henry, R. C.

    1986-01-01

    Chemiluminescent nightglow emission of the nitric oxide delta and gamma bands was measured from a sounding rocket launched on April 27, 1981, near local midnight. The integrated band emission rates for this near zenith observation above 205 km were less than 10 Rayleighs. The solar zenith angle was 127 deg. The branching ratio from the C2Pi state to the A2Sigma(+) state of NO was determined from comparison of the total emission rate of the delta band system to that of the gamma band system and found to be 0.30 + or - 0.06. The branching ratios within each of the band systems were found to be consistent with previous theoretical and experimental determinations. The vertical atomic nitrogen distribution, derived with the use of a model atmosphere, was found to have a peak density of 2.0 x 10 to the 7th atoms/cu cm at an altitude of 205 km. The analysis of these data indicate the presence of residual NO emission above 270 km at local midnight on the order of 1 Rayleigh of total band emission.

  18. 1.65μm (H-band) surface photometry of galaxies. II. Observations of 297 galaxies with the TIRGO 1.5m telescope.

    NASA Astrophysics Data System (ADS)

    Gavazzi, G.; Pierini, D.; Baffa, C.; Lisi, F.; Hunt, L. K.; Randone, I.; Boselli, A.

    1996-12-01

    We present near-infrared H-band (1.65μm) surface photometry of 297 galaxies (mostly) in the Coma Supercluster obtained with the Arcetri NICMOS3 camera, ARNICA, mounted on the Gornergrat Infrared Telescope. Magnitudes and diameters within the 21.5mag/arcsec^2^ isophote, concentration indices, and total H magnitudes are derived. Combining these observations with those obtained similarly using the Calar Alto telescopes (Paper I, 1996A&AS..120..489G) we find a strong positive correlation between the near-infrared concentration index and the galaxy H-band luminosity, and we analyze the consequent dependence of near-infrared growth-curves on H-band luminosity.

  19. Ku/Ka band observations over polar ice sheets

    NASA Astrophysics Data System (ADS)

    Thibaut, Pierre; Lasne, Yannick; Guillot, Amandine; Picot, Nicolas; Rémy, Frédérique

    2015-04-01

    For the first time, comparisons between Ku and Ka altimeter measurements are possible thanks to the new AltiKa instrument embarked onboard the Saral mission launched on February 25, 2013. This comparison is of particular interest when dealing with ice sheet observations because both frequencies have different penetration characteristics. We propose in this paper to revisit the estimation of the ice sheet topography (and other related parameters) with altimeter systems and to present illustrations of the differences observed in Ku and Ka bands using AltiKa, Envisat/RA-2 but also Cryosat-2 measurements. Working on AltiKa waveforms in the frame of the PEACHI project has allowed us to better understand the impact of the penetration depth on the echo shape, to improve the estimation algorithm and to compare its output with historical results obtained on Envisat and ERS missions. In particular, analyses at cross-overs of the Cryosat-2 and Saral data will be presented. Sentinel-3 mission should be launch during 2015. Operating in Ku band and in delay/doppler mode, it will be crucial to account for penetration effects in order to accurately derive the ice sheet heights and trends. The results of the work presented here, will benefit to the Sentinel-3 mission.

  20. Strategies on solar observation of Atacama Large Millimeter/submillimeter Array (ALMA) band-1 receiver

    NASA Astrophysics Data System (ADS)

    Chiong, Chau-Ching; Chiang, Po-Han; Hwang, Yuh-Jing; Huang, Yau-De

    2016-07-01

    ALMA covering 35-950 GHz is the largest existing telescope array in the world. Among the 10 receiver bands, Band-1, which covers 35-50 GHz, is the lowest. Due to its small dimension and its time-variant frequency-dependent gain characteristics, current solar filter located above the cryostat cannot be applied to Band-1 for solar observation. Here we thus adopt new strategies to fulfill the goals. Thanks to the flexible dc biasing scheme of the HEMT-based amplifier in Band-1 front-end, bias adjustment of the cryogenic low noise amplifier is investigated to accomplish solar observation without using solar filter. Large power handling range can be achieved by the de-tuning bias technique with little degradation in system performance.

  1. Multi-band, multi-epoch observations of the transiting warm Jupiter WASP-80b

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Fukui, Akihiko; Kuroda, Daisuke; Kawashima, Yui

    WASP-80b is a warm Jupiter transiting a bright late-K/early-M dwarf, providing a good opportunity to extend the atmospheric study of hot Jupiters toward the lower temperature regime. We report multi-band, multi-epoch transit observations of WASP-80b by using three ground-based telescopes covering from optical (g', R{sub c}, and I{sub c} bands) to near-infrared (NIR; J, H, and K{sub s} bands) wavelengths. We observe 5 primary transits, each in 3 or 4 different bands simultaneously, obtaining 17 independent transit light curves. Combining them with results from previous works, we find that the observed transmission spectrum is largely consistent with both a solarmore » abundance and thick cloud atmospheric models at a 1.7σ discrepancy level. On the other hand, we find a marginal spectral rise in the optical region compared to the NIR region at the 2.9σ level, which possibly indicates the existence of haze in the atmosphere. We simulate theoretical transmission spectra for a solar abundance but hazy atmosphere, finding that a model with equilibrium temperature of 600 K can explain the observed data well, having a discrepancy level of 1.0σ. We also search for transit timing variations, but find no timing excess larger than 50 s from a linear ephemeris. In addition, we conduct 43 day long photometric monitoring of the host star in the optical bands, finding no significant variation in the stellar brightness. Combined with the fact that no spot-crossing event is observed in the five transits, our results confirm previous findings that the host star appears quiet for spot activities, despite the indications of strong chromospheric activities.« less

  2. Second-harmonic generation at angular incidence in a negative-positive index photonic band-gap structure.

    PubMed

    D'Aguanno, Giuseppe; Mattiucci, Nadia; Scalora, Michael; Bloemer, Mark J

    2006-08-01

    In the spectral region where the refractive index of the negative index material is approximately zero, at oblique incidence, the linear transmission of a finite structure composed of alternating layers of negative and positive index materials manifests the formation of a new type of band gap with exceptionally narrow band-edge resonances. In particular, for TM-polarized (transverse magnetic) incident waves, field values that can be achieved at the band edge may be much higher compared to field values achievable in standard photonic band-gap structures. We exploit the unique properties of these band-edge resonances for applications to nonlinear frequency conversion, second-harmonic generation, in particular. The simultaneous availability of high field localization and phase matching conditions may be exploited to achieve second-harmonic conversion efficiencies far better than those achievable in conventional photonic band-gap structures. Moreover, we study the role played by absorption within the negative index material, and find that the process remains efficient even for relatively high values of the absorption coefficient.

  3. Mini-RF S- and X-band Bistatic Observations of the Floor of Cabeus Crater

    NASA Astrophysics Data System (ADS)

    Patterson, Gerald Wesley; Stickle, Angela; Turner, Franklin; Jensen, James; Cahill, Joshua; Mini-RF Team

    2017-10-01

    The Mini-RF instrument aboard NASA’s Lunar Reconnaissance Orbiter (LRO) is a hybrid dual-polarized synthetic aperture radar (SAR) and operates in concert with the Arecibo Observatory (AO) and the Goldstone deep space communications complex 34 meter antenna DSS-13 to collect S- and X-band bistatic radar data of the Moon. Bistatic radar data provide a means to probe the near subsurface for the presence of water ice, which exhibits a strong response in the form of a Coherent Backscatter Opposition Effect (CBOE). This effect has been observed in radar data for the icy surfaces of the Galilean satellites, the polar caps of Mars, polar craters on Mercury, and terrestrial ice sheets in Greenland. Previous work using Mini-RF S-band (12.6 cm) bistatic data suggests the presence of a CBOE associated with the floor of the lunar south polar crater Cabeus. The LRO spacecraft has begun its third extended mission. For this phase of operations Mini-RF is leveraging the existing AO architecture to make S-band radar observations of additional polar craters (e.g., Haworth, Shoemaker, Faustini). The purpose of acquiring these data is to determine whether other polar craters exhibit the response observed for Cabeus. Mini-RF has also initiated a new mode of operation that utilizes the X-band (4.2cm) capability of the instrument receiver and a recently commissioned X/C-band transmitter within the Deep Space Network’s (DSN) Goldstone complex to collect bistatic X-band data of the Moon. The purpose of acquiring these data is to constrain the depth/thickness of materials that exhibit a CBOE response - with an emphasis on observing the floor of Cabeus. Recent Mini-RF X-band observations of the floors of the craters Cabeus do not show evidence for a CBOE. This would suggest that the upper ~0.5 meters of the regolith for the floor of Cabeus do not harber water ice in a form detectable at 4.2 cm wavelengths.

  4. Calibration of VIIRS F1 Sensor Fire Detection Band Using lunar Observations

    NASA Technical Reports Server (NTRS)

    McIntire, Jeff; Efremova, Boryana; Xiong, Xiaoxiong

    2012-01-01

    Visible Infrared Imager Radiometer Suite (VIIRS) Fight 1 (Fl) sensor includes a fire detection band at roughly 4 microns. This spectral band has two gain states; fire detection occurs in the low gain state above approximately 345 K. The thermal bands normally utilize an on-board blackbody to provide on-orbit calibration. However, as the maximum temperature of this blackbody is 315 K, the low gain state of the 4 micron band cannot be calibrated in the same manner as the rest of the thermal bands. Regular observations of the moon provide an alternative calibration source. The lunar surface temperature has been recently mapped by the DIVINER sensor on the LRO platform. The periodic on-board high gain calibration along with the DIVINER surface temperatures was used to determine the emissivity and solar reflectance of the lunar surface at 4 microns; these factors and the lunar data are then used to fit the low gain calibration coefficients of the 4 micron band. Furthermore, the emissivity of the lunar surface is well known near 8.5 microns due to the Christiansen feature (an emissivity maximum associated with Si-O stretching vibrations) and the solar reflectance is negligible. Thus, the 8.5 micron band is used for relative calibration with the 4 micron band to de-trend any temporal variations. In addition, the remaining thermal bands are analyzed in a similar fashion, with both calculated emissivities and solar reflectances produced.

  5. Effects of surface condition on the work function and valence-band position of ZnSnN2

    NASA Astrophysics Data System (ADS)

    Shing, Amanda M.; Tolstova, Yulia; Lewis, Nathan S.; Atwater, Harry A.

    2017-12-01

    ZnSnN2 is an emerging wide band gap earth-abundant semiconductor with potential applications in photonic devices such as solar cells, LEDs, and optical sensors. We report the characterization by ultraviolet photoelectron spectroscopy and X-ray photoelectron spectroscopy of reactively radio-frequency sputtered II-IV-nitride ZnSnN2 thin films. For samples transferred in high vacuum, the ZnSnN2 surface work function was 4.0 ± 0.1 eV below the vacuum level, with a valence-band onset of 1.2 ± 0.1 eV below the Fermi level. The resulting band diagram indicates that the degenerate bulk Fermi level position in ZnSnN2 shifts to mid-gap at the surface due to band bending that results from equilibration with delocalized surface states within the gap. Brief (< 10 s) exposures to air, a nitrogen-plasma treatment, or argon-ion sputtering caused significant chemical changes at the surface, both in surface composition and interfacial energetics. The relative band positioning of the n-type semiconductor against standard redox potentials indicated that ZnSnN2 has an appropriate energy band alignment for use as a photoanode to effect the oxygen-evolution reaction.

  6. X/X/Ka-band prime focus feed antenna for the Mars Observer beacon spacecraft

    NASA Technical Reports Server (NTRS)

    Stanton, P.; Reilly, H.; Esquivel, M.

    1988-01-01

    The results of an X/X/Ka-band feed design concept demonstration are presented. The purpose is to show the feasibility of adding a Ka-band beacon to the Mars Observer spacecraft. Scale model radiation patterns were made and analyzed.

  7. Combined observations of Arctic sea ice with near-coincident colocated X-band, C-band, and L-band SAR satellite remote sensing and helicopter-borne measurements

    NASA Astrophysics Data System (ADS)

    Johansson, A. M.; King, J. A.; Doulgeris, A. P.; Gerland, S.; Singha, S.; Spreen, G.; Busche, T.

    2017-01-01

    In this study, we compare colocated near-coincident X-, C-, and L-band fully polarimetry SAR satellite images with helicopter-borne ice thickness measurements acquired during the Norwegian Young sea ICE 2015 (N-ICE2015) expedition in the region of the Arctic Ocean north of Svalbard in April 2015. The air-borne surveys provide near-coincident snow plus ice thickness, surface roughness data, and photographs. This unique data set allows us to investigate how the different frequencies can complement one another for sea ice studies, but also to raise awareness of limitations. X-band and L-band satellite scenes were shown to be a useful complement to the standard SAR frequency for sea ice monitoring (C-band) for lead ice and newly formed sea ice identification. This may be in part be due to the frequency but also the high spatial resolution of these sensors. We found a relatively low correlation between snow plus ice thickness and surface roughness. Therefore, in our dataset ice thickness cannot directly be observed by SAR which has important implications for operational ice charting based on automatic segmentation.

  8. Evaluation of Detector-to-Detector and Mirror Side Differences for Terra MODIS Reflective Solar Bands Using Simultaneous MISR Observations

    NASA Technical Reports Server (NTRS)

    Wu, Aisheng; Xiong, Xiaoxiong; Angal, A.; Barnes, W.

    2011-01-01

    The Moderate Resolution Imaging Spectroradiometer (MODIS) is one of the five Earth-observing instruments on-board the National Aeronautics and Space Administration (NASA) Earth-Observing System(EOS) Terra spacecraft, launched in December 1999. It has 36 spectral bands with wavelengths ranging from 0.41 to 14.4 mm and collects data at three nadir spatial resolutions: 0.25 km for 2 bands with 40 detectors each, 0.5 km for 5 bands with 20 detectors each and 1 km for the remaining 29 bands with 10 detectors each. MODIS bands are located on four separate focal plane assemblies (FPAs) according to their spectral wavelengths and aligned in the cross-track direction. Detectors of each spectral band are aligned in the along-track direction. MODIS makes observations using a two-sided paddle-wheel scan mirror. Its on-board calibrators (OBCs) for the reflective solar bands (RSBs) include a solar diffuser (SD), a solar diffuser stability monitor (SDSM) and a spectral-radiometric calibration assembly (SRCA). Calibration is performed for each band, detector, sub-sample (for sub-kilometer resolution bands) and mirror side. In this study, a ratio approach is applied to MODIS observed Earth scene reflectances to track the detector-to-detector and mirror side differences. Simultaneous observed reflectances from the Multi-angle Imaging Spectroradiometer (MISR), also onboard the Terra spacecraft, are used with MODIS observed reflectances in this ratio approach for four closely matched spectral bands. Results show that the detector-to-detector difference between two adjacent detectors within each spectral band is typically less than 0.2% and, depending on the wavelengths, the maximum difference among all detectors varies from 0.5% to 0.8%. The mirror side differences are found to be very small for all bands except for band 3 at 0.44 mm. This is the band with the shortest wavelength among the selected matching bands, showing a time-dependent increase for the mirror side difference. This

  9. Examples L-Band Interference will be Presented and Discussed, as well as the Importance of L-Band Soil Moisture Observations

    NASA Technical Reports Server (NTRS)

    Kim, Edward

    2010-01-01

    Examples of L-band interference will be presented and discussed, as well as the importance of L-band soil moisture observations, as part of this one-day GEOSS workshop XXXVII on "Data Quality and Radio Spectrum Allocation Impact on Earth Observations" will address the broad challenges of data quality and the impact of generating reliable information for decision makers who are Earth data users but not necessarily experts in the Earth observation field. GEO has initiated a data quality assessment task (DA-09-01a) and workshop users will review and debate the directions and challenges of this effort. Radio spectrum allocation is an element of data availability and data quality, and is also associated with a GEO task (AR-06-11). A recent U.S. National Research Council report on spectrum management will be addressed as part of the workshop. Key representatives from industry, academia, and government will provide invited talks on these and related issues that impact GEOSS implementation.

  10. Experimental observations of shear band nucleation and propagation in a bulk metallic glass using wedge-like cylindrical indentation

    NASA Astrophysics Data System (ADS)

    Antoniou, Antonia Maki

    2006-12-01

    process zone front and presents an included angle of 78°-80°. The other set of bands evolves at a later stage of loading within the originally formed ones but with consistently higher included angle of around 87°. The band spacing is found to scale with the local average of maximum in-plane shear strain such that the local strain energy is minimized. The measurements shed light on the critical shear strain needed to initiate these bands. The richness of the shear band network establishes a basis for calibration of constitutive models. Experimental in-plane deformation maps show the amount of total strain that builds prior to the initiation of localized deformation. Furthermore, the maps help examine the change imposed on the surrounding strain field by the appearance of shear bands. It was verified that shear bands relax the asymptotic field by changing the order of singularity. Finally, it was seen that the shear bands are not the only accumulation of permanent deformation but that the surrounding material can accrue relatively high level of inelastic deformation (up to 5%). To rationalize these findings, the Johnson cavity expansion model is adapted and modified to account for pressure-dependent yielding conditions. The elasto-plastic boundary from such analysis is used to scale the experimental measurements for all indenter radii, loading level and spatial position beneath the indenter. The continuum finite element simulations have shown that the macroscopic measurements of force-depth indentation curves would predict a lower value of the pressure sensitivity than those observed from the detailed microscopic measurements. Moreover, a transition from pressure insensitive response to progressive pressure sensitivity is observed by decreasing the indenter radius, or in effect by increasing the level of hydrostatic pressure under the indenter. This leads to the belief that the BMG's pressure sensitivity parameter is in itself dependent on the level of the applied

  11. Diffuse Interstellar Bands. A Survey of Observational Facts

    NASA Astrophysics Data System (ADS)

    Krełowski, J.

    2018-07-01

    The paper presents and documents the most important observational results concerning the enigmatic diffuse interstellar bands (DIBs) that have remained unidentified since 1922. It demonstrates why the bands are commonly considered as having originated in many still unknown carriers. The mutual correlations of different DIBs, aiming at finding “families” of common origin, are briefly discussed. It was found that the strength ratio of the major DIBs, 5780 and 5797, is heavily variable; at the same E(B‑V), the DIB intensities may vary by as much as a factor of three or more. Certain DIB strength ratios seem to be related to intensities of the known features of simple molecular species; this led to the introduction of the so-called σ and ζ type interstellar clouds. In the former (prototype HD147165), broad DIBs are very strong, while the narrow ones and molecular features are weak. In the latter (prototype HD149757), narrow DIBs, as well as bands of simple radicals, are strong while the broad DIBs are weak (in relation to E(B‑V)). Details of the profiles of narrow DIBs, documenting their molecular origin, are presented. The relative DIB strengths as well as those of the simple radicals seem to be related to the shapes of interstellar extinction curves. Possible carriers of DIBs are only mentioned, as all of the proposed ones remain uncertain. The survey is biased in the sense that it presents the author’s point of view. It was prepared for the thirtieth anniversary of the first DIB survey, published in PASP (Krełowski 1988), and demonstrates how far our knowledge has evolved since then.

  12. Direct observation of strain-induced orbital valence band splitting in HfSe2 by sodium intercalation

    NASA Astrophysics Data System (ADS)

    Eknapakul, T.; Fongkaew, I.; Siriroj, S.; Jindata, W.; Chaiyachad, S.; Mo, S.-K.; Thakur, S.; Petaccia, L.; Takagi, H.; Limpijumnong, S.; Meevasana, W.

    2018-05-01

    By using angle-resolved photoemission spectroscopy (ARPES), the variation of the electronic structure of HfSe2 has been studied as a function of sodium intercalation. We observe how this drives a band splitting of the p -orbital valence bands and a simultaneous reduction of the indirect band gap by values of up to 400 and 280 meV, respectively. Our calculations indicate that such behavior is driven by the band deformation potential, which is a result of our observed strain induced by sodium intercalation. The applied uniaxial strain calculations based on density functional theory agree strongly with the experimental ARPES data. These findings should assist in studying the physical relationship between intercalation and strain, as well as for large-scale two-dimensional straintronics.

  13. Modelling Ground Based X- and Ku-Band Observations of Tundra Snow

    NASA Astrophysics Data System (ADS)

    Kasurak, A.; King, J. M.; Kelly, R. E.

    2012-12-01

    As part of a radar-based remote sensing field experiment in Churchill, Manitoba ground based Ku- and X-band scatterometers were deployed to observe changing tundra snowpack conditions from November 2010 to March 2011. The research is part of the validation effort for the Cold Regions Hydrology High-resolution Observatory (CoReH2O) mission, a candidate in the European Space Agency's Earth Explorer program. This paper focuses on the local validation of the semi-empirical radiative transfer (sRT) model proposed for use in snow property retrievals as part of the CoReH2O mission. In this validation experiment, sRT was executed in the forward mode, simulating backscatter to assess the ability of the model. This is a necessary precursor to any inversion attempt. Two experiments are considered, both conducted in a hummocky tundra environment with shallow snow cover. In both cases, scatterometer observations were acquired over a field of view of approximately 10 by 20 meters. In the first experiment, radar observations were made of a snow field and then repeated after the snow had been removed. A ground-based scanning LiDAR system was used to characterize the spatial variability of snow depth through measurements of the snow and ground surface. Snow properties were determined in the field of view from two snow pits, 12 density core measurements, and Magnaprobe snow depth measurements. In the second experiment, a site was non-destructively observed from November through March, with snow properties measured out-of-scene, to characterize the snow evolution response. The model results from sRT fit the form of the observations from the two scatterometer field experiments but do not capture the backscatter magnitude. A constant offset for the season of 5 dB for X-band co- and cross-polarization response was required to match observations, in addition to a 3 dB X- and Ku-band co-polarization offset after the 6th of December. To explain these offsets, it is recognized that the two

  14. Observation of high-spin bands with large moments of inertia in Xe 124

    DOE PAGES

    Nag, Somnath; Singh, A. K.; Hagemann, G. B.; ...

    2016-09-07

    In this paper, high-spin states in 124Xe have been populated using the 80Se( 48Ca, 4n) reaction at a beam energy of 207 MeV and high-multiplicity, γ-ray coincidence events were measured using the Gammasphere spectrometer. Six high-spin rotational bands with moments of inertia similar to those observed in neighboring nuclei have been observed. The experimental results are compared with calculations within the framework of the Cranked Nilsson-Strutinsky model. Finally, it is suggested that the configurations of the bands involve excitations of protons across the Z = 50 shell gap coupled to neutrons within the N = 50 - 82 shell ormore » excited across the N = 82 shell closure.« less

  15. Ka Band Objects: Observation and Monitoring (KaBOOM)

    NASA Astrophysics Data System (ADS)

    Geldzahler, B.

    2012-09-01

    NASA has embarked on a path that will enable the implementation of a high power, high resolution X/Ka band radar system using widely spaced 12m antennas to better track and characterize near Earth objects and orbital debris. This radar system also has applications for cost effective space situational awareness. We shall demonstrate Ka band coherent uplink arraying with real-time atmospheric compensation using three 12m antennas at the Kennedy Space Center (KSC). Our proposed radar system can complement and supplement the activities of the Space Fence. The proposed radar array has the advantages of filling the gap between dusk and dawn and offers the possibility of high range resolution (4 cm) and high spatial resolution (?10 cm at GEO) when used in a VLBI mode. KSC was chosen because [a] of reduced implementation costs, [b] there is a lot of water vapor in the air (not Ka band friendly), and [c] the test satellites have a low elevation adding more attenuation and turbulence to the demonstration. If Ka band coherent uplink arraying can be made to work at KSC, it will work anywhere. We expect to rebaseline X-band in 2013, and demonstrate Ka band uplink arraying in 2014.

  16. Examining Scattering Mechanisms within Bubbled Freshwater Lake Ice using a Time-Series of RADARSAT-2 (C-band) and UW-Scat (X-, Ku-band) Polarimetric Observations

    NASA Astrophysics Data System (ADS)

    Gunn, Grant; Duguay, Claude; Atwood, Don

    2017-04-01

    This study identifies the dominant scattering mechanism for C-, X- and Ku-band for bubbled freshwater lake ice in the Hudson Bay Lowlands near Churchill, Canada, using a winter time series of fully polarimetric ground-based (X- and Ku-band, UW-Scat) scatterometer and spaceborne (C-band) synthetic aperture radar (SAR, Radarsat-2) observations collected coincidentally to in-situ snow and ice measurements. Scatterometer observations identify two dominant backscatter sources from the ice cover: the snow-ice, and ice-water interface. Using in-situ measurements as ground-truth, a winter time series of scatterometer and satellite acquisitions show increases in backscatter from the ice-water interface prior to the timing of tubular bubble development in the ice cover. This timing indicates that scattering in the ice is independent of double-bounce scatter caused by tubular bubble inclusions. Concurrently, the co-polarized phase difference of interactions at the ice-water interface from both scatterometer and SAR observations are centred at 0° throughout the time series, indicating a scattering regime other than double bounce. A Yamaguchi three-component decomposition of SAR observations is presented for C-band acquisitions indicating a dominant single-bounce scattering mechanism regime, which is hypothesized to be a result of an ice-water interface that presents a rough surface or a surface composed of preferentially oriented facets. This study is the first to present a winter time series of coincident ground-based and spaceborne fully polarimetric active microwave observations for bubbled freshwater lake ice.

  17. Use of abnormal preprophase bands to decipher division plane determination

    NASA Technical Reports Server (NTRS)

    Granger, C.; Cyr, R.

    2001-01-01

    Many premitotic plant cells possess a cortical preprophase band of microtubules and actin filaments that encircles the nucleus. In vacuolated cells, the preprophase band is visibly connected to the nucleus by a cytoplasmic raft of actin filaments and microtubules termed the phragmosome. Typically, the location of the preprophase band and phragmosome corresponds to, and thus is thought to influence, the location of the cell division plane. To better understand the function of the preprophase band and phragmosome in orienting division, we used a green fluorescent protein-based microtubule reporter protein to observe mitosis in living tobacco bright yellow 2 cells possessing unusual preprophase bands. Observations of mitosis in these unusual cells support the involvement of the preprophase band/phragmosome in properly positioning the preprophase nucleus, influencing spindle orientation such that the cytokinetic phragmoplast initially grows in an appropriate direction, and delineating a region in the cell cortex that attracts microtubules and directs later stages of phragmoplast growth. Thus, the preprophase band/phragmosome appears to perform several interrelated functions to orient the division plane. However, functional information associated with the preprophase band is not always used or needed and there appears to be an age or distance-dependent character to the information. Cells treated with the anti-actin drug, latrunculin B, are still able to position the preprophase nucleus suggesting that microtubules may play a dominant role in premitotic positioning. Furthermore, in treated cells, spindle location and phragmoplast insertion are frequently abnormal suggesting that actin plays a significant role in nuclear anchoring and phragmoplast guidance. Thus, the microtubule and actin components of the preprophase band/phragmosome execute complementary activities to ensure proper orientation of the division plane.

  18. Double Bright Band Observations with High-Resolution Vertically Pointing Radar, Lidar, and Profiles

    NASA Technical Reports Server (NTRS)

    Emory, Amber E.; Demoz, Belay; Vermeesch, Kevin; Hicks, Michael

    2014-01-01

    On 11 May 2010, an elevated temperature inversion associated with an approaching warm front produced two melting layers simultaneously, which resulted in two distinct bright bands as viewed from the ER-2 Doppler radar system, a vertically pointing, coherent X band radar located in Greenbelt, MD. Due to the high temporal resolution of this radar system, an increase in altitude of the melting layer of approximately 1.2 km in the time span of 4 min was captured. The double bright band feature remained evident for approximately 17 min, until the lower atmosphere warmed enough to dissipate the lower melting layer. This case shows the relatively rapid evolution of freezing levels in response to an advancing warm front over a 2 h time period and the descent of an elevated warm air mass with time. Although observations of double bright bands are somewhat rare, the ability to identify this phenomenon is important for rainfall estimation from spaceborne sensors because algorithms employing the restriction of a radar bright band to a constant height, especially when sampling across frontal systems, will limit the ability to accurately estimate rainfall.

  19. Double bright band observations with high-resolution vertically pointing radar, lidar, and profilers

    NASA Astrophysics Data System (ADS)

    Emory, Amber E.; Demoz, Belay; Vermeesch, Kevin; Hicks, Micheal

    2014-07-01

    On 11 May 2010, an elevated temperature inversion associated with an approaching warm front produced two melting layers simultaneously, which resulted in two distinct bright bands as viewed from the ER-2 Doppler radar system, a vertically pointing, coherent X band radar located in Greenbelt, MD. Due to the high temporal resolution of this radar system, an increase in altitude of the melting layer of approximately 1.2 km in the time span of 4 min was captured. The double bright band feature remained evident for approximately 17 min, until the lower atmosphere warmed enough to dissipate the lower melting layer. This case shows the relatively rapid evolution of freezing levels in response to an advancing warm front over a 2 h time period and the descent of an elevated warm air mass with time. Although observations of double bright bands are somewhat rare, the ability to identify this phenomenon is important for rainfall estimation from spaceborne sensors because algorithms employing the restriction of a radar bright band to a constant height, especially when sampling across frontal systems, will limit the ability to accurately estimate rainfall.

  20. Reduction of EAO Positional Observations Database

    NASA Astrophysics Data System (ADS)

    Nefedyev, Yuri; Andreev, Alexey; Demina, Natalya; Churkin, Konstantin

    2016-07-01

    There is a large data bank of positional observations of Solar System bodies at Engelhadt Astronomical Observatory (EAO). The positional observations include the major planets, except Jupiter. Modern technologies replace classical methods of observations in astronomy and in astrometry as well. At the same time many positional observations have been gathered at astronomical observatories. So taking into account that observations of the past epochs have presenteda great value for astronomy and as times goes by their importance is growing it is obvious that positional astrometry will not lose its practical importance. This was noted in B3 XXIV IAU resolution by the General Assembly. The results of reduction of solar system bodies observations were published mainly in Proceeding of EAO and Transactions of Kazan City Astronomical Observatory. Earlier there have been made about three thousand observations at EAO and Zelenchuk station with the Zeiss telescope (D=400mm, f=2000mm), AFR-18 (photo visual, D=200, f=2000), refractor (D=400mm, f=3450mm), Meniscus camera (D=340mm, f=1200mm), Schmidt camera (D=350mm, f=2000mm). The major planets except Pluto and Neptune were observed with a special cassette chamber equipped with a rotating disk which had an open sector to reduce the brightness of the planets. The dimension of the sector was chosen accordingto the brightness of the planets. The disk was placed in the centre of the astrograph's field. The stars' true brightness was preserved. A large number of catalogues were compiled by the end of the 20th century. We used Tycho-2 catalogue for reducing our observations. As it is known the catalogue Tycho-2 (Tycho-2 catalogue, 2000) includes 2539913 stars. The stars' proper motions given in the catalogue were obtained by comparing positions from Tycho-2 with positions from the Astrographic Catalogue. Therefore they are considered to be highly accurate. The accuracy of stellar positions in Tycho-2 is about 60 mas and the accuracy of

  1. Observations of Multi-band Structures in Double Star TC-1 PEACE Electron and HIA Ion Data

    NASA Astrophysics Data System (ADS)

    Mohan Narasimhan, K.; Fazakerley, A. N.; Grimald, S.; Dandouras, I. S.; Mihaljcic, B.; Kistler, L. M.; Owen, C. J.

    2015-12-01

    Several authors have reported inner magnetosphere observations of proton distributions confined to narrow energy bands in the range 1 - 25 keV (Smith and Hoffman (1974), etc). These structures have been described as "nose structures", with reference to their appearance in energy-time spectrograms and are also known as "bands" if they occur for extended periods of time. Multi-nose structures have been observed if 2 or more noses appear at the same time (Vallat et al., 2007). Gaps between "noses" (or "bands") have been explained in terms of the competing corotation, convection and magnetic gradient drifts. Charge exchange losses in slow drift paths for steady state scenarios and the role of substorm injections have also been considered (Li et al., 2000; Ebihara et al., 2004). We analyse observations of electron and ion multi-band structures frequently seen in Double-Star TC1 PEACE and HIA data. We present results from statistical surveys conducted using data from the duration of the mission. Furthermore, using a combination of both statistics and simulations, we test previous theories as to possible formation mechanisms and explore other possible explanations.

  2. The hierarchically organized splitting of chromosome bands into sub-bands analyzed by multicolor banding (MCB).

    PubMed

    Lehrer, H; Weise, A; Michel, S; Starke, H; Mrasek, K; Heller, A; Kuechler, A; Claussen, U; Liehr, T

    2004-01-01

    To clarify the nature of chromosome sub-bands in more detail, the multicolor banding (MCB) probe-set for chromosome 5 was hybridized to normal metaphase spreads of GTG band levels at approximately 850, approximately 550, approximately 400 and approximately 300. It could be observed that as the chromosomes became shorter, more of the initial 39 MCB pseudo-colors disappeared, ending with 18 MCB pseudo-colored bands at the approximately 300-band level. The hierarchically organized splitting of bands into sub-bands was analyzed by comparing the disappearance or appearance of pseudo-color bands of the four different band levels. The regions to split first are telomere-near, centromere-near and in 5q23-->q31, followed by 5p15, 5p14, and all GTG dark bands in 5q apart from 5q12 and 5q32 and finalized by sub-band building in 5p15.2, 5q21.2-->q21.3, 5q23.1 and 5q34. The direction of band splitting towards the centromere or the telomere could be assigned to each band separately. Pseudo-colors assigned to GTG-light bands were resistant to band splitting. These observations are in concordance with the recently proposed concept of chromosome region-specific protein swelling. Copyright 2003 S. Karger AG, Basel

  3. Post-seismic relaxation following the 2009 April 6, L'Aquila (Italy), earthquake revealed by the mass position of a broad-band seismometer

    NASA Astrophysics Data System (ADS)

    Pino, Nicola Alessandro

    2012-06-01

    Post-seismic relaxation is known to occur after large or moderate earthquakes, on time scales ranging from days to years or even decades. In general, long-term deformation following seismic events has been detected by means of standard geodetic measurements, although seismic instruments are only used to estimate short timescale transient processes. Albeit inertial seismic sensors are also sensitive to rotation around their sensitive axes, the recording of very slow inclination of the ground surface at their standard output channels is practically impossible, because of their design characteristics. However, modern force-balance, broad-band seismometers provide the possibility to detect and measure slow surface inclination, through the analysis of the mass position signal. This output channel represents the integral of the broad-band velocity and is generally considered only for state-of-health diagnostics. In fact, the analysis of mass position data recorded at the time of the 2009 April 6, L'Aquila (MW= 6.3) earthquake, by a closely located STS-2 seismometer, evidenced the occurrence of a very low frequency signal, starting right at the time of the seismic event. This waveform is only visible on the horizontal components and is not related to the usual drift coupled with the temperature changes. This analysis suggests that the observed signal is to be ascribed to slowly developing ground inclination at the station site, caused by post-seismic relaxation following the main shock. The observed tilt reached 1.7 × 10-5 rad in about 2 months. This estimate is in very good agreement with the geodetic observations, giving comparable tilt magnitude and direction at the same site. This study represents the first seismic analysis ever for the mass position signal, suggesting useful applications for usually neglected data.

  4. CONSTRAINING THE SOLAR CORONAL MAGNETIC FIELD STRENGTH USING SPLIT-BAND TYPE II RADIO BURST OBSERVATIONS

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Kishore, P.; Ramesh, R.; Hariharan, K.

    2016-11-20

    We report on low-frequency radio (85–35 MHz) spectral observations of four different type II radio bursts, which exhibited fundamental-harmonic emission and split-band structure. Each of the bursts was found to be closely associated with a whitelight coronal mass ejection (CME) close to the Sun. We estimated the coronal magnetic field strength from the split-band characteristics of the bursts, by assuming a model for the coronal electron density distribution. The choice of the model was constrained, based on the following criteria: (1) when the radio burst is observed simultaneously in the upper and lower bands of the fundamental component, the locationmore » of the plasma level corresponding to the frequency of the burst in the lower band should be consistent with the deprojected location of the leading edge (LE) of the associated CME; (2) the drift speed of the type II bursts derived from such a model should agree closely with the deprojected speed of the LE of the corresponding CMEs. With the above conditions, we find that: (1) the estimated field strengths are unique to each type II burst, and (2) the radial variation of the field strength in the different events indicate a pattern. It is steepest for the case where the heliocentric distance range over which the associated burst is observed is closest to the Sun, and vice versa.« less

  5. Monitoring deformation at the Geysers Geothermal Field, California using C-band and X-band interferometric synthetic aperture radar

    DOE PAGES

    Vasco, D. W.; Rutqvist, Jonny; Ferretti, Alessandro; ...

    2013-06-07

    In this study, we resolve deformation at The Geysers Geothermal Field using two distinct sets of interferometric synthetic aperture radar (InSAR) data. The first set of observations utilize archived European Space Agency C-band synthetic aperture radar data from 1992 through 1999 to image the long-term and large-scale subsidence at The Geysers. The peak range velocity of approximately 50 mm/year agrees with previous estimates from leveling and global positioning system observations. Data from a second set of measurements, acquired by TerraSAR-X satellites, extend from May 2011 until April 2012 and overlap the C-band data spatially but not temporally. These X-band data,more » analyzed using a combined permanent and distributed scatterer algorithm, provide a higher density of scatterers (1122 per square kilometer) than do the C-band data (12 per square kilometer). The TerraSAR-X observations resolve 1 to 2 cm of deformation due to water injection into a Northwest Geysers enhanced geothermal system well, initiated on October 2011. Lastly, the temporal variation of the deformation is compatible with estimates from coupled numerical modeling.« less

  6. 1.65 μm (H-band) surface photometry of galaxies. III. observations of 558 galaxies with the TIRGO 1.5 m telescope

    NASA Astrophysics Data System (ADS)

    Gavazzi, G.; Franzetti, P.; Scodeggio, M.; Boselli, A.; Pierini, D.; Baffa, C.; Lisi, F.; Hunt, L. K.

    2000-02-01

    We present near-infrared H-band (1.65 μm ) surface photometry of 558 galaxies in the Coma Supercluster and in the Virgo cluster. This data set, obtained with the Arcetri NICMOS3 camera ARNICA mounted on the Gornergrat Infrared Telescope, is aimed at complementing, with observations of mostly early-type objects, our NIR survey of spiral galaxies in these regions, presented in previous papers of this series. Magnitudes at the optical radius, total magnitudes, isophotal radii and light concentration indices are derived. We confirm the existence of a positive correlation between the near-infrared concentration index and the galaxy H-band luminosity Based on observations taken at TIRGO (Gornergrat, Switzerland). TIRGO is operated by CAISMI-CNR, Arcetri, Firenze, Italy. Tables 1 and 2 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html

  7. Inter-comparison of SMAP, Aquarius and SMOS L-band brightness temperature observations

    USDA-ARS?s Scientific Manuscript database

    Soil Moisture Active Passive (SMAP) mission is scheduled for launch on January 29, 2015. SMAP will make observations with an L-band radar and radiometer using a shared 6 m rotating reflector antenna. SMAP is a fully polarimetric radiometer with the center frequency of 1.41 GHz. The target accuracy o...

  8. The occurrence and wave properties of H+-, He+-, and O+-band EMIC waves observed by the Van Allen Probes

    NASA Astrophysics Data System (ADS)

    Saikin, A. A.; Zhang, J.-C.; Allen, R. C.; Smith, C. W.; Kistler, L. M.; Spence, H. E.; Torbert, R. B.; Kletzing, C. A.; Jordanova, V. K.

    2015-09-01

    We perform a statistical study of electromagnetic ion cyclotron (EMIC) waves detected by the Van Allen Probes mission to investigate the spatial distribution of their occurrence, wave power, ellipticity, and normal angle. The Van Allen Probes have been used which allow us to explore the inner magnetosphere (1.1 to 5.8 RE). Magnetic field measurements from the Electric and Magnetic Field Instrument Suite and Integrated Science on board the Van Allen Probes are used to identify EMIC wave events for the first 22 months of the mission operation (8 September 2012 to 30 June 2014). EMIC waves are examined in H+, He+, and O+ bands. Over 700 EMIC wave events have been identified over the three different wave bands (265 H+-band events, 438 He+-band events, and 68 O+-band events). EMIC wave events are observed between L = 2-8, with over 140 EMIC wave events observed below L = 4. Results show that H+-band EMIC waves have two peak magnetic local time (MLT) occurrence regions: prenoon (09:00 < MLT ≤ 12:00) and afternoon (15:00 < MLT ≤ 17:00) sectors. He+-band EMIC waves feature an overall stronger dayside occurrence. O+-band EMIC waves have one peak region located in the morning sector at lower L shells (L < 4). He+-band EMIC waves average the highest wave power overall (>0.1 nT2/Hz), especially in the afternoon sector. Ellipticity observations reveal that linearly polarized EMIC waves dominate in lower L shells.

  9. W-band spaceborne radar observations of atmospheric river events

    NASA Astrophysics Data System (ADS)

    Matrosov, S. Y.

    2010-12-01

    While the main objective of the world first W-band radar aboard the CloudSat satellite is to provide vertically resolved information on clouds, it proved to be a valuable tool for observing precipitation. The CloudSat radar is generally able to resolve precipitating cloud systems in their vertical entirety. Although measurements from the liquid hydrometer layer containing rainfall are strongly attenuated, special retrieval approaches can be used to estimate rainfall parameters. These approaches are based on vertical gradients of observed radar reflectivity factor rather than on absolute estimates of reflectivity. Concurrent independent estimations of ice cloud parameters in the same vertical column allow characterization of precipitating systems and provide information on coupling between clouds and rainfall they produce. The potential of CloudSat for observations atmospheric river events affecting the West Coast of North America is evaluated. It is shown that spaceborne radar measurements can provide high resolution information on the height of the freezing level thus separating areas of rainfall and snowfall. CloudSat precipitation rate estimates complement information from the surface-based radars. Observations of atmospheric rivers at different locations above the ocean and during landfall help to understand evolutions of atmospheric rivers and their structures.

  10. Orbiter global positioning system design and Ku-band problems investigation, exhibit B, revision 1

    NASA Technical Reports Server (NTRS)

    Chie, C. M.; Braun, W. R.

    1981-01-01

    The LinCom effort in supporting the JSC study of the use of the Global Positioning System (GPS) on the space shuttle and in Ku-band problem investigation is documented. LinCom was tasked to evaluate system implementation, performance, and integration aspects of the shuttle GPS and to provide independent technical assessment of reports submitted to JSC regarding integration studies, system studies and navigation analyses.

  11. Direct observation of a surface resonance state and surface band inversion control in black phosphorus

    NASA Astrophysics Data System (ADS)

    Ehlen, N.; Sanna, A.; Senkovskiy, B. V.; Petaccia, L.; Fedorov, A. V.; Profeta, G.; Grüneis, A.

    2018-01-01

    We report a Cs-doping-induced band inversion and the direct observation of a surface resonance state with an elliptical Fermi surface in black phosphorus (BP) using angle-resolved photoemission spectroscopy. By selectively inducing a higher electron concentration (1.7 ×1014cm-2 ) in the topmost layer, the changes in the Coulomb potential are sufficiently large to cause surface band inversion between the parabolic valence band of BP and a parabolic surface state around the Γ point of the BP Brillouin zone. Tight-binding calculations reveal that band gap openings at the crossing points in the two high-symmetry directions of the Brillouin zone require out-of-plane hopping and breaking of the glide mirror symmetry. Ab initio calculations are in very good agreement with the experiment if a stacking fault on the BP surface is taken into account. The demonstrated level of control over the band structure suggests the potential application of few-layer phosphorene in topological field-effect transistors.

  12. Aquarius L-Band Radiometers Calibration Using Cold Sky Observations

    NASA Technical Reports Server (NTRS)

    Dinnat, Emmanuel P.; Le Vine, David M.; Piepmeier, Jeffrey R.; Brown, Shannon T.; Hong, Liang

    2015-01-01

    An important element in the calibration plan for the Aquarius radiometers is to look at the cold sky. This involves rotating the satellite 180 degrees from its nominal Earth viewing configuration to point the main beams at the celestial sky. At L-band, the cold sky provides a stable, well-characterized scene to be used as a calibration reference. This paper describes the cold sky calibration for Aquarius and how it is used as part of the absolute calibration. Cold sky observations helped establish the radiometer bias, by correcting for an error in the spillover lobe of the antenna pattern, and monitor the long-term radiometer drift.

  13. Observation of a novel stapler band in 75As

    NASA Astrophysics Data System (ADS)

    Li, C. G.; Chen, Q. B.; Zhang, S. Q.; Xu, C.; Hua, H.; Li, X. Q.; Wu, X. G.; Hu, S. P.; Meng, J.; Xu, F. R.; Liang, W. Y.; Li, Z. H.; Ye, Y. L.; Jiang, D. X.; Sun, J. J.; Han, R.; Niu, C. Y.; Chen, X. C.; Li, P. J.; Wang, C. G.; Wu, H. Y.; Li, G. S.; He, C. Y.; Zheng, Y.; Li, C. B.; Chen, Q. M.; Zhong, J.; Zhou, W. K.

    2017-03-01

    The heavy ion fusion-evaporation reaction study for the high-spin spectroscopy of 75As has been performed via the reaction channel 70Zn(9Be, 1p3n)75As at a beam energy of 42 MeV. The collective structure especially a dipole band in 75As is established for the first time. The properties of this dipole band are investigated in terms of the self-consistent tilted axis cranking covariant density functional theory. Based on the theoretical description and the examination of the angular momentum components, this dipole band can be interpreted as a novel stapler band, where the valence neutrons in (1g9/2) orbital rather than the collective core are responsible for the closing of the stapler of angular momentum.

  14. Longwave Band-by-band Cloud Radiative Effect and its Application in GCM Evaluation

    NASA Technical Reports Server (NTRS)

    Huang, Xianglei; Cole, Jason N. S.; He, Fei; Potter, Gerald L.; Oreopoulos, Lazaros; Lee, Dongmin; Suarez, Max; Loeb, Norman G.

    2012-01-01

    The cloud radiative effect (CRE) of each longwave (LW) absorption band of a GCM fs radiation code is uniquely valuable for GCM evaluation because (1) comparing band-by-band CRE avoids the compensating biases in the broadband CRE comparison and (2) the fractional contribution of each band to the LW broadband CRE (f(sub CRE)) is sensitive to cloud top height but largely insensitive to cloud fraction, presenting thus a diagnostic metric to separate the two macroscopic properties of clouds. Recent studies led by the first author have established methods to derive such band ]by ]band quantities from collocated AIRS and CERES observations. We present here a study that compares the observed band-by-band CRE over the tropical oceans with those simulated by three different atmospheric GCMs (GFDL AM2, NASA GEOS-5, and CCCma CanAM4) forced by observed SST. The models agree with observation on the annual ]mean LW broadband CRE over the tropical oceans within +/-1W/sq m. However, the differences among these three GCMs in some bands can be as large as or even larger than +/-1W/sq m. Observed seasonal cycles of f(sub CRE) in major bands are shown to be consistent with the seasonal cycle of cloud top pressure for both the amplitude and the phase. However, while the three simulated seasonal cycles of f(sub CRE) agree with observations on the phase, the amplitudes are underestimated. Simulated interannual anomalies from GFDL AM2 and CCCma CanAM4 are in phase with observed anomalies. The spatial distribution of f(sub CRE) highlights the discrepancies between models and observation over the low-cloud regions and the compensating biases from different bands.

  15. Narrow Band Gap Lead Sulfide Hole Transport Layers for Quantum Dot Photovoltaics.

    PubMed

    Zhang, Nanlin; Neo, Darren C J; Tazawa, Yujiro; Li, Xiuting; Assender, Hazel E; Compton, Richard G; Watt, Andrew A R

    2016-08-24

    The band structure of colloidal quantum dot (CQD) bilayer heterojunction solar cells is optimized using a combination of ligand modification and QD band gap control. Solar cells with power conversion efficiencies of up to 9.33 ± 0.50% are demonstrated by aligning the absorber and hole transport layers (HTL). Key to achieving high efficiencies is optimizing the relative position of both the valence band and Fermi energy at the CQD bilayer interface. By comparing different band gap CQDs with different ligands, we find that a smaller band gap CQD HTL in combination with a more p-type-inducing CQD ligand is found to enhance hole extraction and hence device performance. We postulate that the efficiency improvements observed are largely due to the synergistic effects of narrower band gap QDs, causing an upshift of valence band position due to 1,2-ethanedithiol (EDT) ligands and a lowering of the Fermi level due to oxidation.

  16. HRO: A New Forward-Scatter Observation Method Using a Ham-Band Beacon

    NASA Astrophysics Data System (ADS)

    Maegawa, K.

    1999-02-01

    A new forward-scatter meteor observation method has been used since 1996 in Japan. It uses its own 50 W continuous wave beacon with a broad directivity antenna on 53.750 MHz. To compensate for the weak echo power from the beacon, observers use SSB mode receivers and narrow band echo detection methods with Fast Fourier Transform software on personal computers. More than 250000 echoes have been counted per year so far. >From these results, diurnal and seasonal variations have been derived and are presented and discussed here. This method (HRO) will continue to play a leading radio observation role in Japan for the future.

  17. Near-infrared observations of galaxies in Pisces-Perseus. I. vec H-band surface photometry of 174 spiral

    NASA Astrophysics Data System (ADS)

    Moriondo, G.; Baffa, C.; Casertano, S.; Chincarini, G.; Gavazzi, G.; Giovanardi, C.; Hunt, L. K.; Pierini, D.; Sperandio, M.; Trinchieri, G.

    1999-05-01

    We present near-infrared, H-band (1.65 $() μm), surface photometry of 174 spiral galaxies in the area of the Pisces-Perseus supercluster. The images, acquired with the ARNICA camera mounted on various telescopes, are used to derive radial profiles of surface brightness, ellipticities, and position angles, together with global parameters such as H-band magnitudes and diameters Radial profiles in tabular form and images FITS files are also available upon request from gmorio@arcetri.astro.it.}. The mean relation between H-band isophotal diameter D_{21.5} and the B-band D25 implies a B-H color of the outer disk bluer than 3.5; moreover, D_{21.5}/D25 depends on (global) color and absolute luminosity. The correlations among the various photometric parameters suggest a ratio between isophotal radius D_{21.5}/2 and disk scale length of ~ m3.5 and a mean disk central brightness ~ meq 17.5 H-mag arcsec^{-2}. We confirm the trend of the concentration index C31$ with absolute luminosity and, to a lesser degree, with morphological type. We also assess the influence of non-axisymmetric structures on the radial profiles and on the derived parameters. Based on observations at the TIRGO, NOT, and VATT telescopes. TIRGO (Gornergrat, CH) is operated by CAISMI-CNR, Arcetri, Firenze. NOT (La Palma, Canary Islands) is operated by NOTSA, the Nordic Observatory Scientific Association. VATT (Mt. Graham, Az) is operated by VORG, the Vatican Observatory Research Group Table 3 and Fig. 4 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html.

  18. Surveying the Lunar Surface for New Craters with Mini-RF/Goldstone X-Band Bistatic Observations

    NASA Astrophysics Data System (ADS)

    Cahill, J. T.; Patterson, G.; Turner, F. S.; Morgan, G.; Stickle, A. M.; Speyerer, E. J.; Espiritu, R. C.; Thomson, B. J.

    2017-12-01

    A multi-look temporal imaging survey by Speyerer et al. (2016) using Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Camera (NAC) has highlighted detectable and frequent impact bombardment processes actively modifying the lunar surface. Over 220 new resolvable impacts have been detected since NASA's Lunar Reconnaissance Orbiter (LRO) entered orbit around the Moon, at a flux that is substantially higher than anticipated from previous studies (Neukum et al., 2001). The Miniature Radio Frequency (Mini-RF) instrument aboard LRO is a hybrid dual-polarized synthetic aperture radar (SAR) that now operates in concert with the Arecibo Observatory (AO) and the Goldstone deep space communications complex 34-meter antenna DSS-13 to collect S- and X-band (12.6 and 4.2 cm, respectively) bistatic radar data of the Moon, respectively. Here we targeted some of the larger (>30 m) craters identified by Speyerer et al. (2016) and executed bistatic X-band radar observations both to evaluate our ability to detect and resolve these impact features and further characterize the spatial extent and material size of their ejecta outside optical wavelengths. Data acquired during Mini-RF monostatic operations, when the transmitter was active, show no coverage of the regions in question before or after two of the new impacts occurred. This makes Mini-RF and Earth-based bistatic observations all the more valuable for examination of these fresh new geologic features. Preliminary analyses of Arecibo/Greenbank and Mini-RF/Goldstone observations are unable to resolve the new crater cavities (due to our current resolving capability of 100 m/px), but they further confirm lunar surface roughness changes occurred between 2008 and 2017. Mini-RF X-band observations show newly ejected material was dispersed on the order of 100-300 meters from the point of impact. Scattering observed in the X-band data suggests the presence of rocky ejecta 4 - 45 cm in diameter on the surface and buried to depths of

  19. Observation of spontaneous spin-splitting in the band structure of an n-type zinc-blende ferromagnetic semiconductor

    PubMed Central

    Anh, Le Duc; Hai, Pham Nam; Tanaka, Masaaki

    2016-01-01

    Large spin-splitting in the conduction band and valence band of ferromagnetic semiconductors, predicted by the influential mean-field Zener model and assumed in many spintronic device proposals, has never been observed in the mainstream p-type Mn-doped ferromagnetic semiconductors. Here, using tunnelling spectroscopy in Esaki-diode structures, we report the observation of such a large spontaneous spin-splitting energy (31.7–50 meV) in the conduction band bottom of n-type ferromagnetic semiconductor (In,Fe)As, which is surprising considering the very weak s-d exchange interaction reported in several zinc-blende type semiconductors. The mean-field Zener model also fails to explain consistently the ferromagnetism and the spin-splitting energy of (In,Fe)As, because we found that the Curie temperature values calculated using the observed spin-splitting energies are much lower than the experimental ones by a factor of 400. These results urge the need for a more sophisticated theory of ferromagnetic semiconductors. PMID:27991502

  20. Direct Mapping of Band Positions in Doped and Undoped Hematite during Photoelectrochemical Water Splitting

    DOE PAGES

    Shavorskiy, Andrey; Ye, Xiaofei; Karslgolu, Osman; ...

    2017-10-30

    Photoelectrochemical water splitting is a promising pathway for the direct conversion of renewable solar energy to easy to store and use chemical energy. The performance of a photoelectrochemical device is determined in large part by the heterogeneous interface between the photoanode and the electrolyte, which we here characterize directly under operating conditions using interface-specific probes. Utilizing X-ray photoelectron spectroscopy as a noncontact probe of local electrical potentials, we demonstrate direct measurements of the band alignment at the semiconductor/electrolyte interface of an operating hematite/KOH photoelectrochemical cell as a function of solar illumination, applied potential, and doping. Here, we provide evidence formore » the absence of in-gap states in this system, which is contrary to previous measurements using indirect methods, and give a comprehensive description of shifts in the band positions and limiting processes during the photoelectrochemical reaction.« less

  1. Observation of the four wave mixing photonic band gap signal in electromagnetically induced grating.

    PubMed

    Ullah, Zakir; Wang, Zhiguo; Gao, Mengqin; Zhang, Dan; Zhang, Yiqi; Gao, Hong; Zhang, Yanpeng

    2014-12-01

    For the first time, we experimentally and theoretically research about the probe transmission signal (PTS), the reflected four wave mixing band gap signal(FWM BGS) and fluorescence signal (FLS) under the double dressing effect in an inverted Y-type four level system. FWM BGS results from photonic band gap structure. We demonstrate that the characteristics of PTS, FWM BGS and FLS can be controlled by power, phase and the frequency detuning of the dressing beams. It is observed in our experiment that FWM BGS switches from suppression to enhancement, corresponding to the switch from transmission enhancement to absorption enhancement in the PTS with changing the relative phase. We also observe the relation among the three signals, which satisfy the law of conservation of energy. Such scheme could have potential applications in optical diodes, amplifiers and quantum information processing.

  2. Limitations to Dual Frequency Ionosphere Corrections for Frequency Switched K-Q-Band Observations with the VLBA

    NASA Technical Reports Server (NTRS)

    Lanyi, Gabor; Gordon, David; Sovers, Ojars J.

    2004-01-01

    A series of VLBA experiments were carried out at K and Q bands for astrometry and imaging within the KQ VLBI Survey Collaboration. The paired K and Q observations of each source are separated by approximately 3 minutes of time. We investigate the delay effect of the ionosphere between K and Q bands involving the interscan separation. This differential delay effect is intermixed with the differential fluctuation effect of the troposphere.

  3. Vibrational spectroscopic characterization of growth bands in Porites coral from South China Sea

    NASA Astrophysics Data System (ADS)

    Song, Yinxian; Yu, Kefu; Ayoko, Godwin A.; Frost, Ray L.; Shi, Qi; Feng, Yuexing; Zhao, Jianxin

    2013-08-01

    A series of samples from different growth bands of Porites coral skeleton were studied using Raman, infrared reflectance methods. The Raman spectra proved that skeleton samples from different growth bands have the same mineral phase as aragonite, but a band at 133 cm-1 for the top layer shows a transition from ˜120 cm-1 for vaterite to ˜141 cm-1 for aragonite. It is inferred that the vaterite should be the precursor of aragonite of coral skeleton. The positional shift in the infrared spectra of the skeleton samples from growth bands correlate significantly to their minor elements (Li, Mg, Sr, Mn, Fe and U) contents. Mg, Sr and U especially have significant negative correlations with the positions of the antisymmetric stretching band ν3 at ˜1469 cm-1. And Li shows a high negative correlation with ν2 band (˜855 cm-1), while Sr and Mn show similar negative correlation with ν4 band (˜712 cm-1). And Mn also shows a negative correlation with ν1 band (˜1082 cm-1). A significantly negative correlation is observed for U with ν1 + ν4 band (˜1786 cm-1). However, Fe shows positive correlation with ν1, ν2, ν3, ν4 and ν1 + ν4 bands shifts, especially a significant correlation with ν1 band (˜1082 cm-1). New insights into the characteristics of coral at different growth bands of skeleton are given in present work.

  4. Association between HRP-2/pLDH rapid diagnostic test band positivity and malaria-related anemia at a peripheral health facility in Western Uganda.

    PubMed

    Boyce, Ross; Reyes, Raquel; Ntaro, Moses; Mulogo, Edgar; Matte, Michael; Boum, Yap; Siedner, Mark J

    2015-12-01

    The detection of severe malaria in resource-constrained settings is often difficult because of requirements for laboratory infrastructure and/or clinical expertise. The aim of this study, therefore, was to explore the utility of a multiple antigen (HRP-2/pLDH) rapid diagnostic test (RDT) as a low-cost, surrogate marker of patients at high risk for complications of severe malaria. We reviewed programmatic data at a peripheral health center in Western Uganda. Available demographic and clinical data on all individuals presenting to the center who underwent an RDT for suspected malaria infection were reviewed. We fit logistic regression models to identify correlates of two outcomes of interest: 1) severe malaria-related anemia, defined here as hemoglobin ≤7g/dL and 2) receipt of parenteral quinine. 1509 patients underwent malaria testing with an SD FK60 RDT during the observation period. A total of 637 (42%) RDTs were positive for at least one species of malaria, of which 326 (51%) exhibited a single HRP-2 band and 307 (48%) exhibited both HRP-2 and pLDH bands, while 4 exhibited only a single pLDH band. There was a trend towards more severe anemia in patients with a HRP-2/pLDH positive RDT compared to a HRP-2 only RDT (β = -0.99 g/dl, 95% CI -1.99 to 0.02, P = 0.055). A HRP-2/pLDH positive RDT was associated with an increased risk of severe malaria-related anemia compared to a negative RDT (adjusted odds ratio (AOR) 18.8, 95% CI 4.32 to 82.0, P < 0.001) and to a HRP-2 only RDT (AOR 2.46, 95% CI 0.75 to 8.04, P = 0.14). There was no significant association between RDT result and the administration of parenteral quinine. These results offer preliminary evidence that specific patterns of antigen positivity on RDTs could be utilized to identify patients at an increased risk for complications of severe malaria.

  5. Satellite Based Soil Moisture Product Validation Using NOAA-CREST Ground and L-Band Observations

    NASA Astrophysics Data System (ADS)

    Norouzi, H.; Campo, C.; Temimi, M.; Lakhankar, T.; Khanbilvardi, R.

    2015-12-01

    Soil moisture content is among most important physical parameters in hydrology, climate, and environmental studies. Many microwave-based satellite observations have been utilized to estimate this parameter. The Advanced Microwave Scanning Radiometer 2 (AMSR2) is one of many remotely sensors that collects daily information of land surface soil moisture. However, many factors such as ancillary data and vegetation scattering can affect the signal and the estimation. Therefore, this information needs to be validated against some "ground-truth" observations. NOAA - Cooperative Remote Sensing and Technology (CREST) center at the City University of New York has a site located at Millbrook, NY with several insitu soil moisture probes and an L-Band radiometer similar to Soil Moisture Passive and Active (SMAP) one. This site is among SMAP Cal/Val sites. Soil moisture information was measured at seven different locations from 2012 to 2015. Hydra probes are used to measure six of these locations. This study utilizes the observations from insitu data and the L-Band radiometer close to ground (at 3 meters height) to validate and to compare soil moisture estimates from AMSR2. Analysis of the measurements and AMSR2 indicated a weak correlation with the hydra probes and a moderate correlation with Cosmic-ray Soil Moisture Observing System (COSMOS probes). Several differences including the differences between pixel size and point measurements can cause these discrepancies. Some interpolation techniques are used to expand point measurements from 6 locations to AMSR2 footprint. Finally, the effect of penetration depth in microwave signal and inconsistencies with other ancillary data such as skin temperature is investigated to provide a better understanding in the analysis. The results show that the retrieval algorithm of AMSR2 is appropriate under certain circumstances. This validation algorithm and similar study will be conducted for SMAP mission. Keywords: Remote Sensing, Soil

  6. Octupole Deformation Bands of πh11/2 in Neutron-Rich 145,147La Nuclei

    NASA Astrophysics Data System (ADS)

    Zhu, Sheng-jiang; S, Zhu J.; Wang, Mu-ge; J, Hamilton H.; A, Ramayya V.; B, Babu R. S.; W, Ma C.; Long, Gui-lu; Zhu, Ling-yan; Li, Ming; A, Sakhaee; Gan, Cui-yun; Yang, Li-ming; J, Komicki; J, Cole D.; R, Aryaeinejad; M, Drigert W.; J, Rasmussen O.; M, Stoyer A.; S, Chu Y.; K, Gregorich E.; M, Mohar F.; S, Prussin G.; I, Lee Y.; Yu, Oganessian Ts; G, Ter-Akopian M.; A, Daniel V.

    1999-03-01

    Octupole deformation bands built on πh11/2 orbital in neutron-rich odd-Z 145,147La nuclei have been investigated by measuring the prompt γ-rays emitted from the 252Cf source. The alternating parity band structures and strong E1 transitions observed between negative- and positive-parity bands in both nuclei indicate the octupole deformation enhanced by the h11/2 single proton coupling. According to observed energy displacements the octupole deformation becomes stable at the intermediate spin states.

  7. Band-notched spiral antenna

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Jeon, Jae; Chang, John

    A band-notched spiral antenna having one or more spiral arms extending from a radially inner end to a radially outer end for transmitting or receiving electromagnetic radiation over a frequency range, and one or more resonance structures positioned adjacent one or more segments of the spiral arm associated with a notch frequency band or bands of the frequency range so as to resonate and suppress the transmission or reception of electromagnetic radiation over said notch frequency band or bands.

  8. Monitoring the On-Orbit Calibration of Terra MODIS Reflective Solar Bands Using Simultaneous Terra MISR Observations

    NASA Technical Reports Server (NTRS)

    Angal, Amit; Xiong, Xiaoxiong; Wu, Aisheng

    2016-01-01

    On December 18, 2015, the Terra spacecraft completed 16 years of successful operation in space. Terra has five instruments designed to facilitate scientific measurements of the earths land, ocean, and atmosphere. The Moderate Resolution Imaging Spectroradiometer (MODIS) and the Multiangle Imaging Spectroradiometer (MISR) instruments provide information for the temporal studies of the globe. After providing over 16 years of complementary measurements, a synergistic use of the measurements obtained from these sensors is beneficial for various science products. The 20 reflective solar bands (RSBs) of MODIS are calibrated using a combination of solar diffuser and lunar measurements, supplemented by measurements from pseudoinvariant desert sites. MODIS views the on-board calibrators and the earth via a two-sided scan mirror at three spatial resolutions: 250 m using 40 detectors in bands 1 and 2, 500 m using 20 detectors in bands 3 and 4, and 1000 m using 10 detectors in bands 819 and 26. Simultaneous measurements of the earths surface are acquired in a push-broom fashion by MISR at nine view angles spreading out in the forward and backward directions along the flight path. While the swath width for MISR acquisitions is 360 km, MODIS scans a wider swath of 2330 km via its two-sided scan mirror. The reflectance of the MODIS scan mirror has an angle dependence characterized by the response versus scan angle (RVS). Its on-orbit change is derived using the gain from a combination of on-board and earth-view measurements. The on-orbit RVS for MODIS has experienced a significant change, especially for the short-wavelength bands. The on-orbit RVS change for the short-wavelength bands (bands 3, 8, and 9) at nadir is observed to be greater than 10 over the mission lifetime. Due to absence of a scanning mechanism, MISR can serve as an effective tool to evaluate and monitor the on-orbit performance of the MODIS RVS. Furthermore, it can also monitor the detector and scan

  9. Evaluating the potential use of a high-resolution X-band polarimetric radar observations in Urban Hydrology

    NASA Astrophysics Data System (ADS)

    Anagnostou, Marios N.; Kalogiros, John; Marzano, Frank S.; Anagnostou, Emmanouil N.; Baldini, Luca; Nikolopoulos, EfThymios; Montopoli, Mario; Picciotti, Errico

    2014-05-01

    The Mediterranean area concentrates the major natural risks related to the water cycle, including heavy precipitation and flash-flooding during the fall season. Every year in central and south Europe we witness several fatal and economical disasters from severe storm rainfall triggering Flash Floods, and its impacts are increasing worldwide, but remain very difficult to manage. The spatial scale of flash flood occurrence is such that its vulnerability is often focused on dispersed urbanization, transportation and tourism infrastructures (De Marchi and Scolobig 2012). Urbanized and industrialized areas shows peculiar hydrodynamic and meteo-oceanographic features and they concentrate the highest rates of flash floods and fatal disasters. The main causes of disturbance being littoral urban development and harbor activities, the building of littoral rail- and highways, and the presence of several polluted discharges. All the above mentioned characteristics limit our ability to issue timely flood warnings. Precipitation estimates based on raingauge networks are usually associated with low coverage density, particularly at high altitudes. On the other hand, operational weather radar networks may provide valuable information of precipitation at these regimes but reliability of their estimates is often limited due to retrieval (e.g. variability in the reflectivity-to-rainfall relationship) and spatial extent constrains (e.g. blockage issues, overshooting effects). As a result, we currently lack accurate precipitation estimates over urban complex terrain areas, which essentially means that we lack accurate knowledge of the triggering factor for a number of hazards like flash floods and debris flows/landslides occurring in those areas. A potential solution to overcome sampling as well as retrieval uncertainty limitations of current observational networks might be the use of network of low-power dual-polarization X-band radars as complement to raingauges and gap-filling to

  10. Observing position and movements in hydrotherapy: a pilot study.

    PubMed

    Stark, Mary Ann; Rudell, Barb; Haus, George

    2008-01-01

    To observe and describe the positions and movements women choose while immersed in water during the first stage of labor. Descriptive, observational pilot study. A rural community hospital that provided hydrotherapy in labor. Women (N = 7) who intended to use hydrotherapy in labor were recruited prenatally from a midwife-managed practice. For 15 minutes of each hour during the first stage of labor, position and movements of the participants were observed and recorded on a laptop computer. The observational tool was developed for this study from a review of the literature and interviews with nursing experts; 435 observations were recorded. Women were free to choose when and how long to use hydrotherapy and had no restriction on their positions and movements. Only 3 of the 7 participants labored in the tub. Women demonstrated a greater range of positions and movements in the tub than in bed, both throughout labor and during late first-stage labor (7-10 cm of dilatation). Women had more contractions and made more rhythmic movements while in the tub than in bed. Hydrotherapy may encourage upright positions and movements that facilitate labor progress and coping, helping women avoid unnecessary interventions.

  11. Soil moisture estimation by assimilating L-band microwave brightness temperature with geostatistics and observation localization.

    PubMed

    Han, Xujun; Li, Xin; Rigon, Riccardo; Jin, Rui; Endrizzi, Stefano

    2015-01-01

    The observation could be used to reduce the model uncertainties with data assimilation. If the observation cannot cover the whole model area due to spatial availability or instrument ability, how to do data assimilation at locations not covered by observation? Two commonly used strategies were firstly described: One is covariance localization (CL); the other is observation localization (OL). Compared with CL, OL is easy to parallelize and more efficient for large-scale analysis. This paper evaluated OL in soil moisture profile characterizations, in which the geostatistical semivariogram was used to fit the spatial correlated characteristics of synthetic L-Band microwave brightness temperature measurement. The fitted semivariogram model and the local ensemble transform Kalman filter algorithm are combined together to weight and assimilate the observations within a local region surrounding the grid cell of land surface model to be analyzed. Six scenarios were compared: 1_Obs with one nearest observation assimilated, 5_Obs with no more than five nearest local observations assimilated, and 9_Obs with no more than nine nearest local observations assimilated. The scenarios with no more than 16, 25, and 36 local observations were also compared. From the results we can conclude that more local observations involved in assimilation will improve estimations with an upper bound of 9 observations in this case. This study demonstrates the potentials of geostatistical correlation representation in OL to improve data assimilation of catchment scale soil moisture using synthetic L-band microwave brightness temperature, which cannot cover the study area fully in space due to vegetation effects.

  12. Soil Moisture Estimation by Assimilating L-Band Microwave Brightness Temperature with Geostatistics and Observation Localization

    PubMed Central

    Han, Xujun; Li, Xin; Rigon, Riccardo; Jin, Rui; Endrizzi, Stefano

    2015-01-01

    The observation could be used to reduce the model uncertainties with data assimilation. If the observation cannot cover the whole model area due to spatial availability or instrument ability, how to do data assimilation at locations not covered by observation? Two commonly used strategies were firstly described: One is covariance localization (CL); the other is observation localization (OL). Compared with CL, OL is easy to parallelize and more efficient for large-scale analysis. This paper evaluated OL in soil moisture profile characterizations, in which the geostatistical semivariogram was used to fit the spatial correlated characteristics of synthetic L-Band microwave brightness temperature measurement. The fitted semivariogram model and the local ensemble transform Kalman filter algorithm are combined together to weight and assimilate the observations within a local region surrounding the grid cell of land surface model to be analyzed. Six scenarios were compared: 1_Obs with one nearest observation assimilated, 5_Obs with no more than five nearest local observations assimilated, and 9_Obs with no more than nine nearest local observations assimilated. The scenarios with no more than 16, 25, and 36 local observations were also compared. From the results we can conclude that more local observations involved in assimilation will improve estimations with an upper bound of 9 observations in this case. This study demonstrates the potentials of geostatistical correlation representation in OL to improve data assimilation of catchment scale soil moisture using synthetic L-band microwave brightness temperature, which cannot cover the study area fully in space due to vegetation effects. PMID:25635771

  13. Characterisation of false-positive observations in botanical surveys

    PubMed Central

    2017-01-01

    Errors in botanical surveying are a common problem. The presence of a species is easily overlooked, leading to false-absences; while misidentifications and other mistakes lead to false-positive observations. While it is common knowledge that these errors occur, there are few data that can be used to quantify and describe these errors. Here we characterise false-positive errors for a controlled set of surveys conducted as part of a field identification test of botanical skill. Surveys were conducted at sites with a verified list of vascular plant species. The candidates were asked to list all the species they could identify in a defined botanically rich area. They were told beforehand that their final score would be the sum of the correct species they listed, but false-positive errors counted against their overall grade. The number of errors varied considerably between people, some people create a high proportion of false-positive errors, but these are scattered across all skill levels. Therefore, a person’s ability to correctly identify a large number of species is not a safeguard against the generation of false-positive errors. There was no phylogenetic pattern to falsely observed species; however, rare species are more likely to be false-positive as are species from species rich genera. Raising the threshold for the acceptance of an observation reduced false-positive observations dramatically, but at the expense of more false negative errors. False-positive errors are higher in field surveying of plants than many people may appreciate. Greater stringency is required before accepting species as present at a site, particularly for rare species. Combining multiple surveys resolves the problem, but requires a considerable increase in effort to achieve the same sensitivity as a single survey. Therefore, other methods should be used to raise the threshold for the acceptance of a species. For example, digital data input systems that can verify, feedback and inform the

  14. High resolution observations with Artemis-IV and the NRH. I. Type IV associated narrow-band bursts

    NASA Astrophysics Data System (ADS)

    Bouratzis, C.; Hillaris, A.; Alissandrakis, C. E.; Preka-Papadema, P.; Moussas, X.; Caroubalos, C.; Tsitsipis, P.; Kontogeorgos, A.

    2016-02-01

    Context. Narrow-band bursts appear on dynamic spectra from microwave to decametric frequencies as fine structures with very small duration and bandwidth. They are believed to be manifestations of small scale energy release through magnetic reconnection. Aims: We analyzed 27 metric type IV events with embedded narrow-band bursts, which were observed by the ARTEMIS-IV radio spectrograph from 30 June 1999 to 1 August 2010. We examined the morphological characteristics of isolated narrow-band structures (mostly spikes) and groups or chains of structures. Methods: The events were recorded with the SAO high resolution (10 ms cadence) receiver of ARTEMIS-IV in the 270-450 MHz range. We measured the duration, spectral width, and frequency drift of ~12 000 individual narrow-band bursts, groups, and chains. Spike sources were imaged with the Nançay radioheliograph (NRH) for the event of 21 April 2003. Results: The mean duration of individual bursts at fixed frequency was ~100 ms, while the instantaneous relative bandwidth was ~2%. Some bursts had measurable frequency drift, either positive or negative. Quite often spikes appeared in chains, which were closely spaced in time (column chains) or in frequency (row chains). Column chains had frequency drifts similar to type-IIId bursts, while most of the row chains exhibited negative frequently drifts with a rate close to that of fiber bursts. From the analysis of NRH data, we found that spikes were superimposed on a larger, slowly varying, background component. They were polarized in the same sense as the background source, with a slightly higher degree of polarization of ~65%, and their size was about 60% of their size in total intensity. Conclusions: The duration and bandwidth distributions did not show any clear separation in groups. Some chains tended to assume the form of zebra, lace stripes, fiber bursts, or bursts of the type-III family, suggesting that such bursts might be resolved in spikes when viewed with high

  15. Observation of Dirac-like band dispersion in LaAgSb 2

    DOE PAGES

    Shi, X.; Richard, P.; Wang, Kefeng; ...

    2016-02-16

    In this paper, we present a combined angle-resolved photoemission spectroscopy (ARPES) and first-principles calculations study of the electronic structure of LaAgSb 2 in the entire first Brillouin zone. We observe a Dirac-cone-like structure in the vicinity of the Fermi level formed by the crossing of two linear energy bands, as well as the nested segments of a Fermi surface pocket emerging from the cone. In conclusion, our ARPES results show the close relationship of the Dirac cone to the charge-density-wave ordering, providing consistent explanations for exotic behaviors in this material.

  16. DEEP U BAND AND R IMAGING OF GOODS-SOUTH: OBSERVATIONS, DATA REDUCTION AND FIRST RESULTS ,

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Nonino, M.; Cristiani, S.; Vanzella, E.

    2009-08-01

    We present deep imaging in the U band covering an area of 630 arcmin{sup 2} centered on the southern field of the Great Observatories Origins Deep Survey (GOODS). The data were obtained with the VIMOS instrument at the European Southern Observatory (ESO) Very Large Telescope. The final images reach a magnitude limit U {sub lim} {approx} 29.8 (AB, 1{sigma}, in a 1'' radius aperture), and have good image quality, with full width at half-maximum {approx}0.''8. They are significantly deeper than previous U-band images available for the GOODS fields, and better match the sensitivity of other multiwavelength GOODS photometry. The deepermore » U-band data yield significantly improved photometric redshifts, especially in key redshift ranges such as 2 < z < 4, and deeper color-selected galaxy samples, e.g., Lyman break galaxies at z {approx} 3. We also present the co-addition of archival ESO VIMOS R-band data, with R {sub lim} {approx} 29 (AB, 1{sigma}, 1'' radius aperture), and image quality {approx}0.''75. We discuss the strategies for the observations and data reduction, and present the first results from the analysis of the co-added images.« less

  17. Laparoscopic Band-Separated One Anastomosis Gastric Bypass.

    PubMed

    Ospanov, Oral B

    2016-09-01

    This video demonstrates laparoscopic band-separated one anastomosis gastric bypass-combining the advantages of banding and gastric bypass without stapler and cutter use. This is basically a gastrojejunal loop bypass above an obstructive band in the upper stomach. An adjustable low pressure "Medsil" gastric band was introduced in the abdomen and retracted through the retrogastric tunnel. The front wall of the stomach below the band was displaced in the upward direction through the ring band, increasing the size of the anterior portion of the stomach pouch so that a gastroenteroanastomosis could be created at this point. Gastro-gastric sutures were placed to create a gastro-gastric plication around the band and hold it in position. The band tubing was exteriorized and connected to a special port, which was secured to the abdominal wall fascia. A jejunal loop was created about 200 cm from the ligament of Treitz and anastomosed to the gastric pouch by hand using Vicryl 2/0 sutures. Between November 2015 and February 2016, the study was performed on 10 patients. The average operating time for all cases was 75 min (range 63-87). There was no morbidity or mortality. No complications were observed, including band erosion and band infection. Operation costs were about $2000 lower with this method than with standard gastric bypass surgery. Postop the patients lost weight by 3-4 kg per month. Preliminary results show that laparoscopic band-separated one anastomosis gastric bypass have feasibility, safety, efficacy, and reduced operating costs.

  18. Measurement of InAsSb bandgap energy and InAs/InAsSb band edge positions using spectroscopic ellipsometry and photoluminescence spectroscopy

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Webster, P. T.; Riordan, N. A.; Liu, S.

    2015-12-28

    The structural and optical properties of lattice-matched InAs{sub 0.911}Sb{sub 0.089} bulk layers and strain-balanced InAs/InAs{sub 1−x}Sb{sub x} (x ∼ 0.1–0.4) superlattices grown on (100)-oriented GaSb substrates by molecular beam epitaxy are examined using X-ray diffraction, spectroscopic ellipsometry, and temperature dependent photoluminescence spectroscopy. The photoluminescence and ellipsometry measurements determine the ground state bandgap energy and the X-ray diffraction measurements determine the layer thickness and mole fraction of the structures studied. Detailed modeling of the X-ray diffraction data is employed to quantify unintentional incorporation of approximately 1% Sb into the InAs layers of the superlattices. A Kronig-Penney model of the superlattice miniband structure ismore » used to analyze the valence band offset between InAs and InAsSb, and hence the InAsSb band edge positions at each mole fraction. The resulting composition dependence of the bandgap energy and band edge positions of InAsSb are described using the bandgap bowing model; the respective low and room temperature bowing parameters for bulk InAsSb are 938 and 750 meV for the bandgap, 558 and 383 meV for the conduction band, and −380 and −367 meV for the valence band.« less

  19. FTIR Spectrum of the ν 4Band of DCOOD

    NASA Astrophysics Data System (ADS)

    Tan, T. L.; Goh, K. L.; Ong, P. P.; Teo, H. H.

    1999-06-01

    The FTIR spectrum of the ν4band of deuterated formic acid (DCOOD) has been measured with a resolution of 0.004 cm-1in the frequency range of 1120 to 1220 cm-1. A total of 1866 assigned transitions have been analyzed and fitted using a Watson'sA-reduced Hamiltonian in theIrrepresentation to derive rovibrational constants for the upper state (v4= 1) with a standard deviation of 0.00036 cm-1. In the course of the analysis, the constants for the ground state were improved by a simultaneous fit of microwave frequencies and combination differences from the infrared measurements. Due to the relatively unperturbed nature of the band, the constants can be used to accurately calculate the infrared line positions for the whole band. Although the band is a hybrid typeAandB, onlya-type transitions were strong enough to be observed. The band center is at 1170.79980 ± 0.00002 cm-1.

  20. Alpha-band rhythm suppression during memory recall reflecting memory performance.

    PubMed

    Yokosawa, Koichi; Kimura, Keisuke; Chitose, Ryota; Momiki, Takuya; Kuriki, Shinya

    2016-08-01

    Alpha-band rhythm is thought to be involved in memory processes, similarly to other spontaneous brain rhythms. Ten right-handed healthy volunteers participated in our proposed sequential short-term memory task that provides a serial position effect in accuracy rate. We recorded alpha-band rhythms by magnetoencephalography during performance of the task and observed that the amplitude of the rhythm was suppressed dramatically in the memory recall period. The suppressed region was estimated to be in the occipital lobe, suggesting that alpha-band rhythm is suppressed by activation of the occipital attentional network. Additionally, the alpha-band suppression reflected accuracy rate, that is, the amplitude was suppressed more when recalling items with higher accuracy rate. The sensors with a significant correlation between alpha-band amplitude and accuracy rate were located widely from the frontal to occipital regions mainly in the right hemisphere. The results suggests that alpha-band rhythm is involved in memory recall and can be index of memory performance.

  1. Soil moisture observations using L-, C-, and X-band microwave radiometers

    NASA Astrophysics Data System (ADS)

    Bolten, John Dennis

    The purpose of this thesis is to further the current understanding of soil moisture remote sensing under varying conditions using L-, C-, and X-band. Aircraft and satellite instruments are used to investigate the effects of frequency and spatial resolution on soil moisture sensitivity. The specific objectives of the research are to examine multi-scale observed and modeled microwave radiobrightness, evaluate new EOS Aqua Advanced Microwave Scanning Radiometer (AMSR-E) brightness temperature and soil moisture retrievals, and examine future satellite-based technologies for soil moisture sensing. The cycling of Earth's water, energy and carbon is vital to understanding global climate. Over land, these processes are largely dependent on the amount of moisture within the top few centimeters of the soil. However, there are currently no methods available that can accurately characterize Earth's soil moisture layer at the spatial scales or temporal resolutions appropriate for climate modeling. The current work uses ground truth, satellite and aircraft remote sensing data from three large-scale field experiments having different land surface, topographic and climate conditions. A physically-based radiative transfer model is used to simulate the observed aircraft and satellite measurements using spatially and temporally co-located surface parameters. A robust analysis of surface heterogeneity and scaling is possible due to the combination of multiple datasets from a range of microwave frequencies and field conditions. Accurate characterization of spatial and temporal variability of soil moisture during the three field experiments is achieved through sensor calibration and algorithm validation. Comparisons of satellite observations and resampled aircraft observations are made using soil moisture from a Numerical Weather Prediction (NWP) model in order to further demonstrate a soil moisture correlation where point data was unavailable. The influence of vegetation, spatial

  2. Thermally switchable photonic band-edge to random laser emission in dye-doped cholesteric liquid crystals

    NASA Astrophysics Data System (ADS)

    Ye, Lihua; Wang, Yan; Feng, Yangyang; Liu, Bo; Gu, Bing; Cui, Yiping; Lu, Yanqing

    2018-03-01

    By changing the doping concentration of the chiral agent to adjust the relative position of the reflection band of cholesteric liquid crystals and the fluorescence emission spectrum of the dye, photonic band-edge and random lasing were observed, respectively. The reflection band of the cholesteric phase liquid crystal can also be controlled by adjusting the temperature: the reflection band is blue-shifted with increasing temperature, and a reversible switch from photonic band-edge to random lasing is obtained. Furthermore, the laser line width can be thermally adjusted from 1.1 nm (at 27 °C) to 4.6 nm (at 32.1 °C). A thermally tunable polarization state of a random laser from dual cells was observed, broadening the field of application liquid crystal random lasers.

  3. The occurrence and wave properties of H⁺-, He⁺-, and O⁺-band EMIC waves observed by the Van Allen Probes

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Saikin, A. A.; Zhang, J. -C.; Allen, R. C.

    2015-09-26

    We perform a statistical study of electromagnetic ion cyclotron (EMIC) waves detected by the Van Allen Probes mission to investigate the spatial distribution of their occurrence, wave power, ellipticity, and normal angle. The Van Allen Probes have been used which allow us to explore the inner magnetosphere (1.1 to 5.8 RE). Magnetic field measurements from the Electric and Magnetic Field Instrument Suite and Integrated Science on board the Van Allen Probes are used to identify EMIC wave events for the first 22 months of the mission operation (8 September 2012 to 30 June 2014). EMIC waves are examined in H⁺-,more » He⁺-, and O⁺-bands. Over 700 EMIC wave events have been identified over the three different wave bands (265 H⁺-band events, 438 He⁺-band events, and 68 O⁺-band events). EMIC wave events are observed between L = 2 – 8, with over 140 EMIC wave events observed below L = 4. The results show that H⁺-band EMIC waves have two peak magnetic local time (MLT) occurrence regions: pre-noon (09:00 < MLT ≤ 12:00) and afternoon (15:00 < MLT ≤ 17:00) sectors. He⁺-band EMIC waves feature an overall stronger dayside occurrence. O⁺-band EMIC waves have one peak region located in the morning sector at lower L shells (L < 4). He⁺-band EMIC waves average the highest wave power overall (>0.1 nT²/Hz), especially in the afternoon sector. Ellipticity observations reveal that linearly polarized EMIC waves dominate in lower L shells.« less

  4. The occurrence, spatial distribution, and wave properties of hydrogen-, helium-, and oxygen-band EMIC waves observed by the Van Allen Probes

    NASA Astrophysics Data System (ADS)

    Saikin, A.; Zhang, J.; Allen, R. C.; Smith, C. W.; Kistler, L. M.; Spence, H. E.; Torbert, R. B.; Kletzing, C.; Jordanova, V.

    2014-12-01

    Electromagnetic ion cyclotron (EMIC) waves play an important role in the overall dynamics of the Earth's magnetosphere, including the energization and loss of particles. We perform a statistical study of EMIC waves detected by the Van Allen Probes mission to investigate their occurrence, spatial distribution, and properties (e.g., wave power, normal angle, and ellipticity). Magnetic field measurements from the Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) onboard Van Allen Probes are used to identify EMIC wave events from the beginning of the mission (September, 2012) to the present. EMIC waves are examined in hydrogen, helium and oxygen bands. So far, about 280 EMIC wave events have been identified over the three different bands. Preliminary results show that hydrogen-band EMIC waves have been primarily observed in the dusk sector, while helium-band EMIC waves have been observed in all Magnetic Local Times (MLTs). Particularly, the Van Allen Probes provide a better resolution of lower frequencies (0.2-0.9 Hz), within which oxygen-band EMIC waves can occur in the inner magnetosphere. This allows us to obtain better insight into the characteristics of this previously largely unavailable band of EMIC waves, and allows for comparisons amongst EMIC waves in different bands.

  5. Whistler anisotropy instabilities as the source of banded chorus: Van Allen Probes observations and particle-in-cell simulations

    DOE PAGES

    Fu, Xiangrong; Cowee, Misa M.; Friedel, Reinhard H.; ...

    2014-10-22

    Magnetospheric banded chorus is enhanced whistler waves with frequencies ω r < Ω e, where Ω e is the electron cyclotron frequency, and a characteristic spectral gap at ω r ≃ Ω e/2. This paper uses spacecraft observations and two-dimensional particle-in-cell simulations in a magnetized, homogeneous, collisionless plasma to test the hypothesis that banded chorus is due to local linear growth of two branches of the whistler anisotropy instability excited by two distinct, anisotropic electron components of significantly different temperatures. The electron densities and temperatures are derived from Helium, Oxygen, Proton, and Electron instrument measurements on the Van Allen Probesmore » A satellite during a banded chorus event on 1 November 2012. The observations are consistent with a three-component electron model consisting of a cold (a few tens of eV) population, a warm (a few hundred eV) anisotropic population, and a hot (a few keV) anisotropic population. The simulations use plasma and field parameters as measured from the satellite during this event except for two numbers: the anisotropies of the warm and the hot electron components are enhanced over the measured values in order to obtain relatively rapid instability growth. The simulations show that the warm component drives the quasi-electrostatic upper band chorus and that the hot component drives the electromagnetic lower band chorus; the gap at ~Ω e/2 is a natural consequence of the growth of two whistler modes with different properties.« less

  6. Estimating Sea Surface Salinity and Wind Using Combined Passive and Active L-Band Microwave Observations

    NASA Technical Reports Server (NTRS)

    Yueh, Simon H.; Chaubell, Mario J.

    2012-01-01

    Several L-band microwave radiometer and radar missions have been, or will be, operating in space for land and ocean observations. These include the NASA Aquarius mission and the Soil Moisture Active Passive (SMAP) mission, both of which use combined passive/ active L-band instruments. Aquarius s passive/active L-band microwave sensor has been designed to map the salinity field at the surface of the ocean from space. SMAP s primary objectives are for soil moisture and freeze/thaw detection, but it will operate continuously over the ocean, and hence will have significant potential for ocean surface research. In this innovation, an algorithm has been developed to retrieve simultaneously ocean surface salinity and wind from combined passive/active L-band microwave observations of sea surfaces. The algorithm takes advantage of the differing response of brightness temperatures and radar backscatter to salinity, wind speed, and direction, thus minimizing the least squares error (LSE) measure, which signifies the difference between measurements and model functions of brightness temperatures and radar backscatter. The algorithm uses the conjugate gradient method to search for the local minima of the LSE. Three LSE measures with different measurement combinations have been tested. The first LSE measure uses passive microwave data only with retrieval errors reaching 1 to 2 psu (practical salinity units) for salinity, and 1 to 2 m/s for wind speed. The second LSE measure uses both passive and active microwave data for vertical and horizontal polarizations. The addition of active microwave data significantly improves the retrieval accuracy by about a factor of five. To mitigate the impact of Faraday rotation on satellite observations, the third LSE measure uses measurement combinations invariant under the Faraday rotation. For Aquarius, the expected RMS SSS (sea surface salinity) error will be less than about 0.2 psu for low winds, and increases to 0.3 psu at 25 m/s wind speed

  7. Observations of LHR noise with banded structure by the sounding rocket S29 barium-GEOS

    NASA Technical Reports Server (NTRS)

    Koskinen, H. E. J.; Holmgren, G.; Kintner, P. M.

    1983-01-01

    The measurement of electrostatic noise near the lower hybrid frequency made by the sounding rocket S29 barium-GEOS is reported. The noise is related to the spin of the rocket and reaches well below the local lower hybrid resonance frequency. Above the altitude of 300 km the noise shows banded structure roughly organized by the hydrogen cyclotron frequency. Simultaneously with the banded structure a signal near the hydrogen cyclotron frequency is detected. This signal is also spin modulated. The character of the noise strongly suggests that it is locally generated by the rocket payload disturbing the plasma. If this interpretation is correct, plasma wave experiments on other spacecrafts are expected to observe similar phenomena.

  8. Precise Point Positioning Based on BDS and GPS Observations

    NASA Astrophysics Data System (ADS)

    Gao, ZhouZheng; Zhang, Hongping; Shen, Wenbin

    2014-05-01

    BeiDou Navigation Satellite System (BDS) has obtained the ability applying initial navigation and precise point services for the Asian-Pacific regions at the end of 2012 with the constellation of 5 Geostationary Earth Orbit (GEO), 5 Inclined Geosynchronous Orbit (IGSO) and 4 Medium Earth Orbit (MEO). Till 2020, it will consist with 5 GEO, 3 IGSO and 27 MEO, and apply global navigation service similar to GPS and GLONASS. As we known, GPS precise point positioning (PPP) is a powerful tool for crustal deformation monitoring, GPS meteorology, orbit determination of low earth orbit satellites, high accuracy kinematic positioning et al. However, it accuracy and convergence time are influenced by the quality of pseudo-range observations and the observing geometry between user and Global navigation satellites system (GNSS) satellites. Usually, it takes more than 30 minutes even hours to obtain centimeter level position accuracy for PPP while using GPS dual-frequency observations only. In recent years, many researches have been done to solve this problem. One of the approaches is smooth pseudo-range by carrier-phase observations to improve pseudo-range accuracy. By which can improve PPP initial position accuracy and shorten PPP convergence time. Another sachems is to change position dilution of precision (PDOP) with multi-GNSS observations. Now, BDS has the ability to service whole Asian-Pacific regions, which make it possible to use GPS and BDS for precise positioning. In addition, according to researches on GNSS PDOP distribution, BDS can improve PDOP obviously. Therefore, it necessary to do some researches on PPP performance using both GPS observations and BDS observations, especially in Asian-Pacific regions currently. In this paper, we focus on the influences of BDS to GPS PPP mainly in three terms including BDS PPP accuracy, PDOP improvement and convergence time of PPP based on GPS and BDS observations. Here, the GPS and BDS two-constellation data are collected from

  9. The Fundamental Quadrupole Band of (14)N2: Line Positions from High-Resolution Stratospheric Solar Absorption Spectra

    NASA Technical Reports Server (NTRS)

    Rinsland, C. P.; Zander, R.; Goldman, A.; Murcray, F. J.; Murcray, D. G.; Grunson, M. R.; Farmer, C. B.

    1991-01-01

    The purpose of this note is to report accurate measurements of the positions of O- and S-branch lines of the (1-0) vibration-rotation quadrupole band of molecular nitrogen ((14)N2) and improved Dunham coefficients derived from a simultaneous least-squares analysis of these measurements and selected infrared and far infrared data taken from the literature. The new measurements have been derived from stratospheric solar occultation spectra recorded with Fourier transform spectrometer (FTS) instruments operated at unapodized spectral resolutions of 0.002 and 0.01 /cm. The motivation for the present investigation is the need for improved N2 line parameters for use in IR atmospheric remote sensing investigations. The S branch of the N2 (1-0) quadrupole band is ideal for calibrating the line-of-sight airmasses of atmospheric spectra since the strongest lines are well placed in an atmospheric window, their absorption is relatively insensitive to temperature and is moderately strong (typical line center depths of 10 to 50% in high-resolution ground-based solar spectra and in lower stratospheric solar occultation spectra), and the volume mixing ratio of nitrogen is constant in the atmosphere and well known. However, a recent investigation has'shown the need to improve the accuracies of the N2 fine positions, intensities, air-broadened half-widths, and their temperature dependences to fully exploit this calibration capability (1). The present investigation addresses the problem of improving the accuracy of the N2 line positions.

  10. A Robust Indoor Autonomous Positioning System Using Particle Filter Based on ISM Band Wireless Communications

    NASA Astrophysics Data System (ADS)

    Ikeda, Takeshi; Kawamoto, Mitsuru; Sashima, Akio; Suzuki, Keiji; Kurumatani, Koichi

    In the field of the ubiquitous computing, positioning systems which can provide users' location information have paid attention as an important technical element which can be applied to various services, for example, indoor navigation services, evacuation services, market research services, guidance services, and so on. A lot of researchers have proposed various outdoor and indoor positioning systems. In this paper, we deal with indoor positioning systems. Many conventional indoor positioning systems use expensive infrastructures, because the propagated times of radio waves are used to measure users' positions with high accuracy. In this paper, we propose an indoor autonomous positioning system using radio signal strengths (RSSs) based on ISM band communications. In order to estimate users' positions, the proposed system utilizes a particle filter that is one of the Monte Carlo methods. Because the RSS information is used in the proposed system, the equipments configuring the system are not expensive compared with the conventional indoor positioning systems and it can be installed easily. Moreover, because the particle filter is used to estimate user's position, even if the RSS fluctuates due to, for example, multi-paths, the system can carry out position estimation robustly. We install the proposed system in one floor of a building and carry out some experiments in order to verify the validity of the proposed system. As a result, we confirmed that the average of the estimation errors of the proposed system was about 1.8 m, where the result is enough accuracy for achieving the services mentioned above.

  11. Observation of Wakefield Suppression in a Photonic-Band-Gap Accelerator Structure

    DOE PAGES

    Simakov, Evgenya I.; Arsenyev, Sergey A.; Buechler, Cynthia E.; ...

    2016-02-10

    We report experimental observation of higher order mode (HOM) wakefield suppression in a room-temperature traveling-wave photonic band gap (PBG) accelerating structure at 11.700 GHz. It has been long recognized that PBG structures have potential for reducing long-range wakefields in accelerators. The first ever demonstration of acceleration in a room-temperature PBG structure was conducted in 2005. Since then, the importance of PBG accelerator research has been recognized by many institutions. However, the full experimental characterization of the wakefield spectrum and demonstration of wakefield suppression when the accelerating structure is excited by an electron beam has not been performed to date. Wemore » conducted an experiment at the Argonne Wakefield Accelerator (AWA) test facility and observed wakefields excited by a single high charge electron bunch when it passes through a PBG accelerator structure. Lastly, excellent HOM suppression properties of the PBG accelerator were demonstrated in the beam test.« less

  12. PAHs and the Diffuse Interstellar Bands. What have we Learned from the New Generation of Laboratory and Observational Studies?

    NASA Technical Reports Server (NTRS)

    Salama, Farid

    2005-01-01

    Polycyclic Aromatic Hydrocarbons (PAHs) are an important and ubiquitous component of carbon-bearing materials in space. PAHs are the best-known candidates to account for the IR emission bands (UIR bands) and PAH spectral features are now being used as new probes of the ISM. PAHs are also thought to be among the carriers of the diffuse interstellar absorption bands (DIBs). In the model dealing with the interstellar spectral features, PAHs are present as a mixture of radicals, ions and neutral species. PAH ionization states reflect the ionization balance of the medium while PAH size, composition, and structure reflect the energetic and chemical history of the medium. A major challenge for laboratory astrophysics is to reproduce (in a realistic way) the physical conditions that exist in the emission and/or absorption interstellar zones, An extensive laboratory program has been developed at NASA Ames to characterize the physical and chemical properties of PAHs in astrophysical environments and to describe how they influence the radiation and energy balance in space and the interstellar chemistry. In particular, laboratory experiments provide measurements of the spectral characteristics of interstellar PAH analogs from the ultraviolet and visible range to the infrared range for comparison with astronomical data. This paper will focus on the recent progress made in the laboratory to measure the direct absorption spectra of neutral and ionized PAHs in the gas phase in the near-W and visible range in astrophysically relevant environments. These measurements provide data on PAHs and nanometer-sized particles that can now be directly compared to astronomical observations. The harsh physical conditions of the IS medium - characterized by a low temperature, an absence of collisions and strong V W radiation fields - are simulated in the laboratory by associating a molecular beam with an ionizing discharge to generate a cold plasma expansion. PAH ions are formed from the neutral

  13. Atomic-Monolayer MoS2 Band-to-Band Tunneling Field-Effect Transistor.

    PubMed

    Lan, Yann-Wen; Torres, Carlos M; Tsai, Shin-Hung; Zhu, Xiaodan; Shi, Yumeng; Li, Ming-Yang; Li, Lain-Jong; Yeh, Wen-Kuan; Wang, Kang L

    2016-11-01

    The experimental observation of band-to-band tunneling in novel tunneling field-effect transistors utilizing a monolayer of MoS 2 as the conducting channel is demonstrated. Our results indicate that the strong gate-coupling efficiency enabled by two-dimensional materials, such as monolayer MoS 2 , results in the direct manifestation of a band-to-band tunneling current and an ambipolar transport. © 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.

  14. Assessment of Thematic Mapper Band-to-band Registration by the Block Correlation Method

    NASA Technical Reports Server (NTRS)

    Card, D. H.; Wrigley, R. C.; Mertz, F. C.; Hall, J. R.

    1984-01-01

    The design of the Thematic Mapper (TM) multispectral radiometer makes it susceptible to band-to-band misregistration. To estimate band-to-band misregistration a block correlation method is employed. This method is chosen over other possible techniques (band differencing and flickering) because quantitative results are produced. The method correlates rectangular blocks of pixels from one band against blocks centered on identical pixels from a second band. The block pairs are shifted in pixel increments both vertically and horizontally with respect to each other and the correlation coefficient for each shift position is computed. The displacement corresponding to the maximum correlation is taken as the best estimate of registration error for each block pair. Subpixel shifts are estimated by a bi-quadratic interpolation of the correlation values surrounding the maximum correlation. To obtain statistical summaries for each band combination post processing of the block correlation results performed. The method results in estimates of registration error that are consistent with expectations.

  15. Isotropic band gaps and freeform waveguides observed in hyperuniform disordered photonic solids

    PubMed Central

    Man, Weining; Florescu, Marian; Williamson, Eric Paul; He, Yingquan; Hashemizad, Seyed Reza; Leung, Brian Y. C.; Liner, Devin Robert; Torquato, Salvatore; Chaikin, Paul M.; Steinhardt, Paul J.

    2013-01-01

    Recently, disordered photonic media and random textured surfaces have attracted increasing attention as strong light diffusers with broadband and wide-angle properties. We report the experimental realization of an isotropic complete photonic band gap (PBG) in a 2D disordered dielectric structure. This structure is designed by a constrained optimization method, which combines advantages of both isotropy due to disorder and controlled scattering properties due to low-density fluctuations (hyperuniformity) and uniform local topology. Our experiments use a modular design composed of Al2O3 walls and cylinders arranged in a hyperuniform disordered network. We observe a complete PBG in the microwave region, in good agreement with theoretical simulations, and show that the intrinsic isotropy of this unique class of PBG materials enables remarkable design freedom, including the realization of waveguides with arbitrary bending angles impossible in photonic crystals. This experimental verification of a complete PBG and realization of functional defects in this unique class of materials demonstrate their potential as building blocks for precise manipulation of photons in planar optical microcircuits and has implications for disordered acoustic and electronic band gap materials. PMID:24043795

  16. Angular dependent XPS study of surface band bending on Ga-polar n-GaN

    NASA Astrophysics Data System (ADS)

    Huang, Rong; Liu, Tong; Zhao, Yanfei; Zhu, Yafeng; Huang, Zengli; Li, Fangsen; Liu, Jianping; Zhang, Liqun; Zhang, Shuming; Dingsun, An; Yang, Hui

    2018-05-01

    Surface band bending and composition of Ga-polar n-GaN with different surface treatments were characterized by using angular dependent X-ray photoelectron spectroscopy. Upward surface band bending of varying degree was observed distinctly upon to the treatment methods. Besides the nitrogen vacancies, we found that surface states of oxygen-containing absorbates (O-H component) also contribute to the surface band bending, which lead the Fermi level pined at a level further closer to the conduction band edge on n-GaN surface. The n-GaN surface with lower surface band bending exhibits better linear electrical properties for Ti/GaN Ohmic contacts. Moreover, the density of positively charged surface states could be derived from the values of surface band bending.

  17. Extrapolation of earth-based solar irradiance measurements to exoatmospheric levels for broad-band and selected absorption-band observations

    NASA Technical Reports Server (NTRS)

    Reagan, John A.; Pilewskie, Peter A.; Scott-Fleming, Ian C.; Herman, Benjamin M.; Ben-David, Avishai

    1987-01-01

    Techniques for extrapolating earth-based spectral band measurements of directly transmitted solar irradiance to equivalent exoatmospheric signal levels were used to aid in determining system gain settings of the Halogen Occultation Experiment (HALOE) sunsensor being developed for the NASA Upper Atmosphere Research Satellite and for the Stratospheric Aerosol and Gas (SAGE) 2 instrument on the Earth Radiation Budget Satellite. A band transmittance approach was employed for the HALOE sunsensor which has a broad-band channel determined by the spectral responsivity of a silicon detector. A modified Langley plot approach, assuming a square-root law behavior for the water vapor transmittance, was used for the SAGE-2 940 nm water vapor channel.

  18. Ku-band ocean radar backscatter observations during SWADE

    NASA Technical Reports Server (NTRS)

    Nghiem, S. V.; Li, F. K.; Lou, S. H.; Neumann, G.

    1993-01-01

    We present results obtained by an airborne Ku-band scatterometer during the Surface Wave Dynamics Experiment (SWADE). The specific objective of this study is to improve our understanding of the relationship between ocean radar backscatter and near surface winds. The airborne scatterometer, NUSCAT, was flown on the NASA Ames C-130 over an instrumented oceanic area near 37 deg N and 74 deg W. A total of 10 flights from 27 Feb. to 9 Mar. 1991 were conducted. Radar backscatter at incidence angles of 0 to 60 deg were obtained. For each incidence angle, the NUSCAT antenna was azimuthally scanned in multiple complete circles to measure the azimuthal backscatter modulations. Both horizontal and vertical polarization backscatter measurements were made. In some of the flights, the cross-polarization backscatter was measured as well. Internal calibrations were carried out throughout each of the flights. Preliminary results indicate that the radar was stable to +/-0.3 dB for each flight. In this paper, we present studies of the backscatter measurements over several crossings of the Gulf Stream. In these crossings, large air-sea temperature differences were encountered and substantial changes in the radar cross section were observed. We summarize the observations and compare them to the changes of several wind variables across the Gulf Stream boundary. In one of the flights, the apparent wind near the cold side of the Gulf Stream was very low (less than 3 m/s). The behavior of the radar cross sections at such low wind speeds and a comparison with models are presented. A case study of the effects of swell on the absolute cross section and the azimuthal modulation pattern is presented. Significant wave heights larger than m were observed during SWADE. The experimentally observed effects of the swell on the radar backscatter are discussed. The effects are used to assess the uncertainties in wind retrieval due to underlying waves. A summary of azimuthal modulation from our ten

  19. Terra MODIS Band 27 Electronic Crosstalk Effect and Its Removal

    NASA Technical Reports Server (NTRS)

    Sun, Junqiang; Xiong, Xiaoxiong; Madhavan, Sriharsha; Wenny, Brian

    2012-01-01

    The MODerate-resolution Imaging Spectroradiometer (MODIS) is one of the primary instruments in the NASA Earth Observing System (EOS). The first MODIS instrument was launched in December, 1999 on-board the Terra spacecraft. MODIS has 36 bands, covering a wavelength range from 0.4 micron to 14.4 micron. MODIS band 27 (6.72 micron) is a water vapor band, which is designed to be insensitive to Earth surface features. In recent Earth View (EV) images of Terra band 27, surface feature contamination is clearly seen and striping has become very pronounced. In this paper, it is shown that band 27 is impacted by electronic crosstalk from bands 28-30. An algorithm using a linear approximation is developed to correct the crosstalk effect. The crosstalk coefficients are derived from Terra MODIS lunar observations. They show that the crosstalk is strongly detector dependent and the crosstalk pattern has changed dramatically since launch. The crosstalk contributions are positive to the instrument response of band 27 early in the mission but became negative and much larger in magnitude at later stages of the mission for most detectors of the band. The algorithm is applied to both Black Body (BB) calibration and MODIS L1B products. With the crosstalk effect removed, the calibration coefficients of Terra MODIS band 27 derived from the BB show that the detector differences become smaller. With the algorithm applied to MODIS L1B products, the Earth surface features are significantly removed and the striping is substantially reduced in the images of the band. The approach developed in this report for removal of the electronic crosstalk effect can be applied to other MODIS bands if similar crosstalk behaviors occur.

  20. Precipitation Estimation Using L-Band and C-Band Soil Moisture Retrievals

    NASA Technical Reports Server (NTRS)

    Koster, Randal D.; Brocca, Luca; Crow, Wade T.; Burgin, Mariko S.; De Lannoy, Gabrielle J. M.

    2016-01-01

    An established methodology for estimating precipitation amounts from satellite-based soil moisture retrievals is applied to L-band products from the Soil Moisture Active Passive (SMAP) and Soil Moisture and Ocean Salinity (SMOS) satellite missions and to a C-band product from the Advanced Scatterometer (ASCAT) mission. The precipitation estimates so obtained are evaluated against in situ (gauge-based) precipitation observations from across the globe. The precipitation estimation skill achieved using the L-band SMAP and SMOS data sets is higher than that obtained with the C-band product, as might be expected given that L-band is sensitive to a thicker layer of soil and thereby provides more information on the response of soil moisture to precipitation. The square of the correlation coefficient between the SMAP-based precipitation estimates and the observations (for aggregations to approximately100 km and 5 days) is on average about 0.6 in areas of high rain gauge density. Satellite missions specifically designed to monitor soil moisture thus do provide significant information on precipitation variability, information that could contribute to efforts in global precipitation estimation.

  1. Automated coregistration of MTI spectral bands

    NASA Astrophysics Data System (ADS)

    Theiler, James P.; Galbraith, Amy E.; Pope, Paul A.; Ramsey, Keri A.; Szymanski, John J.

    2002-08-01

    In the focal plane of a pushbroom imager, a linear array of pixels is scanned across the scene, building up the image one row at a time. For the Multispectral Thermal Imager (MTI), each of fifteen different spectral bands has its own linear array. These arrays are pushed across the scene together, but since each band's array is at a different position on the focal plane, a separate image is produced for each band. The standard MTI data products (LEVEL1B_R_COREG and LEVEL1B_R_GEO) resample these separate images to a common grid and produce coregistered multispectral image cubes. The coregistration software employs a direct ``dead reckoning' approach. Every pixel in the calibrated image is mapped to an absolute position on the surface of the earth, and these are resampled to produce an undistorted coregistered image of the scene. To do this requires extensive information regarding the satellite position and pointing as a function of time, the precise configuration of the focal plane, and the distortion due to the optics. These must be combined with knowledge about the position and altitude of the target on the rotating ellipsoidal earth. We will discuss the direct approach to MTI coregistration, as well as more recent attempts to tweak the precision of the band-to-band registration using correlations in the imagery itself.

  2. Dust bands in the asteroid belt

    NASA Technical Reports Server (NTRS)

    Sykes, Mark V.; Greenberg, Richard; Dermott, Stanley F.; Nicholson, Philip D.; Burns, Joseph A.

    1989-01-01

    This paper describes the original IRAS observations leading to the discovery of the three dust bands in the asteroid belt and the analysis of data. Special attention is given to an analytical model of the dust band torus and to theories concerning the origin of the dust bands, with special attention given to the collisional equilibrium (asteroid family), the nonequilibrium (random collision), and the comet hypotheses of dust-band origin. It is noted that neither the equilibrium nor nonequilibrium models, as currently formulated, present a complete picture of the IRAS dust-band observations.

  3. Extrapolation of Earth-based solar irradiance measurements to exoatmospheric levels for broad-band and selected absorption-band observations

    NASA Technical Reports Server (NTRS)

    Reagan, J. A.; Pilewskie, P. A.; Scott-Fleming, I. C.; Hermann, B. M.

    1986-01-01

    Techniques for extrapolating Earth-based spectral band measurements of directly transmitted solar irradiance to equivalent exoatmospheric signal levels were used to aid in determining system gain settings of the Halogen Occultation Experiment (HALOE) sunsensor system being developed for the NASA Upper Atmosphere Research Satellite and for the Stratospheric Aerosol and Gas (SAGE) 2 instrument on the Earth Radiation Budget Satellite. A band transmittance approach was employed for the HALOE sunsensor which has a broad-band channel determined by the spectral responsivity of a silicon detector. A modified Langley plot approach, assuming a square-root law behavior for the water vapor transmittance, was used for the SAGE-2 940 nm water vapor channel.

  4. Wideband Motion Control by Position and Acceleration Input Based Disturbance Observer

    NASA Astrophysics Data System (ADS)

    Irie, Kouhei; Katsura, Seiichiro; Ohishi, Kiyoshi

    The disturbance observer can observe and suppress the disturbance torque within its bandwidth. Recent motion systems begin to spread in the society and they are required to have ability to contact with unknown environment. Such a haptic motion requires much wider bandwidth. However, since the conventional disturbance observer attains the acceleration response by the second order derivative of position response, the bandwidth is limited due to the derivative noise. This paper proposes a novel structure of a disturbance observer. The proposed disturbance observer uses an acceleration sensor for enlargement of bandwidth. Generally, the bandwidth of an acceleration sensor is from 1Hz to more than 1kHz. To cover DC range, the conventional position sensor based disturbance observer is integrated. Thus, the performance of the proposed Position and Acceleration input based disturbance observer (PADO) is superior to the conventional one. The PADO is applied to position control (infinity stiffness) and force control (zero stiffness). The numerical and experimental results show viability of the proposed method.

  5. Weekly Gridded Aquarius L-band Radiometer-Scatterometer Observations and Salinity Retrievals over the Polar Regions - Part 2: Initial Product Analysis

    NASA Technical Reports Server (NTRS)

    Brucker, L.; Dinnat, E. P.; Koenig, L. S.

    2014-01-01

    Following the development and availability of Aquarius weekly polar-gridded products, this study presents the spatial and temporal radiometer and scatterometer observations at L band (frequency1.4 GHz) over the cryosphere including the Greenland and Antarctic ice sheets, sea ice in both hemispheres, and over sub-Arctic land for monitoring the soil freeze-thaw state. We provide multiple examples of scientific applications for the L-band data over the cryosphere. For example, we show that over the Greenland Ice Sheet, the unusual 2012 melt event lead to an L-band brightness temperature (TB) sustained decrease of 5 K at horizontal polarization. Over the Antarctic ice sheet, normalized radar cross section (NRCS) observations recorded during ascending and descending orbits are significantly different, highlighting the anisotropy of the ice cover. Over sub-Arctic land, both passive and active observations show distinct values depending on the soil physical state (freeze-thaw). Aquarius sea surface salinity (SSS) retrievals in the polar waters are also presented. SSS variations could serve as an indicator of fresh water input to the ocean from the cryosphere, however the presence of sea ice often contaminates the SSS retrievals, hindering the analysis. The weekly grided Aquarius L-band products used a redistributed by the US Snow and Ice Data Center at http:nsidc.orgdataaquariusindex.html, and show potential for cryospheric studies.

  6. Exact nonparametric confidence bands for the survivor function.

    PubMed

    Matthews, David

    2013-10-12

    A method to produce exact simultaneous confidence bands for the empirical cumulative distribution function that was first described by Owen, and subsequently corrected by Jager and Wellner, is the starting point for deriving exact nonparametric confidence bands for the survivor function of any positive random variable. We invert a nonparametric likelihood test of uniformity, constructed from the Kaplan-Meier estimator of the survivor function, to obtain simultaneous lower and upper bands for the function of interest with specified global confidence level. The method involves calculating a null distribution and associated critical value for each observed sample configuration. However, Noe recursions and the Van Wijngaarden-Decker-Brent root-finding algorithm provide the necessary tools for efficient computation of these exact bounds. Various aspects of the effect of right censoring on these exact bands are investigated, using as illustrations two observational studies of survival experience among non-Hodgkin's lymphoma patients and a much larger group of subjects with advanced lung cancer enrolled in trials within the North Central Cancer Treatment Group. Monte Carlo simulations confirm the merits of the proposed method of deriving simultaneous interval estimates of the survivor function across the entire range of the observed sample. This research was supported by the Natural Sciences and Engineering Research Council (NSERC) of Canada. It was begun while the author was visiting the Department of Statistics, University of Auckland, and completed during a subsequent sojourn at the Medical Research Council Biostatistics Unit in Cambridge. The support of both institutions, in addition to that of NSERC and the University of Waterloo, is greatly appreciated.

  7. Improvement of the Database on the 1.13-microns Band of Water Vapor

    NASA Technical Reports Server (NTRS)

    Giver, Lawrence P.; Schwenke, David W.; Chackerian, Charles, Jr.; Varanasi, Prasad; Freedman, Richard S.; Gore, Warren J. (Technical Monitor)

    2000-01-01

    Corrections have recently been reported (Giver et al.) on the short-wave (visible and near-infrared) line intensities of water vapor that were catalogued in the spectroscopic database known as HITRAN. These updates have been posted on www.hitran.com, and are being used to reanalyze the polar stratospheric absorption in the 0.94 microns band as observed in POAM. We are currently investigating additional improvement in the 1.13 microns band using data obtained by us with an absorption path length of 1.107 km and 4 torr of water vapor and the ab initio line list of Partridge and Schwenke (needs ref). We are proposing the following four types of improvement of the HITRAN database in this region: 1) HITRAN has nearly 200 lines in this region without proper assignments of rotational quantum levels. Nearly all of them can now be assigned. 2) We have measured positions of the observable H2O-17 and H2O-18 lines. These lines in HITRAN currently have approximate positions based upon rather aged computations. 3) Some additional lines are observed and assigned which should be included in the database. 4) Corrections are necessary for the lower state energies E" for the HITRAN lines of the 121-010 "hot" band.

  8. The outflow structure of GW170817 from late-time broad-band observations

    NASA Astrophysics Data System (ADS)

    Troja, E.; Piro, L.; Ryan, G.; van Eerten, H.; Ricci, R.; Wieringa, M. H.; Lotti, S.; Sakamoto, T.; Cenko, S. B.

    2018-07-01

    We present our broad-band study of GW170817 from radio to hard X-rays, including NuSTAR and Chandra observations up to 165 d after the merger, and a multimessenger analysis including LIGO constraints. The data are compared with predictions from a wide range of models, providing the first detailed comparison between non-trivial cocoon and jet models. Homogeneous and power-law shaped jets, as well as simple cocoon models are ruled out by the data, while both a Gaussian shaped jet and a cocoon with energy injection can describe the current data set for a reasonable range of physical parameters, consistent with the typical values derived from short GRB afterglows. We propose that these models can be unambiguously discriminated by future observations measuring the post-peak behaviour, with Fν ∝ t˜-1.0 for the cocoon and Fν∝ t˜-2.5 for the jet model.

  9. Shear-band thickness and shear-band cavities in a Zr-based metallic glass

    DOE PAGES

    Liu, C.; Roddatis, V.; Kenesei, P.; ...

    2017-08-14

    Strain localization into shear bands in metallic glasses is typically described as a mechanism that occurs at the nano-scale, leaving behind a shear defect with a thickness of 10–20 nm. Here we sample the structure of a single system-spanning shear band that has carried all plastic flow with high-angle annular dark field scanning transmission electron microscopy (HAADF-STEM) and high-energy x-ray tomography (XRT). It is found that the shear-band thickness and the density change relative to the matrix sensitively depend on position along the shear band. A wide distribution of shear-band thickness (10 nm–210 nm) and density change (–1% to –12%)more » is revealed. There is no obvious correlation between shear-band thickness and density change, but larger thicknesses correspond typically to higher density changes. More than 100 micron-size shear-band cavities were identified on the shear-band plane, and their three-dimensional arrangement suggests a strongly fluctuating local curvature of the shear plane. As a result, these findings urge for a more complex view of a shear band than a simple nano-scale planar defect.« less

  10. Shear-band thickness and shear-band cavities in a Zr-based metallic glass

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Liu, C.; Roddatis, V.; Kenesei, P.

    Strain localization into shear bands in metallic glasses is typically described as a mechanism that occurs at the nano-scale, leaving behind a shear defect with a thickness of 10–20 nm. Here we sample the structure of a single system-spanning shear band that has carried all plastic flow with high-angle annular dark field scanning transmission electron microscopy (HAADF-STEM) and high-energy x-ray tomography (XRT). It is found that the shear-band thickness and the density change relative to the matrix sensitively depend on position along the shear band. A wide distribution of shear-band thickness (10 nm–210 nm) and density change (–1% to –12%)more » is revealed. There is no obvious correlation between shear-band thickness and density change, but larger thicknesses correspond typically to higher density changes. More than 100 micron-size shear-band cavities were identified on the shear-band plane, and their three-dimensional arrangement suggests a strongly fluctuating local curvature of the shear plane. As a result, these findings urge for a more complex view of a shear band than a simple nano-scale planar defect.« less

  11. Observations of silicate reststrahlen bands in lunar infrared spectra

    NASA Technical Reports Server (NTRS)

    Potter, A. E., Jr.; Morgan, T. H.

    1982-01-01

    Thermal emission spectra of three lunar sites (Apollo 11, Descartes Formation, and Tycho central peak) are measured in the 8-14 micron spectral range. Transmission and instrument effects are accounted for by forming ratios of the Descartes and Tycho spectra to the Apollo 11 spectrum. The ratio spectra are compared with ratios of published laboratory spectra of returned lunar samples and also with ratio spectra calculated using the Aronson-Emslie (1975) model. The comparisons show pyroxene bands in the Descartes ratio spectrum and plagioclase bands in the Tycho ratio spectrum. The Tycho spectrum is found to be consistent with the existence of fine plagioclase dust (approximately 1 micron) at the rock surface and a higher-than-usual sodium content of the plagioclase.

  12. Thematic mapper studies band correlation analysis

    NASA Technical Reports Server (NTRS)

    Ungar, S. G.; Kiang, R.

    1976-01-01

    Spectral data representative of thematic mapper candidate bands 1 and 3 to 7 were obtained by selecting appropriate combinations of bands from the JSC 24 channel multispectral scanner. Of all the bands assigned, only candidate bands 4 (.74 mu to .80 mu) and 5 (.80 mu to .91 mu) showed consistently high intercorrelation from region to region and time to time. This extremely high correlation persisted when looking at the composite data set in a multitemporal, multilocation domain. The GISS investigations lend positive confirmation to the hypothesis, that TM bands 4 and 5 are redundant.

  13. "Fullerene-like" Raman bands in UHP metamorphic diamonds: Metastable intermediate phases for diamond formation

    NASA Astrophysics Data System (ADS)

    Harada, Y.; Igarashi, M.; Hashiguchi, Y.; Ogasawara, Y.

    2011-12-01

    Mysterious Raman bands at 1430-1480 cm-1 suggesting carbon (or carbon-bearing) species have been discovered in UHP metamorphic microdiamonds entirely enclosed in dolomite marble from Kokchetav Massif (Igarashi et al., 2011). Such Raman bands first discovered at some domains in a T-type (see Ishida et al., 2003) diamond in dolomite marble in 2005, but we have not reported this because of the possibility of misidentification by contamination. Later, similar bands were also found in the rim and the core of S-type and R-type. The relative intensities of these Raman bands to diamond (at 1332 cm-1) were 10-40 % in average (max. 90-110 %) and FWHMs are broad (25-45 cm-1). The possibility of the appearance of these Raman bands was low. As we used ordinary polished thin sections (thickness: 25 μm) and the organic materials used in thin section making have Raman bands at ca. 1450 cm-1, we carefully examined observed Raman spectra and the positions of the source materials of these bands to exclude the possibility of contaminations. Examined microdiamond grains are entirely enclosed in the host garnet, and no crack was observed in the host. We conducted 2D Raman mappings at different depths with 2 μm intervals. The result showed that the domains having these Raman bands were located within diamond grains and limited area (1-3 μm). These bands were never detected from outside diamond grains (e.g., host garnet). Thus, the unknown Raman bands at 1430-1480 cm-1 were attributed to some materials inside microdiamonds entirely included in the host garnet. The possibility of contamination was denied. Recently, we found similar Raman bands in the microdiamonds in garnet in Grt-Bt gneiss. Examined microdiamonds are entirely enclosed in garnet grain and no extra phase observed near laser spots in these microdiamond grains under an optical microscope. The Raman bands at 1430-1480 cm-1 were found from 4 microdiamond grains. The peak positions and FWHMs of these bands were as follows: (a

  14. Are TiC Grains a Carrier of the 21 Micron Emission Band Observed around Post-Asymptotic Giant Branch Objects?

    NASA Astrophysics Data System (ADS)

    Chigai, Takeshi; Yamamoto, Tetsuo; Kaito, Chihiro; Kimura, Yuki

    2003-04-01

    The carrier of the 21 μm band observed in post-asymptotic giant branch (post-AGB) stars is examined. We analyze the infrared spectra of the TiC clusters measured by von Helden et al. in 2000 and determine the absorption efficiency Q in the 21 μm band. Using Q, we estimate the Ti/Si abundance ratios needed to realize the flux ratios of the 21 and 11 μm emission observed in the infrared spectra of the post-AGB stars exhibiting both 21 and 11 μm emission. In view of the nature of the TiC condensation by which TiC grains are quickly mantled by graphite, we calculate the emission spectra of the graphite-coated TiC grains and other possible types of core-mantle grains and compare with the observed spectra. Both the abundance and condensation considerations strongly suggest that TiC is an implausible carrier of the observed infrared 21 μm feature around carbon-rich post-AGB stars.

  15. Observations of the initial stages of colloidal band formation

    NASA Astrophysics Data System (ADS)

    Li, Yanrong; Tagawa, Yoshiyuki; Yee, Andrew; Yoda, Minami

    2017-11-01

    A number of studies have shown that particles suspended in a conducting fluid near a wall are subject to wall-normal repulsive ``lift'' forces, even in the absence of interparticle interactions, in a flowing suspension. Evanescent-wave visualizations have shown that colloidal particles in a dilute (volume fractions <0.4%) suspension are instead attracted to the wall when the suspension is driven through 30 μm deep channels by a pressure gradient and an electric field when the resulting combined Poiseuille and electroosmotic (EO) flow are in opposite direction, i.e., ``counterflow,'' although the particles and channel walls both have negative zeta-potentials. Above a minimum ``threshold'' electric field magnitude |Emin | , the particles assemble into dense ``bands'' with cross-sectional dimensions of a few μm and length comparable to that of the channel (i.e., a few cm). The results suggest that the threshold field |Emin | is large enough so that there is a region of ``reverse'' flow, along the direction of the EO flow, near the wall. Visualization of a large segment of the channel (>300 hydraulic diameters) at frame rates as great as 1 kHz is used to determine banding maps for a variety of dilute colloidal suspensions and to investigate the initial stages of band formation over a wide range of flow conditions. Supported by US Army Research Office.

  16. VizieR Online Data Catalog: TrES-2b multi-band transit observations (Mislis+, 2010)

    NASA Astrophysics Data System (ADS)

    Mislis, D.; Schroeter, S.; Schmitt, J. H. M. M.; Cordes, O.; Reif, K.

    2010-02-01

    The OLT data were taken on 11 April 2009 using a 3Kx3K CCD with a 1x1 FOV and an I-band filter as in our previous observing run (Paper I, Mislis & Schmitt, 2009, Cat. ). The Calar Alto data were taken on 28 May 2009 using BUSCA and the 2.2m telescope. (1 data file).

  17. Observations of Radar Backscatter at Ku and C Bands in the Presence of Large Waves during the Surface Wave Dynamics Experiment

    NASA Technical Reports Server (NTRS)

    Nghiem, S. V.; Li, Fuk K.; Lou, Shu-Hsiang; Neumann, Gregory; McIntosh, Robert E.; Carson, Steven C.; Carswell, James R.; Walsh, Edward J.; Donelan, Mark A.; Drennan, William M.

    1995-01-01

    Ocean radar backscatter in the presence of large waves is investigated using data acquired with the Jet Propulsion Laboratory NUSCAT radar at Ku band for horizontal and vertical polarizations and the University of Massachusetts CSCAT radar at C band for vertical polarization during the Surface Wave Dynamics Experiment. Off-nadir backscatter data of ocean surfaces were obtained in the presence of large waves with significant wave height up to 5.6 m. In moderate-wind cases, effects of large waves are not detectable within the measurement uncertainty and no noticeable correlation between backscatter coefficients and wave height is found. Under high-wave light-wind conditions, backscatter is enhanced significantly at large incidence angles with a weaker effect at small incidence angles. Backscatter coefficients in the wind speed range under consideration are compared with SASS-2 (Ku band), CMOD3-H1 (C band), and Plant's model results which confirm the experimental observations. Variations of the friction velocity, which can give rise to the observed backscatter behaviors in the presence of large waves, are presented.

  18. First Results of Exoplanet Observations with the Gran Telescopio Canarias: Narrow-Band Transit Photometry Capable of Detecting Super-Earth-size Planets

    NASA Astrophysics Data System (ADS)

    Ford, Eric B.; Colon, K. D.; Blake, C.; Lee, B.; Mahadevan, S.

    2010-01-01

    We present the first exoplanet observations from the Gran Telescopio Canarias (GTC) using the OSIRIS tunable filter imager. Our narrow-band transit follow-up observations set a new record for ground-based, narrow-band photometric precision of an exoplanet transit. The demonstrated precision would allow the detection of a transiting super-Earth-sized planet at near-infrared wavelengths. Such high-precision follow-up observations could significantly improve measurements of the size and orbit of transiting super-Earth and Earth-like planets to be discovered by the CoRoT and Kepler space missions (Colon & Ford 2009). OSIRIS is one of two first light instruments for the GTC and features a tunable filter imaging mode. We observed the planet's host star along with several nearby reference stars during each transit, rapidly alternating observations between multiple narrow band-passes. The GTC's large aperture results in small photon noise and minimal scintillation noise, so care must be taken to minimize other potential systematic noise sources. The use of a narrow bandpass (2nm) reduces the effects of differential extinction, and we chose bandpasses that minimize atmospheric absorption and variability. We measure the flux of the target star relative to an ensemble of reference stars, using an aperture photometry algorithm adapted to allow for: 1) the center of the band-pass varying across the field and resulting in sky rings, and 2) a significant defocus to reduce flat fielding uncertainties and increase observing efficiency. We present results from the first tunable filter observations of an exoplanet transit and outline the exciting prospects for future GTC/OSIRIS observations to study super-Earth planets and the atmospheres of giant planets via occultation photometry. Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma.

  19. The Potential for a Ka-band (32 GHz) Worldwide VLBI Network

    NASA Astrophysics Data System (ADS)

    Jacobs, C. S.; Bach, U.; Colomer, F.; Garcá-Miró, C.; Gómez-González, J.; Gulyaev, S.; Horiuchi, S.; Ichikawa, R.; Kraus, A.; Kronschnabl, G.; López-Fernández, J. A.; Lovell, J.; Majid, W.; T; Natusch; Neidhardt, A.; Phillips, C.; Porcas, R.; Romero-Wolf, A.; Saldana, L.; Schreiber, U.; Sotuela, I.; Takeuchi, H.; Trinh, J.; Tzioumis, A.; de Vincente, P.; Zharov, V.

    2012-12-01

    Ka-band (32 GHz, 9 mm) Very Long Baseline Interferometric (VLBI) networking has now begun and has tremendous potential for expansion over the next few years. Ka-band VLBI astrometry from NASA's Deep Space Network has already developed a catalog of 470 observable sources with highly accurate positions. Now, several antennas worldwide are planning or are considering adding Ka-band VLBI capability. Thus, there is now an opportunity to create a worldwide Ka-band network with potential for high resolution imaging and astrometry. With baselines approaching a Giga-lambda, a Ka-band network would be able to probe source structure at the nano-radian (200 as) level (100X better than Hubble) and thus gain insight into the astrophysics of the most compact regions of emission in active galactic nuclei. We discuss the advantages of Ka-band, show the known sources and candidates, simulate projected baseline (uv) coverage, and discuss potential radio frequency feeds. The combination of these elements demonstrates the feasibility of a worldwide Ka network within the next few years.

  20. The Potential for a Ka-band (32 GHz) Worldwide VLBI Network

    NASA Technical Reports Server (NTRS)

    Jacobs, C. S.; Bach, U.; Colomer, F.; Garcia-Miro, C.; Gomez-Gonzalez, J.; Gulyaev, S.; Horiuchi, S.; Ichikawa, R.; Kraus, A.; Kronschnabl, G.; hide

    2012-01-01

    Ka-band (32 GHz, 9mm) Very Long Baseline Interferometric (VLBI) networking has now begun and has tremendous potential for expansion over the next few years. Ka-band VLBI astrometry from NASA's Deep Space Network has already developed a catalog of 470 observable sources with highly accurate positions. Now, several antennas worldwide are planning or are considering adding Ka-band VLBI capability. Thus, there is now an opportunity to create a worldwide Ka-band network with potential for high resolution imaging and astrometry. With baselines approaching a Giga-lambda, a Ka-band network would be able to probe source structure at the nano-radian (200 as) level ( 100X better than Hubble) and thus gain insight into the astrophysics of the most compact regions of emission in active galactic nuclei. We discuss the advantages of Ka-band, show the known sources and candidates, simulate projected baseline (uv) coverage, and discuss potential radio frequency feeds. The combination of these elements demonstrates the feasibility of a worldwide Ka network within the next few years!

  1. Generation of Multi-band Chorus by Lower Band Cascade in the Earth's Magnetosphere

    NASA Astrophysics Data System (ADS)

    Gao, X.; Lu, Q.; Chen, L.; Bortnik, J.; Li, W.; Wang, S.

    2016-12-01

    Chorus waves are intense electromagnetic whistler-mode emissions in the magnetosphere, typically falling into two distinct frequency bands: a lower band (0.1-0.5fce) and an upper band (0.5-0.8fce) with a power gap at about 0.5fce. In this letter, with the THEMIS satellite, we observed two special chorus events, which are called as multi-band chorus because upper band chorus is located at harmonics of lower band chorus. We propose a new potential generation mechanism for multi-band chorus, which is called as lower band cascade. In this scenario, a density mode with a frequency equal to that of lower band chorus is caused by the ponderomotive effect (inhomogeneity of the electric amplitude) along the wave vector, and then upper band chorus with the frequency twice that of lower band chorus is generated through wave-wave couplings between lower band chorus and the density mode. The mechanism provides a new insight into the evolution of whistler-mode chorus in the Earth's magnetosphere.

  2. PCR-based verification of positive rapid diagnostic tests for intestinal protozoa infections with variable test band intensity.

    PubMed

    Becker, Sören L; Müller, Ivan; Mertens, Pascal; Herrmann, Mathias; Zondie, Leyli; Beyleveld, Lindsey; Gerber, Markus; du Randt, Rosa; Pühse, Uwe; Walter, Cheryl; Utzinger, Jürg

    2017-10-01

    Stool-based rapid diagnostic tests (RDTs) for pathogenic intestinal protozoa (e.g. Cryptosporidium spp. and Giardia intestinalis) allow for prompt diagnosis and treatment in resource-constrained settings. Such RDTs can improve individual patient management and facilitate population-based screening programmes in areas without microbiological laboratories for confirmatory testing. However, RDTs are difficult to interpret in case of 'trace' results with faint test band intensities and little is known about whether such ambiguous results might indicate 'true' infections. In a longitudinal study conducted in poor neighbourhoods of Port Elizabeth, South Africa, a total of 1428 stool samples from two cohorts of schoolchildren were examined on the spot for Cryptosporidium spp. and G. intestinalis using an RDT (Crypto/Giardia DuoStrip; Coris BioConcept). Overall, 121 samples were positive for G. intestinalis and the RDT suggested presence of cryptosporidiosis in 22 samples. After a storage period of 9-10 months in cohort 1 and 2-3 months in cohort 2, samples were subjected to multiplex PCR (BD Max™ Enteric Parasite Panel, Becton Dickinson). Ninety-three percent (112/121) of RDT-positive samples for G. intestinalis were confirmed by PCR, with a correlation between RDT test band intensity and quantitative pathogen load present in the sample. For Cryptosporidium spp., all positive RDTs had faintly visible lines and these were negative on PCR. The performance of the BD Max™ PCR was nearly identical in both cohorts, despite the prolonged storage at disrupted cold chain conditions in cohort 1. The Crypto/Giardia DuoStrip warrants further validation in communities with a high incidence of diarrhoea. Copyright © 2017 Elsevier B.V. All rights reserved.

  3. Broadening of effective photonic band gaps in biological chiral structures: From intrinsic narrow band gaps to broad band reflection spectra

    NASA Astrophysics Data System (ADS)

    Vargas, W. E.; Hernández-Jiménez, M.; Libby, E.; Azofeifa, D. E.; Solis, Á.; Barboza-Aguilar, C.

    2015-09-01

    Under normal illumination with non-polarized light, reflection spectra of the cuticle of golden-like and red Chrysina aurigans scarabs show a structured broad band of left-handed circularly polarized light. The polarization of the reflected light is attributed to a Bouligand-type left-handed chiral structure found through the scarab's cuticle. By considering these twisted structures as one-dimensional photonic crystals, a novel approach is developed from the dispersion relation of circularly polarized electromagnetic waves traveling through chiral media, to show how the broad band characterizing these spectra arises from an intrinsic narrow photonic band gap whose spectral position moves through visible and near-infrared wavelengths.

  4. Weekly gridded Aquarius L-band radiometer/scatterometer observations and salinity retrievals over the polar regions - Part 2: Initial product analysis

    NASA Astrophysics Data System (ADS)

    Brucker, L.; Dinnat, E. P.; Koenig, L. S.

    2014-05-01

    Following the development and availability of Aquarius weekly polar-gridded products, this study presents the spatial and temporal radiometer and scatterometer observations at L band (frequency ~1.4 GHz) over the cryosphere including the Greenland and Antarctic ice sheets, sea ice in both hemispheres, and over sub-Arctic land for monitoring the soil freeze/thaw state. We provide multiple examples of scientific applications for the L-band data over the cryosphere. For example, we show that over the Greenland Ice Sheet, the unusual 2012 melt event lead to an L-band brightness temperature (TB) sustained decrease of ~5 K at horizontal polarization. Over the Antarctic ice sheet, normalized radar cross section (NRCS) observations recorded during ascending and descending orbits are significantly different, highlighting the anisotropy of the ice cover. Over sub-Arctic land, both passive and active observations show distinct values depending on the soil physical state (freeze/thaw). Aquarius sea surface salinity (SSS) retrievals in the polar waters are also presented. SSS variations could serve as an indicator of fresh water input to the ocean from the cryosphere, however the presence of sea ice often contaminates the SSS retrievals, hindering the analysis. The weekly grided Aquarius L-band products used are distributed by the US Snow and Ice Data Center at http://nsidc.org/data/aquarius/index.html , and show potential for cryospheric studies.

  5. An observation of LHR noise with banded structure by the sounding rocket S29 Barium-GEOS

    NASA Technical Reports Server (NTRS)

    Koskinen, H. E. J.; Holmgren, G.; Kintner, P. M.

    1982-01-01

    The measurement of electrostatic and obviously locally produced noise near the lower hybrid frequency made by the sounding rocket S29 Barium-GEOS is reported. The noise is strongly related to the spin of the rocket and reaches well below the local lower hybrid resonance frequency. Above the altitude of 300 km the noise shows banded structure roughly organized by the hydrogen cyclotron frequency. Simultaneously with the banded structure, a signal near the hydrogen cyclotron frequency is detected. This signal is also spin related. The characteristics of the noise suggest that it is locally generated by the rocket payload disturbing the plasma. If this interpretation is correct we expect plasma wave experiments on other spacecrafts, e.g., the space shuttle to observe similar phenomena.

  6. Towards an improved soil moisture retrieval for organic-rich soils from SMOS passive microwave L-band observations

    NASA Astrophysics Data System (ADS)

    Bircher, Simone; Richaume, Philippe; Mahmoodi, Ali; Mialon, Arnaud; Fernandez-Moran, Roberto; Wigneron, Jean-Pierre; Demontoux, François; Jonard, François; Weihermüller, Lutz; Andreasen, Mie; Rautiainen, Kimmo; Ikonen, Jaakko; Schwank, Mike; Drusch, Mattias; Kerr, Yann H.

    2017-04-01

    From the passive L-band microwave radiometer onboard the Soil Moisture and Ocean Salinity (SMOS) space mission global surface soil moisture data is retrieved every 2 - 3 days. Thus far, the empirical L-band Microwave Emission of the Biosphere (L-MEB) radiative transfer model applied in the SMOS soil moisture retrieval algorithm is exclusively calibrated over test sites in dry and temperate climate zones. Furthermore, the included dielectric mixing model relating soil moisture to relative permittivity accounts only for mineral soils. However, soil moisture monitoring over the higher Northern latitudes is crucial since these regions are especially sensitive to climate change. A considerable positive feedback is expected if thawing of these extremely organic soils supports carbon decomposition and release to the atmosphere. Due to differing structural characteristics and thus varying bound water fractions, the relative permittivity of organic material is lower than that of the most mineral soils at a given water content. This assumption was verified by means of L-band relative permittivity laboratory measurements of organic and mineral substrates from various sites in Denmark, Finland, Scotland and Siberia using a resonant cavity. Based on these data, a simple empirical dielectric model for organic soils was derived and implemented in the SMOS Soil Moisture Level 2 Prototype Processor (SML2PP). Unfortunately, the current SMOS retrieved soil moisture product seems to show unrealistically low values compared to in situ soil moisture data collected from organic surface layers in North America, Europe and the Tibetan Plateau so that the impact of the dielectric model for organic soils cannot really be tested. A simplified SMOS processing scheme yielding higher soil moisture levels has recently been proposed and is presently under investigation. Furthermore, recalibration of the model parameters accounting for vegetation and roughness effects that were thus far only

  7. Modeling L-band synthetic aperture radar observations through dielectric changes in soil moisture and vegetation over shrublands

    USDA-ARS?s Scientific Manuscript database

    L-band airborne synthetic aperture radar observations were made over California shrublands to better understand the effects by soil and vegetation parameters on backscatter. Temporal changes in radar backscattering coefficient (s0) of up to 3 dB were highly correlated to surface soil moisture but no...

  8. Morphologies of omega band auroras

    NASA Astrophysics Data System (ADS)

    Sato, Natsuo; Yukimatu, Akira Sessai; Tanaka, Yoshimasa; Hori, Tomoaki

    2017-08-01

    We examined the morphological signatures of 315 omega band aurora events observed using the Time History of Events and Macroscale Interactions during Substorm ground-based all-sky imager network over a period of 8 years. We find that omega bands can be classified into the following three subtypes: (1) classical (O-type) omega bands, (2) torch or tongue (T-type) omega bands, and (3) combinations of classical and torch or tongue (O/T-type) omega bands. The statistical results show that T-type bands occur the most frequently (45%), followed by O/T-type bands (35%) and O-type bands (18%). We also examined the morphologies of the omega bands during their formation, from the growth period to the declining period through the maximum period. Interestingly, the omega bands are not stable, but rather exhibit dynamic changes in shape, intensity, and motion. They grow from small-scale bumps (seeds) at the poleward boundary of preexisting east-west-aligned auroras, rather than via the rotation or shear motion of preexisting east-west-aligned auroras, and do not exhibit any shear motion during the periods of auroral activity growth. Furthermore, the auroral luminosity is observed to increase during the declining period, and the total time from the start of the growth period to the end of the declining period is found to be about 20 min. Such dynamical signatures may be important in determining the mechanism responsible for omega band formation.

  9. Inferring Land Surface Model Parameters for the Assimilation of Satellite-Based L-Band Brightness Temperature Observations into a Soil Moisture Analysis System

    NASA Technical Reports Server (NTRS)

    Reichle, Rolf H.; De Lannoy, Gabrielle J. M.

    2012-01-01

    The Soil Moisture and Ocean Salinity (SMOS) satellite mission provides global measurements of L-band brightness temperatures at horizontal and vertical polarization and a variety of incidence angles that are sensitive to moisture and temperature conditions in the top few centimeters of the soil. These L-band observations can therefore be assimilated into a land surface model to obtain surface and root zone soil moisture estimates. As part of the observation operator, such an assimilation system requires a radiative transfer model (RTM) that converts geophysical fields (including soil moisture and soil temperature) into modeled L-band brightness temperatures. At the global scale, the RTM parameters and the climatological soil moisture conditions are still poorly known. Using look-up tables from the literature to estimate the RTM parameters usually results in modeled L-band brightness temperatures that are strongly biased against the SMOS observations, with biases varying regionally and seasonally. Such biases must be addressed within the land data assimilation system. In this presentation, the estimation of the RTM parameters is discussed for the NASA GEOS-5 land data assimilation system, which is based on the ensemble Kalman filter (EnKF) and the Catchment land surface model. In the GEOS-5 land data assimilation system, soil moisture and brightness temperature biases are addressed in three stages. First, the global soil properties and soil hydraulic parameters that are used in the Catchment model were revised to minimize the bias in the modeled soil moisture, as verified against available in situ soil moisture measurements. Second, key parameters of the "tau-omega" RTM were calibrated prior to data assimilation using an objective function that minimizes the climatological differences between the modeled L-band brightness temperatures and the corresponding SMOS observations. Calibrated parameters include soil roughness parameters, vegetation structure parameters

  10. Positivity effect in healthy aging in observational but not active feedback-learning.

    PubMed

    Bellebaum, Christian; Rustemeier, Martina; Daum, Irene

    2012-01-01

    The present study investigated the impact of healthy aging on the bias to learn from positive or negative performance feedback in observational and active feedback learning. In active learning, a previous study had already shown a negative learning bias in healthy seniors older than 75 years, while no bias was found for younger seniors. However, healthy aging is accompanied by a 'positivity effect', a tendency to primarily attend to stimuli with positive valence. Based on recent findings of dissociable neural mechanisms in active and observational feedback learning, the positivity effect was hypothesized to influence older participants' observational feedback learning in particular. In two separate experiments, groups of young (mean age 27) and older participants (mean age 60 years) completed an observational or active learning task designed to differentially assess positive and negative learning. Older but not younger observational learners showed a significant bias to learn better from positive than negative feedback. In accordance with previous findings, no bias was found for active learning. This pattern of results is discussed in terms of differences in the neural underpinnings of active and observational learning from performance feedback.

  11. Accurate band-to-band registration of AOTF imaging spectrometer using motion detection technology

    NASA Astrophysics Data System (ADS)

    Zhou, Pengwei; Zhao, Huijie; Jin, Shangzhong; Li, Ningchuan

    2016-05-01

    This paper concerns the problem of platform vibration induced band-to-band misregistration with acousto-optic imaging spectrometer in spaceborne application. Registrating images of different bands formed at different time or different position is difficult, especially for hyperspectral images form acousto-optic tunable filter (AOTF) imaging spectrometer. In this study, a motion detection method is presented using the polychromatic undiffracted beam of AOTF. The factors affecting motion detect accuracy are analyzed theoretically, and calculations show that optical distortion is an easily overlooked factor to achieve accurate band-to-band registration. Hence, a reflective dual-path optical system has been proposed for the first time, with reduction of distortion and chromatic aberration, indicating the potential of higher registration accuracy. Consequently, a spectra restoration experiment using additional motion detect channel is presented for the first time, which shows the accurate spectral image registration capability of this technique.

  12. Examining the Displacement of Energy during Formation of Shear Bands

    NASA Astrophysics Data System (ADS)

    Hernandez, M.; Hilley, G. E.

    2011-12-01

    M.X. Hernandez, G. Hilley Department of Geological and Environmental Sciences, Stanford University, Stanford, CA This study has originated from an experimental (sandbox) setting that we have previously used to document the link between the kinematics and dynamics of deforming sand in the verge of frictional failure. Our initial experimental setting included a load control system that allowed us to track the changes in load, that when applied to the sand, deform and generate individual shear bands or localized faults. Over the course of earlier experiments, three cameras located at different positions outside the sandbox monitored the movement throughout the run. This current stage of analysis includes using computer programs such as QuickTime to create image sequences of the shear band formation, and Microsoft Excel to visually graph and plot each data sequence. This allows us to investigate the correlation between changes in work measured within our experiments, the construction of topography, slip along shear bands, and the creation of new shear bands. We observed that the measured load generally increased during the experiment to maintain a constant displacement rate as the sand wedge thickened and modeled topography increased. Superposed on this trend were periodic drops in load that appeared temporally coincident with the formation of shear bands in the sand. Using the time series of the loads applied during the experiment, changes in the position of the backstop over time, and the loads measured before, during, and after the time of each shear band formation, we are examining the fraction of the apples work that is absorbed by friction and shear band formation, and what fraction of the apples work is expended in increasing the potential energy of the thickening sand wedge. Our results indicate that before the formation of a continuous shear band, the rate of work done on the sand by the experimental apparatus decreases. This may suggest that once formed, work

  13. Observation of ν1+νn combination bands of the HOOO and DOOO radicals using infrared action spectroscopy

    NASA Astrophysics Data System (ADS)

    Derro, Erika L.; Sechler, Timothy D.; Murray, Craig; Lester, Marsha I.

    2008-06-01

    Hydrogen trioxy (HOOO) and its deuterated analog (DOOO) have been generated in a supersonic free-jet expansion through association of photolytically generated OH or OD and molecular oxygen. The radicals were detected using infrared action spectroscopy, a highly sensitive double resonance technique. Rotationally resolved spectra of combination bands of HOOO and DOOO comprising one quantum of OH or OD stretch (ν1) and one quantum of a lower frequency mode (ν1+νn where n=3-6), including H/DOO bend (ν3), OOO bend (ν4), central OO stretch (ν5), and H/DOOO torsion (ν6), have been observed and assigned to the trans conformer. All but one of these bands are accompanied by unstructured features which are tentatively assigned to the corresponding vibration of the cis conformer. In total, five additional bands of HOOO and four of DOOO have been recorded and assigned. These data represent the first gas-phase observation of the low-frequency modes of HOOO and DOOO and they are found to differ significantly from previous matrix studies and theoretical predictions. Accurate knowledge of the vibrational frequencies is crucial in assessing thermochemical properties of HOOO and present possible means of detection in the atmosphere.

  14. Evidence of chiral bands in even-even nuclei

    NASA Astrophysics Data System (ADS)

    Petrache, C. M.; Lv, B. F.; Astier, A.; Dupont, E.; Wang, Y. K.; Zhang, S. Q.; Zhao, P. W.; Ren, Z. X.; Meng, J.; Greenlees, P. T.; Badran, H.; Cox, D. M.; Grahn, T.; Julin, R.; Juutinen, S.; Konki, J.; Pakarinen, J.; Papadakis, P.; Partanen, J.; Rahkila, P.; Sandzelius, M.; Saren, J.; Scholey, C.; Sorri, J.; Stolze, S.; Uusitalo, J.; Cederwall, B.; Aktas, Ö.; Ertoprak, A.; Liu, H.; Matta, S.; Subramaniam, P.; Guo, S.; Liu, M. L.; Zhou, X. H.; Wang, K. L.; Kuti, I.; Timár, J.; Tucholski, A.; Srebrny, J.; Andreoiu, C.

    2018-04-01

    Evidence for chiral doublet bands has been observed for the first time in the even-even nucleus 136Nd. One chiral band was firmly established. Four other candidates for chiral bands were also identified, which can contribute to the realization of the multiple pairs of chiral doublet bands (M χ D ) phenomenon. The observed bands are investigated by the constrained and tilted axis cranking covariant density functional theory (TAC-CDFT). Possible configurations have been explored. The experimental energy spectra, angular momenta, and B (M 1 )/B (E 2 ) values for the assigned configurations are globally reproduced by TAC-CDFT. Calculated results support the chiral interpretation of the observed bands, which correspond to shapes with maximum triaxiality induced by different multiquasiparticle configurations in 136Nd.

  15. Weekly Gridded Aquarius L-band Radiometer-scatterometer Observations and Salinity Retrievals over the Polar Regions - Part 1: Product Description

    NASA Technical Reports Server (NTRS)

    Brucker, Ludovic; Dinnat, Emmanuel Phillippe; Koenig, Lora S.

    2014-01-01

    Passive and active observations at L band (frequency (is) approximately 1.4 GHz) from the Aquarius/SAC-D mission offer new capabilities to study the polar regions. Due to the lack of polar-gridded products, however, applications over the cryosphere have been limited. We present three weekly polar-gridded products of Aquarius data to improve our understanding of L-band observations of ice sheets, sea ice, permafrost, and the polar oceans. Additionally, these products intend to facilitate access to L-band data, and can be used to assist in algorithm developments. Aquarius data at latitudes higher than 50 degrees are averaged and gridded into weekly products of brightness temperature (TB), normalized radar cross section (NRCS), and sea surface salinity (SSS). Each grid cell also contains sea ice fraction, the standard deviation of TB, NRCS, and SSS, and the number of footprint observations collected during the seven-day cycle. The largest 3 dB footprint dimensions are 97 km×156 km and 74 km×122 km (along × across track) for the radiometers and scatterometer, respectively. The data is gridded to the Equal-Area Scalable Earth version 2.0 (EASE2.0) grid, with a grid cell resolution of 36 km. The data sets start in August 2011, with the first Aquarius observations and will be updated on a monthly basis following the release schedule of the Aquarius Level 2 data sets. The weekly gridded products are distributed by the US National Snow and Ice Data Center at http://nsidc.org/data/aquarius/index.html

  16. Airborne Remote Observations of L-Band Radio Frequency Interference and Implications for Satellite Missions

    NASA Technical Reports Server (NTRS)

    Laymon, Charles; Srinivasan, Karthik; Limaye, Ashutosh

    2011-01-01

    Passive remote sensing of the Earth s surface and atmosphere from space has significant importance in operational and research environmental studies, in particular for the scientific understanding, monitoring and prediction of climate change and its impacts. Passive remote sensing requires the measurement of naturally occurring radiations, usually of very low power levels, which contain essential information on the physical process under investigation. As such, these sensed radio frequency bands are a unique natural resource enabling space borne passive sensing of the atmosphere and the Earth s surface that deserves adequate allocation to the Earth Exploration Satellite Service and absolute protection from interference. Unfortunately, radio frequency interference (RFI) is an increasing problem for Earth remote sensing, particularly for passive observations of natural emissions. Because these natural signals tend to be very weak, even low levels of interference received by a passive sensor may degrade the fidelity of scientific data. The characteristics of RFI (low-level interference and radar-pulse noise) are not well known because there has been no systematic surveillance, spectrum inventory or mapping of RFI. While conducting a flight experiment over central Tennessee in May 2010, RFI, a concern for any instrument operating in the passive L band frequency, was observed across 16 subbands between 1402-1427 MHz. Such a survey provides rare characterization data from which to further develop mitigation technologies as well as to identify bandwidths to avoid in future sensor formulation.

  17. Observation of an electron band above the Fermi level in FeTe₀.₅₅Se₀.₄₅ from in-situ surface doping

    DOE PAGES

    Zhang, P.; Richard, P.; Xu, N.; ...

    2014-10-27

    We used in-situ potassium (K) evaporation to dope the surface of the iron-based superconductor FeTe₀.₅₅Se₀.₄₅. The systematic study of the bands near the Fermi level confirms that electrons are doped into the system, allowing us to tune the Fermi level of this material and to access otherwise unoccupied electronic states. In particular, we observe an electron band located above the Fermi level before doping that shares similarities with a small three-dimensional pocket observed in the cousin, heavily-electron-doped KFe₂₋ xSe₂ compound.

  18. N2 triplet band systems and atomic oxygen in the dayglow

    NASA Astrophysics Data System (ADS)

    Broadfoot, A. L.; Hatfield, D. B.; Anderson, E. R.; Stone, T. C.; Sandel, B. R.; Gardner, J. A.; Murad, E.; Knecht, D. J.; Pike, C. P.; Viereck, R. A.

    1997-06-01

    New spectrographic observations of the Earth's dayglow have been acquired by the Arizona Airglow Experiment (GLO) flown on the space shuttle. GLO is an imaging spectrograph that records simultaneous vertical profiles of prominent Earth limb emissions occurring at wavelengths between 115 and 900 nm. This study addresses the measured emissions from the N2 triplet states (first positive, second positive, and Vegard-Kaplan band systems) and their excitation by the local photoelectron flux. The triplet state population distributions modeled for aurora by Cartwright [1978] are modified for dayglow conditions by changing to a photoelectron-flux energy distribution and including resonance scattering by the first positive system. Modeled and observed intensities are in excellent agreement, in contrast to the well-studied auroral case. This work concentrates on dayglow conditions at 200 km altitude near the subsolar point. Parameters to infer the local photoelectron flux from the emission band intensities are provided. Several atomic oxygen dayglow emission features were analyzed to complement the N2 analysis. The photoelectron-excited O I(135.6, 777.4 nm) lines were found to be 3 to 4 times weaker than predicted while the O I(630.0, 844.6 nm) lines were in close agreement with the model prediction.

  19. VI-band follow-up observations of ultra-long-period Cepheid candidates in M31

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Ngeow, Chow-Choong; Yang, Michael Ting-Chang; Lin, Chi-Sheng

    2015-02-01

    The ultra-long-period Cepheids (ULPCs) are classical Cepheids with pulsation periods exceeding ≈80 days. The intrinsic brightness of ULPCs are ∼1 to ∼3 mag brighter than their shorter period counterparts. This makes them attractive in future distance scale work to derive distances beyond the limit set by the shorter period Cepheids. We have initiated a program to search for ULPCs in M31, using the single-band data taken from the Palomar Transient Factory, and identified eight possible candidates. In this work, we presented the VI-band follow-up observations of these eight candidates. Based on our VI-band light curves of these candidates and theirmore » locations in the color–magnitude diagram and the Period–Wesenheit diagram, we verify two candidates as being truly ULPCs. The six other candidates are most likely other kinds of long-period variables. With the two confirmed M31 ULPCs, we tested the applicability of ULPCs in distance scale work by deriving the distance modulus of M31. It was found to be μ{sub M31,ULPC}=24.30±0.76 mag. The large error in the derived distance modulus, together with the large intrinsic dispersion of the Period–Wesenheit (PW) relation and the small number of ULPCs in a given host galaxy, means that the question of the suitability of ULPCs as standard candles is still open. Further work is needed to enlarge the sample of calibrating ULPCs and reduce the intrinsic dispersion of the PW relation before re-considering ULPCs as suitable distance indicators.« less

  20. Fluctuation diamagnetism in two-band superconductors

    NASA Astrophysics Data System (ADS)

    Adachi, Kyosuke; Ikeda, Ryusuke

    2016-04-01

    Anomalously large fluctuation diamagnetism around the superconducting critical temperature has been recently observed in iron selenide (FeSe) [Kasahara et al. (unpublished)]. This indicates that superconducting fluctuations (SCFs) play a more significant role in FeSe, which supposedly has a two-band structure, than in the familiar single-band superconductors. Motivated by the data on FeSe, SCF-induced diamagnetism is examined in a two-band system, on the basis of a phenomenological approach with a Ginzburg-Landau functional. The obtained results indicate that the SCF-induced diamagnetism may be more enhanced than that in a single-band system due to the existence of two distinct fluctuation modes. Such enhancement of diamagnetism unique to a two-band system seems consistent with the large diamagnetism observed in FeSe, though still far from a quantitative agreement.

  1. Building blocks of topological quantum chemistry: Elementary band representations

    NASA Astrophysics Data System (ADS)

    Cano, Jennifer; Bradlyn, Barry; Wang, Zhijun; Elcoro, L.; Vergniory, M. G.; Felser, C.; Aroyo, M. I.; Bernevig, B. Andrei

    2018-01-01

    The link between chemical orbitals described by local degrees of freedom and band theory, which is defined in momentum space, was proposed by Zak several decades ago for spinless systems with and without time reversal in his theory of "elementary" band representations. In a recent paper [Bradlyn et al., Nature (London) 547, 298 (2017), 10.1038/nature23268] we introduced the generalization of this theory to the experimentally relevant situation of spin-orbit coupled systems with time-reversal symmetry and proved that all bands that do not transform as band representations are topological. Here we give the full details of this construction. We prove that elementary band representations are either connected as bands in the Brillouin zone and are described by localized Wannier orbitals respecting the symmetries of the lattice (including time reversal when applicable), or, if disconnected, describe topological insulators. We then show how to generate a band representation from a particular Wyckoff position and determine which Wyckoff positions generate elementary band representations for all space groups. This theory applies to spinful and spinless systems, in all dimensions, with and without time reversal. We introduce a homotopic notion of equivalence and show that it results in a finer classification of topological phases than approaches based only on the symmetry of wave functions at special points in the Brillouin zone. Utilizing a mapping of the band connectivity into a graph theory problem, we show in companion papers which Wyckoff positions can generate disconnected elementary band representations, furnishing a natural avenue for a systematic materials search.

  2. Efficient Band-to-Trap Tunneling Model Including Heterojunction Band Offset

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Gao, Xujiao; Huang, Andy; Kerr, Bert

    In this paper, we present an efficient band-to-trap tunneling model based on the Schenk approach, in which an analytic density-of-states (DOS) model is developed based on the open boundary scattering method. The new model explicitly includes the effect of heterojunction band offset, in addition to the well-known field effect. Its analytic form enables straightforward implementation into TCAD device simulators. It is applicable to all one-dimensional potentials, which can be approximated to a good degree such that the approximated potentials lead to piecewise analytic wave functions with open boundary conditions. The model allows for simulating both the electric-field-enhanced and band-offset-enhanced carriermore » recombination due to the band-to-trap tunneling near the heterojunction in a heterojunction bipolar transistor (HBT). Simulation results of an InGaP/GaAs/GaAs NPN HBT show that the proposed model predicts significantly increased base currents, due to the hole-to-trap tunneling enhanced by the emitter-base junction band offset. Finally, the results compare favorably with experimental observation.« less

  3. Efficient Band-to-Trap Tunneling Model Including Heterojunction Band Offset

    DOE PAGES

    Gao, Xujiao; Huang, Andy; Kerr, Bert

    2017-10-25

    In this paper, we present an efficient band-to-trap tunneling model based on the Schenk approach, in which an analytic density-of-states (DOS) model is developed based on the open boundary scattering method. The new model explicitly includes the effect of heterojunction band offset, in addition to the well-known field effect. Its analytic form enables straightforward implementation into TCAD device simulators. It is applicable to all one-dimensional potentials, which can be approximated to a good degree such that the approximated potentials lead to piecewise analytic wave functions with open boundary conditions. The model allows for simulating both the electric-field-enhanced and band-offset-enhanced carriermore » recombination due to the band-to-trap tunneling near the heterojunction in a heterojunction bipolar transistor (HBT). Simulation results of an InGaP/GaAs/GaAs NPN HBT show that the proposed model predicts significantly increased base currents, due to the hole-to-trap tunneling enhanced by the emitter-base junction band offset. Finally, the results compare favorably with experimental observation.« less

  4. On the origin of the low-temperature band in depolarization current spectra of poled multicomponent silicate glasses

    NASA Astrophysics Data System (ADS)

    Brunkov, P. N.; Kaasik, V. P.; Lipovskii, A. A.; Tagantsev, D. K.

    2018-04-01

    Thermally stimulated depolarization current spectra of poled silicate multicomponent glasses in the vicinity of room temperature (220-320 K) have been recorded and two bands, typical for such glasses, have been observed. It was shown that the high-temperature band (at about 290 K) is related to the relaxation of poled glass structure in the bulk, while the low-temperature band (at about 230-270 K) should be attributed to the surface phenomenon—absorption/desorption of positive species of ambient atmosphere, supposedly, water cluster ions H+(H2O)n.

  5. Observation of γ-vibrations and alignments built on non-ground-state configurations in ¹⁵⁶Dy

    DOE PAGES

    Zhu, C. -H.; Hartley, D. J.; Riedinger, L. L.; ...

    2015-03-26

    The exact nature of the lowest K π=2⁺ rotational bands in all deformed nuclei remains obscure. Traditionally they are assumed to be collective vibrations of the nuclear shape in the γ degree of freedom perpendicular to the nuclear symmetry axis. Very few such γ-bands have been traced past the usual back-bending rotational alignments of high-j nucleons. We have investigated the structure of positive-parity bands in the N=90 nucleus ¹⁵⁶Dy, using the ¹⁴⁸Nd(¹²C,4n)¹⁵⁶Dy reaction at 65 MeV, observing the resulting γ-ray transitions with the Gammasphere array. The even- and odd-spin members of the π=2⁺ γ-band are observed to 32⁺ and 31⁺more » respectively. This rotational band faithfully tracks the ground-state configuration to the highest spins. The members of a possible γ-vibration built on the aligned yrast S-band are observed to spins 28⁺ and 27⁺. An even-spin positive-parity band, observed to spin 24⁺, is a candidate for an aligned S-band built on the seniority-zero configuration of the 0₂⁺ state at 676 keV. As a result, the crossing of this band with the 0₂⁺ band is at hw c = 0.28(1) MeV and is consistent with the configuration of the 0₂⁺ band not producing any blocking of the monopole pairing.« less

  6. K-band observations of boxy bulges - I. Morphology and surface brightness profiles

    NASA Astrophysics Data System (ADS)

    Bureau, M.; Aronica, G.; Athanassoula, E.; Dettmar, R.-J.; Bosma, A.; Freeman, K. C.

    2006-08-01

    In this first paper of a series on the structure of boxy and peanut-shaped (B/PS) bulges, Kn-band observations of a sample of 30 edge-on spiral galaxies are described and discussed. Kn-band observations best trace the dominant luminous galactic mass and are minimally affected by dust. Images, unsharp-masked images, as well as major-axis and vertically summed surface brightness profiles are presented and discussed. Galaxies with a B/PS bulge tend to have a more complex morphology than galaxies with other bulge types, more often showing centred or off-centred X structures, secondary maxima along the major-axis and spiral-like structures. While probably not uniquely related to bars, those features are observed in three-dimensional N-body simulations of barred discs and may trace the main bar orbit families. The surface brightness profiles of galaxies with a B/PS bulge are also more complex, typically containing three or more clearly separated regions, including a shallow or flat intermediate region (Freeman Type II profiles). The breaks in the profiles offer evidence for bar-driven transfer of angular momentum and radial redistribution of material. The profiles further suggest a rapid variation of the scaleheight of the disc material, contrary to conventional wisdom but again as expected from the vertical resonances and instabilities present in barred discs. Interestingly, the steep inner region of the surface brightness profiles is often shorter than the isophotally thick part of the galaxies, itself always shorter than the flat intermediate region of the profiles. The steep inner region is also much more prominent along the major-axis than in the vertically summed profiles. Similarly to other recent work but contrary to the standard `bulge + disc' model (where the bulge is both thick and steep), we thus propose that galaxies with a B/PS bulge are composed of a thin concentrated disc (a disc-like bulge) contained within a partially thick bar (the B/PS bulge), itself

  7. Weekly gridded Aquarius L-band radiometer/scatterometer observations and salinity retrievals over the polar regions - Part 1: Product description

    NASA Astrophysics Data System (ADS)

    Brucker, L.; Dinnat, E. P.; Koenig, L. S.

    2014-05-01

    Passive and active observations at L band (frequency ~1.4 GHz) from the Aquarius/SAC-D mission offer new capabilities to study the polar regions. Due to the lack of polar-gridded products, however, applications over the cryosphere have been limited. We present three weekly polar-gridded products of Aquarius data to improve our understanding of L-band observations of ice sheets, sea ice, permafrost, and the polar oceans. Additionally, these products intend to facilitate access to L-band data, and can be used to assist in algorithm developments. Aquarius data at latitudes higher than 50° are averaged and gridded into weekly products of brightness temperature (TB), normalized radar cross section (NRCS), and sea surface salinity (SSS). Each grid cell also contains sea ice fraction, the standard deviation of TB, NRCS, and SSS, and the number of footprint observations collected during the seven-day cycle. The largest 3 dB footprint dimensions are 97 km × 156 km and 74 km × 122 km (along × across track) for the radiometers and scatterometer, respectively. The data is gridded to the Equal-Area Scalable Earth version 2.0 (EASE2.0) grid, with a grid cell resolution of 36 km. The data sets start in August 2011, with the first Aquarius observations and will be updated on a monthly basis following the release schedule of the Aquarius Level 2 data sets. The weekly gridded products are distributed by the US National Snow and Ice Data Center at http://nsidc.org/data/aquarius/index.html .

  8. ESO Diffuse Interstellar Bands Large Exploration Survey (EDIBLES) - Merging Observations and Laboratory Data

    NASA Technical Reports Server (NTRS)

    Salama, Farid

    2016-01-01

    The Diffuse Interstellar Bands (DIBs) are a set of 500 absorption bands that are detected in the spectra of stars with interstellar clouds in the line of sight. DIBs are found from the NUV to the NIR in the spectra of reddened stars spanning different interstellar environments in our local, and in other galaxies. DIB carriers are a significant part of the interstellar chemical inventory. They are stable and ubiquitous in a broad variety of environments and play a unique role in interstellar physics/chemistry. It has long been realized that the solving of the DIB problem requires a strong synergy between astronomical observations, laboratory astrophysics, and astrophysical modeling of line-of-sights. PAHs are among the molecular species that have been proposed as DIB carriers. We will present an assessment of the PAH-DIB model in view of the progress and the advances that have been achieved over the past years through a series of studies involving astronomical observations of DIBs, laboratory simulation of interstellar analogs for neutrals and ionized PAHs, theoretical calculations of PAH spectra and the modelization of diffuse and translucent interstellar clouds. We will present a summary of what has been learned from these complementary studies, the constraints that can now be derived for the PAHs as DIB carriers in the context of the PAH-DIB model and how these constraints can be applied to the EDIBLES project. The spectra of several neutral and ionized PAHs isolated in the gas phase at low temperature have been measured in the laboratory under experimental conditions that mimic interstellar conditions and are compared with an extensive set of astronomical spectra of reddened, early type stars. The comparisons of astronomical and laboratory data provide upper limits for the abundances of specific neutral PAH molecules and ions along specific lines-of-sight. Something that is not attainable from infrared observations alone. We present the characteristics of the

  9. A Circumstellar Disk around HD 169142 in the Mid-Infrared (N-Band)

    NASA Astrophysics Data System (ADS)

    Okamoto, Yoshiko Kataza; Kataza, Hirokazu; Honda, M.; Yamashita, T.; Fujiyoshi, T.; Miyata, T.; Sako, S.; Fujiwara, H.; Sakon, I.; Fukagawa, M.; Momose, M.; Onaka, T.

    2017-07-01

    The Herbig Ae star HD 169142 is one of the objects that show complex structure, such as multiple (innermost, middle, and outer) disks, gaps, and unresolved sources. We made N-band (8-13 μm) observations of HD 169142 with the Cooled Mid-Infrared Camera and Spectrometer on the 8.2 m Subaru Telescope. The images are spatially resolved out to an ˜1″ radius in all the observed bands. We made a simple disk model composed of an unresolved central source (representing the innermost disk/halo) and the ring at a radius r ˜ 25 au (corresponding to the inner wall or edge of a middle disk at ˜25-40 au). The radial intensity profile within the central region (≲0.″3 or ≲ 40 au) is well reproduced by the model. Furthermore, we subtracted the model image from the observed one to search for additional structures. In the model-subtracted images, we found an unresolved west source separated by 17.0 ± 2.9 au in the direction of position angle 260° ± 5° from the original emission peak, which is supposed to correspond to the position of the central star, and a bright east arc located at r ˜ 60 au. The west source is different from the L‧-band unresolved source recently found in coronagraphic observations. It could be a structure related to planet formation in the disk, such as a circumplanetary disk or clumpy disk structure. The east arc corresponds to the inner wall or edge of the outer disk. Based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.

  10. Near-infrared Spectroscopic Observations of Comet C/2013 R1 (Lovejoy) by WINERED: CN Red-system Band Emission

    NASA Astrophysics Data System (ADS)

    Shinnaka, Yoshiharu; Kawakita, Hideyo; Kondo, Sohei; Ikeda, Yuji; Kobayashi, Naoto; Hamano, Satoshi; Sameshima, Hiroaki; Fukue, Kei; Matsunaga, Noriyuki; Yasui, Chikako; Izumi, Natsuko; Mizumoto, Misaki; Otsubo, Shogo; Takenaka, Keiichi; Watase, Ayaka; Kawanishi, Takafumi; Nakanishi, Kenshi; Nakaoka, Tetsuya

    2017-08-01

    Although high-resolution spectra of the CN red-system band are considered useful in cometary sciences, e.g., in the study of isotopic ratios of carbon and nitrogen in cometary volatiles, there have been few reports to date due to the lack of high-resolution (R ≡ λ/Δλ > 20,000) spectrographs in the near-infrared region around ˜1 μm. Here, we present the high-resolution emission spectrum of the CN red-system band in comet C/2013 R1 (Lovejoy), acquired by the near-infrared high-resolution spectrograph WINERED mounted on the 1.3 m Araki telescope at the Koyama Astronomical Observatory, Kyoto, Japan. We applied our fluorescence excitation models for CN, based on modern spectroscopic studies, to the observed spectrum of comet C/2013 R1 (Lovejoy) to search for CN isotopologues (13C14N and 12C15N). We used a CN fluorescence excitation model involving both a “pure” fluorescence excitation model for the outer coma and a “fully collisional” fluorescence excitation model for the inner coma region. Our emission model could reproduce the observed 12C14N red-system band of comet C/2013 R1 (Lovejoy). The derived mixing ratio between the two excitation models was 0.94(+0.02/-0.03):0.06(+0.03/-0.02), corresponding to the radius of the collision-dominant region of ˜800-1600 km from the nucleus. No isotopologues were detected. The observed spectrum is consistent, within error, with previous estimates in comets of 12C/13C (˜90) and 14N/15N (˜150).

  11. Band gap and band offset of (GaIn)(PSb) lattice matched to InP

    NASA Astrophysics Data System (ADS)

    Köhler, F.; Böhm, G.; Meyer, R.; Amann, M.-C.

    2005-07-01

    Metastable (GaxIn1-x)(PySb1-y) layers were grown on (001) InP substrates by gas source molecular beam epitaxy. Low-temperature photoluminescence spectroscopy was applied to these heterostructures and revealed spatially indirect band-to-band recombination of electrons localized in the InP with holes in the (GaxIn1-x)(PySb1-y). In addition, samples with layer thicknesses larger than 100nm showed direct PL across the band gap of (GaxIn1-x)(PySb1-y). Band-gap energies and band offset energies of (GaxIn1-x)(PySb1-y) relative to InP were derived from these PL data. A strong bowing parameter was observed.

  12. Study on observation planning of LAMOST focal plane positioning system and its simulation

    NASA Astrophysics Data System (ADS)

    Zhai, Chao; Jin, Yi; Peng, Xiaobo; Xing, Xiaozheng

    2006-06-01

    Fiber Positioning System of LAMOST focal plane based on subarea thinking, adopts a parallel controllable positioning plan, the structure is designed as a round area and overlapped each other in order to eliminate the un-observation region. But it also makes the observation efficiency of the system become an important problem. In this paper According to the system, the model of LAMOST focal plane Observation Planning including 4000 fiber positioning units is built, Stars are allocated using netflow algorithm and mechanical collisions are diminished through the retreat algorithm, then the simulation of the system's observation efficiency is carried out. The problem of observation efficiency of LAMOST focal plane is analysed systemic and all-sided from the aspect of overlapped region, fiber positioning units, observation radius, collisions and so on. The observation efficiency of the system in theory is describes and the simulation indicates that the system's observation efficiency is acceptable. The analyses play an indicative role on the design of the LAMOST focal plane structure.

  13. Observations of magnetospheric ionization enhancements using upper-hybrid resonance noise band data from the RAE-1 satellite

    NASA Technical Reports Server (NTRS)

    Mosier, S. R.

    1975-01-01

    Noise bands associated with the upper-hybrid resonance were used to provide direct evidence for the existence of regions of enhanced density in the equatorial magnetosphere near L = 2. Density enhancements ranging from several percent to as high as 45 percent are observed with radial dimensions of several hundred kilometers. The enhancement characteristics strongly suggest their identification as magnetospheric whistler ducts.

  14. Delocalization of positive charge in π-stacked multi-benzene rings in multilayered cyclophanes.

    PubMed

    Fujitsuka, Mamoru; Tojo, Sachiko; Shibahara, Masahiko; Watanabe, Motonori; Shinmyozu, Teruo; Majima, Tetsuro

    2011-02-10

    In the present study, delocalization of a positive charge in π-stacked multi-benzene rings in multilayered para- and meta-cyclophanes, in which benzene rings are connected by propyl chains to form a chromophore array with the face-to-face structure, was investigated by means of transient absorption spectroscopy during the pulse radiolysis using dichloroethane as a solvent. The local excitation and charge resonance (CR) bands were successfully observed. It was revealed that the CR band shifted to the longer wavelength side with the number of the benzene rings. The stabilization energy estimated from the peak position of the CR band showed the efficient charge delocalization over the cyclophanes. Furthermore, the CR bands showed the slight spectral change attributable to the change in distribution of the conformers. The substantially long lifetime of the CR band can be explained on the basis of the smaller charge distribution on the outer layers of the multilayered cyclophanes.

  15. Observation of Dirac-like energy band and ring-torus Fermi surface associated with the nodal line in topological insulator CaAgAs

    NASA Astrophysics Data System (ADS)

    Takane, Daichi; Nakayama, Kosuke; Souma, Seigo; Wada, Taichi; Okamoto, Yoshihiko; Takenaka, Koshi; Yamakawa, Youichi; Yamakage, Ai; Mitsuhashi, Taichi; Horiba, Koji; Kumigashira, Hiroshi; Takahashi, Takashi; Sato, Takafumi

    2018-01-01

    One of key challenges in current material research is to search for new topological materials with inverted bulk-band structure. In topological insulators, the band inversion caused by strong spin-orbit coupling leads to opening of a band gap in the entire Brillouin zone, whereas an additional crystal symmetry such as point-group and nonsymmorphic symmetries sometimes prohibits the gap opening at/on specific points or line in momentum space, giving rise to topological semimetals. Despite many theoretical predictions of topological insulators/semimetals associated with such crystal symmetries, the experimental realization is still relatively scarce. Here, using angle-resolved photoemission spectroscopy with bulk-sensitive soft-x-ray photons, we experimentally demonstrate that hexagonal pnictide CaAgAs belongs to a new family of topological insulators characterized by the inverted band structure and the mirror reflection symmetry of crystal. We have established the bulk valence-band structure in three-dimensional Brillouin zone, and observed the Dirac-like energy band and ring-torus Fermi surface associated with the line node, where bulk valence and conducting bands cross on a line in the momentum space under negligible spin-orbit coupling. Intriguingly, we found that no other bands cross the Fermi level and therefore the low-energy excitations are solely characterized by the Dirac-like band. CaAgAs provides an excellent platform to study the interplay among low-energy electron dynamics, crystal symmetry, and exotic topological properties.

  16. Quasiparticle band gap in the topological insulator Bi2Te3

    NASA Astrophysics Data System (ADS)

    Nechaev, I. A.; Chulkov, E. V.

    2013-10-01

    We present a theoretical study of dispersion of states that form the bulk band-gap edges in the three-dimensional topological insulator Bi2Te3. Within density functional theory, we analyze the effect of atomic positions varied within the error range of the available experimental data and approximation chosen for the exchange-correlation functional on the bulk band gap and k-space location of valence- and conduction-band extrema. For each set of the positions with different exchange-correlation functionals, we show how many-body corrections calculated within a one-shot GW approach affect the mentioned characteristics of electronic structure of Bi2Te3. We thus also illustrate to what degree the one-shot GW results are sensitive to the reference one-particle band structure in the case of bismuth telluride. We found that for this topological insulator the GW corrections enlarge the fundamental band gap and for certain atomic positions and reference band structure bring its value in close agreement with experiment.

  17. Observations of the J = 10 manifold of the pure rotational band of phosphine on Saturn

    NASA Technical Reports Server (NTRS)

    Haas, M. R.; Erickson, E. F.; Goorvitch, D.; Mckibbin, D. D.; Rank, D. M.

    1986-01-01

    Saturn was observed in the vicinity of the J = 10 manifold of the pure rotational band of phosphine on 1984 July 10 and 12 from NASA's Kuiper Airborne Observatory with the facility far-infrared cooled grating spectrometer. On each night observations of the full disk plus rings were made at 4 to 6 discrete wavelengths which selectively sampled the manifold and the adjacent continuum. The previously reported detection of this manifold is confirmed. After subtraction of the flux due to the rings, the data are compared with disk-averaged models of Saturn. It is found that PH3 must be strongly depleted above the thermal inversion (approx. 70 mbar). The best fitting models consistent with other observational constaints indicate that PH3 is significantly depleted at even deeper atmospheric levels ( or = 500 mbar), implying an eddy diffusion coefficient for Saturn of 10 to the 4 cm sq/sec.

  18. Determination of Primary Spectral Bands for Remote Sensing of Aquatic Environments

    PubMed Central

    Lee, ZhongPing; Carder, Kendall; Arnone, Robert; He, MingXia

    2007-01-01

    About 30 years ago, NASA launched the first ocean-color observing satellite: the Coastal Zone Color Scanner. CZCS had 5 bands in the visible-infrared domain with an objective to detect changes of phytoplankton (measured by concentration of chlorophyll) in the oceans. Twenty years later, for the same objective but with advanced technology, the Sea-viewing Wide Field-of-view Sensor (SeaWiFS, 7 bands), the Moderate-Resolution Imaging Spectrometer (MODIS, 8 bands), and the Medium Resolution Imaging Spectrometer (MERIS, 12 bands) were launched. The selection of the number of bands and their positions was based on experimental and theoretical results achieved before the design of these satellite sensors. Recently, Lee and Carder (2002) demonstrated that for adequate derivation of major properties (phytoplankton biomass, colored dissolved organic matter, suspended sediments, and bottom properties) in both oceanic and coastal environments from observation of water color, it is better for a sensor to have ∼15 bands in the 400 – 800 nm range. In that study, however, it did not provide detailed analyses regarding the spectral locations of the 15 bands. Here, from nearly 400 hyperspectral (∼ 3-nm resolution) measurements of remote-sensing reflectance (a measure of water color) taken in both coastal and oceanic waters covering both optically deep and optically shallow waters, first- and second-order derivatives were calculated after interpolating the measurements to 1-nm resolution. From these derivatives, the frequency of zero values for each wavelength was accounted for, and the distribution spectrum of such frequencies was obtained. Furthermore, the wavelengths that have the highest appearance of zeros were identified. Because these spectral locations indicate extrema (a local maximum or minimum) of the reflectance spectrum or inflections of the spectral curvature, placing the bands of a sensor at these wavelengths maximizes the potential of capturing (and then

  19. Determination of Primary Spectral Bands for Remote Sensing of Aquatic Environments.

    PubMed

    Lee, ZhongPing; Carder, Kendall; Arnone, Robert; He, MingXia

    2007-12-20

    About 30 years ago, NASA launched the first ocean-color observing satellite:the Coastal Zone Color Scanner. CZCS had 5 bands in the visible-infrared domain with anobjective to detect changes of phytoplankton (measured by concentration of chlorophyll) inthe oceans. Twenty years later, for the same objective but with advanced technology, theSea-viewing Wide Field-of-view Sensor (SeaWiFS, 7 bands), the Moderate-ResolutionImaging Spectrometer (MODIS, 8 bands), and the Medium Resolution ImagingSpectrometer (MERIS, 12 bands) were launched. The selection of the number of bands andtheir positions was based on experimental and theoretical results achieved before thedesign of these satellite sensors. Recently, Lee and Carder (2002) demonstrated that foradequate derivation of major properties (phytoplankton biomass, colored dissolved organicmatter, suspended sediments, and bottom properties) in both oceanic and coastalenvironments from observation of water color, it is better for a sensor to have ~15 bands inthe 400 - 800 nm range. In that study, however, it did not provide detailed analysesregarding the spectral locations of the 15 bands. Here, from nearly 400 hyperspectral (~ 3-nm resolution) measurements of remote-sensing reflectance (a measure of water color)taken in both coastal and oceanic waters covering both optically deep and optically shallowwaters, first- and second-order derivatives were calculated after interpolating themeasurements to 1-nm resolution. From these derivatives, the frequency of zero values foreach wavelength was accounted for, and the distribution spectrum of such frequencies wasobtained. Furthermore, the wavelengths that have the highest appearance of zeros wereidentified. Because these spectral locations indicate extrema (a local maximum orminimum) of the reflectance spectrum or inflections of the spectral curvature, placing the bands of a sensor at these wavelengths maximizes the potential of capturing (and then restoring) the spectral curve

  20. Polarimetric C-/X-band Synthetic Aperture Radar Observations of Melting Sea Ice in the Canadian Arctic Archipelago

    NASA Astrophysics Data System (ADS)

    Casey, J. A.; Beckers, J. F.; Brossier, E.; Haas, C.

    2013-12-01

    Operational ice information services rely heavily on space-borne synthetic aperture radar (SAR) data for the production of ice charts to meet their mandate of providing timely and accurate sea ice information to support safe and efficient marine operations. During the summer melt period, the usefulness of SAR data for sea ice monitoring is limited by the presence of wet snow and melt ponds on the ice surface, which can mask the signature of the underlying ice. This is a critical concern for ice services whose clients (e.g. commercial shipping, cruise tourism, resource exploration and extraction) are most active at this time of year when sea ice is at its minimum extent, concentration and thickness. As a result, there is a need to further quantify the loss of ice information in SAR data during the melt season and to identify what information can still be retrieved about ice surface conditions and melt pond evolution at this time of year. To date the majority of studies have been limited to analysis of single-polarization C-band SAR data. This study will investigate the potential complimentary and unique sea ice information that polarimetric C- and X-band SAR data can provide to supplement the information available from traditional single co-polarized C-band SAR data. A time-series of polarimetric C- and X-band SAR data was acquired over Jones Sound in the Canadian Arctic Archipelago, in the vicinity of the Grise Fiord, Nunavut. Five RADARSAT-2 Wide Fine Quad-pol images and 11 TerraSAR-X StripMap dual-pol (HH/VV) images were acquired. The time-series begins at the onset of melt in early June and extends through advanced melt conditions in late July. Over this period several ponding and drainage events and two snowfall events occurred. Field observations of sea ice properties were collected using an Ice Mass Balance (IMB) buoy, hourly photos from a time-lapse camera deployed on a coastal cliff, and manual in situ measurements of snow thickness and melt pond depth

  1. Exact folded-band chaotic oscillator.

    PubMed

    Corron, Ned J; Blakely, Jonathan N

    2012-06-01

    An exactly solvable chaotic oscillator with folded-band dynamics is shown. The oscillator is a hybrid dynamical system containing a linear ordinary differential equation and a nonlinear switching condition. Bounded oscillations are provably chaotic, and successive waveform maxima yield a one-dimensional piecewise-linear return map with segments of both positive and negative slopes. Continuous-time dynamics exhibit a folded-band topology similar to Rössler's oscillator. An exact solution is written as a linear convolution of a fixed basis pulse and a discrete binary sequence, from which an equivalent symbolic dynamics is obtained. The folded-band topology is shown to be dependent on the symbol grammar.

  2. Warm-Up Activities of Middle and High School Band Directors Participating in State-Level Concert Band Assessments

    ERIC Educational Resources Information Center

    Ward, Justin P.; Hancock, Carl B.

    2016-01-01

    The purpose of this study was to examine the warm-ups chosen by concert band directors participating in state-level performance assessments. We observed 29 middle and high school bands and coded the frequency and duration of warm-up activities and behaviors. Results indicated that most bands rehearsed music and played scales, long tones, and…

  3. Near-infrared Spectroscopic Observations of Comet C/2013 R1 (Lovejoy) by WINERED: CN Red-system Band Emission

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Shinnaka, Yoshiharu; Yasui, Chikako; Izumi, Natsuko

    Although high-resolution spectra of the CN red-system band are considered useful in cometary sciences, e.g., in the study of isotopic ratios of carbon and nitrogen in cometary volatiles, there have been few reports to date due to the lack of high-resolution ( R  ≡  λ /Δ λ  > 20,000) spectrographs in the near-infrared region around ∼1 μ m. Here, we present the high-resolution emission spectrum of the CN red-system band in comet C/2013 R1 (Lovejoy), acquired by the near-infrared high-resolution spectrograph WINERED mounted on the 1.3 m Araki telescope at the Koyama Astronomical Observatory, Kyoto, Japan. We applied our fluorescence excitation models for CN, based onmore » modern spectroscopic studies, to the observed spectrum of comet C/2013 R1 (Lovejoy) to search for CN isotopologues ({sup 13}C{sup 14}N and {sup 12}C{sup 15}N). We used a CN fluorescence excitation model involving both a “pure” fluorescence excitation model for the outer coma and a “fully collisional” fluorescence excitation model for the inner coma region. Our emission model could reproduce the observed {sup 12}C{sup 14}N red-system band of comet C/2013 R1 (Lovejoy). The derived mixing ratio between the two excitation models was 0.94(+0.02/−0.03):0.06(+0.03/−0.02), corresponding to the radius of the collision-dominant region of ∼800–1600 km from the nucleus. No isotopologues were detected. The observed spectrum is consistent, within error, with previous estimates in comets of {sup 12}C/{sup 13}C (∼90) and {sup 14}N/{sup 15}N (∼150).« less

  4. Synthesizing folded band chaos.

    PubMed

    Corron, Ned J; Hayes, Scott T; Pethel, Shawn D; Blakely, Jonathan N

    2007-04-01

    A randomly driven linear filter that synthesizes Lorenz-like, reverse-time chaos is shown also to produce Rössler-like folded band wave forms when driven using a different encoding of the random source. The relationship between the topological entropy of the random source, dissipation in the linear filter, and the positive Lyapunov exponent for the reverse-time wave form is exposed. The two drive encodings are viewed as grammar restrictions on a more general encoding that produces a chaotic superset encompassing both the Lorenz butterfly and Rössler folded band paradigms of nonlinear dynamics.

  5. Influence of Scleral Buckling Surgery with Encircling Band on Subfoveal Choroidal Thickness in Long-Term Observations

    PubMed Central

    Laudańska-Olszewska, Iwona; Gozdek, Piotr; Maroszyński, Mariusz; Amon, Michael

    2013-01-01

    Purpose. The aim of this study is the presentation of subfoveal choroidal thickness with enhanced depth imaging spectral-domain optical coherence tomography (EDI-OCT) several months after scleral buckling with encircling band surgery. Methods. 48 patients who underwent scleral buckling with encircling band surgery for unilateral rhegmatogenous retinal detachment were included in the retrospective observational study. The mean time from scleral buckling surgery to the final EDI-OCT examination was 22±6.7 months. We compare choroidal thickness between operated and fellow eyes. Results. In all patients, the macula was detached before the surgery. The subfoveal choroidal thickness in 48 treated eyes was 260.9±45.8 µm (range 155–383 µm) and in the fellow eyes was 217.5±36.7 µm (range 98–326 µm). The subfoveal choroidal thickness of eyes after scleral buckling surgery in long-term EDI-OCT examination was significantly thicker (P<0.001) than in fellow eyes. Conclusions. The subfoveal choroid in eyes undergoing encircling band surgery was significantly thicker than in fellow eyes. We suspect that this may be the result of reduced choroidal blood flow. It also seems that the width and size of the material used in scleral buckling surgery may affect a change in the choroid circulation and increase subfoveal choroidal thickness. PMID:23841077

  6. GRB 050117: Simultaneous Gamma-ray and X-ray Observations with the Swift Satellite

    NASA Technical Reports Server (NTRS)

    Hill, J. E.; Morris, D. C.; Sakamoto, T.; Sato, G.; Burrows, D. N.; Angelini, L.; Pagani, C.; Moretti, A.; Abbey, A. F.; Barthelmy, S.

    2005-01-01

    The Swift Gamma-Ray Burst Explorer performed its first autonomous, X-ray follow-up to a newly detected GRB on 2005 January 17, within 193 seconds of the burst trigger by the Swift Burst Alert Telescope. While the burst was still in progress, the X-ray Telescope obtained a position and an image for an un-catalogued X-ray source; simultaneous with the gamma-ray observation. The XRT observed flux during the prompt emission was 1.1 x 10(exp -8) ergs/sq cm/s in the 0.5-10 keV energy band. The emission in the X-ray band decreased by three orders of magnitude within 700 seconds, following the prompt emission. This is found to be consistent with the gamma-ray decay when extrapolated into the XRT energy band. During the following 6.3 hours, the XRT observed the afterglow in an automated sequence for an additional 947 seconds, until the burst became fully obscured by the Earth limb. A faint, extremely slowly decaying afterglow, alpha=-0.21, was detected. Finally, a break in the lightcurve occurred and the flux decayed with alpha<-1.2. The X-ray position triggered many follow-up observations: no optical afterglow could be confirmed, although a candidate was identified 3 arcsecs from the XRT position.

  7. The ÖX˜ absorption of vinoxy radical revisited: Normal and Herzberg-Teller bands observed via cavity ringdown spectroscopy

    NASA Astrophysics Data System (ADS)

    Thomas, Phillip S.; Chhantyal-Pun, Rabi; Kline, Neal D.; Miller, Terry A.

    2010-03-01

    The ÖX˜ electronic absorption spectrum of vinoxy radical has been investigated using room temperature cavity ringdown spectroscopy. Analysis of the observed bands on the basis of computed vibrational frequencies and rotational envelopes reveals that two distinct types of features are present with comparable intensities. The first type corresponds to "normal" allowed electronic transitions to the origin and symmetric vibrations in the à state. The second type is interpreted in terms of excitations to asymmetric à state vibrations, which are only vibronically allowed by Herzberg-Teller coupling to the B˜ state. Results of electronic structure calculations indicate that the magnitude of the Herzberg-Teller coupling is appropriate to produce vibronically induced transitions with intensities comparable to those of the normal bands.

  8. Band Edge Positions and Their Impact on the Simulated Device Performance of ZnSnN 2-Based Solar Cells

    DOE PAGES

    Arca, Elisabetta; Fioretti, Angela; Lany, Stephan; ...

    2017-12-07

    ZnSnN 2 (ZTN) has been proposed as a new earth abundant absorber material for PV applications. While carrier concentration has been reduced to values suitable for device implementation, other properties such as ionization potential, electron affinity and work function are not known. Here, we experimentally determine the value of ionization potential (5.6 eV), electron affinity (4.1 eV) and work function (4.4 eV) for ZTN thin film samples with Zn cation composition Zn/(Zn+Sn) = 0.56 and carrier concentration n = 2x10 19cm -3. Using both experimental and theoretical results, we build a model to simulate the device performance of a ZTN/Mg:CuCrOmore » 2 solar cell, showing a potential efficiency of 23% in the limit of no defects present. We also investigate the role of band tails and recombination centers on the cell performance. In particular device simulations show that band tails are highly detrimental to the cell efficiency, and recombination centers are a major limitation if present in concentration comparable to the net carrier density. The effect of the position of the band edges of the p-type junction partner was assessed too. Through this study, we determine the major bottlenecks for the development of ZTN-based solar cell and identify avenues to mitigate them.« less

  9. Observations of copolar correlation coefficient through a bright band at vertical incidence

    NASA Technical Reports Server (NTRS)

    Zrnic, D. S.; Raghavan, R.; Chandrasekar, V.

    1994-01-01

    This paper discusses an application of polarimetric measurements at vertical incidence. In particular, the correlation coefficients between linear copolar components are examined, and measurements obtained with the National Severe Storms Laboratory (NSSL)'s and National Center for Atmospheric Research (NCAR)'s polarimetric radars are presented. The data are from two well-defined bright bands. A sharp decrease of the correlation coefficient, confined to a height interval of a few hundred meters, marks the bottom of the bright band.

  10. Observations on the correlation between posture and jaw position: a pilot study.

    PubMed

    Bracco, P; Deregibus, A; Piscetta, R; Ferrario, G

    1998-10-01

    The aim of this pilot study was twofold. The first was to show a method for having an objective and dynamic analysis of body posture, evaluating weight distribution and its connections with different mandibular positions. The second was to verify if a neuromuscularly stimulated occlusal position, called myocentric occlusal position, is associated with a positive or negative postural charge. For the second aim a group of 20 subjects (including both males and females), was chosen. Posture of each subject was analyzed in three different conditions: centric occlusion, rest position and myocentric position. To evaluate the dynamic of posture a platform capable of measuring the weight on the feet supporting points and the related variations during time of observation and the swinging of body barycenter was used. The data showed that there is an improvement in the position of the barycenter from the centric occlusion to the myocentric position. Such an improvement can't be observed from the intercuspal position to the rest position. The results of this pilot study are discussed.

  11. Does the chromatic Mach bands effect exist?

    PubMed

    Tsofe, Avital; Spitzer, Hedva; Einav, Shmuel

    2009-06-30

    The achromatic Mach bands effect is a well-known visual illusion, discovered over a hundred years ago. This effect has been investigated thoroughly, mainly for its brightness aspect. The existence of Chromatic Mach bands, however, has been disputed. In recent years it has been reported that Chromatic Mach bands are not perceived under controlled iso-luminance conditions. However, here we show that a variety of Chromatic Mach bands, consisting of chromatic and achromatic regions, separated by a saturation ramp, can be clearly perceived under iso-luminance and iso-brightness conditions. In this study, observers' eye movements were recorded under iso-brightness conditions. Several observers were tested for their ability to perceive the Chromatic Mach bands effect and its magnitude, across different cardinal and non-cardinal Chromatic Mach bands stimuli. A computational model of color adaptation, which predicted color induction and color constancy, successfully predicts this variation of Chromatic Mach bands. This has been tested by measuring the distance of the data points from the "achromatic point" and by calculating the shift of the data points from predicted complementary lines. The results suggest that the Chromatic Mach bands effect is a specific chromatic induction effect.

  12. Band Edge Dynamics and Multiexciton Generation in Narrow Band Gap HgTe Nanocrystals.

    PubMed

    Livache, Clément; Goubet, Nicolas; Martinez, Bertille; Jagtap, Amardeep; Qu, Junling; Ithurria, Sandrine; Silly, Mathieu G; Dubertret, Benoit; Lhuillier, Emmanuel

    2018-04-11

    Mercury chalcogenide nanocrystals and especially HgTe appear as an interesting platform for the design of low cost mid-infrared (mid-IR) detectors. Nevertheless, their electronic structure and transport properties remain poorly understood, and some critical aspects such as the carrier relaxation dynamics at the band edge have been pushed under the rug. Some of the previous reports on dynamics are setup-limited, and all of them have been obtained using photon energy far above the band edge. These observations raise two main questions: (i) what are the carrier dynamics at the band edge and (ii) should we expect some additional effect (multiexciton generation (MEG)) as such narrow band gap materials are excited far above the band edge? To answer these questions, we developed a high-bandwidth setup that allows us to understand and compare the carrier dynamics resonantly pumped at the band edge in the mid-IR and far above the band edge. We demonstrate that fast (>50 MHz) photoresponse can be obtained even in the mid-IR and that MEG is occurring in HgTe nanocrystal arrays with a threshold around 3 times the band edge energy. Furthermore, the photoresponse can be effectively tuned in magnitude and sign using a phototransistor configuration.

  13. Real-time morphologic changes of the iliotibial band during therapeutic stretching; an ultrasonographic study.

    PubMed

    Wang, Hsing-Kuo; Ting-Fang Shih, Tiffany; Lin, Kwan-Hwa; Wang, Tyng-Guey

    2008-08-01

    The purpose of this study was to evaluate the utility of ultrasonography (US) in determining the morphological changes of the iliotibial band (ITB) with the modified Ober maneuver. Forty-four subjects (23 men and 21 women, mean age (+/- SD), 24.7+/-4.7 years) who had no previous history of lower back, gluteus, hip or knee pain and satisfied additional inclusion criteria were recruited. Twenty out of the 44 subjects were initially examined by both MRI and US for measurement confirmation. Band width of the left ITB (the measures of which were highly correlated between techniques) was then assessed for these 44 subjects by US with the modified Ober maneuver in three gradually increased hip adduction positions; neutral, adducted and adducted with weight in these 44 subjects. In addition, examiner reliability was assessed by conducting duplicate measurements in 20 randomly chosen subjects. Results demonstrated that measures of band width, but not thickness, were highly correlated between MRI and US (p<0.001, r=0.850). Significant reductions in band width were observed between the three positions with the modified Ober maneuver (p<0.001). Intratester reliability was high (intraclass correlation coefficient (ICC)=0.86-0.94). Band width changes indicated that the ITB was subjected to a significant stretching force during hip adduction. We conclude that US is a reliable means to directly assess the real-time effects of stretching exercises.

  14. Multi-band transit observations of the TrES-2b exoplanet

    NASA Astrophysics Data System (ADS)

    Mislis, D.; Schröter, S.; Schmitt, J. H. M. M.; Cordes, O.; Reif, K.

    2010-02-01

    We present a new data set of transit observations of the TrES-2b exoplanet taken in spring 2009, using the 1.2 m Oskar-Lühning telescope (OLT) of Hamburg Observatory and the 2.2 m telescope at Calar Alto Observatory using BUSCA (Bonn University Simultaneous CAmera). Both the new OLT data, taken with the same instrumental setup as our data taken in 2008, as well as the simultaneously recorded multicolor BUSCA data confirm the low inclination values reported previously, and in fact suggest that the TrES-2b exoplanet has already passed the first inclination threshold (imin,1 = 83.417°) and is not eclipsing the full stellar surface any longer. Using the multi-band BUSCA data we demonstrate that the multicolor light curves can be consistently fitted with a given set of limb darkening coefficients without the need to adjust these coefficients, and further, we can demonstrate that wavelength dependent stellar radius changes must be small as expected from theory. Our new observations provide further evidence for a change of the orbit inclination of the transiting extrasolar planet TrES-2b reported previously. We examine in detail possible causes for this inclination change and argue that the observed change should be interpreted as nodal regression. While the assumption of an oblate host star requires an unreasonably large second harmonic coefficient, the existence of a third body in the form of an additional planet would provide a very natural explanation for the observed secular orbit change. Given the lack of clearly observed short-term variations of transit timing and our observed secular nodal regression rate, we predict a period between approximately 50 and 100 days for a putative perturbing planet of Jovian mass. Such an object should be detectable with present-day radial velocity (RV) techniques, but would escape detection through transit timing variations. Photometric transit data are only available in electronic form at the CDS via anonymous ftp to cdsarc

  15. Glucose Absorption by the Bacillary Band of Trichuris muris

    PubMed Central

    Hansen, Michael; Nejsum, Peter; Mejer, Helena; Denwood, Matthew; Thamsborg, Stig M.

    2016-01-01

    Background A common characteristic of Trichuris spp. infections in humans and animals is the variable but low efficacy of single-dose benzimidazoles currently used in mass drug administration programmes against human trichuriasis. The bacillary band, a specialised morphological structure of Trichuris spp., as well as the unique partly intracellular habitat of adult Trichuris spp. may affect drug absorption and perhaps contribute to the low drug accumulation in the worm. However, the exact function of the bacillary band is still unknown. Methodology We studied the dependency of adult Trichuris muris on glucose and/or amino acids for survival in vitro and the absorptive function of the bacillary band. The viability of the worms was evaluated using a motility scale from 0 to 3, and the colorimetric assay Alamar Blue was utilised to measure the metabolic activity. The absorptive function of the bacillary band in living worms was explored using a fluorescent glucose analogue (6-NBDG) and confocal microscopy. To study the absorptive function of the bacillary band in relation to 6-NBDG, the oral uptake was minimised or excluded by sealing the oral cavity with glue and agarose. Principal Findings Glucose had a positive effect on both the motility (p < 0.001) and metabolic activity (p < 0.001) of T. muris in vitro, whereas this was not the case for amino acids. The 6-NBDG was observed in the pores of the bacillary band and within the stichocytes of the living worms, independent of oral sealing. Conclusions/Significance Trichuris muris is dependent on glucose for viability in vitro, and the bacillary band has an absorptive function in relation to 6-NBDG, which accumulates within the stichocytes. The absorptive function of the bacillary band calls for an exploration of its possible role in the uptake of anthelmintics, and as a potential anthelmintic target relevant for future drug development. PMID:27588682

  16. Glucose Absorption by the Bacillary Band of Trichuris muris.

    PubMed

    Hansen, Tina V A; Hansen, Michael; Nejsum, Peter; Mejer, Helena; Denwood, Matthew; Thamsborg, Stig M

    2016-09-01

    A common characteristic of Trichuris spp. infections in humans and animals is the variable but low efficacy of single-dose benzimidazoles currently used in mass drug administration programmes against human trichuriasis. The bacillary band, a specialised morphological structure of Trichuris spp., as well as the unique partly intracellular habitat of adult Trichuris spp. may affect drug absorption and perhaps contribute to the low drug accumulation in the worm. However, the exact function of the bacillary band is still unknown. We studied the dependency of adult Trichuris muris on glucose and/or amino acids for survival in vitro and the absorptive function of the bacillary band. The viability of the worms was evaluated using a motility scale from 0 to 3, and the colorimetric assay Alamar Blue was utilised to measure the metabolic activity. The absorptive function of the bacillary band in living worms was explored using a fluorescent glucose analogue (6-NBDG) and confocal microscopy. To study the absorptive function of the bacillary band in relation to 6-NBDG, the oral uptake was minimised or excluded by sealing the oral cavity with glue and agarose. Glucose had a positive effect on both the motility (p < 0.001) and metabolic activity (p < 0.001) of T. muris in vitro, whereas this was not the case for amino acids. The 6-NBDG was observed in the pores of the bacillary band and within the stichocytes of the living worms, independent of oral sealing. Trichuris muris is dependent on glucose for viability in vitro, and the bacillary band has an absorptive function in relation to 6-NBDG, which accumulates within the stichocytes. The absorptive function of the bacillary band calls for an exploration of its possible role in the uptake of anthelmintics, and as a potential anthelmintic target relevant for future drug development.

  17. A spectral line survey of Orion KL in the bands 486-492 and 541-577 GHz with the Odin satellite. I. The observational data

    NASA Astrophysics Data System (ADS)

    Olofsson, A. O. H.; Persson, C. M.; Koning, N.; Bergman, P.; Bernath, P. F.; Black, J. H.; Frisk, U.; Geppert, W.; Hasegawa, T. I.; Hjalmarson, Å.; Kwok, S.; Larsson, B.; Lecacheux, A.; Nummelin, A.; Olberg, M.; Sandqvist, Aa.; Wirström, E. S.

    2007-12-01

    Aims:Spectral line surveys are useful since they allow identification of new molecules and new lines in uniformly calibrated data sets. The subsequent multi-transition analysis will provide improved knowledge of molecular abundances, cloud temperatures and densities, and may also reveal previously unsuspected blends of molecular lines, which otherwise may lead to erroneous conclusions. Nonetheless, large portions of the sub-millimetre spectral regime remain unexplored due to severe absorptions by H{2}O and O{2} in the terrestrial atmosphere. The purpose of the measurements presented here is to cover wavelength regions at and around 0.55 mm - regions largely unobservable from the ground. Methods: Using the Odin astronomy/aeronomy satellite, we performed the first spectral survey of the Orion KL molecular cloud core in the bands 486-492 and 541-576 GHz with rather uniform sensitivity (22-25 mK baseline noise). Odin's 1.1 m size telescope, equipped with four cryo-cooled tuneable mixers connected to broad band spectrometers, was used in a satellite position-switching mode. Two mixers simultaneously observed different 1.1 GHz bands using frequency steps of 0.5 GHz (25 h each). An on-source integration time of 20 h was achieved for most bands. The entire campaign consumed 1100 orbits, each containing one hour of serviceable astro-observation. Results: We identified 280 spectral lines from 38 known interstellar molecules (including isotopologues) having intensities in the range 80 to 0.05 K. An additional 64 weak lines remain unidentified. Apart from the ground state rotational 1{1,0}-1{0,1} transitions of ortho-H{2}O, H{2}18O and H{2}17O, the high energy 6{2,4}-7{1,7} line of para-H{2}O (Eu=867 K) and the HDO(2{0,2}-1{1,1}) line have been observed, as well as the 1{0}-0{1} lines from NH{3} and its rare isotopologue 15NH{3}. We suggest assignments for some unidentified features, notably the new interstellar molecules ND and SH-. Severe blends have been detected in the

  18. Global Positioning System: Observations on Quarterly Reports from the Air Force

    DTIC Science & Technology

    2016-10-17

    Positioning System : Observations on Quarterly Reports from the Air Force The satellite-based Global Positioning System (GPS) provides positioning, navigation...infrastructure, and transportation safety. The Department of Defense (DOD)—specifically, the Air Force—develops and operates the GPS system , which...programs, including the most recent detailed assessment of the next generation operational control system (OCX) and development of military GPS

  19. The Position and Attitude of Sub-reflector Modeling for TM65 m Radio Telescope

    NASA Astrophysics Data System (ADS)

    Sun, Z. X.; Chen, L.; Wang, J. Q.

    2016-01-01

    In the course of astronomical observations, with changes in angle of pitch, the large radio telescope will have different degrees of deformation in the sub-reflector support, back frame, main reflector etc, which will lead to the dramatic decline of antenna efficiency in both high and low elevation. A sub-reflector system of the Tian Ma 65 m radio telescope has been installed in order to compensate for the gravitational deformations of the sub-reflector support and the main reflector. The position and attitude of the sub-reflector are variable in order to improve the pointing performance and the efficiency at different elevations. In this paper, it is studied that the changes of position and attitude of the sub-reflector have influence on the efficiency of antenna in the X band and Ku band. A model has been constructed to determine the position and attitude of the sub-reflector with elevation, as well as the point compensation model, by observing the radio source. In addition, antenna efficiency was tested with sub-reflector position adjusted and fixed. The results show that the model of sub-reflector can effectively improve the efficiency of the 65 m radio telescope. In X band, the aperture efficiency of the radio telescope reaches more than 60% over the entire elevation range.

  20. Revealing the Faraday depth structure of radio galaxy NGC 612 with broad-band radio polarimetric observations

    NASA Astrophysics Data System (ADS)

    Kaczmarek, J. F.; Purcell, C. R.; Gaensler, B. M.; Sun, X.; O'Sullivan, S. P.; McClure-Griffiths, N. M.

    2018-05-01

    We present full-polarization, broad-band observations of the radio galaxy NGC 612 (PKS B0131-637) from 1.3 to 3.1 GHz using the Australia Telescope Compact Array. The relatively large angular scale of the radio galaxy makes it a good candidate with which to investigate the polarization mechanisms responsible for the observed Faraday depth structure. By fitting complex polarization models to the polarized spectrum of each pixel, we find that a single polarization component can adequately describe the observed signal for the majority of the radio galaxy. While we cannot definitively rule out internal Faraday rotation, we argue that the bulk of the Faraday rotation is taking place in a thin skin that girts the polarized emission. Using minimum energy estimates, we find an implied total magnetic field strength of 4.2 μG.

  1. Band head spin assignment of superdeformed bands in Hg isotopes through power index formula

    NASA Astrophysics Data System (ADS)

    Sharma, Honey; Mittal, H. M.

    2018-05-01

    The power index formula has been used to obtain the band head spin (I 0) of all the superdeformed (SD) bands in Hg isotopes. A least squares fitting approach is used. The root mean square deviations between the determined and the observed transition energies are calculated by extracting the model parameters using the power index formula. Whenever definite spins are available, the determined and the observed transition energies are in accordance with each other. The computed values of dynamic moment of inertia J (2) obtained by using the power index formula and its deviation with the rotational frequency is also studied. Excellent agreement is shown between the calculated and the experimental results for J (2) versus the rotational frequency. Hence, the power index formula works very well for all the SD bands in Hg isotopes expect for 195Hg(2, 3, 4).

  2. C-H Hot Bands in the Near-IR Emission Spectra of Leonids

    NASA Technical Reports Server (NTRS)

    Freund, F. T.; Scoville, J.; Holm, R.; Seelemann, R.; Freund, M. M.

    2002-01-01

    The reported infrared (IR) emission spectra from 1999 Leonid fireballs show a 3.4 micron C-H emission band and unidentified bands at longer wavelengths. Upon atmospheric entry, the Leonid meteorites were flash-heated to temperatures around 2400K, which would destroy any organics on the surface of the meteorite grains. We propose that the nu(sub )CH emission band in the Leonid emission spectra arises from matrix-embedded C(sub n)-H-O entities that are protected from instant pyrolysis. Our model is based on IR absorption nu(sub )CH bands, which we observed in laboratory-grown MgO and natural olivine single crystals, where they arise from C(sub n)-H-O units imbedded in the mineral matrix, indicative of aliphatic -CH2- and -CH3 organics. Instead of being pyrolyzed, the C(sub n)-H-O entities in the Leonid trails become vibrationally excited to higher levels n = 1, 2, 3 etc. During de-excitation they emit at 3.4 microns, due to the (0 => 1) transition, and at longer wavelengths, due to hot bands. As a first step toward verifying this hypothesis we measured the C-H vibrational manifold of hexane (C6H14). The calculated positions of the (2 => l ) , (3 => 2), and possibly (4 => 3) hot bands agree with the Leonid emission bands at 3.5, 3.8 and 4.l microns.

  3. Relative properties of smooth terminating bands

    NASA Astrophysics Data System (ADS)

    Afanasjev, A. V.; Ragnarsson, I.

    1998-01-01

    The relative properties of smooth terminating bands observed in the A ∼ 110 mass region are studied within the effective alignment approach. Theoretical values of ietf are calculated using the configuration-dependent shell-correction model with the cranked Nilsson potential. Reasonable agreement with experiment shows that previous interpretations of these bands are consistent with the present study. Contrary to the case of superdeformed bands, the effective alignments of these bands deviate significantly from the pure single-particle alignments of the corresponding orbitals. This indicates that in the case of smooth terminating bands, the effects associated with changes in equilibrium deformations contribute significantly to the effective alignment.

  4. Improvement in the observation system for the GPS/A seafloor positioning

    NASA Astrophysics Data System (ADS)

    Fujimoto, H.; Kido, M.; Osada, Y.

    2010-12-01

    GPS/Acoustic seafloor positioning has become an indispensable geodetic observation for the monitoring of crustal activities near plate boundaries. There remain, however, substantial differences from GPS observation on land. Our group in Tohoku University has been working to cope with the problems under the program of the DONET, JAMSTEC.One of critical problems regarding the present GPS/A observation lies in the campaign style observation spending one or two days to measure the position of an array of acoustic transponders (PXPs) once or twice a year. It is similar to the triangulation observation on land before the age of the GPS. Chadwell et al. (2009, AGU Fall Meeting) made a step forward for this problem by carrying out a continuous GPS/A observation with a moored buoy. We are also developing a system using a moored small buoy. Precision of seafloor positioning by GPS/A is another critical problems. Considering that plate motions are several centimeters per year in most cases, precision of a few centimeters by GPS/A is a big difference from a few millimeters by GPS on land. We estimate that lateral variations in the sound velocity in the ocean can be a key to improve the precision in the positioning and to reduce the required time for the measurement, we have tried to estimate the lateral variations in the acoustic velocity by using 4-5 PXPs (Kido et al., 2006; Kido et al., this meeting). Long-term attitude stability of the position of a PXP deployed on thick sediment has been a basic problem in the GPS/A observation. While a pillar of a GPS antenna for an observation point is set up firmly on the ground, a PXP is deployed on the seafloor after a free fall from the sea surface. It is a serious problem to detect coseismic crustal movements on the seafloor. M7-class earthquakes occurred in 2004 off Kii Peninsula, Central Japan, gave us an opportunity to study the problem. By using an ROV (remotely operated vehicle), we visually observed ten PXPs in 2006, seven of

  5. Yrare low-spin positive-parity states in N = 88 66 154 Dy

    NASA Astrophysics Data System (ADS)

    Zimba, G. L.; Bvumbi, S. P.; Masiteng, L. P.; Jones, P.; Sharpey-Schafer, J. F.; Majola, S. N. T.; Dinoko, T. S.; Shirinda, O.; Lawrie, J. J.; Easton, J. E.; Khumalo, N. A.; Msebi, L.; Mashita, P. I.; Papka, P.; Roux, D. G.; Negi, D.

    2018-04-01

    Low-spin positive-parity yrare states of 66 154 Dy88 were established using the 155Gd(3He,4n) reaction at a beam energy of E_{lab} = 37.5 MeV. The AFRODITE spectrometer array at iThemba LABS was used to record γγ coincidences and measure DCO ratios and polarisation asymmetries. The K^{π}=2+ γ band has been observed up to spin 13+ in the odd spins and to 12+ in the even spins. The staggering parameter S( I) of the γ band is compared to that found in other N = 88 isotones. Different behaviour of S( I) with increasing spin is observed for each of the isotones. We conjecture that the variation in S( I) is mainly due to mixing of the even-spin states with the same spin and parity states in neighbouring rotational bands. A second K^{π}=2+ band has been established up to a spin of 12+ in the even spins. We suggest that this is a γ band based on the J^{π} = 0+ state at Ex = 660.6 keV.

  6. Unique Positioning for Using Elastic Resistance Band in Providing Strengthening Exercise to the Muscles Surrounding the Ankle

    PubMed Central

    Bandy, William D.

    2007-01-01

    Ankle sprains are among the most common injuries incurred by participants in athletics. Conservative management of the patient after an ankle sprain includes a comprehensive rehabilitation program of which the resistance exercises are a part and are frequently advised by the clinician, many times as part of a home exercise program. The purpose of this Clinical Suggestion is to present a unique method of using elastic resistance band to provide strengthening activities to the inverters, ever-tors, plantarflexors, and dorsiflexors of the ankle. The method is unique, as well as convenient and efficient, as it allows the subject to perform all four exercises with a minimum of change in position, while staying seated in a chair. PMID:21522203

  7. Polygonal deformation bands in sandstone

    NASA Astrophysics Data System (ADS)

    Antonellini, Marco; Nella Mollema, Pauline

    2017-04-01

    We report for the first time the occurrence of polygonal faults in sandstone, which is compelling given that layer-bound polygonal fault systems have been observed so far only in fine-grained sediments such as clay and chalk. The polygonal faults are dm-wide zones of shear deformation bands that developed under shallow burial conditions in the lower portion of the Jurassic Entrada Fm (Utah, USA). The edges of the polygons are 1 to 5 meters long. The shear deformation bands are organized as conjugate faults along each edge of the polygon and form characteristic horst-like structures. The individual deformation bands have slip magnitudes ranging from a few mm to 1.5 cm; the cumulative average slip magnitude in a zone is up to 10 cm. The deformation bands heaves, in aggregate form, accommodate a small isotropic horizontal extension (strain < 0.005). The individual shear deformation bands show abutting T-junctions, veering, curving, and merging where they mechanically interact. Crosscutting relationships are rare. The interactions of the deformation bands are similar to those of mode I opening fractures. Density inversion, that takes place where under-compacted and over-pressurized layers (Carmel Fm) lay below normally compacted sediments (Entrada Sandstone), may be an important process for polygonal deformation bands formation. The gravitational sliding and soft sediment structures typically observed within the Carmel Fm support this hypothesis. Soft sediment deformation may induce polygonal faulting in the section of the Entrada Sandstone just above the Carmel Fm. The permeability of the polygonal deformation bands is approximately 10-14 to 10-13 m2, which is less than the permeability of the host, Entrada Sandstone (range 10-12 to 10-11 m2). The documented fault networks have important implications for evaluating the geometry of km-scale polygonal fault systems in the subsurface, top seal integrity, as well as constraining paleo-tectonic stress regimes.

  8. Variation of Static-PPP Positioning Accuracy Using GPS-Single Frequency Observations (Aswan, Egypt)

    NASA Astrophysics Data System (ADS)

    Farah, Ashraf

    2017-06-01

    Precise Point Positioning (PPP) is a technique used for position computation with a high accuracy using only one GNSS receiver. It depends on highly accurate satellite position and clock data rather than broadcast ephemeries. PPP precision varies based on positioning technique (static or kinematic), observations type (single or dual frequency) and the duration of collected observations. PPP-(dual frequency receivers) offers comparable accuracy to differential GPS. PPP-single frequency receivers has many applications such as infrastructure, hydrography and precision agriculture. PPP using low cost GPS single-frequency receivers is an area of great interest for millions of users in developing countries such as Egypt. This research presents a study for the variability of single frequency static GPS-PPP precision based on different observation durations.

  9. Energy-banded ions in Saturn's magnetosphere

    NASA Astrophysics Data System (ADS)

    Thomsen, M. F.; Badman, S. V.; Jackman, C. M.; Jia, X.; Kivelson, M. G.; Kurth, W. S.

    2017-05-01

    Using data from the Cassini Plasma Spectrometer ion mass spectrometer, we report the first observation of energy-banded ions at Saturn. Observed near midnight at relatively high magnetic latitudes, the banded ions are dominantly H+, and they occupy the range of energies typically associated with the thermal pickup distribution in the inner magnetosphere (L < 10), but their energies decline monotonically with increasing radial distance (or time or decreasing latitude). Their pitch angle distribution suggests a source at low (or slightly southern) latitudes. The band energies, including their pitch angle dependence, are consistent with a bounce-resonant interaction between thermal H+ ions and the standing wave structure of a field line resonance. There is additional evidence in the pitch angle dependence of the band energies that the particles in each band may have a common time of flight from their most recent interaction with the wave, which may have been at slightly southern latitudes. Thus, while the particles are basically bounce resonant, their energization may be dominated by their most recent encounter with the standing wave.Plain Language SummaryDuring an outbound passage by the Cassini spacecraft through Saturn's inner magnetosphere, ion energy distributions were <span class="hlt">observed</span> that featured discrete flux peaks at regularly spaced energies. The peaks persisted over several hours and several Saturn radii of distance away from the planet. We show that these "<span class="hlt">bands</span>" of ions are plausibly the result of an interaction between the Saturnian plasma and standing waves that form along the magnetospheric magnetic field lines. These <span class="hlt">observations</span> are the first reported evidence that such standing waves may be present in the inner magnetosphere, where they could contribute to the radial transport of Saturn's radiation belt particles.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/23185586','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/23185586"><span>Dissociation between active and <span class="hlt">observational</span> learning from <span class="hlt">positive</span> and negative feedback in Parkinsonism.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Kobza, Stefan; Ferrea, Stefano; Schnitzler, Alfons; Pollok, Bettina; Südmeyer, Martin; Bellebaum, Christian</p> <p>2012-01-01</p> <p>Feedback to both actively performed and <span class="hlt">observed</span> behaviour allows adaptation of future actions. <span class="hlt">Positive</span> feedback leads to increased activity of dopamine neurons in the substantia nigra, whereas dopamine neuron activity is decreased following negative feedback. Dopamine level reduction in unmedicated Parkinson's Disease patients has been shown to lead to a negative learning bias, i.e. enhanced learning from negative feedback. Recent findings suggest that the neural mechanisms of active and <span class="hlt">observational</span> learning from feedback might differ, with the striatum playing a less prominent role in <span class="hlt">observational</span> learning. Therefore, it was hypothesized that unmedicated Parkinson's Disease patients would show a negative learning bias only in active but not in <span class="hlt">observational</span> learning. In a between-group design, 19 Parkinson's Disease patients and 40 healthy controls engaged in either an active or an <span class="hlt">observational</span> probabilistic feedback-learning task. For both tasks, transfer phases aimed to assess the bias to learn better from <span class="hlt">positive</span> or negative feedback. As expected, actively learning patients showed a negative learning bias, whereas controls learned better from <span class="hlt">positive</span> feedback. In contrast, no difference between patients and controls emerged for <span class="hlt">observational</span> learning, with both groups showing better learning from <span class="hlt">positive</span> feedback. These findings add to neural models of reinforcement-learning by suggesting that dopamine-modulated input to the striatum plays a minor role in <span class="hlt">observational</span> learning from feedback. Future research will have to elucidate the specific neural underpinnings of <span class="hlt">observational</span> learning.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1371527-conduction-band-position-tuning-ga-doping-cd-zn-alloy-thin-films','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1371527-conduction-band-position-tuning-ga-doping-cd-zn-alloy-thin-films"><span>Conduction <span class="hlt">band</span> <span class="hlt">position</span> tuning and Ga-doping in (Cd,Zn)S alloy thin films</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Baranowski, Lauryn L.; Christensen, Steven; Welch, Adam W.; ...</p> <p>2017-02-13</p> <p>In recent years, the number of novel photovoltaic absorber materials under exploration has rapidly increased. However, to reap the most benefit from these new absorbers, alternative device structures and components must also be considered. In particular, the choice of a heterojunction partner, or contact layer, is critical to device optimization. In this work, we explore alternative n-type contact layer candidates that could be widely applicable to a variety of new absorbers. We use theory to calculate the <span class="hlt">band</span> edge tuning provided by a variety of II-VI alloy systems, and select the (Cd,Zn)S system as one that affords a wide rangemore » of conduction <span class="hlt">band</span> tuning. The synthesis of (Cd,Zn)S alloys is explored using atomic layer deposition, which afforded precise compositional control and produced crystalline thin films. The predicted tuning of the <span class="hlt">band</span> gap and conduction <span class="hlt">band</span> minimum is confirmed through X-ray photoelectron spectroscopy and optical absorption measurements. In addition, we investigated Ga-doping in Cd 0.6Zn 0.4S films to decrease their series resistance when used as contact layers in photovoltaic devices. In conclusion, this study provides a framework for exploring and optimizing alternative contact layer materials, which will prove critical to the success of new PV absorbers.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3764527','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3764527"><span>First report on C-<span class="hlt">banding</span>, fluorochrome staining and NOR location in holocentric chromosomes of Elasmolomus (Aphanus) sordidus Fabricius, 1787 (Heteroptera, Rhyparochromidae)</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Suman, Vikas; Kaur, Harbhajan</p> <p>2013-01-01</p> <p>Abstract In spite of various cytogenetic works on suborder Heteroptera, the chromosome organization, function and its evolution in this group is far from being fully understood. Cytologically, the family Rhyparochromidae constitutes a heterogeneous group differing in chromosome numbers. This family possesses XY sex mechanism in the majority of the species with few exceptions. In the present work, multiple <span class="hlt">banding</span> techniques viz., C-<span class="hlt">banding</span>, base-specific fluorochromes (DAPI/CMA3) and silver nitrate staining have been used to cytologically characterize the chromosomes of the seed plant pest Elasmolomus (Aphanus) sordidus Fabricius, 1787 having 2n=12=8A+2m+XY. One pair of the autosomes was large while three others were of almost equal size. At diplotene, C-<span class="hlt">banding</span> technique revealed, that three autosomal bivalents show terminal constitutive heterochromatic <span class="hlt">bands</span> while one medium sized bivalent was euchromatic. Microchromosomes (m-chromosomes) were <span class="hlt">positively</span> heteropycnotic. After DAPI and CMA3 staining, all the autosomal bivalents showed equal fluorescence, except CMA3 <span class="hlt">positive</span> signals, <span class="hlt">observed</span> at both telomeric heterochromatic regions of one medium sized autosomal bivalent. Silver nitrate staining further revealed that this chromosome pair carries Nucleolar Organizer Regions (NORs) at the location of CMA3 <span class="hlt">positive</span> signals. The X chromosome showed a thick C-<span class="hlt">band</span>, <span class="hlt">positive</span> to both DAPI /CMA3 while Y, otherwise C-negative, was weakly <span class="hlt">positive</span> to DAPI and negative to CMA3, m-chromosomes were DAPI bright and CMA3 dull. PMID:24039525</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018JGRC..123.1924P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018JGRC..123.1924P"><span>Oil Slick <span class="hlt">Observation</span> at Low Incidence Angles in Ku-<span class="hlt">Band</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Panfilova, M. A.; Karaev, V. Y.; Guo, Jie</p> <p>2018-03-01</p> <p>On the 20 April 2010 the oil platform Deep Water Horizon in the Gulf of Mexico suffered an explosion during the final phases of drilling an exploratory well. As a result, an oil film covered the sea surface area of several thousand square kilometers. In the present paper the data of the Ku-<span class="hlt">band</span> Precipitation Radar, which operates at low incidence angles, were used to explore the oil spill event. The two-scale model of the scattering surface was used to describe radar backscatter from the sea surface. The algorithm for retrieval of normalized radar cross section at nadir and the total slope variance of large-scale waves compared to the wavelength of electromagnetic wave (22 mm) was developed for the Precipitation Radar swath. It is shown that measurements at low incidence angles can be used for oil spill detection. This is the first time that the dependence of mean square slope of large-scale waves on wind speed has been obtained for oil slicks from Ku-<span class="hlt">band</span> data, and compared to mean square slope obtained by Cox and Munk from optical data.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19850046049&hterms=Auto&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3DAuto','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19850046049&hterms=Auto&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3DAuto"><span>Polycyclic aromatic hydrocarbons and the unidentified infrared emission <span class="hlt">bands</span> - Auto exhaust along the Milky Way</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Allamandola, L. J.; Tielens, A. G. G. M.; Barker, J. R.</p> <p>1985-01-01</p> <p>The unidentified infrared emission features (UIR <span class="hlt">bands</span>) are attributed to a collection of partially hydrogenated, <span class="hlt">positively</span> charged polycyclic aromatic hydrocarbons (PAHs). This assignment is based on a spectroscopic analysis of the UIR <span class="hlt">bands</span>. Comparison of the <span class="hlt">observed</span> interstellar 6.2 and 7.7-micron <span class="hlt">bands</span> with the laboratory measured Raman spectrum of a collection of carbon-based particulates (auto exhaust) shows a very good agreement, supporting this identification. The infrared emission is due to relaxation from highly vibrationally and electronically excited states. The excitation is probably caused by UV photon absorption. The infrared fluorescence of one particular, highly vibrationally excited PAH (chrysene) is modeled. In this analysis the species is treated as a molecule rather than bulk material and the non-thermodynamic equilibrium nature of the emission is fully taken into account. From a comparison of the <span class="hlt">observed</span> ratio of the 3.3 to 11.3-micron UIR <span class="hlt">bands</span> with the model calculations, the average number of carbon atoms per molecule is estimated to be about 20. The abundance of interstellar PAHs is calculated to be about 2 x 10 to the -7th with respect to hydrogen.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20080038044&hterms=Time+series&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D90%26Ntt%3DTime%2Bseries','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20080038044&hterms=Time+series&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D90%26Ntt%3DTime%2Bseries"><span>A Vegetation Correction Methodology for Time Series Based Soil Moisture Retrieval From C-<span class="hlt">band</span> Radar <span class="hlt">Observations</span></span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Joseph, Alicia T.; O'Neil, P. E.; vanderVelde, R.; Gish, T.</p> <p>2008-01-01</p> <p>A methodology is presented to correct backscatter (sigma(sup 0)) <span class="hlt">observations</span> for the effect of vegetation. The proposed methodology is based on the concept that the ratio of the surface scattering over the total amount of scattering (sigma(sup 0)(sub soil)/sigma(sup 0)) is only affected by the vegetation and can be described as a function of the vegetation water content. Backscatter <span class="hlt">observations</span> sigma(sup 0) from the soil are not influenced by vegetation. Under bare soil conditions (sigma(sup 0)(sub soil)/sigma(sup 0)) equals 1. Under low to moderate biomass and soil moisture conditions, vegetation affects the <span class="hlt">observed</span> sigma(sup 0) through absorption of the surface scattering and contribution of direct scattering by the vegetation itself. Therefore, the contribution of the surface scattering is smaller than the <span class="hlt">observed</span> total amount of scattering and decreases as the biomass increases. For dense canopies scattering interactions between the soil surface and vegetation elements (e.g. leaves and stems) also become significant. Because these higher order scattering mechanisms are influenced by the soil surface, an increase in (sigma(sup 0)(sub soil)/sigma(sup 0)) may be <span class="hlt">observed</span> as the biomass increases under densely vegetated conditions. This methodology is applied within the framework of time series based approach for the retrieval of soil moisture. The data set used for this investigation has been collected during a campaign conducted at USDA's Optimizing Production Inputs for Economic and Environmental Enhancement OPE-3) experimental site in Beltsville, Maryland (USA). This campaign took place during the corn growth cycle from May 10th to 0ctober 2nd, 2002. In this period the corn crops reached a vegetation water content of 5.1 kg m(exp -2) at peak biomass and a soil moisture range varying between 0.00 to 0.26 cubic cm/cubic cm. One of the deployed microwave instruments operated was a multi-frequency (C-<span class="hlt">band</span> (4.75 GHz) and L-<span class="hlt">band</span> (1.6 GHz)) quad-polarized (HH, HV</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/11852898','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/11852898"><span>A study of blood contamination of Siqveland matrix <span class="hlt">bands</span>.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Lowe, A H; Bagg, J; Burke, F J T; MacKenzie, D; McHugh, S</p> <p>2002-01-12</p> <p>AIMS To use a sensitive forensic test to measure blood contamination of used Siqveland matrix <span class="hlt">bands</span> following routine cleaning and sterilisation procedures in general dental practice. Sixteen general dental practices in the West of Scotland participated. Details of instrument cleaning procedures were recorded for each practice. A total of 133 Siqveland matrix <span class="hlt">bands</span> were recovered following cleaning and sterilisation and were examined for residual blood contamination by the Kastle-Meyer test, a well-recognised forensic technique. Ultrasonic baths were used for the cleaning of 62 (47%) <span class="hlt">bands</span> and retainers and the remainder (53%) were hand scrubbed prior to autoclaving. Overall, 21% of the matrix <span class="hlt">bands</span> and 19% of the retainers gave a <span class="hlt">positive</span> Kastle-Meyer test, indicative of residual blood contamination, following cleaning and sterilisation. In relation to cleaning method, 34% of hand-scrubbed <span class="hlt">bands</span> and 32% of hand-scrubbed retainers were <span class="hlt">positive</span> for residual blood by the Kastle-Meyer test compared with 6% and 3% respectively of ultrasonically cleaned <span class="hlt">bands</span> and retainers (P < 0.001). If Siqveland matrix <span class="hlt">bands</span> are re-processed in the assembled state, then adequate pre-sterilisation cleaning cannot be achieved reliably. Ultrasonic baths are significantly more effective than hand cleaning for these items of equipment.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016JAP...119e5702K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016JAP...119e5702K"><span>Multi-<span class="hlt">band</span> analysis of temperature-dependent transport coefficients (conductivity, Hall, Seebeck, and Nernst) of Ni-doped CoSb3</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kajikawa, Y.</p> <p>2016-02-01</p> <p>The experimental data on the temperature dependence of the four transport coefficients, i.e., the electrical conductivity (σ), Hall coefficient (RH), Seebeck coefficient (S), and Nernst coefficient (Q), of n-type Co0.999Ni0.001Sb3 reported by Sun et al. [Nat. Commun. 6, 7475 (2015)] have been analyzed in a multi-<span class="hlt">band</span> model, especially focusing on the low temperature data. The multi-<span class="hlt">band</span> model includes not only the lowest valley of the conduction <span class="hlt">band</span> at the Γ point but also satellite valleys at the second minima together with an impurity <span class="hlt">band</span>. The lowest valley at the Γ point is assumed to split into the c1 <span class="hlt">band</span> and the spin-orbit split-off (so) <span class="hlt">band</span>. For the analysis, the general expression of the Nernst coefficient in the multi-<span class="hlt">band</span> model is derived. At such low temperatures that the other <span class="hlt">bands</span> than the c1 and the impurity <span class="hlt">band</span> can be neglected, this expression is shown to be approximated as the sum of three terms: the intrinsic terms due to the Nernst coefficients in the two <span class="hlt">bands</span> themselves and a cross term proportional to the difference of Seebeck coefficients between the two <span class="hlt">bands</span>. As a result of the analysis, it is proved that the anomalous <span class="hlt">positive</span> peak of S(T) <span class="hlt">observed</span> around T = 20 K as well as the sharp rise of the Hall mobility <span class="hlt">observed</span> from 15 K to 40 K are due to the transition from hopping conduction in the impurity <span class="hlt">band</span> to conduction in the c1 <span class="hlt">band</span>. On the other hand, the pronounced peak of Q(T) <span class="hlt">observed</span> slightly below 40 K is proved to be due to the cross term between the impurity <span class="hlt">band</span> and the c1 <span class="hlt">band</span>. In addition, a shoulder of Q(T) appeared around T = 80 K lends clear evidence of the existence of the so <span class="hlt">band</span>, while the increase in both of σ(T) and | S ( T ) | above 150 K suggests the existence of the satellite valleys.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28947824','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28947824"><span>Direct <span class="hlt">observation</span> of mode-specific phonon-<span class="hlt">band</span> gap coupling in methylammonium lead halide perovskites.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Kim, Heejae; Hunger, Johannes; Cánovas, Enrique; Karakus, Melike; Mics, Zoltán; Grechko, Maksim; Turchinovich, Dmitry; Parekh, Sapun H; Bonn, Mischa</p> <p>2017-09-25</p> <p>Methylammonium lead iodide perovskite is an outstanding semiconductor for photovoltaics. One of its intriguing peculiarities is that the <span class="hlt">band</span> gap of this perovskite increases with increasing lattice temperature. Despite the presence of various thermally accessible phonon modes in this soft material, the understanding of how precisely these phonons affect macroscopic material properties and lead to the peculiar temperature dependence of the <span class="hlt">band</span> gap has remained elusive. Here, we report a strong coupling of a single phonon mode at the frequency of ~ 1 THz to the optical <span class="hlt">band</span> gap by monitoring the transient <span class="hlt">band</span> edge absorption after ultrafast resonant THz phonon excitation. Excitation of the 1 THz phonon causes a blue shift of the <span class="hlt">band</span> gap over the temperature range of 185 ~ 300 K. Our results uncover the mode-specific coupling between one phonon and the optical properties, which contributes to the temperature dependence of the gap in the tetragonal phase.Methylammonium lead iodide perovskite, a promising material for efficient photovoltaics, shows a unique temperature dependence of its optical properties. Kim et al. quantify the coupling between the optical gap and a lattice phonon at 1 THz, which favorably contributes to the thermal variation of the gap.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014ASPC..485...95L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014ASPC..485...95L"><span>Cone of Darkness: Finding Blank-sky <span class="hlt">Positions</span> for Multi-object Wide-field <span class="hlt">Observations</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Lorente, N. P. F.</p> <p>2014-05-01</p> <p>We present the Cone of Darkness, an application to automatically configure blank-sky <span class="hlt">positions</span> for a series of stacked, wide-field <span class="hlt">observations</span>, such as those carried out by the SAMI instrument on the Anglo-Australian Telescope (AAT). The Sydney-AAO Multi-object Integral field spectrograph (SAMI) uses a plug-plate to mount its 13×61 core imaging fibre bundles (hexabundles) in the optical plane at the telescope's prime focus. To make the most efficient use of each plug-plate, several <span class="hlt">observing</span> fields are typically stacked to produce a single plate. When choosing blank-sky <span class="hlt">positions</span> for the <span class="hlt">observations</span> it is most effective to select these such that one set of 26 holes gives valid sky <span class="hlt">positions</span> for all fields on the plate. However, when carried out manually this selection process is tedious and includes a significant risk of error. The Cone of Darkness software aims to provide uniform blank-sky <span class="hlt">position</span> coverage over the field of <span class="hlt">observation</span>, within the limits set by the distribution of target <span class="hlt">positions</span> and the chosen input catalogs. This will then facilitate the production of the best representative median sky spectrum for use in sky subtraction. The application, written in C++, is configurable, making it usable for a range of instruments. Given the plate characteristics and the <span class="hlt">positions</span> of target holes, the software segments the unallocated space on the plate and determines the <span class="hlt">position</span> which best fits the uniform distribution requirement. This <span class="hlt">position</span> is checked, for each field, against the selected catalog using a TAP ADQL search. The process is then repeated until the desired number of sky <span class="hlt">positions</span> is attained.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018PhRvC..97b4308H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018PhRvC..97b4308H"><span>Multiple <span class="hlt">band</span> structures in 70Ge</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Haring-Kaye, R. A.; Morrow, S. I.; Döring, J.; Tabor, S. L.; Le, K. Q.; Allegro, P. R. P.; Bender, P. C.; Elder, R. M.; Medina, N. H.; Oliveira, J. R. B.; Tripathi, Vandana</p> <p>2018-02-01</p> <p>High-spin states in 70Ge were studied using the 55Mn(18O,p 2 n ) fusion-evaporation reaction at a beam energy of 50 MeV. Prompt γ -γ coincidences were measured using the Florida State University Compton-suppressed Ge array consisting of three Clover detectors and seven single-crystal detectors. An investigation of these coincidences resulted in the addition of 31 new transitions and the rearrangement of four others in the 70Ge level scheme, providing a more complete picture of the high-spin decay pattern involving both <span class="hlt">positive</span>- and negative-parity states with multiple <span class="hlt">band</span> structures. Spins were assigned based on directional correlation of oriented nuclei ratios, which many times also led to unambiguous parity determinations based on the firm assignments for low-lying states made in previous work. Total Routhian surface calculations, along with the <span class="hlt">observed</span> trends in the experimental kinematic moment of inertia with rotational frequency, support the multiquasiparticle configurations of the various crossing <span class="hlt">bands</span> proposed in recent studies. The high-spin excitation spectra predicted by previous shell-model calculations compare favorably with the experimental one determined from this study.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_9");'>9</a></li> <li><a href="#" onclick='return showDiv("page_10");'>10</a></li> <li class="active"><span>11</span></li> <li><a href="#" onclick='return showDiv("page_12");'>12</a></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_11 --> <div id="page_12" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_10");'>10</a></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li class="active"><span>12</span></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="221"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3503978','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3503978"><span>Dissociation between Active and <span class="hlt">Observational</span> Learning from <span class="hlt">Positive</span> and Negative Feedback in Parkinsonism</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Kobza, Stefan; Ferrea, Stefano; Schnitzler, Alfons; Pollok, Bettina</p> <p>2012-01-01</p> <p>Feedback to both actively performed and <span class="hlt">observed</span> behaviour allows adaptation of future actions. <span class="hlt">Positive</span> feedback leads to increased activity of dopamine neurons in the substantia nigra, whereas dopamine neuron activity is decreased following negative feedback. Dopamine level reduction in unmedicated Parkinson’s Disease patients has been shown to lead to a negative learning bias, i.e. enhanced learning from negative feedback. Recent findings suggest that the neural mechanisms of active and <span class="hlt">observational</span> learning from feedback might differ, with the striatum playing a less prominent role in <span class="hlt">observational</span> learning. Therefore, it was hypothesized that unmedicated Parkinson’s Disease patients would show a negative learning bias only in active but not in <span class="hlt">observational</span> learning. In a between-group design, 19 Parkinson’s Disease patients and 40 healthy controls engaged in either an active or an <span class="hlt">observational</span> probabilistic feedback-learning task. For both tasks, transfer phases aimed to assess the bias to learn better from <span class="hlt">positive</span> or negative feedback. As expected, actively learning patients showed a negative learning bias, whereas controls learned better from <span class="hlt">positive</span> feedback. In contrast, no difference between patients and controls emerged for <span class="hlt">observational</span> learning, with both groups showing better learning from <span class="hlt">positive</span> feedback. These findings add to neural models of reinforcement-learning by suggesting that dopamine-modulated input to the striatum plays a minor role in <span class="hlt">observational</span> learning from feedback. Future research will have to elucidate the specific neural underpinnings of <span class="hlt">observational</span> learning. PMID:23185586</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017AGUFM.H21E1507Z','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017AGUFM.H21E1507Z"><span>Comparison of High Resolution Quantitative Extreme Precipitation Estimation from GPM Dual-frequency Radar and S-<span class="hlt">band</span> Radar <span class="hlt">Observation</span> over Southern China</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Zhang, A.; Chen, S.; Fan, S.; Min, C.</p> <p>2017-12-01</p> <p>Precipitation is one of the basic elements of regional and global climate change. Not only does the precipitation have a great impact on the earth's hydrosphere, but also plays a crucial role in the global energy balance. S-<span class="hlt">band</span> ground-based dual-polarization radar has the excellent performance of identifying the different phase states of precipitation, which can dramatically improve the accuracy of hail identification and quantitative precipitation estimation (QPE). However, the ground-based radar cannot measure the precipitation in mountains, sparsely populated plateau, desert and ocean because of the ground-based radar void. The Unites States National Aeronautics and Space Administration (NASA) and Japan Aerospace Exploration Agency (JAXA) have launched the Global Precipitation Measurement (GPM) for almost three years. GPM is equipped with a GPM Microwave Imager (GMI) and a Dual-frequency (Ku- and Ka-<span class="hlt">band</span>) Precipitation Radar (DPR) that covers the globe between 65°S and 65°N. The main parameters and the detection method of DPR are different from those of ground-based radars, thus, the DPR's reliability and capability need to be investigated and evaluated by the ground-based radar. This study compares precipitation derived from the ground-based radar measurement to that derived from the DPR's <span class="hlt">observations</span>. The ground-based radar is a S-<span class="hlt">band</span> dual-polarization radar deployed near an airport in the west of Zhuhai city. The ground-based quantitative precipitation estimates are with a high resolution of 1km×1km×6min. It shows that this radar covers the whole Pearl River Delta of China, including Hong Kong and Macao. In order to quantify the DPR precipitation quantification capabilities relative to the S-<span class="hlt">band</span> radar, statistical metrics used in this study are as follows: the difference (Dif) between DPR and the S-<span class="hlt">band</span> radar <span class="hlt">observation</span>, root-mean-squared error (RMSE) and correlation coefficient (CC). Additionally, Probability of Detection (POD) and False Alarm Ratio</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017ApJS..230....9N','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017ApJS..230....9N"><span>An Application of Multi-<span class="hlt">band</span> Forced Photometry to One Square Degree of SERVS: Accurate Photometric Redshifts and Implications for Future Science</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Nyland, Kristina; Lacy, Mark; Sajina, Anna; Pforr, Janine; Farrah, Duncan; Wilson, Gillian; Surace, Jason; Häußler, Boris; Vaccari, Mattia; Jarvis, Matt</p> <p>2017-05-01</p> <p>We apply The Tractor image modeling code to improve upon existing multi-<span class="hlt">band</span> photometry for the Spitzer Extragalactic Representative Volume Survey (SERVS). SERVS consists of post-cryogenic Spitzer <span class="hlt">observations</span> at 3.6 and 4.5 μm over five well-studied deep fields spanning 18 deg2. In concert with data from ground-based near-infrared (NIR) and optical surveys, SERVS aims to provide a census of the properties of massive galaxies out to z ≈ 5. To accomplish this, we are using The Tractor to perform “forced photometry.” This technique employs prior measurements of source <span class="hlt">positions</span> and surface brightness profiles from a high-resolution fiducial <span class="hlt">band</span> from the VISTA Deep Extragalactic <span class="hlt">Observations</span> survey to model and fit the fluxes at lower-resolution <span class="hlt">bands</span>. We discuss our implementation of The Tractor over a square-degree test region within the XMM Large Scale Structure field with deep imaging in 12 NIR/optical <span class="hlt">bands</span>. Our new multi-<span class="hlt">band</span> source catalogs offer a number of advantages over traditional <span class="hlt">position</span>-matched catalogs, including (1) consistent source cross-identification between <span class="hlt">bands</span>, (2) de-blending of sources that are clearly resolved in the fiducial <span class="hlt">band</span> but blended in the lower resolution SERVS data, (3) a higher source detection fraction in each <span class="hlt">band</span>, (4) a larger number of candidate galaxies in the redshift range 5 < z < 6, and (5) a statistically significant improvement in the photometric redshift accuracy as evidenced by the significant decrease in the fraction of outliers compared to spectroscopic redshifts. Thus, forced photometry using The Tractor offers a means of improving the accuracy of multi-<span class="hlt">band</span> extragalactic surveys designed for galaxy evolution studies. We will extend our application of this technique to the full SERVS footprint in the future.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22661122-application-multi-band-forced-photometry-one-square-degree-servs-accurate-photometric-redshifts-implications-future-science','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22661122-application-multi-band-forced-photometry-one-square-degree-servs-accurate-photometric-redshifts-implications-future-science"><span>An Application of Multi-<span class="hlt">band</span> Forced Photometry to One Square Degree of SERVS: Accurate Photometric Redshifts and Implications for Future Science</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Nyland, Kristina; Lacy, Mark; Sajina, Anna</p> <p></p> <p>We apply The Tractor image modeling code to improve upon existing multi-<span class="hlt">band</span> photometry for the Spitzer Extragalactic Representative Volume Survey (SERVS). SERVS consists of post-cryogenic Spitzer <span class="hlt">observations</span> at 3.6 and 4.5 μ m over five well-studied deep fields spanning 18 deg{sup 2}. In concert with data from ground-based near-infrared (NIR) and optical surveys, SERVS aims to provide a census of the properties of massive galaxies out to z  ≈ 5. To accomplish this, we are using The Tractor to perform “forced photometry.” This technique employs prior measurements of source <span class="hlt">positions</span> and surface brightness profiles from a high-resolution fiducial <span class="hlt">band</span> from themore » VISTA Deep Extragalactic <span class="hlt">Observations</span> survey to model and fit the fluxes at lower-resolution <span class="hlt">bands</span>. We discuss our implementation of The Tractor over a square-degree test region within the XMM Large Scale Structure field with deep imaging in 12 NIR/optical <span class="hlt">bands</span>. Our new multi-<span class="hlt">band</span> source catalogs offer a number of advantages over traditional <span class="hlt">position</span>-matched catalogs, including (1) consistent source cross-identification between <span class="hlt">bands</span>, (2) de-blending of sources that are clearly resolved in the fiducial <span class="hlt">band</span> but blended in the lower resolution SERVS data, (3) a higher source detection fraction in each <span class="hlt">band</span>, (4) a larger number of candidate galaxies in the redshift range 5 <  z  < 6, and (5) a statistically significant improvement in the photometric redshift accuracy as evidenced by the significant decrease in the fraction of outliers compared to spectroscopic redshifts. Thus, forced photometry using The Tractor offers a means of improving the accuracy of multi-<span class="hlt">band</span> extragalactic surveys designed for galaxy evolution studies. We will extend our application of this technique to the full SERVS footprint in the future.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012AGUFM.C12A..07K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012AGUFM.C12A..07K"><span>Addressing sub-scan variability of tundra snow properties in ground-based Ku- and X-<span class="hlt">band</span> scatterometer <span class="hlt">observations</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>King, J. M.; Kasurak, A.; Kelly, R. E.; Duguay, C. R.; Derksen, C.; Rutter, N.; Sandells, M.; Watts, T.</p> <p>2012-12-01</p> <p>During the winter of 2010-2011 ground-based Ku- (17.2 GHz) and X-<span class="hlt">band</span> (9.6 GHz) scatterometers were deployed near Churchill, Manitoba, Canada to evaluate the potential for dual-frequency <span class="hlt">observation</span> of tundra snow properties. Field-based scatterometer <span class="hlt">observations</span> when combined with in-situ snowpack properties and physically based models, provide the means necessary to develop and evaluate local scale property retrievals. To form meaningful analysis of the <span class="hlt">observed</span> physical interaction space, potential sources of bias and error in the <span class="hlt">observed</span> backscatter must be identified and quantified. This paper explores variation in <span class="hlt">observed</span> Ku- and X-<span class="hlt">band</span> backscatter in relation to the physical complexities of shallow tundra snow whose properties evolve at scales smaller than the <span class="hlt">observing</span> instrument. The University of Waterloo scatterometer (UW-Scat) integrates <span class="hlt">observations</span> over wide azimuth sweeps, several meters in length, to minimize errors resulting from radar fade and poor signal-to-noise ratios. Under ideal conditions, an assumption is made that the <span class="hlt">observed</span> snow target is homogeneous. Despite an often-outward appearance of homogeneity, topographic elements of the Canadian open tundra produce significant local scale variability in snow properties, including snow water equivalent (SWE). Snow at open tundra sites <span class="hlt">observed</span> during this campaign was found to vary by as much as 20 cm in depth and 40 mm in SWE within the scatterometer field of view. Previous studies suggest that changes in snow properties on this order will produce significant variation in backscatter, potentially introducing bias into products used for analysis. To assess the influence of sub-scan variability, extensive snow surveys were completed within the scatterometer field of view immediately after each scan at 32 sites. A standardized sampling protocol captured a grid of geo-located measurements, characterizing the horizontal variability of bulk properties including depth, density, and SWE. Based upon</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017AnGeo..35.1069P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017AnGeo..35.1069P"><span>Statistical study of auroral omega <span class="hlt">bands</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Partamies, Noora; Weygand, James M.; Juusola, Liisa</p> <p>2017-09-01</p> <p>The presence of very few statistical studies on auroral omega <span class="hlt">bands</span> motivated us to test-use a semi-automatic method for identifying large-scale undulations of the diffuse aurora boundary and to investigate their occurrence. Five identical all-sky cameras with overlapping fields of view provided data for 438 auroral omega-like structures over Fennoscandian Lapland from 1996 to 2007. The results from this set of omega <span class="hlt">band</span> events agree remarkably well with previous <span class="hlt">observations</span> of omega <span class="hlt">band</span> occurrence in magnetic local time (MLT), lifetime, location between the region 1 and 2 field-aligned currents, as well as current density estimates. The average peak emission height of omega forms corresponds to the estimated precipitation energies of a few keV, which experienced no significant change during the events. Analysis of both local and global magnetic indices demonstrates that omega <span class="hlt">bands</span> are <span class="hlt">observed</span> during substorm expansion and recovery phases that are more intense than average substorm expansion and recovery phases in the same region. The omega occurrence with respect to the substorm expansion and recovery phases is in a very good agreement with an earlier <span class="hlt">observed</span> distribution of fast earthward flows in the plasma sheet during expansion and recovery phases. These findings support the theory that omegas are produced by fast earthward flows and auroral streamers, despite the rarity of good conjugate <span class="hlt">observations</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20140002677','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20140002677"><span>Equatorial Precession in the Control Software of the Ka-<span class="hlt">Band</span> Object <span class="hlt">Observation</span> and Monitoring Experiment</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Jakeman, Hali L.</p> <p>2013-01-01</p> <p>The Ka-<span class="hlt">Band</span> Object <span class="hlt">Observation</span> and Monitoring, or KaBOOM, project is designed mainly to track and characterize near Earth objects. However, a smaller goal of the project would be to monitor pulsars and study their radio frequency signals for use as a clock in interstellar travel. The use of pulsars and their timing accuracy has been studied for decades, but never in the Ka-<span class="hlt">band</span> of the radio frequency spectrum. In order to begin the use of KaBOOM for this research, the control systems need to be analyzed to ensure its capability. Flaws in the control documentation leave it unclear as to whether the control software processes coordinates from the J200 epoch. This experiment will examine the control software of the Intertronic 12m antennas used for the KaBOOM project and detail its capabilities in its "equatorial mode." The antennas will be pointed at 4 chosen points in the sky on several days while probing the virtual azimuth and elevation (horizon coordinate) registers. The input right ascension and declination coordinates will then be converted separately from the control software to horizontal coordinates and compared, thus determining the ability of the control software to process equatorial coordinates.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018GeoRL..45.1218L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018GeoRL..45.1218L"><span>Flow Shears at the Poleward Boundary of Omega <span class="hlt">Bands</span> <span class="hlt">Observed</span> During Conjunctions of Swarm and THEMIS ASI</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Liu, Jiang; Lyons, L. R.; Archer, W. E.; Gallardo-Lacourt, B.; Nishimura, Y.; Zou, Ying; Gabrielse, C.; Weygand, J. M.</p> <p>2018-02-01</p> <p>Omega <span class="hlt">bands</span> are curved aurora forms that evolve from a quiet arc located along the poleward edge of a diffuse auroral <span class="hlt">band</span> within the midnight to morningside auroral oval. They usually propagate eastward. Because omega <span class="hlt">bands</span> are a significant contributor to an active magnetotail, knowledge about their generation is important for understanding tail dynamics. Previous studies have shown that auroral streamers, footprints of fast flows in the tail, can propagate into omega <span class="hlt">bands</span>. Such events, however, are limited, and it is still unclear whether and how the flows trigger the <span class="hlt">bands</span>. The ionospheric flows associated with omega <span class="hlt">bands</span> may provide valuable information on the driving mechanisms of the <span class="hlt">bands</span>. We examine these flows taking advantage of the conjunctions between the Swarm spacecraft and Time History of Events and Macroscale Interactions during Substorms all-sky imagers, which allow us to demonstrate the relative location of the flows to the omega <span class="hlt">bands</span>' bright arcs for the first time. We find that a strong eastward ionospheric flow is consistently present immediately poleward of the omega <span class="hlt">band</span>'s bright arc, resulting in a sharp flow shear near the poleward boundary of the <span class="hlt">band</span>. This ionospheric flow shear should correspond to a flow shear near the inner edge of the plasma sheet. This plasma sheet shear may drive a Kelvin-Helmholz instability which then distorts the quiet arc to form omega <span class="hlt">bands</span>. It seems plausible that the strong eastward flows are driven by streamer-related fast flows or enhanced convection in the magnetotail.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.jstor.org/stable/3809358','USGSPUBS'); return false;" href="http://www.jstor.org/stable/3809358"><span>Neck-<span class="hlt">band</span> retention for Canada geese in the Mississippi (USA) flyway</span></a></p> <p><a target="_blank" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p>Samuel, M.D.; Weiss, N.T.; Rusch, D.H.; Craven, S.R.; Trost, R.E.; Caswell, F.D.</p> <p>1990-01-01</p> <p>We used capture, harvest, and <span class="hlt">observation</span> histories of Canada geese (Branta canadensis) <span class="hlt">banded</span> in the Mississippi flyway, 1974-88, to examine the problem of neck-<span class="hlt">band</span> retention. Methods for the analysis of survival data were used to estimate rates of neck-<span class="hlt">band</span> retention and to evaluate factors associated with neck-<span class="hlt">band</span> loss. Sex, age of bird at <span class="hlt">banding</span>, rivet use, and neck-<span class="hlt">band</span> type significantly influenced neck-<span class="hlt">band</span> retention. For most of the resulting cohorts (e.g., sex, age, rivet, and neck-<span class="hlt">band</span> type categories), neck-<span class="hlt">band</span> retention rates decreased through time. We caution against using small samples or data collected during short-term studies to determine retention rates. We suggest that <span class="hlt">observation</span> data be used in neck-<span class="hlt">band</span> retention studies to increase the efficiency of estimating retention time.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2006A%26A...445.1015O','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2006A%26A...445.1015O"><span>High angular resolution N-<span class="hlt">band</span> <span class="hlt">observation</span> of the silicate carbon star IRAS08002-3803 with the VLTI/MIDI instrument . Dusty environment spatially resolved</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ohnaka, K.; Driebe, T.; Hofmann, K.-H.; Leinert, Ch.; Morel, S.; Paresce, F.; Preibisch, Th.; Richichi, A.; Schertl, D.; Schöller, M.; Waters, L. B. F. M.; Weigelt, G.; Wittkowski, M.</p> <p>2006-01-01</p> <p>We present the results of N-<span class="hlt">band</span> spectro-interferometric <span class="hlt">observations</span> of the silicate carbon star IRAS08002-3803 with the MID-infrared Interferometric instrument (MIDI) at the Very Large Telescope Interferometer (VLTI) of the European Southern Observatory (ESO). The <span class="hlt">observations</span> were carried out using two unit telescopes (UT2 and UT3) with projected baseline lengths ranging from 39 to 47 m. Our <span class="hlt">observations</span> of IRAS08002-3803 have spatially resolved the dusty environment of a silicate carbon star for the first time and revealed an unexpected wavelength dependence of the angular size in the N <span class="hlt">band</span>: the uniform-disk diameter is found to be constant and 36 mas (72 Rstar) between 8 and 10 μm, while it steeply increases longward of 10 μm to reach 53 mas (106 Rstar) at 13 μm. Model calculations with our Monte Carlo radiative transfer code show that neither spherical shell models nor axisymmetric disk models consisting of silicate grains alone can simultaneously explain the <span class="hlt">observed</span> wavelength dependence of the visibility and the spectral energy distribution (SED). We propose that the circumstellar environment of IRAS08002-3803 may consist of two grain species coexisting in the disk: silicate and a second grain species, for which we consider amorphous carbon, large silicate grains, and metallic iron grains. Comparison of the <span class="hlt">observed</span> visibilities and SED with our models shows that such disk models can fairly - though not entirely satisfactorily - reproduce the <span class="hlt">observed</span> SED and N-<span class="hlt">band</span> visibilities. Our MIDI <span class="hlt">observations</span> and the radiative transfer calculations lend support to the picture where oxygen-rich material around IRAS08002-3803 is stored in a circumbinary disk surrounding the carbon-rich primary star and its putative low-luminosity companion.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19820009688','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19820009688"><span>Characterizing user requirements for future land <span class="hlt">observing</span> satellites</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Barker, J. L.; Cressy, P. J.; Schnetzler, C. C.; Salomonson, V. V.</p> <p>1981-01-01</p> <p>The objective procedure was developed for identifying probable sensor and mission characteristics for an operational satellite land <span class="hlt">observing</span> system. Requirements were systematically compiled, quantified and scored by type of use, from surveys of federal, state, local and private communities. Incremental percent increases in expected value of data were estimated for critical system improvements. Comparisons with costs permitted selection of a probable sensor system, from a set of 11 options, with the following characteristics: 30 meter spatial resolution in 5 <span class="hlt">bands</span> and 15 meters in 1 <span class="hlt">band</span>, spectral <span class="hlt">bands</span> nominally at Thematic Mapper (TM) <span class="hlt">bands</span> 1 through 6 <span class="hlt">positions</span>, and 2 day data turn around for receipt of imagery. Improvements are suggested for both the form of questions and the procedures for analysis of future surveys in order to provide a more quantitatively precise definition of sensor and mission requirements.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28251847','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28251847"><span>First-Principles Study of the <span class="hlt">Band</span> Diagrams and Schottky-Type Barrier Heights of Aqueous Ta3N5 Interfaces.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Watanabe, Eriko; Ushiyama, Hiroshi; Yamashita, Koichi</p> <p>2017-03-22</p> <p>The photo(electro)chemical production of hydrogen by water splitting is an efficient and sustainable method for the utilization of solar energy. To improve photo(electro)catalytic activity, a Schottky-type barrier is typically useful to separate excited charge carriers in semiconductor electrodes. Here, we focused on studying the <span class="hlt">band</span> diagrams and the Schottky-type barrier heights of Ta 3 N 5 , which is one of the most promising materials as a photoanode for water splitting. The <span class="hlt">band</span> alignments of the undoped and n-type Ta 3 N 5 with adsorbents in a vacuum were examined to determine how impurities and adsorbents affect the <span class="hlt">band</span> <span class="hlt">positions</span> and Fermi energies. The <span class="hlt">band</span> edge <span class="hlt">positions</span> as well as the density of surface states clearly depended on the density of O N impurities in the bulk and surface regions. Finally, the <span class="hlt">band</span> diagrams of the n-type Ta 3 N 5 /water interfaces were calculated with an improved interfacial model to include the effect of electrode potential with explicit water molecules. We <span class="hlt">observed</span> partial Fermi level pinning in our calculations at the Ta 3 N 5 /water interface, which affects the driving force for charge separation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014APS..MARB44008S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014APS..MARB44008S"><span>Relating the defect <span class="hlt">band</span> gap and the density functional <span class="hlt">band</span> gap</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Schultz, Peter; Edwards, Arthur</p> <p>2014-03-01</p> <p>Density functional theory (DFT) is an important tool to probe the physics of materials. The Kohn-Sham (KS) gap in DFT is typically (much) smaller than the <span class="hlt">observed</span> <span class="hlt">band</span> gap for materials in nature, the infamous ``<span class="hlt">band</span> gap problem.'' Accurate prediction of defect energy levels is often claimed to be a casualty--the <span class="hlt">band</span> gap defines the energy scale for defect levels. By applying rigorous control of boundary conditions in size-converged supercell calculations, however, we compute defect levels in Si and GaAs with accuracies of ~0.1 eV, across the full gap, unhampered by a <span class="hlt">band</span> gap problem. Using GaAs as a theoretical laboratory, we show that the defect <span class="hlt">band</span> gap--the span of computed defect levels--is insensitive to variations in the KS gap (with functional and pseudopotential), these KS gaps ranging from 0.1 to 1.1 eV. The defect gap matches the experimental 1.52 eV gap. The computed defect gaps for several other III-V, II-VI, I-VII, and other compounds also agree with the experimental gap, and show no correlation with the KS gap. Where, then, is the <span class="hlt">band</span> gap problem? This talk presents these results, discusses why the defect gap and the KS gap are distinct, implying that current understanding of what the ``<span class="hlt">band</span> gap problem'' means--and how to ``fix'' it--need to be rethought. Sandia National Laboratories is a multi-program laboratory managed and operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Company, for the U.S. Department of Energy's NNSA under contract DE-AC04-94AL85000.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28036221','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28036221"><span>Einstein-Podolsky-Rosen Entanglement of Narrow-<span class="hlt">Band</span> Photons from Cold Atoms.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Lee, Jong-Chan; Park, Kwang-Kyoon; Zhao, Tian-Ming; Kim, Yoon-Ho</p> <p>2016-12-16</p> <p>Einstein-Podolsky-Rosen (EPR) entanglement introduced in 1935 deals with two particles that are entangled in their <span class="hlt">positions</span> and momenta. Here we report the first experimental demonstration of EPR <span class="hlt">position</span>-momentum entanglement of narrow-<span class="hlt">band</span> photon pairs generated from cold atoms. By using two-photon quantum ghost imaging and ghost interference, we demonstrate explicitly that the narrow-<span class="hlt">band</span> photon pairs violate the separability criterion, confirming EPR entanglement. We further demonstrate continuous variable EPR steering for <span class="hlt">positions</span> and momenta of the two photons. Our new source of EPR-entangled narrow-<span class="hlt">band</span> photons is expected to play an essential role in spatially multiplexed quantum information processing, such as, storage of quantum correlated images, quantum interface involving hyperentangled photons, etc.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016PhRvL.117y0501L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016PhRvL.117y0501L"><span>Einstein-Podolsky-Rosen Entanglement of Narrow-<span class="hlt">Band</span> Photons from Cold Atoms</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Lee, Jong-Chan; Park, Kwang-Kyoon; Zhao, Tian-Ming; Kim, Yoon-Ho</p> <p>2016-12-01</p> <p>Einstein-Podolsky-Rosen (EPR) entanglement introduced in 1935 deals with two particles that are entangled in their <span class="hlt">positions</span> and momenta. Here we report the first experimental demonstration of EPR <span class="hlt">position</span>-momentum entanglement of narrow-<span class="hlt">band</span> photon pairs generated from cold atoms. By using two-photon quantum ghost imaging and ghost interference, we demonstrate explicitly that the narrow-<span class="hlt">band</span> photon pairs violate the separability criterion, confirming EPR entanglement. We further demonstrate continuous variable EPR steering for <span class="hlt">positions</span> and momenta of the two photons. Our new source of EPR-entangled narrow-<span class="hlt">band</span> photons is expected to play an essential role in spatially multiplexed quantum information processing, such as, storage of quantum correlated images, quantum interface involving hyperentangled photons, etc.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=21848','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=21848"><span>An empirical basis for Mach <span class="hlt">bands</span></span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Lotto, R. Beau; Williams, S. Mark; Purves, Dale</p> <p>1999-01-01</p> <p>Mach <span class="hlt">bands</span>, the illusory brightness maxima and minima perceived at the initiation and termination of luminance gradients, respectively, are generally considered a direct perceptual manifestation of lateral inhibitory interactions among retinal or other lower order visual neurons. Here we examine an alternative explanation, namely that Mach <span class="hlt">bands</span> arise as a consequence of real-world luminance gradients. In this first of two companion papers, we analyze the natural sources of luminance gradients, demonstrating that real-world gradients arising from curved surfaces are ordinarily adorned by photometric highlights and lowlights in the <span class="hlt">position</span> of the illusory <span class="hlt">bands</span>. The prevalence of such gradients provides an empirical basis for the generation of this perceptual phenomenon. PMID:10220450</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018PhRvL.120m0503T','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018PhRvL.120m0503T"><span>Topological Maxwell Metal <span class="hlt">Bands</span> in a Superconducting Qutrit</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Tan, Xinsheng; Zhang, Dan-Wei; Liu, Qiang; Xue, Guangming; Yu, Hai-Feng; Zhu, Yan-Qing; Yan, Hui; Zhu, Shi-Liang; Yu, Yang</p> <p>2018-03-01</p> <p>We experimentally explore the topological Maxwell metal <span class="hlt">bands</span> by mapping the momentum space of condensed-matter models to the tunable parameter space of superconducting quantum circuits. An exotic <span class="hlt">band</span> structure that is effectively described by the spin-1 Maxwell equations is imaged. Threefold degenerate points dubbed Maxwell points are <span class="hlt">observed</span> in the Maxwell metal <span class="hlt">bands</span>. Moreover, we engineer and <span class="hlt">observe</span> the topological phase transition from the topological Maxwell metal to a trivial insulator, and report the first experiment to measure the Chern numbers that are higher than one.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/20482079','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/20482079"><span>Valence-<span class="hlt">band</span> structure of the ferromagnetic semiconductor GaMnAs studied by spin-dependent resonant tunneling spectroscopy.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Ohya, Shinobu; Muneta, Iriya; Hai, Pham Nam; Tanaka, Masaaki</p> <p>2010-04-23</p> <p>The valence-<span class="hlt">band</span> structure and the Fermi level (E(F)) <span class="hlt">position</span> of ferromagnetic-semiconductor GaMnAs are quantitatively investigated by electrically detecting the resonant tunneling levels of a GaMnAs quantum well (QW) in double-barrier heterostructures. The resonant level from the heavy-hole first state is clearly <span class="hlt">observed</span> in the metallic GaMnAs QW, indicating that holes have a high coherency and that E(F) exists in the <span class="hlt">band</span> gap. Clear enhancement of tunnel magnetoresistance induced by resonant tunneling is demonstrated in these double-barrier heterostructures.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012PhRvC..86d4305W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012PhRvC..86d4305W"><span>Rotational <span class="hlt">band</span> properties of 173W</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wang, H. X.; Zhang, Y. H.; Zhou, X. H.; Liu, M. L.; Ding, B.; Li, G. S.; Hua, W.; Zhou, H. B.; Guo, S.; Qiang, Y. H.; Oshima, M.; Koizumi, M.; Toh, Y.; Kimura, A.; Harada, H.; Furutaka, K.; Kitatani, F.; Nakamura, S.; Hatsukawa, Y.; Ohta, M.; Hara, K.; Kin, T.; Meng, J.</p> <p>2012-10-01</p> <p>High-spin states in 173W have been studied using the 150Nd(28Si,5n)173W reaction at beam energies of 135 and 140 MeV. The previously known <span class="hlt">bands</span> associated with the 7/2+[633], 5/2-[512], and 1/2-[521] configurations are extended significantly, and the unfavored signature branch of the 1/2-[521] <span class="hlt">band</span> is established for the first time. The <span class="hlt">band</span> properties, such as level spacings, <span class="hlt">band</span>-crossing frequencies, alignment gains, and signature splittings, are discussed with an emphasis on the low-spin signature inversion <span class="hlt">observed</span> in the 5/2-[512] <span class="hlt">band</span>. By comparing the experimental B(M1)/B(E2) ratios with the theoretical values, we conclude that the configuration of the 5/2-[512] <span class="hlt">band</span> is quite pure at low spins without appreciable admixture of the 5/2-[523] orbit, in conflict with the particle rotor model calculated results.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017EGUGA..19.1583D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017EGUGA..19.1583D"><span><span class="hlt">Positive</span> and negative ion outflow at Rhea as <span class="hlt">observed</span> by Cassini</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Desai, Ravindra; Jones, Geraint; Regoli, Leonardo; Cowee, Misa; Coates, Andrew; Kataria, Dhiren</p> <p>2017-04-01</p> <p>Rhea is Saturn's largest icy moon and hosts an ethereal oxygen and carbon-dioxide atmosphere as was detected when Cassini <span class="hlt">observed</span> <span class="hlt">positive</span> and negative pickup ions outflowing from the moon and an extended neutral exosphere. These pickup ions can form current systems which, with the resulting jxB force, act to slow-down the incident magneto-plasma and cause field-line draping. As well as impacting the plasma interaction, the composition and density of picked up ions provide key diagnostics of the moon's sputter-induced atmosphere and surface. During the first Cassini-Rhea encounter (R1), the Cassini Plasma Spectrometer (CAPS) <span class="hlt">observed</span> <span class="hlt">positively</span> and negatively charged pickup ions before and after passing through the moon's plasma wake respectively, in agreement with their anticipated cycloidal trajectories. On the subsequent more distant wake encounter (R1.5) however, only <span class="hlt">positively</span> charged pickup ions were <span class="hlt">observed</span>, indicating high loss rates of the negative ions in Saturn's magnetosphere. Here, using an updated model of Cassini's Electron Spectrometer response function, we are able to estimate the outward flux of negatively charged pickup ions, the first time such a plasma population has been constrained. Using test-particle simulations we trace both the <span class="hlt">positive</span> and negative particles back to Rhea's exobase to better understand their production and loss processes and the implications for Rhea's sputter-induced exosphere. We also look to examine whether the calculated ion densities could generate ion cyclotron wave activity.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_10");'>10</a></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li class="active"><span>12</span></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_12 --> <div id="page_13" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li><a href="#" onclick='return showDiv("page_12");'>12</a></li> <li class="active"><span>13</span></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="241"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018PhRvB..97p5130E','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018PhRvB..97p5130E"><span>Location of the valence <span class="hlt">band</span> maximum in the <span class="hlt">band</span> structure of anisotropic 1 T'-ReSe2</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Eickholt, P.; Noky, J.; Schwier, E. F.; Shimada, K.; Miyamoto, K.; Okuda, T.; Datzer, C.; Drüppel, M.; Krüger, P.; Rohlfing, M.; Donath, M.</p> <p>2018-04-01</p> <p>Transition-metal dichalcogenides (TMDCs) are a focus of current research due to their fascinating optical and electronic properties with possible technical applications. ReSe2 is an interesting material of the TMDC family, with unique anisotropic properties originating from its distorted 1 T structure (1 T '). To develop a fundamental understanding of the optical and electric properties, we studied the underlying electronic structure with angle-resolved photoemission (ARPES) as well as <span class="hlt">band</span>-structure calculations within the density functional theory (DFT)-local density approximation (LDA) and GdW approximations. We identified the Γ ¯M¯1 direction, which is perpendicular to the a axis, as a distinct direction in k space with the smallest bandwidth of the highest valence <span class="hlt">band</span>. Using photon-energy-dependent ARPES, two valence <span class="hlt">band</span> maxima are identified within experimental limits of about 50 meV: one at the high-symmetry point Z , and a second one at a non-high-symmetry point in the Brillouin zone. Thus, the <span class="hlt">position</span> in k space of the global valence <span class="hlt">band</span> maximum is undecided experimentally. Theoretically, an indirect <span class="hlt">band</span> gap is predicted on a DFT-LDA level, while quasiparticle corrections lead to a direct <span class="hlt">band</span> gap at the Z point.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/29666394','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/29666394"><span>Resonantly enhanced multiple exciton generation through below-<span class="hlt">band</span>-gap multi-photon absorption in perovskite nanocrystals.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Manzi, Aurora; Tong, Yu; Feucht, Julius; Yao, En-Ping; Polavarapu, Lakshminarayana; Urban, Alexander S; Feldmann, Jochen</p> <p>2018-04-17</p> <p>Multi-photon absorption and multiple exciton generation represent two separate strategies for enhancing the conversion efficiency of light into usable electric power. Targeting below-<span class="hlt">band</span>-gap and above-<span class="hlt">band</span>-gap energies, respectively, to date these processes have only been demonstrated independently. Here we report the combined interaction of both nonlinear processes in CsPbBr 3 perovskite nanocrystals. We demonstrate nonlinear absorption over a wide range of below-<span class="hlt">band</span>-gap excitation energies (0.5-0.8 E g ). Interestingly, we discover high-order absorption processes, deviating from the typical two-photon absorption, at specific energetic <span class="hlt">positions</span>. These energies are associated with a strong enhancement of the photoluminescence intensity by up to 10 5 . The analysis of the corresponding energy levels reveals that the <span class="hlt">observed</span> phenomena can be ascribed to the resonant creation of multiple excitons via the absorption of multiple below-<span class="hlt">band</span>-gap photons. This effect may open new pathways for the efficient conversion of optical energy, potentially also in other semiconducting materials.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017PhRvB..95o5310L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017PhRvB..95o5310L"><span>Understanding <span class="hlt">band</span> alignments in semiconductor heterostructures: Composition dependence and type-I-type-II transition of natural <span class="hlt">band</span> offsets in nonpolar zinc-blende AlxGa1 -xN /AlyGa1 -yN composites</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Landmann, M.; Rauls, E.; Schmidt, W. G.</p> <p>2017-04-01</p> <p>The composition dependence of the natural <span class="hlt">band</span> alignment at nonpolar AlxGa1 -xN /AlyGa1 -yN heterojunctions is investigated via hybrid functional based density functional theory. Accurate <span class="hlt">band</span>-gap data are provided using Heyd-Scuseria-Ernzerhof (HSE) type hybrid functionals with a composition dependent exact-exchange contribution. The unstrained <span class="hlt">band</span> alignment between zincblende (zb) AlxGa1 -xN semiconductor alloys is studied within the entire ternary composition range utilizing the Branch-point technique to align the energy levels related to the bulklike direct Γv→Γc and indirect, pseudodirect, respectively, Γv→Xc type transitions in zb-AlxGa1 -xN . While the zb-GaN/AlxGa1 -xN <span class="hlt">band</span> edges consistently show a type-I alignment, the relative <span class="hlt">position</span> of fundamental <span class="hlt">band</span> edges changes to a type-II alignment in the Al-rich composition ranges of zb-AlxGa1 -xN /AlN and zb-AlxGa1 -xN /AlyGa1 -yN systems. The presence of a direct-indirect <span class="hlt">band</span>-gap transition at xc=0.63 in zb-AlxGa1 -xN semiconductor alloys gives rise to a notably different composition dependence of <span class="hlt">band</span> discontinuities in the direct and indirect energy-gap ranges. Below the critical direct-indirect Al/Ga-crossover concentration, the <span class="hlt">band</span> offsets show a close to linear dependence on the alloy composition. In contrast, notable bowing characteristics of all <span class="hlt">band</span> discontinuities are <span class="hlt">observed</span> above the critical crossover composition.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017AGUFMSM51B2432S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017AGUFMSM51B2432S"><span>Statistics of EMIC Rising Tones <span class="hlt">Observed</span> by the Van Allen Probes</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sigsbee, K. M.; Kletzing, C.; Smith, C. W.; Santolik, O.</p> <p>2017-12-01</p> <p>We will present results from an ongoing statistical study of electromagnetic ion cyclotron (EMIC) wave rising tones <span class="hlt">observed</span> by the Van Allen Probes. Using data from the Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) fluxgate magnetometer, we have identified orbits by both Van Allen Probes with EMIC wave events from the start of the mission in fall 2012 through fall 2016. Orbits with EMIC wave events were further examined for evidence of rising tones. Most EMIC wave rising tones were found during H+ <span class="hlt">band</span> EMIC wave events. In Fourier time-frequency power spectrograms of the fluxgate magnetometer data, H+ <span class="hlt">band</span> rising tones generally took the form of triggered emission type events, where the discrete rising tone structures rapidly rise in frequency out of the main <span class="hlt">band</span> of <span class="hlt">observed</span> H+ EMIC waves. A smaller percentage of EMIC wave rising tone events were found in the He+ <span class="hlt">band</span>, where rising tones may appear as discrete structures with a <span class="hlt">positive</span> slope embedded within the main <span class="hlt">band</span> of <span class="hlt">observed</span> He+ EMIC waves, similar in appearance to whistler-mode chorus elements. Understanding the occurrence rate and properties of rising tone EMIC waves will provide <span class="hlt">observational</span> context for theoretical studies indicating that EMIC waves exhibiting non-linear behavior, such as rising tones, may be more effective at scattering radiation belt electrons than ordinary EMIC waves.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1441311-generation-process-large-amplitude-upper-band-chorus-emissions-observed-van-allen-probes','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1441311-generation-process-large-amplitude-upper-band-chorus-emissions-observed-van-allen-probes"><span>Generation Process of Large-Amplitude Upper-<span class="hlt">Band</span> Chorus Emissions <span class="hlt">Observed</span> by Van Allen Probes</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Kubota, Yuko; Omura, Yoshiharu; Kletzing, Craig; ...</p> <p>2018-04-19</p> <p>In this paper, we analyze large-amplitude upper-<span class="hlt">band</span> chorus emissions measured near the magnetic equator by the Electric and Magnetic Field Instrument Suite and Integrated Science instrument package on board the Van Allen Probes. In setting up the parameters of source electrons exciting the emissions based on theoretical analyses and <span class="hlt">observational</span> results measured by the Helium Oxygen Proton Electron instrument, we calculate threshold and optimum amplitudes with the nonlinear wave growth theory. We find that the optimum amplitude is larger than the threshold amplitude obtained in the frequency range of the chorus emissions and that the wave amplitudes grow between themore » threshold and optimum amplitudes. Finally, in the frame of the wave growth process, the nonlinear growth rates are much greater than the linear growth rates.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/1441311-generation-process-large-amplitude-upper-band-chorus-emissions-observed-van-allen-probes','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/1441311-generation-process-large-amplitude-upper-band-chorus-emissions-observed-van-allen-probes"><span>Generation Process of Large-Amplitude Upper-<span class="hlt">Band</span> Chorus Emissions <span class="hlt">Observed</span> by Van Allen Probes</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Kubota, Yuko; Omura, Yoshiharu; Kletzing, Craig</p> <p></p> <p>In this paper, we analyze large-amplitude upper-<span class="hlt">band</span> chorus emissions measured near the magnetic equator by the Electric and Magnetic Field Instrument Suite and Integrated Science instrument package on board the Van Allen Probes. In setting up the parameters of source electrons exciting the emissions based on theoretical analyses and <span class="hlt">observational</span> results measured by the Helium Oxygen Proton Electron instrument, we calculate threshold and optimum amplitudes with the nonlinear wave growth theory. We find that the optimum amplitude is larger than the threshold amplitude obtained in the frequency range of the chorus emissions and that the wave amplitudes grow between themore » threshold and optimum amplitudes. Finally, in the frame of the wave growth process, the nonlinear growth rates are much greater than the linear growth rates.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://elibrary.unm.edu/sora/JFO/v066n04/p0582-p0589.pdf','USGSPUBS'); return false;" href="http://elibrary.unm.edu/sora/JFO/v066n04/p0582-p0589.pdf"><span>A colored leg <span class="hlt">banding</span> technique for Amazona parrots</span></a></p> <p><a target="_blank" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p>Meyers, J.M.</p> <p>1995-01-01</p> <p>A technique for individual identification of Amazona was developed using plastic leg <span class="hlt">bands</span>. <span class="hlt">Bands</span> were made from 5- and 7-mm-wide strips of laminated PVC coiled 2.5 times with an inside diameter 4-5 mm gt the maximum diameter of the parrot's leg. Seventeen parrots were captured in Puerto Rico, marked with individual plastic leg <span class="hlt">bands</span>, and <span class="hlt">observed</span> for 204-658 d with only one lost or damaged plastic <span class="hlt">band</span>. Plastic leg <span class="hlt">bands</span> did not cause injury to or calluses on parrots' legs. The plastic material used for making leg <span class="hlt">bands</span> was available in 18 colors in 1994, which would allow unique marking of 306 individuals using one plastic leg <span class="hlt">band</span> on each leg.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19840017711','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19840017711"><span>Analysis of carbon dioxide <span class="hlt">bands</span> near 2.2 micrometers</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Abubaker, M. S.; Shaw, J. H.</p> <p>1984-01-01</p> <p>Carbon dioxide is one of the more important atmospheric infrared-absorbing gases due to its relatively high, and increasing, concentration. The spectral parameters of its <span class="hlt">bands</span> are required for understanding radiative heat transfer in the atmosphere. The line intensities, <span class="hlt">positions</span>, line half-widths, rotational constants, and <span class="hlt">band</span> centers of three overlapping <span class="hlt">bands</span> of CO2 near 2.2 microns are presented. Non-linear least squares (NLLS) regression procedures were employed to determine these parameters.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018GeoRL..45..511M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018GeoRL..45..511M"><span>Simultaneous <span class="hlt">Observations</span> of Lower <span class="hlt">Band</span> Chorus Emissions at the Equator and Microburst Precipitating Electrons in the Ionosphere</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Mozer, F. S.; Agapitov, O. V.; Blake, J. B.; Vasko, I. Y.</p> <p>2018-01-01</p> <p>On 11 December 2016 at 00:12:30 UT, Van Allen Probe-B, at the equator and near midnight, and AC6-B, in the ionosphere, were on magnetic field lines whose 100 km altitude foot points were separated by 600 km. Van Allen Probe-B <span class="hlt">observed</span> a 30 s burst of lower <span class="hlt">band</span> chorus waves (with maximum amplitudes >1 nT) at the same time that AC6-B <span class="hlt">observed</span> intense microburst electrons in the loss cone. One second averaged variations of the chorus intensity and the microburst electron flux were well correlated. The low-altitude electron flux expected from quasi-linear diffusion of the equatorial electrons by the equatorial chorus is in excellent agreement with the <span class="hlt">observed</span>, 1 s averaged, low-altitude electron flux. However, the large-amplitude, <0.5 s duration, low-altitude electron pulses require nonlinear processes for their explanation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28932668','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28932668"><span>Local Bonding Influence on the <span class="hlt">Band</span> Edge and <span class="hlt">Band</span> Gap Formation in Quaternary Chalcopyrites.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Miglio, Anna; Heinrich, Christophe P; Tremel, Wolfgang; Hautier, Geoffroy; Zeier, Wolfgang G</p> <p>2017-09-01</p> <p>Quaternary chalcopyrites have shown to exhibit tunable <span class="hlt">band</span> gaps with changing anion composition. Inspired by these <span class="hlt">observations</span>, the underlying structural and electronic considerations are investigated using a combination of experimentally obtained structural data, molecular orbital considerations, and density functional theory. Within the solid solution Cu 2 ZnGeS 4- x Se x , the anion bond alteration parameter changes, showing larger bond lengths for metal-selenium than for metal-sulfur bonds. The changing bonding interaction directly influences the valence and conduction <span class="hlt">band</span> edges, which result from antibonding Cu-anion and Ge-anion interactions, respectively. The knowledge of the underlying bonding interactions at the <span class="hlt">band</span> edges can help design properties of these quaternary chalcopyrites for photovoltaic and thermoelectric applications.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014OptMa..36.2016Y','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014OptMa..36.2016Y"><span><span class="hlt">Positive</span> hysteresis of Ce-doped GAGG scintillator</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Yanagida, Takayuki; Fujimoto, Yutaka; Koshimizu, Masanori; Watanabe, Kenichi; Sato, Hiroki; Yagi, Hideki; Yanagitani, Takagimi</p> <p>2014-10-01</p> <p><span class="hlt">Positive</span> hysteresis and radiation tolerance to high-dose radiation exposure were investigated for Ce 1% and 3% doped Gd3(Al, Ga)5O12 (Ce:GAGG) crystal scintillator on comparison with other garnet scintillators such Ce:YAG, Ce:LuAG, Pr:LuAG, and ceramic Ce:GAGG. When they were irradiated by several Gy 60Co γ-rays, Ce 1% doped GAGG crystal exhibited ∼20% light yield enhancement (<span class="hlt">positive</span> hysteresis). This is the first time to <span class="hlt">observe</span> <span class="hlt">positive</span> hysteresis in Ce doped GAGG. On the other hand, other garnet materials did not show the <span class="hlt">positive</span> hysteresis and their light yields were stable after 800 Gy irradiation except Pr:LuAG. The light yield of Pr:LuAG decreased largely. When irradiated Ce:GAGG which showed <span class="hlt">positive</span> hysteresis was evaluated in Synchrotron facility (UVSOR), new excitation <span class="hlt">band</span> was created around 60 nm.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016AGUFM.A23A0181H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016AGUFM.A23A0181H"><span>Discussion of vicarious calibration of GOSAT/TANSO-CAI UV-<span class="hlt">band</span> (380nm) and aerosol retrieval in wildfire region in the OCO-2 and GOSAT <span class="hlt">observation</span> campaign at Railroad Valley in 2016</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hashimoto, M.; Kuze, A.; Bruegge, C. J.; Shiomi, K.; Kataoka, F.; Kikuchi, N.; Arai, T.; Kasai, K.; Nakajima, T.</p> <p>2016-12-01</p> <p>The GOSAT (Greenhouse Gases <span class="hlt">Observing</span> Satellite) / TANSO-CAI (Cloud and Aerosol Imager, CAI) is an imaging sensor to measure cloud and aerosol properties and <span class="hlt">observes</span> reflected sunlight from the atmosphere and surface of the ground. The sensor has four <span class="hlt">bands</span> from near ultraviolet (near-UV) to shortwave infrared, 380, 674, 870 and 1600nm. The field of view size is 0.5 km for <span class="hlt">band</span>-1 through <span class="hlt">band</span>-3, and 1.5km for <span class="hlt">band</span>-4. <span class="hlt">Band</span>-1 (380nm) is one of unique function of the CAI. The near-UV <span class="hlt">observation</span> offers several advantages for the remote sensing of aerosols over land: Low reflectance of most surfaces; Sensitivity to absorbing aerosols; Absorption of trace gases is weak (Höller et al., 2004). CAI UV-<span class="hlt">band</span> is useful to distinguish absorbing aerosol (smoke) from cloud. GOSAT-2/TANSO-CAI-2 that will be launched in the future also has UV-<span class="hlt">bands</span>, 340 and 380nm. We carried out an experiment to calibrate CAI UV-<span class="hlt">band</span> radiance using data taken in a field campaign of OCO-2 and GOSAT at Railroad Valley in 2016. The campaign period is June 27 to July 3 in 2016. We measured surface reflectance by using USB4000 Spectrometer with 74-UV collimating lens (Ocean Optics) and Spectralon (Labsphere). USB4000 is a UV spectrometer, and its measurement range from 300 to 520nm. We simulated CAI UV-<span class="hlt">band</span> radiance using a vector type of radiation transfer code, i.e. including polarization calculation, pstar3 (Ota et al., 2010) using measured surface reflectance and atmospheric data, pressure and relative humidity by radiosonde in the same campaign, and aerosol optical depth by AERONET, etc. Then, we evaluated measured UV radiances with the simulated data. We show the result of vicarious calibration of CAI UV-<span class="hlt">band</span> in the campaign, and discuss about this method for future sensor, CAI-2. Around the campaign period, there was wildfire around Los Angeles, and aerosol optical thickness (AOT) <span class="hlt">observed</span> by AERONET at Rail Road valley and Caltech sites is also high. We tried to detect and retrieve aerosol</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2004PhDT........31H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2004PhDT........31H"><span>Spectroscopic study of hafnium silicate alloys prepared by RPECVD: Comparisons between conduction/valence <span class="hlt">band</span> offset energies and optical <span class="hlt">band</span> gaps</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hong, Joon Goo</p> <p></p> <p>Aggressive scaling of devices has continued to improve MOSFET transistor performance. As lateral device dimensions continue to decrease, gate oxide thickness must be scaled down. As one of the promising high k alternative gate oxide materials, HfO2 and its silicates were investigated to understand their direct tunneling behavior by studying <span class="hlt">band</span> offset energies with spectroscopy and electrical characterization. Local bonding change of remote plasma deposited (HfO2)x(SiO 2)1-x alloys were characterized by Fourier transform infrared (FTIR) spectroscopy, x-ray photoelectron spectroscopy (XPS), and Auger electron spectroscopy (AES) as a function of alloy composition, x. Two different precursors with Hf Nitrato and Hf-tert-butoxide were tested to have amorphous deposition. Film composition was determined off-line by Rutherford backscattering spectroscopy (RBS) and these results were calibrated with on-line AES. As deposited Hf-silicate alloys were characterized by off-line XPS and AES for their chemical shifts interpreting with a partial charge transfer model as well as coordination changes. Sigmoidal dependence of valence <span class="hlt">band</span> offset energies was <span class="hlt">observed</span>. Hf 5d* state is fixed at the bottom of the conduction <span class="hlt">band</span> and located at 1.3 +/- 0.2 eV above the top of the Si conduction <span class="hlt">band</span> as a conduction <span class="hlt">band</span> offset by x-ray absorption spectroscopy (XAS). Optical <span class="hlt">band</span> gap energy changes were <span class="hlt">observed</span> with vacuum ultra violet spectroscopic ellipsometry (VUVSE) to verify compositional dependence of conduction and valence <span class="hlt">band</span> offset energy changes. 1 nm EOT normalized tunneling current with Wentzel-Kramer-Brillouin (WKB) simulation based on the <span class="hlt">band</span> offset study and Franz two <span class="hlt">band</span> model showed the minimum at the intermediate composition matching with the experimental data. Non-linear trend in tunneling current was <span class="hlt">observed</span> because the increases in physical thickness were mitigated by reductions in <span class="hlt">band</span> offset energies and effective mass for tunneling. C-V curves were compared</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017AGUFM.A31A2136L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017AGUFM.A31A2136L"><span>StatisticAl Characteristics of Cloud over Beijing, China Obtained FRom Ka <span class="hlt">band</span> Doppler Radar <span class="hlt">Observation</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>LIU, J.; Bi, Y.; Duan, S.; Lu, D.</p> <p>2017-12-01</p> <p>It is well-known that cloud characteristics, such as top and base heights and their layering structure of micro-physical parameters, spatial coverage and temporal duration are very important factors influencing both radiation budget and its vertical partitioning as well as hydrological cycle through precipitation data. Also, cloud structure and their statistical distribution and typical values will have respective characteristics with geographical and seasonal variation. Ka <span class="hlt">band</span> radar is a powerful tool to obtain above parameters around the world, such as ARM cloud radar at the Oklahoma US, Since 2006, Cloudsat is one of NASA's A-Train satellite constellation, continuously <span class="hlt">observe</span> the cloud structure with global coverage, but only twice a day it monitor clouds over same local site at same local time.By using IAP Ka <span class="hlt">band</span> Doppler radar which has been operating continuously since early 2013 over the roof of IAP building in Beijing, we obtained the statistical characteristic of clouds, including cloud layering, cloud top and base heights, as well as the thickness of each cloud layer and their distribution, and were analyzed monthly and seasonal and diurnal variation, statistical analysis of cloud reflectivity profiles is also made. The analysis covers both non-precipitating clouds and precipitating clouds. Also, some preliminary comparison of the results with Cloudsat/Calipso products for same period and same area are made.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2011AGUFM.H41G1136C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2011AGUFM.H41G1136C"><span><span class="hlt">Observations</span> of Heavy Rainfall in a Post Wildland Fire Area Using X-<span class="hlt">Band</span> Polarimetric Radar</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Cifelli, R.; Matrosov, S. Y.; Gochis, D. J.; Kennedy, P.; Moody, J. A.</p> <p>2011-12-01</p> <p>Polarimetric X-<span class="hlt">band</span> radar systems have been used increasingly over the last decade for rainfall measurements. Since X-<span class="hlt">band</span> radar systems are generally less costly, more mobile, and have narrower beam widths (for same antenna sizes) than those operating at lower frequencies (e.g., C and S-<span class="hlt">bands</span>), they can be used for the "gap-filling" purposes for the areas when high resolution rainfall measurements are needed and existing operational radars systems lack adequate coverage and/or resolution for accurate quantitative precipitation estimation (QPE). The main drawback of X-<span class="hlt">band</span> systems is attenuation of radar signals, which is significantly stronger compared to frequencies used by "traditional" precipitation radars operating at lower frequencies. The use of different correction schemes based on polarimetric data can, to a certain degree, overcome this drawback when attenuation does not cause total signal extinction. This presentation will focus on examining the use of high-resolution data from the NOAA Earth System Research Laboratory (ESRL) mobile X-<span class="hlt">band</span> dual polarimetric radar for the purpose of estimating precipitation in a post-wildland fire area. The NOAA radar was deployed in the summer of 2011 to examine the impact of gap-fill radar on QPE and the resulting hydrologic response during heavy rain events in the Colorado Front Range in collaboration with colleagues from the National Center for Atmospheric Research (NCAR), Colorado State University (CSU), and the U.S. Geological Survey (USGS). A network of rain gauges installed by NCAR, the Denver Urban Drainage Flood Control District (UDFCD), and the USGS are used to compare with the radar estimates. Supplemental data from NEXRAD and the CSU-CHILL dual polarimetric radar are also used to compare with the NOAA X-<span class="hlt">band</span> and rain gauges. It will be shown that rainfall rates and accumulations estimated from specific differential phase measurements (KDP) at X-<span class="hlt">band</span> are in good agreement with the measurements from the gauge</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19720011057','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19720011057"><span>Excitation of the Werner <span class="hlt">bands</span> of H2 by electron impact</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Stone, E. J.; Zipf, E. C.</p> <p>1972-01-01</p> <p>Absolute cross sections for the excitation of the H2 Werner <span class="hlt">band</span> system were measured from energy threshold to 300 eV for electron impact on H2. The <span class="hlt">bands</span> were <span class="hlt">observed</span> in emission in the wavelength region 1100A to 1250A. The measured cross sections were compared with published transition probabilities, leading to the conclusion that the Werner <span class="hlt">bands</span> are suitable as the basis for a relative spectral response calibration only when the <span class="hlt">bands</span> are <span class="hlt">observed</span> under sufficiently high resolution. The effect of the perturbation between the C 1Pi u and B 1 Sigma-u states of the hydrogen molecule was clearly <span class="hlt">observed</span> in anomalies in the rotational intensity distribution in <span class="hlt">bands</span> of the (3 v '') progression.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA17858.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA17858.html"><span><span class="hlt">Banded</span> Ridges in Hellas</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2014-01-09</p> <p>Low lying areas in the Hellas region, which is the largest impact basin on Mars, often show complex groups of <span class="hlt">banded</span> ridges, furrows, and pits as seen in this <span class="hlt">observation</span> from NASA Mars Reconnaissance Orbiter.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3282488','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3282488"><span>Paranodal reorganization results in the depletion of transverse <span class="hlt">bands</span> in the aged central nervous system</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Shepherd, Mark N.; Pomicter, Anthony D.; Velazco, Cristine S.; Henderson, Scott C.; Dupree, Jeffrey L.</p> <p>2012-01-01</p> <p>Paranodal axo-glial junctional complexes anchor the myelin sheath to the axon and breakdown of these complexes presumably facilitates demyelination. Myelin deterioration is also prominent in the aging central nervous system (CNS); however, the stability of the paranodal complexes in the aged CNS has not been examined. Here, we show that transverse <span class="hlt">bands</span>, prominent components of paranodal junctions, are significantly reduced in the aged CNS; however, the number of paired clusters of both myelin and axonal paranodal proteins is not altered. Ultrastructural analyses also reveal that thicker myelin sheaths display a “piling” of paranodal loops, the cytoplasm-containing sacs that demarcate the paranode. Loops involved in piling are <span class="hlt">observed</span> throughout the paranode and are not limited to loops <span class="hlt">positioned</span> in either the nodal- or juxtanodal-most regions. Here, we propose that as myelination continues, previously anchored loops lose their transverse <span class="hlt">bands</span> and recede away from the axolemma. Newly juxtaposed loops then lose their transverse <span class="hlt">bands</span>, move laterally to fill in the gap left by the receded loops and finally reform their transverse <span class="hlt">bands</span>. This paranodal reorganization results in conservation of paranodal length, which may be important in maintaining ion channel spacing and axonal function. Furthermore, we propose that transverse <span class="hlt">band</span> reformation is less efficient in the aged CNS, resulting in the significant reduction of these junctional components. Although demyelination was not <span class="hlt">observed</span>, we propose that loss of transverse <span class="hlt">bands</span> facilitates myelin degeneration and may predispose the aged CNS to a poorer prognosis following a secondary insult. PMID:20888080</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.dtic.mil/docs/citations/ADA202522','DTIC-ST'); return false;" href="http://www.dtic.mil/docs/citations/ADA202522"><span>Microscopic <span class="hlt">Observations</span> of Adiabatic Shear <span class="hlt">Bands</span> in Three Different Steels</span></a></p> <p><a target="_blank" href="http://www.dtic.mil/">DTIC Science & Technology</a></p> <p></p> <p>1988-09-01</p> <p>low thermal conductivity, and a high thermal softening rate. Examples include alloys of titanium. aluminum, copper , as well as steels [5-221... steels : 1 (1) an AISI 1018 cold rolled steel , (2) a high strength low alloy structural steel , and deformation in shear was impo.ed to produce shear <span class="hlt">bands</span>...stecls: (1) an AISI 1018 cold rolled steel , (2) a high strength low alloy structural steel , and (3) an AISI 4340 VAR steel tempered</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1422593-observed-positive-vegetation-rainfall-feedbacks-sahel-dominated-moisture-recycling-mechanism','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1422593-observed-positive-vegetation-rainfall-feedbacks-sahel-dominated-moisture-recycling-mechanism"><span><span class="hlt">Observed</span> <span class="hlt">positive</span> vegetation-rainfall feedbacks in the Sahel dominated by a moisture recycling mechanism</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Yu, Yan; Notaro, Michael; Wang, Fuyao; ...</p> <p>2017-11-30</p> <p>Classic, model-based theory of land-atmosphere interactions across the Sahel promote <span class="hlt">positive</span> vegetation-rainfall feedbacks dominated by surface albedo mechanism. However, neither the proposed <span class="hlt">positive</span> vegetation-rainfall feedback nor its underlying albedo mechanism has been convincingly demonstrated using <span class="hlt">observational</span> data. Here, we present <span class="hlt">observational</span> evidence for the region’s proposed <span class="hlt">positive</span> vegetation-rainfall feedback on the seasonal to interannual time scale, and find that it is associated with a moisture recycling mechanism, rather than the classic albedo-based mechanism. <span class="hlt">Positive</span> anomalies of remotely sensed vegetation greenness across the Sahel during the late and post-monsoon periods favor enhanced evapotranspiration, precipitable water, convective activity and rainfall, indicative ofmore » amplified moisture recycling. The identified modest low-level cooling and anomalous atmospheric subsidence in response to <span class="hlt">positive</span> vegetation greenness anomalies are counter to the responses expected through the classic vegetation-albedo feedback mechanism. The <span class="hlt">observational</span> analysis further reveals enhanced dust emissions in response to diminished Sahel vegetation growth, potentially contributing to the <span class="hlt">positive</span> vegetation-rainfall feedback.« less</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li><a href="#" onclick='return showDiv("page_12");'>12</a></li> <li class="active"><span>13</span></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_13 --> <div id="page_14" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_12");'>12</a></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li class="active"><span>14</span></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="261"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/1422593','SCIGOV-STC'); return false;" href="https://www.osti.gov/servlets/purl/1422593"><span><span class="hlt">Observed</span> <span class="hlt">positive</span> vegetation-rainfall feedbacks in the Sahel dominated by a moisture recycling mechanism</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Yu, Yan; Notaro, Michael; Wang, Fuyao</p> <p></p> <p>Classic, model-based theory of land-atmosphere interactions across the Sahel promote <span class="hlt">positive</span> vegetation-rainfall feedbacks dominated by surface albedo mechanism. However, neither the proposed <span class="hlt">positive</span> vegetation-rainfall feedback nor its underlying albedo mechanism has been convincingly demonstrated using <span class="hlt">observational</span> data. Here, we present <span class="hlt">observational</span> evidence for the region’s proposed <span class="hlt">positive</span> vegetation-rainfall feedback on the seasonal to interannual time scale, and find that it is associated with a moisture recycling mechanism, rather than the classic albedo-based mechanism. <span class="hlt">Positive</span> anomalies of remotely sensed vegetation greenness across the Sahel during the late and post-monsoon periods favor enhanced evapotranspiration, precipitable water, convective activity and rainfall, indicative ofmore » amplified moisture recycling. The identified modest low-level cooling and anomalous atmospheric subsidence in response to <span class="hlt">positive</span> vegetation greenness anomalies are counter to the responses expected through the classic vegetation-albedo feedback mechanism. The <span class="hlt">observational</span> analysis further reveals enhanced dust emissions in response to diminished Sahel vegetation growth, potentially contributing to the <span class="hlt">positive</span> vegetation-rainfall feedback.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19740021387','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19740021387"><span>ATS-5 ranging receiver and L-<span class="hlt">band</span> experiment. Volume 2: Data reduction and analysis</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>1971-01-01</p> <p>The results of ranging and <span class="hlt">position</span> location experiments performed at the NASA Application Technology Satellite ground station at Mojave California are presented. The experiments are simultaneous C-<span class="hlt">band</span> and L-<span class="hlt">band</span> ranging to ATS-5, simultaneous C-<span class="hlt">band</span> and VHF ranging, simultaneous 24-hour ranging and <span class="hlt">position</span> location using ATS-1, ATS-3, and ATS-5. The data handling and processing technique is also described.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017PhRvB..96x5205M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017PhRvB..96x5205M"><span><span class="hlt">Band-to-band</span> transitions, selection rules, effective mass, and excitonic contributions in monoclinic β -Ga2O3</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Mock, Alyssa; Korlacki, Rafał; Briley, Chad; Darakchieva, Vanya; Monemar, Bo; Kumagai, Yoshinao; Goto, Ken; Higashiwaki, Masataka; Schubert, Mathias</p> <p>2017-12-01</p> <p>We employ an eigenpolarization model including the description of direction dependent excitonic effects for rendering critical point structures within the dielectric function tensor of monoclinic β -Ga2O3 yielding a comprehensive analysis of generalized ellipsometry data obtained from 0.75-9 eV. The eigenpolarization model permits complete description of the dielectric response. We obtain, for single-electron and excitonic <span class="hlt">band-to-band</span> transitions, anisotropic critical point model parameters including their polarization vectors within the monoclinic lattice. We compare our experimental analysis with results from density functional theory calculations performed using the Gaussian-attenuation-Perdew-Burke-Ernzerhof hybrid density functional. We present and discuss the order of the fundamental direct <span class="hlt">band-to-band</span> transitions and their polarization selection rules, the electron and hole effective mass parameters for the three lowest <span class="hlt">band-to-band</span> transitions, and their excitonic contributions. We find that the effective masses for holes are highly anisotropic and correlate with the selection rules for the fundamental <span class="hlt">band-to-band</span> transitions. The <span class="hlt">observed</span> transitions are polarized close to the direction of the lowest hole effective mass for the valence <span class="hlt">band</span> participating in the transition.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018JPRS..137...47J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018JPRS..137...47J"><span>Robust and adaptive <span class="hlt">band-to-band</span> image transform of UAS miniature multi-lens multispectral camera</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jhan, Jyun-Ping; Rau, Jiann-Yeou; Haala, Norbert</p> <p>2018-03-01</p> <p>Utilizing miniature multispectral (MS) or hyperspectral (HS) cameras by mounting them on an Unmanned Aerial System (UAS) has the benefits of convenience and flexibility to collect remote sensing imagery for precision agriculture, vegetation monitoring, and environment investigation applications. Most miniature MS cameras adopt a multi-lens structure to record discrete MS <span class="hlt">bands</span> of visible and invisible information. The differences in lens distortion, mounting <span class="hlt">positions</span>, and viewing angles among lenses mean that the acquired original MS images have significant <span class="hlt">band</span> misregistration errors. We have developed a Robust and Adaptive <span class="hlt">Band-to-Band</span> Image Transform (RABBIT) method for dealing with the <span class="hlt">band</span> co-registration of various types of miniature multi-lens multispectral cameras (Mini-MSCs) to obtain <span class="hlt">band</span> co-registered MS imagery for remote sensing applications. The RABBIT utilizes modified projective transformation (MPT) to transfer the multiple image geometry of a multi-lens imaging system to one sensor geometry, and combines this with a robust and adaptive correction (RAC) procedure to correct several systematic errors and to obtain sub-pixel accuracy. This study applies three state-of-the-art Mini-MSCs to evaluate the RABBIT method's performance, specifically the Tetracam Miniature Multiple Camera Array (MiniMCA), Micasense RedEdge, and Parrot Sequoia. Six MS datasets acquired at different target distances and dates, and locations are also applied to prove its reliability and applicability. Results prove that RABBIT is feasible for different types of Mini-MSCs with accurate, robust, and rapid image processing efficiency.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017PhRvD..96l2006A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017PhRvD..96l2006A"><span>First narrow-<span class="hlt">band</span> search for continuous gravitational waves from known pulsars in advanced detector data</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Abbott, B. P.; Abbott, R.; Abbott, T. D.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.; Adya, V. B.; Affeldt, C.; Afrough, M.; Agarwal, B.; Agathos, M.; Agatsuma, K.; Aggarwal, N.; Aguiar, O. D.; Aiello, L.; Ain, A.; Allen, B.; Allen, G.; Allocca, A.; Altin, P. A.; Amato, A.; Ananyeva, A.; Anderson, S. B.; Anderson, W. G.; Angelova, S. V.; Antier, S.; Appert, S.; Arai, K.; Araya, M. C.; Areeda, J. S.; Arnaud, N.; Arun, K. G.; Ascenzi, S.; Ashton, G.; Ast, M.; Aston, S. M.; Astone, P.; Atallah, D. V.; Aufmuth, P.; Aulbert, C.; AultONeal, K.; Austin, C.; Avila-Alvarez, A.; Babak, S.; Bacon, P.; Bader, M. K. M.; Bae, S.; Baker, P. T.; Baldaccini, F.; Ballardin, G.; Ballmer, S. W.; Banagiri, S.; Barayoga, J. C.; Barclay, S. E.; Barish, B. C.; Barker, D.; Barkett, K.; Barone, F.; Barr, B.; Barsotti, L.; Barsuglia, M.; Barta, D.; Bartlett, J.; Bartos, I.; Bassiri, R.; Basti, A.; Batch, J. C.; Bawaj, M.; Bayley, J. C.; Bazzan, M.; Bécsy, B.; Beer, C.; Bejger, M.; Belahcene, I.; Bell, A. S.; Berger, B. K.; Bergmann, G.; Bero, J. J.; Berry, C. P. L.; Bersanetti, D.; Bertolini, A.; Betzwieser, J.; Bhagwat, S.; Bhandare, R.; Bilenko, I. A.; Billingsley, G.; Billman, C. R.; Birch, J.; Birney, R.; Birnholtz, O.; Biscans, S.; Biscoveanu, S.; Bisht, A.; Bitossi, M.; Biwer, C.; Bizouard, M. A.; Blackburn, J. K.; Blackman, J.; Blair, C. D.; Blair, D. G.; Blair, R. M.; Bloemen, S.; Bock, O.; Bode, N.; Boer, M.; Bogaert, G.; Bohe, A.; Bondu, F.; Bonilla, E.; Bonnand, R.; Boom, B. A.; Bork, R.; Boschi, V.; Bose, S.; Bossie, K.; Bouffanais, Y.; Bozzi, A.; Bradaschia, C.; Brady, P. R.; Branchesi, M.; Brau, J. E.; Briant, T.; Brillet, A.; Brinkmann, M.; Brisson, V.; Brockill, P.; Broida, J. E.; Brooks, A. F.; Brown, D. A.; Brown, D. D.; Brunett, S.; Buchanan, C. C.; Buikema, A.; Bulik, T.; Bulten, H. J.; Buonanno, A.; Buskulic, D.; Buy, C.; Byer, R. L.; Cabero, M.; Cadonati, L.; Cagnoli, G.; Cahillane, C.; Calderón Bustillo, J.; Callister, T. A.; Calloni, E.; Camp, J. B.; Canizares, P.; Cannon, K. C.; Cao, H.; Cao, J.; Capano, C. D.; Capocasa, E.; Carbognani, F.; Caride, S.; Carney, M. F.; Casanueva Diaz, J.; Casentini, C.; Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C. B.; Cerdá-Durán, P.; Cerretani, G.; Cesarini, E.; Chamberlin, S. J.; Chan, M.; Chao, S.; Charlton, P.; Chase, E.; Chassande-Mottin, E.; Chatterjee, D.; Cheeseboro, B. D.; Chen, H. Y.; Chen, X.; Chen, Y.; Cheng, H.-P.; Chia, H.; Chincarini, A.; Chiummo, A.; Chmiel, T.; Cho, H. S.; Cho, M.; Chow, J. H.; Christensen, N.; Chu, Q.; Chua, A. J. K.; Chua, S.; Chung, A. K. W.; Chung, S.; Ciani, G.; Ciolfi, R.; Cirelli, C. E.; Cirone, A.; Clara, F.; Clark, J. A.; Clearwater, P.; Cleva, F.; Cocchieri, C.; Coccia, E.; Cohadon, P.-F.; Cohen, D.; Colla, A.; Collette, C. G.; Cominsky, L. R.; Constancio, M.; Conti, L.; Cooper, S. J.; Corban, P.; Corbitt, T. R.; Cordero-Carrión, I.; Corley, K. R.; Cornish, N.; Corsi, A.; Cortese, S.; Costa, C. A.; Coughlin, M. W.; Coughlin, S. B.; Coulon, J.-P.; Countryman, S. T.; Couvares, P.; Covas, P. B.; Cowan, E. E.; Coward, D. M.; Cowart, M. J.; Coyne, D. C.; Coyne, R.; Creighton, J. D. E.; Creighton, T. D.; Cripe, J.; Crowder, S. G.; Cullen, T. J.; Cumming, A.; Cunningham, L.; Cuoco, E.; Dal Canton, T.; Dálya, G.; Danilishin, S. L.; D'Antonio, S.; Danzmann, K.; Dasgupta, A.; Da Silva Costa, C. F.; Dattilo, V.; Dave, I.; Davier, M.; Davis, D.; Daw, E. J.; Day, B.; De, S.; DeBra, D.; Degallaix, J.; De Laurentis, M.; Deléglise, S.; Del Pozzo, W.; Demos, N.; Denker, T.; Dent, T.; De Pietri, R.; Dergachev, V.; De Rosa, R.; DeRosa, R. T.; De Rossi, C.; DeSalvo, R.; de Varona, O.; Devenson, J.; Dhurandhar, S.; Díaz, M. C.; Di Fiore, L.; Di Giovanni, M.; Di Girolamo, T.; Di Lieto, A.; Di Pace, S.; Di Palma, I.; Di Renzo, F.; Doctor, Z.; Dolique, V.; Donovan, F.; Dooley, K. L.; Doravari, S.; Dorrington, I.; Douglas, R.; Dovale Álvarez, M.; Downes, T. P.; Drago, M.; Dreissigacker, C.; Driggers, J. C.; Du, Z.; Ducrot, M.; Dupej, P.; Dwyer, S. E.; Edo, T. B.; Edwards, M. C.; Effler, A.; Eggenstein, H.-B.; Ehrens, P.; Eichholz, J.; Eikenberry, S. S.; Eisenstein, R. A.; Essick, R. C.; Estevez, D.; Etienne, Z. B.; Etzel, T.; Evans, M.; Evans, T. M.; Factourovich, M.; Fafone, V.; Fair, H.; Fairhurst, S.; Fan, X.; Farinon, S.; Farr, B.; Farr, W. M.; Fauchon-Jones, E. J.; Favata, M.; Fays, M.; Fee, C.; Fehrmann, H.; Feicht, J.; Fejer, M. M.; Fernandez-Galiana, A.; Ferrante, I.; Ferreira, E. C.; Ferrini, F.; Fidecaro, F.; Finstad, D.; Fiori, I.; Fiorucci, D.; Fishbach, M.; Fisher, R. P.; Fitz-Axen, M.; Flaminio, R.; Fletcher, M.; Fong, H.; Font, J. A.; Forsyth, P. W. F.; Forsyth, S. S.; Fournier, J.-D.; Frasca, S.; Frasconi, F.; Frei, Z.; Freise, A.; Frey, R.; Frey, V.; Fries, E. M.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Gabbard, H.; Gadre, B. U.; Gaebel, S. M.; Gair, J. R.; Gammaitoni, L.; Ganija, M. R.; Gaonkar, S. G.; Garcia-Quiros, C.; Garufi, F.; Gateley, B.; Gaudio, S.; Gaur, G.; Gayathri, V.; Gehrels, N.; Gemme, G.; Genin, E.; Gennai, A.; George, D.; George, J.; Gergely, L.; Germain, V.; Ghonge, S.; Ghosh, Abhirup; Ghosh, Archisman; Ghosh, S.; Giaime, J. A.; Giardina, K. D.; Giazotto, A.; Gill, K.; Glover, L.; Goetz, E.; Goetz, R.; Gomes, S.; Goncharov, B.; González, G.; Gonzalez Castro, J. M.; Gopakumar, A.; Gorodetsky, M. L.; Gossan, S. E.; Gosselin, M.; Gouaty, R.; Grado, A.; Graef, C.; Granata, M.; Grant, A.; Gras, S.; Gray, C.; Greco, G.; Green, A. C.; Gretarsson, E. M.; Groot, P.; Grote, H.; Grunewald, S.; Gruning, P.; Guidi, G. M.; Guo, X.; Gupta, A.; Gupta, M. K.; Gushwa, K. E.; Gustafson, E. K.; Gustafson, R.; Halim, O.; Hall, B. R.; Hall, E. D.; Hamilton, E. Z.; Hammond, G.; Haney, M.; Hanke, M. M.; Hanks, J.; Hanna, C.; Hannam, M. D.; Hannuksela, O. A.; Hanson, J.; Hardwick, T.; Harms, J.; Harry, G. M.; Harry, I. W.; Hart, M. J.; Haster, C.-J.; Haughian, K.; Healy, J.; Heidmann, A.; Heintze, M. C.; Heitmann, H.; Hello, P.; Hemming, G.; Hendry, M.; Heng, I. S.; Hennig, J.; Heptonstall, A. W.; Heurs, M.; Hild, S.; Hinderer, T.; Ho, W. C. G.; Hoak, D.; Hofman, D.; Holt, K.; Holz, D. E.; Hopkins, P.; Horst, C.; Hough, J.; Houston, E. A.; Howell, E. J.; Hreibi, A.; Hu, Y. M.; Huerta, E. A.; Huet, D.; Hughey, B.; Husa, S.; Huttner, S. H.; Huynh-Dinh, T.; Indik, N.; Inta, R.; Intini, G.; Isa, H. N.; Isac, J.-M.; Isi, M.; Iyer, B. R.; Izumi, K.; Jacqmin, T.; Jani, K.; Jaranowski, P.; Jawahar, S.; Jiménez-Forteza, F.; Johnson, W. W.; Jones, D. I.; Jones, R.; Jonker, R. J. G.; Ju, L.; Junker, J.; Kalaghatgi, C. V.; Kalogera, V.; Kamai, B.; Kandhasamy, S.; Kang, G.; Kanner, J. B.; Kapadia, S. J.; Karki, S.; Karvinen, K. S.; Kasprzack, M.; Katolik, M.; Katsavounidis, E.; Katzman, W.; Kaufer, S.; Kawabe, K.; Kéfélian, F.; Keitel, D.; Kemball, A. J.; Kennedy, R.; Kent, C.; Key, J. S.; Khalili, F. Y.; Khan, I.; Khan, S.; Khan, Z.; Khazanov, E. A.; Kijbunchoo, N.; Kim, Chunglee; Kim, J. C.; Kim, K.; Kim, W.; Kim, W. S.; Kim, Y.-M.; Kimbrell, S. J.; King, E. J.; King, P. J.; Kinley-Hanlon, M.; Kirchhoff, R.; Kissel, J. S.; Kleybolte, L.; Klimenko, S.; Knowles, T. D.; Koch, P.; Koehlenbeck, S. M.; Koley, S.; Kondrashov, V.; Kontos, A.; Korobko, M.; Korth, W. Z.; Kowalska, I.; Kozak, D. B.; Krämer, C.; Kringel, V.; Krishnan, B.; Królak, A.; Kuehn, G.; Kumar, P.; Kumar, R.; Kumar, S.; Kuo, L.; Kutynia, A.; Kwang, S.; Lackey, B. D.; Lai, K. H.; Landry, M.; Lang, R. N.; Lange, J.; Lantz, B.; Lanza, R. K.; Lartaux-Vollard, A.; Lasky, P. D.; Laxen, M.; Lazzarini, A.; Lazzaro, C.; Leaci, P.; Leavey, S.; Lee, C. H.; Lee, H. K.; Lee, H. M.; Lee, H. W.; Lee, K.; Lehmann, J.; Lenon, A.; Leonardi, M.; Leroy, N.; Letendre, N.; Levin, Y.; Li, T. G. F.; Linker, S. D.; Littenberg, T. B.; Liu, J.; Lo, R. K. L.; Lockerbie, N. A.; London, L. T.; Lord, J. E.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo, G.; Lough, J. D.; Lovelace, G.; Lück, H.; Lumaca, D.; Lundgren, A. P.; Lynch, R.; Ma, Y.; Macas, R.; Macfoy, S.; Machenschalk, B.; MacInnis, M.; Macleod, D. M.; Magaña Hernandez, I.; Magaña-Sandoval, F.; Magaña Zertuche, L.; Magee, R. M.; Majorana, E.; Maksimovic, I.; Man, N.; Mandic, V.; Mangano, V.; Mansell, G. L.; Manske, M.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka, S.; Márka, Z.; Markakis, C.; Markosyan, A. S.; Markowitz, A.; Maros, E.; Marquina, A.; Martelli, F.; Martellini, L.; Martin, I. W.; Martin, R. M.; Martynov, D. V.; Mason, K.; Massera, E.; Masserot, A.; Massinger, T. J.; Masso-Reid, M.; Mastrogiovanni, S.; Matas, A.; Matichard, F.; Matone, L.; Mavalvala, N.; Mazumder, N.; McCarthy, R.; McClelland, D. E.; McCormick, S.; McCuller, L.; McGuire, S. C.; McIntyre, G.; McIver, J.; McManus, D. J.; McNeill, L.; McRae, T.; McWilliams, S. T.; Meacher, D.; Meadors, G. D.; Mehmet, M.; Meidam, J.; Mejuto-Villa, E.; Melatos, A.; Mendell, G.; Mercer, R. A.; Merilh, E. L.; Merzougui, M.; Meshkov, S.; Messenger, C.; Messick, C.; Metzdorff, R.; Meyers, P. M.; Miao, H.; Michel, C.; Middleton, H.; Mikhailov, E. E.; Milano, L.; Miller, A. L.; Miller, B. B.; Miller, J.; Millhouse, M.; Milovich-Goff, M. C.; Minazzoli, O.; Minenkov, Y.; Ming, J.; Mishra, C.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Moffa, D.; Moggi, A.; Mogushi, K.; Mohan, M.; Mohapatra, S. R. P.; Montani, M.; Moore, C. J.; Moraru, D.; Moreno, G.; Morriss, S. R.; Mours, B.; Mow-Lowry, C. M.; Mueller, G.; Muir, A. W.; Mukherjee, Arunava; Mukherjee, D.; Mukherjee, S.; Mukund, N.; Mullavey, A.; Munch, J.; Muñiz, E. A.; Muratore, M.; Murray, P. G.; Napier, K.; Nardecchia, I.; Naticchioni, L.; Nayak, R. K.; Neilson, J.; Nelemans, G.; Nelson, T. J. N.; Nery, M.; Neunzert, A.; Nevin, L.; Newport, J. M.; Newton, G.; Ng, K. K. Y.; Nguyen, T. T.; Nichols, D.; Nielsen, A. B.; Nissanke, S.; Nitz, A.; Noack, A.; Nocera, F.; Nolting, D.; North, C.; Nuttall, L. K.; Oberling, J.; O'Dea, G. D.; Ogin, G. H.; Oh, J. J.; Oh, S. H.; Ohme, F.; Okada, M. A.; Oliver, M.; Oppermann, P.; Oram, Richard J.; O'Reilly, B.; Ormiston, R.; Ortega, L. F.; O'Shaughnessy, R.; Ossokine, S.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pace, A. E.; Page, J.; Page, M. A.; Pai, A.; Pai, S. A.; Palamos, J. R.; Palashov, O.; Palomba, C.; Pal-Singh, A.; Pan, Howard; Pan, Huang-Wei; Pang, B.; Pang, P. T. H.; Pankow, C.; Pannarale, F.; Pant, B. C.; Paoletti, F.; Paoli, A.; Papa, M. A.; Parida, A.; Parker, W.; Pascucci, D.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patil, M.; Patricelli, B.; Pearlstone, B. L.; Pedraza, M.; Pedurand, R.; Pekowsky, L.; Pele, A.; Penn, S.; Perez, C. J.; Perreca, A.; Perri, L. M.; Pfeiffer, H. P.; Phelps, M.; Piccinni, O. J.; Pichot, M.; Piergiovanni, F.; Pierro, V.; Pillant, G.; Pinard, L.; Pinto, I. M.; Pirello, M.; Pitkin, M.; Poe, M.; Poggiani, R.; Popolizio, P.; Porter, E. K.; Post, A.; Powell, J.; Prasad, J.; Pratt, J. W. W.; Pratten, G.; Predoi, V.; Prestegard, T.; Prijatelj, M.; Principe, M.; Privitera, S.; Prodi, G. A.; Prokhorov, L. G.; Puncken, O.; Punturo, M.; Puppo, P.; Pürrer, M.; Qi, H.; Quetschke, V.; Quintero, E. A.; Quitzow-James, R.; Raab, F. J.; Rabeling, D. S.; Radkins, H.; Raffai, P.; Raja, S.; Rajan, C.; Rajbhandari, B.; Rakhmanov, M.; Ramirez, K. E.; Ramos-Buades, A.; Rapagnani, P.; Raymond, V.; Razzano, M.; Read, J.; Regimbau, T.; Rei, L.; Reid, S.; Reitze, D. H.; Ren, W.; Reyes, S. D.; Ricci, F.; Ricker, P. M.; Rieger, S.; Riles, K.; Rizzo, M.; Robertson, N. A.; Robie, R.; Robinet, F.; Rocchi, A.; Rolland, L.; Rollins, J. G.; Roma, V. J.; Romano, R.; Romel, C. L.; Romie, J. H.; Rosińska, D.; Ross, M. P.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Rutins, G.; Ryan, K.; Sachdev, S.; Sadecki, T.; Sadeghian, L.; Sakellariadou, M.; Salconi, L.; Saleem, M.; Salemi, F.; Samajdar, A.; Sammut, L.; Sampson, L. M.; Sanchez, E. J.; Sanchez, L. E.; Sanchis-Gual, N.; Sandberg, V.; Sanders, J. R.; Sassolas, B.; Sathyaprakash, B. S.; Saulson, P. R.; Sauter, O.; Savage, R. L.; Sawadsky, A.; Schale, P.; Scheel, M.; Scheuer, J.; Schmidt, J.; Schmidt, P.; Schnabel, R.; Schofield, R. M. S.; Schönbeck, A.; Schreiber, E.; Schuette, D.; Schulte, B. W.; Schutz, B. F.; Schwalbe, S. G.; Scott, J.; Scott, S. M.; Seidel, E.; Sellers, D.; Sengupta, A. S.; Sentenac, D.; Sequino, V.; Sergeev, A.; Shaddock, D. A.; Shaffer, T. J.; Shah, A. A.; Shahriar, M. S.; Shaner, M. B.; Shao, L.; Shapiro, B.; Shawhan, P.; Sheperd, A.; Shoemaker, D. H.; Shoemaker, D. M.; Siellez, K.; Siemens, X.; Sieniawska, M.; Sigg, D.; Silva, A. D.; Singer, L. P.; Singh, A.; Singhal, A.; Sintes, A. M.; Slagmolen, B. J. J.; Smith, B.; Smith, J. R.; Smith, R. J. E.; Somala, S.; Son, E. J.; Sonnenberg, J. A.; Sorazu, B.; Sorrentino, F.; Souradeep, T.; Spencer, A. P.; Srivastava, A. K.; Staats, K.; Staley, A.; Steinke, M.; Steinlechner, J.; Steinlechner, S.; Steinmeyer, D.; Stevenson, S. P.; Stone, R.; Stops, D. J.; Strain, K. A.; Stratta, G.; Strigin, S. E.; Strunk, A.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.; Sun, L.; Sunil, S.; Suresh, J.; Sutton, P. J.; Swinkels, B. L.; Szczepańczyk, M. J.; Tacca, M.; Tait, S. C.; Talbot, C.; Talukder, D.; Tanner, D. B.; Tápai, M.; Taracchini, A.; Tasson, J. D.; Taylor, J. A.; Taylor, R.; Tewari, S. V.; Theeg, T.; Thies, F.; Thomas, E. G.; Thomas, M.; Thomas, P.; Thorne, K. A.; Thrane, E.; Tiwari, S.; Tiwari, V.; Tokmakov, K. V.; Toland, K.; Tonelli, M.; Tornasi, Z.; Torres-Forné, A.; Torrie, C. I.; Töyrä, D.; Travasso, F.; Traylor, G.; Trinastic, J.; Tringali, M. C.; Trozzo, L.; Tsang, K. W.; Tse, M.; Tso, R.; Tsukada, L.; Tsuna, D.; Tuyenbayev, D.; Ueno, K.; Ugolini, D.; Unnikrishnan, C. S.; Urban, A. L.; Usman, S. A.; Vahlbruch, H.; Vajente, G.; Valdes, G.; van Bakel, N.; van Beuzekom, M.; van den Brand, J. F. J.; Van Den Broeck, C.; Vander-Hyde, D. C.; van der Schaaf, L.; van Heijningen, J. V.; van Veggel, A. A.; Vardaro, M.; Varma, V.; Vass, S.; Vasúth, M.; Vecchio, A.; Vedovato, G.; Veitch, J.; Veitch, P. J.; Venkateswara, K.; Venugopalan, G.; Verkindt, D.; Vetrano, F.; Viceré, A.; Viets, A. D.; Vinciguerra, S.; Vine, D. J.; Vinet, J.-Y.; Vitale, S.; Vo, T.; Vocca, H.; Vorvick, C.; Vyatchanin, S. P.; Wade, A. R.; Wade, L. E.; Wade, M.; Walet, R.; Walker, M.; Wallace, L.; Walsh, S.; Wang, G.; Wang, H.; Wang, J. Z.; Wang, W. H.; Wang, Y. F.; Ward, R. L.; Warner, J.; Was, M.; Watchi, J.; Weaver, B.; Wei, L.-W.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wessel, E. K.; Weßels, P.; Westerweck, J.; Westphal, T.; Wette, K.; Whelan, J. T.; Whiting, B. F.; Whittle, C.; Wilken, D.; Williams, D.; Williams, R. D.; Williamson, A. R.; Willis, J. L.; Willke, B.; Wimmer, M. H.; Winkler, W.; Wipf, C. C.; Wittel, H.; Woan, G.; Woehler, J.; Wofford, J.; Wong, K. W. K.; Worden, J.; Wright, J. L.; Wu, D. S.; Wysocki, D. M.; Xiao, S.; Yamamoto, H.; Yancey, C. C.; Yang, L.; Yap, M. J.; Yazback, M.; Yu, Hang; Yu, Haocun; Yvert, M.; ZadroŻny, A.; Zanolin, M.; Zelenova, T.; Zendri, J.-P.; Zevin, M.; Zhang, L.; Zhang, M.; Zhang, T.; Zhang, Y.-H.; Zhao, C.; Zhou, M.; Zhou, Z.; Zhu, S. J.; Zhu, X. J.; Zucker, M. E.; Zweizig, J.; LIGO Scientific Collaboration; Virgo Collaboration</p> <p>2017-12-01</p> <p>Spinning neutron stars asymmetric with respect to their rotation axis are potential sources of continuous gravitational waves for ground-based interferometric detectors. In the case of known pulsars a fully coherent search, based on matched filtering, which uses the <span class="hlt">position</span> and rotational parameters obtained from electromagnetic <span class="hlt">observations</span>, can be carried out. Matched filtering maximizes the signal-to-noise (SNR) ratio, but a large sensitivity loss is expected in case of even a very small mismatch between the assumed and the true signal parameters. For this reason, narrow-<span class="hlt">band</span> analysis methods have been developed, allowing a fully coherent search for gravitational waves from known pulsars over a fraction of a hertz and several spin-down values. In this paper we describe a narrow-<span class="hlt">band</span> search of 11 pulsars using data from Advanced LIGO's first <span class="hlt">observing</span> run. Although we have found several initial outliers, further studies show no significant evidence for the presence of a gravitational wave signal. Finally, we have placed upper limits on the signal strain amplitude lower than the spin-down limit for 5 of the 11 targets over the <span class="hlt">bands</span> searched; in the case of J1813-1749 the spin-down limit has been beaten for the first time. For an additional 3 targets, the median upper limit across the search <span class="hlt">bands</span> is below the spin-down limit. This is the most sensitive narrow-<span class="hlt">band</span> search for continuous gravitational waves carried out so far.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016AJ....151..154G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016AJ....151..154G"><span>Second Epoch VLBA Calibrator Survey <span class="hlt">Observations</span>: VCS-II</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gordon, David; Jacobs, Christopher; Beasley, Anthony; Peck, Alison; Gaume, Ralph; Charlot, Patrick; Fey, Alan; Ma, Chopo; Titov, Oleg; Boboltz, David</p> <p>2016-06-01</p> <p>Six very successful Very Long Baseline Array (VLBA) calibrator survey campaigns were run between 1994 and 2007 to build up a large list of compact radio sources with <span class="hlt">positions</span> precise enough for use as very long baseline interferometry (VLBI) phase reference calibrators. We report on the results of a second epoch VLBA Calibrator Survey campaign (VCS-II) in which 2400 VCS sources were re-<span class="hlt">observed</span> in the X and S <span class="hlt">bands</span> in order to improve the upcoming third realization of the International Celestial Reference Frame (ICRF3) as well as to improve their usefulness as VLBI phase reference calibrators. In this survey, some 2062 previously detected sources and 324 previously undetected sources were detected and revised <span class="hlt">positions</span> are presented. Average <span class="hlt">position</span> uncertainties for the re-<span class="hlt">observed</span> sources were reduced from 1.14 and 1.98 mas to 0.24 and 0.41 mas in R.A. and decl., respectively, or by nearly a factor of 5. Minimum detected flux values were approximately 15 and 28 mJy in the X and S <span class="hlt">bands</span>, respectively, and median total fluxes are approximately 230 and 280 mJy. The vast majority of these sources are flat-spectrum sources, with ˜82% having spectral indices greater than -0.5.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/29244637','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/29244637"><span>U-shaped Relation between Prestimulus Alpha-<span class="hlt">band</span> and Poststimulus Gamma-<span class="hlt">band</span> Power in Temporal Tactile Perception in the Human Somatosensory Cortex.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Wittenberg, Marc André; Baumgarten, Thomas J; Schnitzler, Alfons; Lange, Joachim</p> <p>2018-04-01</p> <p>Neuronal oscillations are a ubiquitous phenomenon in the human nervous system. Alpha-<span class="hlt">band</span> oscillations (8-12 Hz) have been shown to correlate negatively with attention and performance, whereas gamma-<span class="hlt">band</span> oscillations (40-150 Hz) correlate <span class="hlt">positively</span>. Here, we studied the relation between prestimulus alpha-<span class="hlt">band</span> power and poststimulus gamma-<span class="hlt">band</span> power in a suprathreshold tactile discrimination task. Participants received two electrical stimuli to their left index finger with different SOAs (0 msec, 100 msec, intermediate SOA, intermediate SOA ± 10 msec). The intermediate SOA was individually determined so that stimulation was bistable, and participants perceived one stimulus in half of the trials and two stimuli in the other half. We measured neuronal activity with magnetoencephalography (MEG). In trials with intermediate SOAs, behavioral performance correlated inversely with prestimulus alpha-<span class="hlt">band</span> power but did not correlate with poststimulus gamma-<span class="hlt">band</span> power. Poststimulus gamma-<span class="hlt">band</span> power was high in trials with low and high prestimulus alpha-<span class="hlt">band</span> power and low for intermediate prestimulus alpha-<span class="hlt">band</span> power (i.e., U-shaped). We suggest that prestimulus alpha activity modulates poststimulus gamma activity and subsequent perception: (1) low prestimulus alpha-<span class="hlt">band</span> power leads to high poststimulus gamma-<span class="hlt">band</span> power, biasing perception such that two stimuli were perceived; (2) intermediate prestimulus alpha-<span class="hlt">band</span> power leads to low gamma-<span class="hlt">band</span> power (interpreted as inefficient stimulus processing), consequently, perception was not biased in either direction; and (3) high prestimulus alpha-<span class="hlt">band</span> power leads to high poststimulus gamma-<span class="hlt">band</span> power, biasing perception such that only one stimulus was perceived.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018JQSRT.208...39R','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018JQSRT.208...39R"><span>Photoionization <span class="hlt">bands</span> of rubidium molecule</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Rakić, M.; Pichler, G.</p> <p>2018-03-01</p> <p>We studied the absorption spectrum of dense rubidium vapor generated in a T-type sapphire cell with a special emphasis on the structured photoionization continuum <span class="hlt">observed</span> in the 200-300 nm spectral region. The photoionization spectrum has a continuous atomic contribution with a pronounced Seaton-Cooper minimum at about 250 nm and a molecular photoionization contribution with many broad <span class="hlt">bands</span>. We discuss the possible origin of the photoionization <span class="hlt">bands</span> as stemming from the absorption from the ground state of the Rb2 molecule to excited states of Rb2+* and to doubly excited autoionizing states of Rb2** molecule. All these photoionization <span class="hlt">bands</span> are located above the Rb+ and Rb2+ ionization limits.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018A%26A...611A..98B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018A%26A...611A..98B"><span>ALMA <span class="hlt">Band</span> 5 receiver cartridge. Design, performance, and commissioning</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Belitsky, V.; Bylund, M.; Desmaris, V.; Ermakov, A.; Ferm, S.-E.; Fredrixon, M.; Krause, S.; Lapkin, I.; Meledin, D.; Pavolotsky, A.; Rashid, H.; Shafiee, S.; Strandberg, M.; Sundin, E.; Aghdam, P. Yadranjee; Hesper, R.; Barkhof, J.; Bekema, M. E.; Adema, J.; Haan, R. de; Koops, A.; Boland, W.; Yagoubov, P.; Marconi, G.; Siringo, G.; Humphreys, E.; Tan, G. H.; Laing, R.; Testi, L.; Mroczkowski, T.; Wild, W.; Saini, K. S.; Bryerton, E.</p> <p>2018-04-01</p> <p>We describe the design, performance, and commissioning results for the new ALMA <span class="hlt">Band</span> 5 receiver channel, 163-211 GHz, which is in the final stage of full deployment and expected to be available for <span class="hlt">observations</span> in 2018. This manuscript provides the description of the new ALMA <span class="hlt">Band</span> 5 receiver cartridge and serves as a reference for <span class="hlt">observers</span> using the ALMA <span class="hlt">Band</span> 5 receiver for <span class="hlt">observations</span>. At the time of writing this paper, the ALMA <span class="hlt">Band</span> 5 Production Consortium consisting of NOVA Instrumentation group, based in Groningen, NL, and GARD in Sweden have produced and delivered to ALMA Observatory over 60 receiver cartridges. All 60 cartridges fulfil the new more stringent specifications for <span class="hlt">Band</span> 5 and demonstrate excellent noise temperatures, typically below 45 K single sideband (SSB) at 4 K detector physical temperature and below 35 K SSB at 3.5 K (typical for operation at the ALMA Frontend), providing the average sideband rejection better than 15 dB, and the integrated cross-polarization level better than -25 dB. The 70 warm cartridge assemblies, hosting <span class="hlt">Band</span> 5 local oscillator and DC bias electronics, have been produced and delivered to ALMA by NRAO. The commissioning results confirm the excellent performance of the receivers.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1997APS..SHK..C103D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1997APS..SHK..C103D"><span>Shear <span class="hlt">Band</span> Formation in Plastic-Bonded Explosives (PBX)</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Dey, Thomas N.; Johnson, James N.</p> <p>1997-07-01</p> <p>Adiabatic shear <span class="hlt">bands</span> can be a source of ignition and lead to detonation. At low to moderate deformation rates, 10--1000 s-1, two other mechanisms can also give rise to shear <span class="hlt">bands</span>. These mechanisms are: softening caused by micro-cracking and (2) a constitutive response with a non-associated flow rule as is <span class="hlt">observed</span> in granular material such as soil. Brittle behavior at small strains and the granular nature of HMX suggest that PBX-9501 constitutive behavior may be similar to sand. A constitutive model for each of these mechanims is studied in a series of calculations. A viscoelastic constitutive model for PBX-9501 softens via a statistical crack model, based on the work of Dienes (1986). A sand model is used to provide a non-associated flow rule. Both models generate shear <span class="hlt">band</span> formation at 1--2% strain at nominal strain rates at and below 1000 s-1. Shear <span class="hlt">band</span> formation is suppressed at higher strain rates. The sand model gives qualitative agreement for location and orientation of shear <span class="hlt">bands</span> <span class="hlt">observed</span> in a punch experiment. Both mechanisms may accelerate the formation of adiabatic shear <span class="hlt">bands</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://eric.ed.gov/?q=background+AND+music+AND+classroom&pg=5&id=EJ831693','ERIC'); return false;" href="https://eric.ed.gov/?q=background+AND+music+AND+classroom&pg=5&id=EJ831693"><span>Accentuate the <span class="hlt">Positive</span>! North Carolina <span class="hlt">Band</span> Director Boosts His Students' Confidence and Earns Statewide Leadership Role</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Olson, Catherine Applefeld</p> <p>2009-01-01</p> <p>In this article, the author shares the background of James Daugherty in music education, a <span class="hlt">band</span> director who was elected to serve as president of the North Carolina Bandmasters Association, the highest leadership role for a <span class="hlt">band</span> director in the state. His passion for music only grew in high school, where he gleaned both musical and life lessons…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19800053104&hterms=L37&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3DL37','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19800053104&hterms=L37&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3DL37"><span>X-ray <span class="hlt">observations</span> of the supernova remnant MSH 11-54</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Agrawal, P. C.; Riegler, G. R.</p> <p>1980-01-01</p> <p>Soft X-ray <span class="hlt">observations</span> of the X-ray source H1122-59 in the 0.4-2 keV <span class="hlt">band</span> made with the low-energy detector 1 of the HEAO A-2 experiment are described. Based on <span class="hlt">positional</span> coincidence, the source is identified with the supernova remnant MSH-11-54, thus confirming the report of Share et al. (1980). The object is a bright source in the 0.4-2 keV <span class="hlt">band</span> with an X-ray flux of 9 x 10 to the -11th ergs/sq cm s near the earth. The measured source spectrum implies a plasma temperature of 4 million K and X-ray luminosity in the 0.4-2 keV <span class="hlt">band</span> of 10 to the 37th ergs/s using a distance of 10 kpc for MSH 11-54. The X-ray <span class="hlt">observations</span>, interpreted in terms of an adiabatic shock wave model, give a shock velocity of about 560 km/s and a supernova age of about 2300 yr, in good agreement with the age derived from the radio <span class="hlt">observations</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017ExA....44..359D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017ExA....44..359D"><span>The Cryogenic AntiCoincidence detector for ATHENA X-IFU: a scientific assessment of the <span class="hlt">observational</span> capabilities in the hard X-ray <span class="hlt">band</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>D'Andrea, M.; Lotti, S.; Macculi, C.; Piro, L.; Argan, A.; Gatti, F.</p> <p>2017-12-01</p> <p>ATHENA is a large X-ray observatory, planned to be launched by ESA in 2028 towards an L2 orbit. One of the two instruments of the payload is the X-IFU: a cryogenic spectrometer based on a large array of TES microcalorimeters, able to perform integral field spectrography in the 0.2-12 keV <span class="hlt">band</span> (2.5 eV FWHM at 6 keV). The X-IFU sensitivity is highly degraded by the particle background expected in the L2 orbit, which is induced by primary protons of both galactic and solar origin, and mostly by secondary electrons. To reduce the particle background level and enable the mission science goals, the instrument incorporates a Cryogenic AntiCoincidence detector (CryoAC). It is a 4 pixel TES based detector, placed < 1 mm below the main array. In this paper we report a scientific assessment of the CryoAC <span class="hlt">observational</span> capabilities in the hard X-ray <span class="hlt">band</span> (E > 10 keV). The aim of the study has been to understand if the present detector design can be improved in order to enlarge the X-IFU scientific capability on an energy <span class="hlt">band</span> wider than the TES array. This is beyond the CryoAC baseline, being this instrument aimed to operate as anticoincidence particle detector and not conceived to perform X-ray <span class="hlt">observations</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018JApSp..85..279G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018JApSp..85..279G"><span>Effect of a Nitrogen Impurity on the Fundamental Raman <span class="hlt">Band</span> of Diamond Single Crystals</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gusakov, G. A.; Samtsov, M. P.; Voropay, E. S.</p> <p>2018-05-01</p> <p>The effect of nitrogen defects in natural and synthetic diamond single crystals on the <span class="hlt">position</span> and half-width of the fundamental Raman <span class="hlt">band</span> was investigated. Samples containing the main types of nitrogen lattice defects at impurity contents of 1-1500 ppm were studied. The parameters of the Stokes and anti-Stokes components in Raman spectra of crystals situated in a cell with distilled water to minimize the influence of heating by the exciting laser radiation were analyzed to determine the effect of a nitrogen impurity in the diamond crystal lattice. It was shown that an increase of impurity atoms in the crystals in the studied concentration range resulted in broadening of the Raman <span class="hlt">band</span> from 1.61 to 2.85 cm-1 and shifting of the maximum to lower frequency from 1332.65 to 1332.3 cm-1. The <span class="hlt">observed</span> effect was directly proportional to the impurity concentration and depended on the form of the impurity incorporated into the diamond lattice. It was found that the changes in the <span class="hlt">position</span> and half-width of the fundamental Raman <span class="hlt">band</span> for diamond were consistent with the magnitude of crystal lattice distortions due to the presence of impurity defects and obeyed the Gruneisen law.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20020017758','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20020017758"><span><span class="hlt">Band</span> Anticrossing in Highly Mismatched Compound Semiconductor Alloys</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Yu, Kin Man; Wu, J.; Walukiewicz, W.; Ager, J. W.; Haller, E. E.; Miotkowski, I.; Ramdas, A.; Su, Ching-Hua; Whitaker, Ann F. (Technical Monitor)</p> <p>2001-01-01</p> <p>Compound semiconductor alloys in which metallic anions are partially replaced with more electronegative isoelectronic atoms have recently attracted significant attention. Group IIIN(x)V(1-x), alloys with a small amount of the electronegative N substituting more metallic column V elements has been the most extensively studied class of such Highly Mismatched Alloys (HMAs). We have shown that many of the unusual properties of the IIIN(x),V(1-x) alloys can be well explained by the <span class="hlt">Band</span> Anticrossing (BAC) model that describes the electronic structure in terms of an interaction between highly localized levels of substitutional N and the extended states of the host semiconductor matrix. Most recently the BAC model has been also used to explain similar modifications of the electronic <span class="hlt">band</span> structure <span class="hlt">observed</span> in Te-rich ZnS(x)Te(l-x) and ZnSe(Y)Te(1-y) alloys. To date studies of HMAs have been limited to materials with relatively small concentrations of highly electronegative atoms. Here we report investigations of the electronic structure of ZnSe(y)Te(1-y) alloys in the entire composition range, 0 less than or equal to y less than or equal to 1. The samples used in this study are bulk ZnSe(y)Te(1-y) crystals grown by either a modified Bridgman method or by physical vapor transport. Photomodulated reflection (PR) spectroscopy was used to measure the composition dependence of optical transitions from the valence <span class="hlt">band</span> edge and from the spin-orbit split off <span class="hlt">band</span> to the conduction <span class="hlt">band</span>. The pressure dependence of the <span class="hlt">band</span> gap was measured using optical absorption in a diamond anvil cell. We find that the energy of the spin-orbit split off valence <span class="hlt">band</span> edge does not depend on composition and is located at about 3 eV below the conduction <span class="hlt">band</span> edge of ZnSe. On the Te-rich side the pressure and the composition dependence of the optical transitions are well explained by the BAC model which describes the downward shift of the conduction <span class="hlt">band</span> edge in terms of the interaction between</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3511118','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3511118"><span>Dilatational <span class="hlt">band</span> formation in bone</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Poundarik, Atharva A.; Diab, Tamim; Sroga, Grazyna E.; Ural, Ani; Boskey, Adele L.; Gundberg, Caren M.; Vashishth, Deepak</p> <p>2012-01-01</p> <p>Toughening in hierarchically structured materials like bone arises from the arrangement of constituent material elements and their interactions. Unlike microcracking, which entails micrometer-level separation, there is no known evidence of fracture at the level of bone’s nanostructure. Here, we show that the initiation of fracture occurs in bone at the nanometer scale by dilatational <span class="hlt">bands</span>. Through fatigue and indentation tests and laser confocal, scanning electron, and atomic force microscopies on human and bovine bone specimens, we established that dilatational <span class="hlt">bands</span> of the order of 100 nm form as ellipsoidal voids in between fused mineral aggregates and two adjacent proteins, osteocalcin (OC) and osteopontin (OPN). Laser microdissection and ELISA of bone microdamage support our claim that OC and OPN colocalize with dilatational <span class="hlt">bands</span>. Fracture tests on bones from OC and/or OPN knockout mice (OC−/−, OPN−/−, OC-OPN−/−;−/−) confirm that these two proteins regulate dilatational <span class="hlt">band</span> formation and bone matrix toughness. On the basis of these <span class="hlt">observations</span>, we propose molecular deformation and fracture mechanics models, illustrating the role of OC and OPN in dilatational <span class="hlt">band</span> formation, and predict that the nanometer scale of tissue organization, associated with dilatational <span class="hlt">bands</span>, affects fracture at higher scales and determines fracture toughness of bone. PMID:23129653</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28738679','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28738679"><span>Probability of Two-Step Photoexcitation of Electron from Valence <span class="hlt">Band</span> to Conduction <span class="hlt">Band</span> through Doping Level in TiO2.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Nishikawa, Masami; Shiroishi, Wataru; Honghao, Hou; Suizu, Hiroshi; Nagai, Hideyuki; Saito, Nobuo</p> <p>2017-08-17</p> <p>For an Ir-doped TiO 2 (Ir:TiO 2 ) photocatalyst, we examined the most dominant electron-transfer path for the visible-light-driven photocatalytic performance. The Ir:TiO 2 photocatalyst showed a much higher photocatalytic activity under visible-light irradiation than nondoped TiO 2 after grafting with the cocatalyst of Fe 3+ . For the Ir:TiO 2 photocatalyst, the two-step photoexcitation of an electron from the valence <span class="hlt">band</span> to the conduction <span class="hlt">band</span> through the Ir doping level occurred upon visible-light irradiation, as <span class="hlt">observed</span> by electron spin resonance spectroscopy. The two-step photoexcitation through the doping level was found to be a more stable process with a lower recombination rate of hole-electron pairs than the two-step photoexcitation process through an oxygen vacancy. Once electrons are photoexcited to the conduction <span class="hlt">band</span> by the two-step excitation, the electrons can easily transfer to the surface because the conduction <span class="hlt">band</span> is a continuous electron path, whereas the electrons photoexcited at only the doping level could not easily transfer to the surface because of the discontinuity of this path. The <span class="hlt">observed</span> two-step photoexcitation from the valence <span class="hlt">band</span> to the conduction <span class="hlt">band</span> through the doping level significantly contributes to the enhancement of the photocatalytic performance.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1980ApJS...43..417P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1980ApJS...43..417P"><span>An infrared <span class="hlt">band</span> system of the ZrCl molecule</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Phillips, J. G.; Davis, S. P.; Galehouse, D. C.</p> <p>1980-07-01</p> <p>A series of infrared <span class="hlt">bands</span> in the 0.97-1.15 micron region which is attributed to ZrCl is analyzed in light of the possibility that the <span class="hlt">bands</span> may be <span class="hlt">observable</span> in stellar spectra. Spectra of ZrO and ZrCl were produced by microwave discharge through a mixture of He, O and ZrCl4 and <span class="hlt">observed</span> by Fourier transform spectrometer, resulting in the <span class="hlt">observation</span> of 10 <span class="hlt">bands</span> of the ZrCl system. Rotational quantum number assignments to the lines of the P and R branches <span class="hlt">observed</span> are obtained and used to derive effective rotational constants for each substate, as well as zero-rotation origins of each subband. Shifts in wave numbers of rotational lines of the isotopes (Zr-92)(Cl-35)(Zr-94)(Cl-35) and (Zr-90)(Cl-37) relative to the more abundant (Zr-90)(Cl-35) are also <span class="hlt">observed</span>. The <span class="hlt">observed</span> molecular constants are shown to be in good agreement with those calculated in previous theoretical estimates.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20120010414&hterms=solar+geometry&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dsolar%2Bgeometry','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20120010414&hterms=solar+geometry&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dsolar%2Bgeometry"><span>Using the Moon to Track MODIS Reflective Solar <span class="hlt">Bands</span> Calibration Stability</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Xiong, Xiaoxiong; Geng, Xu; Angal, Amit; Sun, Junqiang; Barnes, William</p> <p>2011-01-01</p> <p>MODIS has 20 reflective solar <span class="hlt">bands</span> (RSB) in the visible (VIS), near infrared (NIR), and short-wave infrared (SWIR) spectral regions. In addition to instrument on-board calibrators (OBC), lunar <span class="hlt">observations</span> have been used by both Terra and Aqua MODIS to track their reflective solar <span class="hlt">bands</span> (RSB) on-orbit calibration stability. On a near monthly basis, lunar <span class="hlt">observations</span> are scheduled and implemented for each instrument at nearly the same lunar phase angles. A time series of normalized detector responses to the Moon is used to monitor its on-orbit calibration stability. The normalization is applied to correct the differences of lunar viewing geometries and the Sun-Moon-Sensor distances among different lunar <span class="hlt">observations</span>. Initially, the lunar calibration stability monitoring was only applied to MODIS <span class="hlt">bands</span> (1-4 and 8-12) that do not saturate while viewing the Moon. As the mission continued, we extended the lunar calibration stability monitoring to other RSB <span class="hlt">bands</span> (<span class="hlt">bands</span> 13-16) that contain saturated pixels. For these <span class="hlt">bands</span>, the calibration stability is monitored by referencing their non-saturated pixels to the matched pixels in a non-saturation <span class="hlt">band</span>. In this paper, we describe this relative approach and apply it to MODIS regularly scheduled lunar <span class="hlt">observations</span>. We present lunar trending results for both Terra and Aqua MODIS over their entire missions. Also discussed in the paper are the advantages and limitations of this approach and its potential applications to other earth-<span class="hlt">observing</span> sensors. Keywords: Terra, Aqua, MODIS, sensor, Moon, calibration, stability</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/1079116-optimization-pulsed-deer-measurements-gd-based-labels-choice-operational-frequencies-pulse-durations-positions-temperature','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/1079116-optimization-pulsed-deer-measurements-gd-based-labels-choice-operational-frequencies-pulse-durations-positions-temperature"><span>Optimization of Pulsed-DEER Measurements for Gd-Based Labels: Choice of Operational Frequencies, Pulse Durations and <span class="hlt">Positions</span>, and Temperature</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Raitsimring, A.; Astashkin, A. V.; Enemark, J. H.</p> <p>2012-12-29</p> <p>In this work, the experimental conditions and parameters necessary to optimize the long-distance (≥ 60 Å) Double Electron-Electron Resonance (DEER) measurements of biomacromolecules labeled with Gd(III) tags are analyzed. The specific parameters discussed are the temperature, microwave <span class="hlt">band</span>, the separation between the pumping and <span class="hlt">observation</span> frequencies, pulse train repetition rate, pulse durations and pulse <span class="hlt">positioning</span> in the electron paramagnetic resonance spectrum. It was found that: (i) in optimized DEER measurements, the <span class="hlt">observation</span> pulses have to be applied at the maximum of the EPR spectrum; (ii) the optimal temperature range for Ka-<span class="hlt">band</span> measurements is 14-17 K, while in W-<span class="hlt">band</span> the optimalmore » temperatures are between 6-9 K; (iii) W-<span class="hlt">band</span> is preferable to Ka-<span class="hlt">band</span> for DEER measurements. Recent achievements and the conditions necessary for short-distance measurements (<15 Å) are also briefly discussed.« less</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_12");'>12</a></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li class="active"><span>14</span></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_14 --> <div id="page_15" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li class="active"><span>15</span></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="281"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018TDM.....5a5008K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018TDM.....5a5008K"><span>Towards <span class="hlt">band</span> structure and <span class="hlt">band</span> offset engineering of monolayer Mo(1-x)W(x)S2 via Strain</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kim, Joon-Seok; Ahmad, Rafia; Pandey, Tribhuwan; Rai, Amritesh; Feng, Simin; Yang, Jing; Lin, Zhong; Terrones, Mauricio; Banerjee, Sanjay K.; Singh, Abhishek K.; Akinwande, Deji; Lin, Jung-Fu</p> <p>2018-01-01</p> <p>Semiconducting transition metal dichalcogenides (TMDs) demonstrate a wide range of optoelectronic properties due to their diverse elemental compositions, and are promising candidates for next-generation optoelectronics and energy harvesting devices. However, effective <span class="hlt">band</span> offset engineering is required to implement practical structures with desirable functionalities. Here, we explore the pressure-induced <span class="hlt">band</span> structure evolution of monolayer WS2 and Mo0.5W0.5S2 using hydrostatic compressive strain applied in a diamond anvil cell (DAC) apparatus and theoretical calculations, in order to study the modulation of <span class="hlt">band</span> structure and explore the possibility of <span class="hlt">band</span> alignment engineering through different compositions. Higher W composition in Mo(1-x)W(x)S2 contributes to a greater pressure-sensitivity of direct <span class="hlt">band</span> gap opening, with a maximum value of 54 meV GPa-1 in WS2. Interestingly, while the conduction <span class="hlt">band</span> minima (CBMs) remains largely unchanged after the rapid gap increase, valence <span class="hlt">band</span> maxima (VBMs) significantly rise above the initial values. It is suggested that the pressure- and composition-engineering could introduce a wide variety of <span class="hlt">band</span> alignments including type I, type II, and type III heterojunctions, and allow to construct precise structures with desirable functionalities. No structural transition is <span class="hlt">observed</span> during the pressure experiments, implying the pressure could provide selective modulation of <span class="hlt">band</span> offset.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018LPICo2070.6061P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018LPICo2070.6061P"><span>Mini-RF S- and X-<span class="hlt">Band</span> Bistatic Radar <span class="hlt">Observations</span> of the Moon</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Patterson, G. W.; Carter, L. M.; Stickle, A. M.; Cahill, J. T. S.; Nolan, M. C.; Morgan, G. A.; Schroeder, D. M.; Mini-RF Team</p> <p>2018-04-01</p> <p>The Mini-RF instrument onboard the NASA LRO mission is collecting S- and X-<span class="hlt">band</span> bistatic radar data to provide new insights regarding regolith development on the Moon, the diversity of lunar volcanism, and the current inventory of polar ice.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19910005603','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19910005603"><span>Correlation properties of interstellar dust: Diffuse interstellar <span class="hlt">bands</span></span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Somerville, W. B.</p> <p>1989-01-01</p> <p>Results are presented from a research program in which an attempt was made to establish the physical nature of the interstellar grains, and the carriers of the diffuse interstellar <span class="hlt">bands</span>, by comparing relations between different <span class="hlt">observed</span> properties; the properties used include the extinction in the optical and ultraviolet (including wavelength 2200 and the far-UV rise), cloud density, atomic depletions, and strengths of the diffuse <span class="hlt">bands</span>. <span class="hlt">Observations</span> and also data from literature were used, selecting particularly sight-lines where some <span class="hlt">observed</span> property was found to have anomalous behavior.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3872230','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3872230"><span>Dual-<span class="hlt">Band</span> Operation of a Microstrip Patch Antenna on a Duroid 5870 Substrate for Ku- and K-<span class="hlt">Bands</span></span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Islam, M. M.; Islam, M. T.; Faruque, M. R. I.</p> <p>2013-01-01</p> <p>The dual-<span class="hlt">band</span> operation of a microstrip patch antenna on a Duroid 5870 substrate for Ku- and K-<span class="hlt">bands</span> is presented. The fabrication of the proposed antenna is performed with slots and a Duroid 5870 dielectric substrate and is excited by a 50 Ω microstrip transmission line. A high-frequency structural simulator (HFSS) is used which is based on the finite element method (FEM) in this research. The measured impedance bandwidth (2 : 1 VSWR) achieved is 1.07 GHz (15.93 GHz–14.86 GHz) on the lower <span class="hlt">band</span> and 0.94 GHz (20.67–19.73 GHz) on the upper <span class="hlt">band</span>. A stable omnidirectional radiation pattern is <span class="hlt">observed</span> in the operating frequency <span class="hlt">band</span>. The proposed prototype antenna behavior is discussed in terms of the comparisons of the measured and simulated results. PMID:24385878</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24385878','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24385878"><span>Dual-<span class="hlt">band</span> operation of a microstrip patch antenna on a Duroid 5870 substrate for Ku- and K-<span class="hlt">bands</span>.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Islam, M M; Islam, M T; Faruque, M R I</p> <p>2013-01-01</p> <p>The dual-<span class="hlt">band</span> operation of a microstrip patch antenna on a Duroid 5870 substrate for Ku- and K-<span class="hlt">bands</span> is presented. The fabrication of the proposed antenna is performed with slots and a Duroid 5870 dielectric substrate and is excited by a 50 Ω microstrip transmission line. A high-frequency structural simulator (HFSS) is used which is based on the finite element method (FEM) in this research. The measured impedance bandwidth (2 : 1 VSWR) achieved is 1.07 GHz (15.93 GHz-14.86 GHz) on the lower <span class="hlt">band</span> and 0.94 GHz (20.67-19.73 GHz) on the upper <span class="hlt">band</span>. A stable omnidirectional radiation pattern is <span class="hlt">observed</span> in the operating frequency <span class="hlt">band</span>. The proposed prototype antenna behavior is discussed in terms of the comparisons of the measured and simulated results.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/10757939','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/10757939"><span>A Simple <span class="hlt">Band</span> for Gastric <span class="hlt">Banding</span>.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Broadbent</p> <p>1993-08-01</p> <p>The author has noted that flexible gastric <span class="hlt">bands</span> have occasionally stenosed the gastric stoma or allowed it to dilate. A <span class="hlt">band</span> was developed using a soft outer silicone rubber tube over a holding mechanism made out of a nylon cable tie passed within the silicone tube. This simple, easily applied <span class="hlt">band</span> is rigid, resisting scar contracture and dilatation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20040090011&hterms=Polycyclic+aromatic+hydrocarbons&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3DPolycyclic%2Baromatic%2Bhydrocarbons','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20040090011&hterms=Polycyclic+aromatic+hydrocarbons&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3DPolycyclic%2Baromatic%2Bhydrocarbons"><span>Assessment of the polycyclic aromatic hydrocarbon-diffuse interstellar <span class="hlt">band</span> proposal</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Salama, F.; Bakes, E. L.; Allamandola, L. J.; Tielens, A. G.</p> <p>1996-01-01</p> <p>The potential link between neutral and/or ionized polycyclic aromatic hydrocarbons (PAHs) and the diffuse interstellar <span class="hlt">band</span> (DIB) carriers is examined. Based on the study of the general physical and chemical properties of PAHs, an assessment is made of their possible contribution to the DIB carriers. It is found that, under the conditions reigning in the diffuse interstellar medium, PAHs can be present in the form of neutral molecules as well as <span class="hlt">positive</span> and/or negative ions. The charge distribution of small PAHs is dominated, however, by two charge states at one time with compact PAHs present only in the neutral and cationic forms. Each PAH has a distinct spectral signature depending on its charge state. Moreover, the spectra of ionized PAHs are always clearly dominated by a single <span class="hlt">band</span> in the DIB spectral range. In the case of compact PAH ions, the strongest absorption <span class="hlt">band</span> is of type A (i.e., the <span class="hlt">band</span> is broad, falls in the high-energy range of the spectrum, and possesses a large oscillator strength), and seems to correlate with strong and broad DIBs. For noncompact PAH ions, the strongest absorption <span class="hlt">band</span> is of type I (i.e., the <span class="hlt">band</span> is narrow, falls in the low-energy range of the spectrum, and possesses a small oscillator strength), and seems to correlate with weak and narrow DIBs. Potential molecular size and structure constraints for interstellar PAHs are derived by comparing known DIB characteristics to the spectroscopic properties of PAHs. It is found that (i) only neutral PAHs larger than about 30 carbon atoms could, if present, contribute to the DIBs. (ii) For compact PAHs, only ions with less than about 250 carbon atoms could, if present, contribute to the DIBs. (iii) The <span class="hlt">observed</span> distribution of the DIBs between strong/moderate and broad <span class="hlt">bands</span> on the one hand and weak and narow <span class="hlt">bands</span> on the other can easily be interpreted in the context of the PAH proposal by a distribution of compact and noncompact PAH ions, respectively. A plausible correlation</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19950035205&hterms=Polycyclic+aromatic+hydrocarbons&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3DPolycyclic%2Baromatic%2Bhydrocarbons','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19950035205&hterms=Polycyclic+aromatic+hydrocarbons&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3DPolycyclic%2Baromatic%2Bhydrocarbons"><span>Polycyclic aromatic hydrocarbon ions and the diffuse interstellar <span class="hlt">bands</span></span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Salama, F.; Allamandola, L. J.</p> <p>1995-01-01</p> <p>Neutral naphthalene (C10H8), phenanthrene (C14H10), and pyrene (C16H10) absorb strongly in the ultraviolet and may contribute to the extinction curve. High abundances are required to produce detectable structures. The cations of these Polycyclic Aromatic Hydrocarbons (PAHs) absorb in the visible. C10H8(+) has 12 discrete absorption <span class="hlt">bands</span> which fall between 6800 and 5000 A. The strongest <span class="hlt">band</span> at 6741 A falls close to the weak 6742 A diffuse interstellar <span class="hlt">band</span> (DIB). Five other weaker <span class="hlt">bands</span> also match DIBs. The possibility that C10H8(+) is responsible for some of the DIBs can be tested by searching for new DIBS at 6520, 6151, and 5965 A, other moderately strong naphthalene cation <span class="hlt">band</span> <span class="hlt">positions</span>. If C10H8(+) is indeed responsible for the 6742 A feature, it accounts for 0.3% of the cosmic carbon. The spectrum of C16H10(+) is dominated by a strong <span class="hlt">band</span> at 4435 A in an Ar matrix and 4395 A in a Ne matrix, a <span class="hlt">position</span> which falls very close to the strongest DIB, that at 4430 A. If C16H10(+), or a closely related pyrene-like ion is indeed responsible for the 4430 A feature, it accounts for 0.2% of the cosmic carbon. We also report an intense, very broad UV-to-visible continuum which is associated with both ions and could explain how PAHs convert interstellar UV and visible radiation into IR.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016EGUGA..1817906G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016EGUGA..1817906G"><span>Simulation of radar backscattering from snowpack at X-<span class="hlt">band</span> and Ku-<span class="hlt">band</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gay, Michel; Phan, Xuan-Vu; Ferro-Famil, Laurent</p> <p>2016-04-01</p> <p>This paper presents a multilayer snowpack electromagnetic backscattering model, based on Dense Media Radiative Transfer (DMRT). This model is capable of simulating the interaction of electromagnetic wave (EMW) at X-<span class="hlt">band</span> and Ku-<span class="hlt">band</span> frequencies with multilayer snowpack. The air-snow interface and snow-ground backscattering components are calculated using the Integral Equation Model (IEM) by [1], whereas the volume backscattering component is calculated based on the solution of Vector Radiative Transfer (VRT) equation at order 1. Case study has been carried out using measurement data from NoSREx project [2], which include SnowScat data in X-<span class="hlt">band</span> and Ku-<span class="hlt">band</span>, TerraSAR-X acquisitions and snowpack stratigraphic in-situ measurements. The results of model simulations show good agreement with the radar <span class="hlt">observations</span>, and therefore allow the DMRT model to be used in various applications, such as data assimilation [3]. [1] A.K. Fung and K.S. Chen, "An update on the iem surface backscattering model," Geoscience and Remote Sensing Letters, IEEE, vol. 1, no. 2, pp. 75 - 77, april 2004. [2] J. Lemmetyinen, A. Kontu, J. Pulliainen, A. Wiesmann, C. Werner, T. Nagler, H. Rott, and M. Heidinger, "Technical assistance for the deployment of an x- to ku-<span class="hlt">band</span> scatterometer during the nosrex ii experiment," Final Report, ESA ESTEC Contract No. 22671/09/NL/JA., 2011. [3] X. V. Phan, L. Ferro-Famil, M. Gay, Y. Durand, M. Dumont, S. Morin, S. Allain, G. D'Urso, and A. Girard, "3d-var multilayer assimilation of x-<span class="hlt">band</span> sar data into a detailed snowpack model," The Cryosphere Discussions, vol. 7, no. 5, pp. 4881-4912, 2013.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20170005484&hterms=images+MODIS&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dimages%2BMODIS','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20170005484&hterms=images+MODIS&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dimages%2BMODIS"><span><span class="hlt">Band-to-Band</span> Misregistration of the Images of MODIS Onboard Calibrators and Its Impact on Calibration</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Wang, Zhipeng; Xiong, Xiaoxiong</p> <p>2017-01-01</p> <p>The Moderate Resolution Imaging Spectroradiometer (MODIS) instruments aboard Terra and Aqua satellites are radiometrically calibrated on-orbit with a set of onboard calibrators (OBCs), including a solar diffuser, a blackbody, and a space view port through which the detectors can view the dark space. As a whisk-broom scanning spectroradiometer, thirty-six MODIS spectral <span class="hlt">bands</span> are assembled in the along-scan direction on four focal plane assemblies (FPAs). These <span class="hlt">bands</span> capture images of the same target sequentially with the motion of a scan mirror. Then the images are coregistered onboard by delaying the appropriate <span class="hlt">band</span>-dependent amount of time, depending on the <span class="hlt">band</span> locations on the FPA. While this coregistration mechanismis functioning well for the far-field remote targets such as earth view scenes or the moon, noticeable <span class="hlt">band-to-band</span> misregistration in the along-scan direction has been <span class="hlt">observed</span> for near field targets, particularly in OBCs. In this paper, the misregistration phenomenon is presented and analyzed. It is concluded that the root cause of the misregistration is that the rotating element of the instrument, the scan mirror, is displaced from the focus of the telescope primary mirror. The amount of the misregistrationis proportional to the <span class="hlt">band</span> location on the FPA and is inversely proportional to the distance between the target and the scan mirror. The impact of this misregistration on the calibration of MODIS <span class="hlt">bands</span> is discussed. In particular, the calculation of the detector gain coefficient m1of <span class="hlt">bands</span> 8-16 (412 nm 870 nm) is improved by up to 1.5% for Aqua MODIS.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27581033','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27581033"><span><span class="hlt">Observations</span> on germ <span class="hlt">band</span> development in the cellar spider Pholcus phalangioides.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Turetzek, Natascha; Prpic, Nikola-Michael</p> <p>2016-11-01</p> <p>Most recent studies of spider embryonic development have focused on representatives of the species-rich group of entelegyne spiders (over 80 % of all extant species). Embryogenesis in the smaller spider groups, however, is less well studied. Here, we describe the development of the germ <span class="hlt">band</span> in the spider species Pholcus phalangioides, a representative of the haplogyne spiders that are phylogenetically the sister group of the entelegyne spiders. We show that the transition from radially symmetric embryonic anlage to the bilaterally symmetric germ <span class="hlt">band</span> involves the accumulation of cells in the centre of the embryonic anlage (primary thickening). These cells then disperse all across the embryonic anlage. A secondary thickening of cells then appears in the centre of the embryonic anlage, and this thickening expands and forms the segment addition zone. We also confirm that the major part of the opisthosoma initially develops as a tube shaped structure, and its segments are then sequentially folded down on the yolk during inversion. This special mode of opisthosoma formation has not been reported for entelegyne spiders, but a more comprehensive sampling of this diverse group is necessary to decide whether this peculiarity is indeed lacking in the entelegyne spiders.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017PhRvP...7c4011M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017PhRvP...7c4011M"><span>Substitutional Electron and Hole Doping of WSe2 : Synthesis, Electrical Characterization, and <span class="hlt">Observation</span> of <span class="hlt">Band-to-Band</span> Tunneling</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Mukherjee, R.; Chuang, H. J.; Koehler, M. R.; Combs, N.; Patchen, A.; Zhou, Z. X.; Mandrus, D.</p> <p>2017-03-01</p> <p>Transition-metal dichalcogenides (TMDs) such as MoS2 , MoSe2 , and WSe2 have emerged as promising two-dimensional semiconductors. Many anticipated applications of these materials require both p -type and n -type TMDs with long-term doping stability. Here, we report on the synthesis of substitutionally doped WSe2 crystals using Nb and Re as p - and n -type dopants, respectively. Hall coefficient and gate-dependent transport measurements reveal drastically different doping properties between nominally 0.5% Nb- and 0.5% Re-doped WSe2 . While 0.5% Nb-doped WSe2 (WSe2∶Nb ) is degenerately hole doped with a nearly temperature-independent carrier density of approximately 1019 cm-3 , electrons in 0.5% Re-doped WSe2 (WSe2 ∶Re ) are largely trapped in localized states below the mobility edge and exhibit thermally activated behavior. Charge transport in both WSe2∶Nb and WSe2 ∶Re is found to be limited by Coulomb scattering from ionized impurities. Furthermore, we fabricate vertical van der Waals-junction diodes consisting of multilayers of WSe2∶Nb and WSe2 ∶Re . Finally, we demonstrate reverse rectifying behavior as a direct proof of <span class="hlt">band-to-band</span> tunneling in our WSe2∶Nb /WSe2∶Re diodes.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/26191917','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/26191917"><span>Enhanced optical transmission through a star-shaped bull's eye at dual resonant-<span class="hlt">bands</span> in UV and the visible spectral range.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Nazari, Tavakol; Khazaeinezhad, Reza; Jung, Woohyun; Joo, Boram; Kong, Byung-Joo; Oh, Kyunghwan</p> <p>2015-07-13</p> <p>Dual resonant <span class="hlt">bands</span> in UV and the visible range were simultaneously <span class="hlt">observed</span> in the enhanced optical transmission (EOT) through star-shaped plasmonic structures. EOTs through four types of polygonal bull's eyes with a star aperture surrounded by the concentric star grooves were analyzed and compared for 3, 4, 5, and 6 corners, using finite difference time domain (FDTD) method. In contrast to plasmonic resonances in the visible range, the UV-<span class="hlt">band</span> resonance intensity was found to scale with the number of corners, which is related with higher order multipole interactions. Spectral <span class="hlt">positions</span> and relative intensities of the dual resonances were analyzed parametrically to find optimal conditions to maximize EOT in UV-visible dual <span class="hlt">bands</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017IPNPR.211B...1M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017IPNPR.211B...1M"><span>Deep-Space Ka-<span class="hlt">Band</span> Flight Experience</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Morabito, D. D.</p> <p>2017-11-01</p> <p>Lower frequency <span class="hlt">bands</span> have become more congested in allocated bandwidth as there is increased competition between flight projects and other entities. Going to higher frequency <span class="hlt">bands</span> offers significantly more bandwidth, allowing for the use of much higher data rates. However, Ka-<span class="hlt">band</span> is more susceptible to weather effects than lower frequency <span class="hlt">bands</span> currently used for most standard downlink telemetry operations. Future or prospective flight projects considering deep-space Ka-<span class="hlt">band</span> (32-GHz) telemetry data links have expressed an interest in understanding past flight experience with received Ka-<span class="hlt">band</span> downlink performance. Especially important to these flight projects is gaining a better understanding of weather effects from the experience of current or past missions that operated Ka-<span class="hlt">band</span> radio systems. We will discuss the historical flight experience of several Ka-<span class="hlt">band</span> missions starting from Mars <span class="hlt">Observer</span> in 1993 up to present-day deep-space missions such as Kepler. The study of historical Ka-<span class="hlt">band</span> flight experience allows one to recommend margin policy for future missions. Of particular interest, we will review previously reported-on flight experience with the Cassini spacecraft Ka-<span class="hlt">band</span> radio system that has been used for radio science investigations as well as engineering studies from 2004 to 2015, when Cassini was in orbit around the planet Saturn. In this article, we will focus primarily on the Kepler spacecraft Ka-<span class="hlt">band</span> link, which has been used for operational telemetry downlink from an Earth trailing orbit where the spacecraft resides. We analyzed the received Ka-<span class="hlt">band</span> signal level data in order to characterize link performance over a wide range of weather conditions and as a function of elevation angle. Based on this analysis of Kepler and Cassini flight data, we found that a 4-dB margin with respect to adverse conditions ensures that we achieve at least a 95 percent data return.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018IJE...105..741S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018IJE...105..741S"><span>Integrated amateur <span class="hlt">band</span> and ultra-wide <span class="hlt">band</span> monopole antenna with multiple <span class="hlt">band</span>-notched</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Srivastava, Kunal; Kumar, Ashwani; Kanaujia, B. K.; Dwari, Santanu</p> <p>2018-05-01</p> <p>This paper presents the integrated amateur <span class="hlt">band</span> and ultra-wide <span class="hlt">band</span> (UWB) monopole antenna with integrated multiple <span class="hlt">band</span>-notched characteristics. It is designed for avoiding the potential interference of frequencies 3.99 GHz (3.83 GHz-4.34 GHz), 4.86 GHz (4.48 GHz-5.63 GHz), 7.20 GHz (6.10 GHz-7.55 GHz) and 8.0 GHz (7.62 GHz-8.47 GHz) with VSWR 4.9, 11.5, 6.4 and 5.3, respectively. Equivalent parallel resonant circuits have been presented for each <span class="hlt">band</span>-notched frequencies of the antenna. Antenna operates in amateur <span class="hlt">band</span> 1.2 GHz (1.05 GHz-1.3 GHz) and UWB <span class="hlt">band</span> from 3.2 GHz-13.9 GHz. Different substrates are used to verify the working of the proposed antenna. Integrated GSM <span class="hlt">band</span> from 0.6 GHz to 1.8 GHz can also be achieved by changing the radius of the radiating patch. Antenna gain varied from 1.4 dBi to 9.8 dBi. Measured results are presented to validate the antenna performances.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/6326644-study-model-hole-superconductivity-multiple-band-cases-its-application-transition-metals','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/6326644-study-model-hole-superconductivity-multiple-band-cases-its-application-transition-metals"><span>Study of the model of hole superconductivity in multiple <span class="hlt">band</span> cases and its application to transition metals</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Hong, X.Q.</p> <p>1992-01-01</p> <p>The authors have studied a simple model consisting of a chain of atoms with two atoms per unit cell. This model develops two <span class="hlt">bands</span> when the inter-cell and intra-cell hopping amplitudes are different. They have found that superconductivity predominantly occurs when the Fermi level is close to the top of the upper <span class="hlt">band</span> where the wavefunction has antibonding feature both inside the unit cell and between unit cells. Superconductivity occurs only in a restricted parameter range when the Fermi level is close to the top of the lower <span class="hlt">band</span> because of the repulsive interaction within the unit cell. They findmore » that pair expectation values that 'mix' carriers of both <span class="hlt">bands</span> can exist when interband interactions other than V12 of Suhl et al are present. But the magnitude of the 'mixed pairs' order parameters is much smaller than that of the intra-<span class="hlt">band</span> pairs. The V12 of Suhl et al is the most important interband interaction that gives rise to the main features of a two-<span class="hlt">band</span> model: a single transition temperature and two different gaps. They have used the model of hole superconductivity to study the variation of T(sub c) among transition metal series--the Matthias rules. They have found that the <span class="hlt">observed</span> T(sub c)'s are consistent with superconductivity of a metal with multiple <span class="hlt">bands</span> at the Fermi level being caused by the single <span class="hlt">band</span> with strongest antibonding character at the Fermi level. When the Fermi level is the lower part of a <span class="hlt">band</span>, there is no T(sub c). As the <span class="hlt">band</span> is gradually filled, T(sub c) rises, passes through a maximum, then drops to zero when the <span class="hlt">band</span> is full. This characteristic feature is independent of any fine structure of the <span class="hlt">band</span>. The <span class="hlt">position</span> of the peak and the width of the peak are correlated. Quantitative agreement with the experimental results is obtained by choosing parameters of onsite Coulomb interaction U, modulated hopping term Delta-t, and nearest neighbor repulsion V to fit the magnitude of T(sub c) and the <span class="hlt">positions</span> of experimental peaks.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20020022486&hterms=selenium&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D80%26Ntt%3Dselenium','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20020022486&hterms=selenium&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D80%26Ntt%3Dselenium"><span><span class="hlt">Band</span> Anticrossing in Highly Mismatched Compound Semiconductor Alloys</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Yu, Kin Man; Wu, J.; Walukiewicz, W.; Ager, J. W.; Haller, E. E.; Miotkowski, I.; Su, Ching-Hua; Curreri, Peter A. (Technical Monitor)</p> <p>2001-01-01</p> <p>Compound semiconductor alloys in which metallic anions are partially replaced with more electronegative isoelectronic atoms have recently attracted significant attention. Group IIIN(sub x)V(sub 1-x) alloys with a small amount of the electronegative N substituting more metallic column V elements has been the most extensively studied class of such Highly Mismatched Alloys (HMAs). We have shown that many of the unusual properties of the IIIN(sub x)V(sub 1-x) alloys can be well explained by the <span class="hlt">Band</span> Anticrossing (BAC) model that describes the electronic structure in terms of an interaction between highly localized levels of substitutional N and the extended states of the host semiconductor matrix. Most recently the BAC model has been also used to explain similar modifications of the electronic <span class="hlt">band</span> structure <span class="hlt">observed</span> in Te-rich ZnS(sub x)Te(sub 1-x) and ZnSe(sub y)Te(sub 1-y) alloys. To date studies of HMAs have been limited to materials with relatively small concentrations of highly electronegative atoms. Here we report investigations of the electronic structure of ZnSe(sub y)Te(sub 1-y) alloys in the entire composition range, y between 0 and 1. The samples used in this study are bulk ZnSe(sub y)Te(sub 1-y) crystals grown by either a modified Bridgman method or by physical vapor transport. Photomodulated reflection (PR) spectroscopy was used to measure the composition dependence of optical transitions from the valence <span class="hlt">band</span> edge and from the spin-orbit split off <span class="hlt">band</span> to the conduction <span class="hlt">band</span>. The pressure dependence of the <span class="hlt">band</span> gap was measured using optical absorption in a diamond anvil cell. We find that the energy of the spin-orbit split off valence <span class="hlt">band</span> edge does not depend on composition and is located at about 3 eV below the conduction <span class="hlt">band</span> edge of ZnSe. On the Te-rich side the pressure and the composition dependence of the optical transitions are well explained by the BAC model which describes the downward shift of the conduction <span class="hlt">band</span> edge in terms of the</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012JPhCS.377a2092G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012JPhCS.377a2092G"><span>Pressure effects on <span class="hlt">band</span> structures in dense lithium</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Goto, Naoyuki; Nagara, Hitose</p> <p>2012-07-01</p> <p>We studied the change of the <span class="hlt">band</span> structures in some structures of Li predicted at high pressures, using GGA and GW calculations. The width of the 1s <span class="hlt">band</span> coming from the 1s electron of Li shows broadening by the pressurization, which is the normal behavior of <span class="hlt">bands</span> at high pressure. The width of the <span class="hlt">band</span> just below the Fermi level decreases by the pressurization, which is an opposite behavior to the normal <span class="hlt">bands</span>. The character of this narrowing <span class="hlt">band</span> is mostly p-like with a little s-like portion. The <span class="hlt">band</span> gaps in some structures are really <span class="hlt">observed</span> even by the GGA calculations. The gaps by the GW calculations increase to about 1.5 times the GGA values. Generally the one-shot GW calculation (diagonal only calculations) gives more reliable values than the GGA, but it may fail to predict <span class="hlt">band</span> gaps for the case where <span class="hlt">band</span> dispersion shows complex crossing near the Fermi level. There remains some structures for which GW calculations with off-diagonal elements taken into account are needed to identify the phase to be metallic or semiconducting.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24340411','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24340411"><span>Decreasing patient identification <span class="hlt">band</span> errors by standardizing processes.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Walley, Susan Chu; Berger, Stephanie; Harris, Yolanda; Gallizzi, Gina; Hayes, Leslie</p> <p>2013-04-01</p> <p>Patient identification (ID) <span class="hlt">bands</span> are an essential component in patient ID. Quality improvement methodology has been applied as a model to reduce ID <span class="hlt">band</span> errors although previous studies have not addressed standardization of ID <span class="hlt">bands</span>. Our specific aim was to decrease ID <span class="hlt">band</span> errors by 50% in a 12-month period. The Six Sigma DMAIC (define, measure, analyze, improve, and control) quality improvement model was the framework for this study. ID <span class="hlt">bands</span> at a tertiary care pediatric hospital were audited from January 2011 to January 2012 with continued audits to June 2012 to confirm the new process was in control. After analysis, the major improvement strategy implemented was standardization of styles of ID <span class="hlt">bands</span> and labels. Additional interventions included educational initiatives regarding the new ID <span class="hlt">band</span> processes and disseminating institutional and nursing unit data. A total of 4556 ID <span class="hlt">bands</span> were audited with a preimprovement ID <span class="hlt">band</span> error average rate of 9.2%. Significant variation in the ID <span class="hlt">band</span> process was <span class="hlt">observed</span>, including styles of ID <span class="hlt">bands</span>. Interventions were focused on standardization of the ID <span class="hlt">band</span> and labels. The ID <span class="hlt">band</span> error rate improved to 5.2% in 9 months (95% confidence interval: 2.5-5.5; P < .001) and was maintained for 8 months. Standardization of ID <span class="hlt">bands</span> and labels in conjunction with other interventions resulted in a statistical decrease in ID <span class="hlt">band</span> error rates. This decrease in ID <span class="hlt">band</span> error rates was maintained over the subsequent 8 months.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2008JaJAP..47.3537S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2008JaJAP..47.3537S"><span>Noncontact Temperature Measurements of Organic Layers in an Organic Light-Emitting Diode Using Wavenumber-Temperature Relations of Raman <span class="hlt">Bands</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sugiyama, Takuro; Furukawa, Yukio</p> <p>2008-05-01</p> <p>We have measured the temperatures of the organic layers in operating organic light-emitting diodes (OLEDs) by Raman spectroscopy. The wavenumbers of the Raman <span class="hlt">bands</span> due to N,N'-di-naphthaleyl-N,N'-diphenyl-1,1'-biphenyl-4,4'-diamine (NPD) and copper phthalocyanine (CuPc) have been measured as a function of temperature in the range of 25-191 °C. The <span class="hlt">observed</span> <span class="hlt">positions</span> of strong <span class="hlt">bands</span> around 1607 cm-1 (NPD) and 1531 cm-1 (CuPc) shifted downward linearly with increasing temperature in the ranges lower than 92 and 191 °C, respectively. We have determined the temperatures of the NPD and CuPc layers in an operating OLED from the wavenumber-temperature relations of these <span class="hlt">bands</span>.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li class="active"><span>15</span></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_15 --> <div id="page_16" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li class="active"><span>16</span></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="301"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19790011018','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19790011018"><span>Shuttle Ku-<span class="hlt">band</span> and S-<span class="hlt">band</span> communications implementations study</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Huth, G. K.; Nessibou, T.; Nilsen, P. W.; Simon, M. K.; Weber, C. L.</p> <p>1979-01-01</p> <p>The interfaces between the Ku-<span class="hlt">band</span> system and the TDRSS, between the S-<span class="hlt">band</span> system and the TDRSS, GSTDN and SGLS networks, and between the S-<span class="hlt">band</span> payload communication equipment and the other Orbiter avionic equipment were investigated. The principal activities reported are: (1) performance analysis of the payload narrowband bent-pipe through the Ku-<span class="hlt">band</span> communication system; (2) performance evaluation of the TDRSS user constraints placed on the S-<span class="hlt">band</span> and Ku-<span class="hlt">band</span> communication systems; (3) assessment of the shuttle-unique S-<span class="hlt">band</span> TDRSS ground station false lock susceptibility; (4) development of procedure to make S-<span class="hlt">band</span> antenna measurements during orbital flight; (5) development of procedure to make RFI measurements during orbital flight to assess the performance degradation to the TDRSS S-<span class="hlt">band</span> communication link; and (6) analysis of the payload interface integration problem areas.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19950029676&hterms=ito&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3Dito','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19950029676&hterms=ito&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3Dito"><span>High-resolution oscillator strength measurements for the A(v') - X(0) <span class="hlt">bands</span> of carbon monoxide with 11 less than or equal to v' less than or equal to 14</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Smith, Peter L.; Stark, G.; Yoshino, K.; Ito, K.</p> <p>1994-01-01</p> <p><span class="hlt">Band</span> oscillator strengths (f-values) for four <span class="hlt">bands</span> of the Fourth <span class="hlt">Positive</span> system (A (1)Pi - Chi(sup 1) Sigma(+)) of CO have been determined from high-resolution (lambda/Delta lambda approximately equal to 150,000) absorption spectra. The <span class="hlt">bands</span>, (14, 0) through (11, 0), are at wavelengths between 121 and 127 nm. Our f-values for the (11, 0) and (12, 0) <span class="hlt">bands</span> support those of Chan, Cooper, & Brion (1993), which have been shown to be consistent with <span class="hlt">observations</span> of CO in the clouds in the line of sight to zeta Oph. Our f-values for the (13, 0) and (14, 0) <span class="hlt">bands</span> are the first directly measured values for these <span class="hlt">bands</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017SPIE10566E..2NK','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017SPIE10566E..2NK"><span>Narrow-<span class="hlt">band</span> filters for ocean colour imager</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Krol, Hélène; Chazallet, Frédéric; Archer, Julien; Kirchgessner, Laurent; Torricini, Didier; Grèzes-Besset, Catherine</p> <p>2017-11-01</p> <p>During the last few years, the evolution of deposition technologies of optical thin films coatings and associated in-situ monitoring methods enables us today to successfully answer the increasingly request of space systems for Earth <span class="hlt">observation</span>. Geostationary satellite COMS-1 (Communication, Ocean, Meteorological Satellite-1) of Astrium has the role of ensuring meteorological <span class="hlt">observation</span> as well as monitoring of the oceans. It is equipped with a colour imager to <span class="hlt">observe</span> the marine ecosystem through 8 <span class="hlt">bands</span> in the visible spectrum with a ground resolution of 500m. For that, this very high technology instrument is constituted with a filters wheel in front of the oceanic colour imager with 8 narrow <span class="hlt">band</span> filters carried out and qualified by Cilas.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018PhLA..382..679L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018PhLA..382..679L"><span>Designing broad phononic <span class="hlt">band</span> gaps for in-plane modes</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Li, Yang Fan; Meng, Fei; Li, Shuo; Jia, Baohua; Zhou, Shiwei; Huang, Xiaodong</p> <p>2018-03-01</p> <p>Phononic crystals are known as artificial materials that can manipulate the propagation of elastic waves, and one essential feature of phononic crystals is the existence of forbidden frequency range of traveling waves called <span class="hlt">band</span> gaps. In this paper, we have proposed an easy way to design phononic crystals with large in-plane <span class="hlt">band</span> gaps. We demonstrated that the gap between two arbitrarily appointed <span class="hlt">bands</span> of in-plane mode can be formed by employing a certain number of solid or hollow circular rods embedded in a matrix material. Topology optimization has been applied to find the best material distributions within the primitive unit cell with maximal <span class="hlt">band</span> gap width. Our results reveal that the centroids of optimized rods coincide with the point <span class="hlt">positions</span> generated by Lloyd's algorithm, which deepens our understandings on the formation mechanism of phononic in-plane <span class="hlt">band</span> gaps.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1996APS..DNP..CB01F','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1996APS..DNP..CB01F"><span>Identical <span class="hlt">Bands</span>: Does ``Seeing Double'' Mean We Learn Twice as Much?</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Fallon, Paul</p> <p>1996-10-01</p> <p>The phenomenon of `identical <span class="hlt">bands</span>' has been under discussion for several years, however the origin of this surprising <span class="hlt">observation</span>, whereby rotational cascades in different nuclei exhibit very similar transition energies (and/or moments of inertia), remains uncertain. The first cases of identical superdeformed <span class="hlt">bands</span> were <span class="hlt">observed</span> when only a small number of superdeformed <span class="hlt">bands</span> were known. Since then many more examples of superdeformation have been found and it is important to see if the number of `identical' <span class="hlt">bands</span> has risen in proportion. In addition the `identical' <span class="hlt">band</span> discussion has been extended to normal deformed nuclei. In this talk I will briefly review the topic of identical <span class="hlt">bands</span> and attempt to address the progress made and add some personal views on what remains to be done. Work supported in part by the U.S. DOE under contract number DE-AC03-76SF0098.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2011ACPD...1130949D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2011ACPD...1130949D"><span>Lidar and radar measurements of the melting layer in the frame of the Convective and Orographically-induced Precipitation Study: <span class="hlt">observations</span> of dark and bright <span class="hlt">band</span> phenomena</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>di Girolamo, P.; Summa, D.; Bhawar, R.; di Iorio, T.; Norton, E. G.; Peters, G.; Dufournet, Y.</p> <p>2011-11-01</p> <p>During the Convective and Orographically-induced Precipitation Study (COPS), lidar dark and bright <span class="hlt">bands</span> were <span class="hlt">observed</span> by the University of BASILicata Raman lidar system (BASIL) during several intensive (IOPs) and special (SOPs) <span class="hlt">observation</span> periods (among others, 23 July, 15 August, and 17 August 2007). Lidar data were supported by measurements from the University of Hamburg cloud radar MIRA 36 (36 GHz), the University of Hamburg dual-polarization micro rain radars (24.1 GHz) and the University of Manchester UHF wind profiler (1.29 GHz). Results from BASIL and the radars for 23 July 2007 are illustrated and discussed to support the comprehension of the microphysical and scattering processes responsible for the appearance of the lidar and radar dark and bright <span class="hlt">bands</span>. Simulations of the lidar dark and bright <span class="hlt">band</span> based on the application of concentric/eccentric sphere Lorentz-Mie codes and a melting layer model are also provided. Lidar and radar measurements and model results are also compared with measurements from a disdrometer on ground and a two-dimensional cloud (2DC) probe on-board the ATR42 SAFIRE.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20080039446','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20080039446"><span>High-Resolution N-<span class="hlt">Band</span> <span class="hlt">Observations</span> of the Nova RS Ophiuchi with the Keck Interferometer Nuller</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Barry, R. K.; Danchi, W. C.; Sokoloski, J. L.; Koresko, C.; Wisniewski, J. P.; Serabyn, E.; Traub, W.; Kuchner, M.; Greenhouse, M. A.</p> <p>2007-01-01</p> <p>We report new <span class="hlt">observations</span> of the nova RS Ophiuchi (RS Oph) using the Keck Interferometer Nulling Instrument, approximately 3.8 days following the most recent outburst that occurred on 2006 February 12. The Keck Interferometer Nuller (KIN) operates in K-<span class="hlt">band</span> from 8 to 12.5 pm in a nulling mode, which means that the central broad-<span class="hlt">band</span> interference fringe is a dark fringe - with an angular width of 25 mas at mid <span class="hlt">band</span> - rather than the bright fringe used ill a conventional optical interferometer. In this mode the stellar light itself is suppressed by the destructive fringe, effectively enhancing the contrast of the circumstellar material located near the star. By subsequently shifting the neighboring bright fringe onto the center of the source brightness distribution and integrating, a second spatial regime dominated by light from the central portion of the source is almost simultaneously sampled. The nulling technique is the sparse aperture equivalent of the conventional corongraphic technique used in filled aperture telescopes. By fitting the unique KIK inner and outer spatial regime data, we have obtained an angular size of the mid-infrared continuum of 6.2, 4.0. or 5.4 mas for a disk profile, gaussian profile (fwhm), and shell profile respectively. The data show evidence of enhanced neutral atomic hydrogen emission located in the inner spatial regime relative to the outer regime. There is also evidence of a 9.7 micron silicate feature seen outside of this region. Importantly, we see spectral lines excited by the nova flash in the outer region before the blast wave reaches these regions. These lines are from neutral, weakly excited atoms which support the following interpretation. We discuss the present results in terms of a unifying model of the system that includes an increase in density in the plane of the orbit of the two stars created by a spiral shock wave caused by the motion of the stars through the cool wind of the red giant star. These data show the power</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19990046421','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19990046421"><span>Granularity of the Diffuse Background <span class="hlt">Observed</span></span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Gruber, D. E.; MacDonald, D.; Rothschild, R. E.; Boldt, E.; Mushotzky, R. F.; Fabian, A. C.</p> <p>1995-01-01</p> <p>First results are reported from a program for measuring the field-to-field fluctuation level of the cosmic diffuse background by using differences between the two background <span class="hlt">positions</span> of each deep exposure with the High Energy X-ray Timing Experiment (HEXTE) instrument on the Remote X Ray Timing Explorer (RXTE). With 8 million live seconds accumulated to date a fluctuation level on the 15-25 keV <span class="hlt">band</span> is <span class="hlt">observed</span> which is consistent with extrapolations from the High Energy Astrophysical Observatory-1 (HEAO-1) measurements. <span class="hlt">Positive</span> results are expected eventually at higher energies. Models of (active galactic nuclei) AGN origin will eventually be constrained by this program.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/865752','DOE-PATENT-XML'); return false;" href="https://www.osti.gov/servlets/purl/865752"><span>Broad-<span class="hlt">band</span> beam buncher</span></a></p> <p><a target="_blank" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p>Goldberg, David A.; Flood, William S.; Arthur, Allan A.; Voelker, Ferdinand</p> <p>1986-01-01</p> <p>A broad-<span class="hlt">band</span> beam buncher is disclosed, comprising an evacuated housing, an electron gun therein for producing an electron beam, a buncher cavity having entrance and exit openings through which the beam is directed, grids across such openings, a source providing a <span class="hlt">positive</span> DC voltage between the cavity and the electron gun, a drift tube through which the electron beam travels in passing through such cavity, grids across the ends of such drift tube, gaps being provided between the drift tube grids and the entrance and exit grids, a modulator for supplying an ultrahigh frequency modulating signal to the drift tube for producing velocity modulation of the electrons in the beam, a drift space in the housing through which the velocity modulated electron beam travels and in which the beam is bunched, and a discharge opening from such drift tube and having a grid across such opening through which the bunched electron beam is discharged into an accelerator or the like. The buncher cavity and the drift tube may be arranged to constitute an extension of a coaxial transmission line which is employed to deliver the modulating signal from a signal source. The extended transmission line may be terminated in its characteristic impedance to afford a broad-<span class="hlt">band</span> response and the device as a whole designed to effect broad-<span class="hlt">band</span> beam coupling, so as to minimize variations of the output across the response <span class="hlt">band</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016MNRAS.460.2706K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016MNRAS.460.2706K"><span><span class="hlt">Observational</span> analysis of the well-correlated diffuse <span class="hlt">bands</span>: 6196 and 6614 Å</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Krełowski, J.; Galazutdinov, G. A.; Bondar, A.; Beletsky, Y.</p> <p>2016-08-01</p> <p>We confirm, using spectra from seven observatories, that the diffuse <span class="hlt">bands</span> 6196 and 6614 are very tightly correlated. However, their strength ratio is not constant as well as profile shapes. Apparently, the two interstellar features do not react in unison to the varying physical conditions of different interstellar clouds.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19820011462','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19820011462"><span>A High Resolution Spectroscopic Study of the Nu2 <span class="hlt">Band</span> of Hydrogen Sulfide and the 1-0 <span class="hlt">Band</span> of Hydrogen Iodide. Ph.D. Thesis - Maryland Univ.</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Strow, L. L.</p> <p>1981-01-01</p> <p>A tunable diode laser spectrometer was constructed and used to study: (1) the effects of centrifugal distortion on the transition frequencies and strengths of the nu sub 2 <span class="hlt">band</span> of H2S, and (2) nuclear quadrupole hyperfine structure in the 1-0 <span class="hlt">band</span> of HI. A total of 126 line frequencies and 94 line strengths in the nu sub 2 <span class="hlt">band</span> of H2S were measured. The average accuracy of the line frequency measurements was + or - 0.0016 cm. The line strengths were measured to an average accuracy of about 3 percent. The effect of the finite spectral width of the diode laser on the measurement of line strengths is discussed. The <span class="hlt">observed</span> H2S line frequencies were fit to Watson's AS and NS reduced Hamiltonian in both the Ir and IIIr coordinate representations in order to determine the best set of rotation distortion constants for the upper state of the nu sub 2 <span class="hlt">band</span>. Comparisons of the <span class="hlt">observed</span> line strengths in this <span class="hlt">band</span> to rigid rotor line strengths are also presented. Nuclear quadrupole hyperfine structure in the low J lines of the 1-0 <span class="hlt">band</span> of HI was <span class="hlt">observed</span>. The upper vibrational state nuclear quadrupole coupling constant, determined from the <span class="hlt">observed</span> splittings, was -1850 MHz + or - 12 MHz or 1.2 percent + or - 0.7 percent larger than the ground state coupling constant.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017JGeod..91..613J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017JGeod..91..613J"><span><span class="hlt">Positive</span> and negative ionospheric responses to the March 2015 geomagnetic storm from BDS <span class="hlt">observations</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jin, Shuanggen; Jin, Rui; Kutoglu, H.</p> <p>2017-06-01</p> <p>The most intense geomagnetic storm in solar cycle 24 occurred on March 17, 2015, and the detailed ionospheric storm morphologies are difficultly obtained from traditional <span class="hlt">observations</span>. In this paper, the Geostationary Earth Orbit (GEO) <span class="hlt">observations</span> of BeiDou Navigation Satellite System (BDS) are for the first time used to investigate the ionospheric responses to the geomagnetic storm. Using BDS GEO and GIMs TEC series, negative and <span class="hlt">positive</span> responses to the March 2015 storm are found at local and global scales. During the main phase, <span class="hlt">positive</span> ionospheric storm is the main response to the geomagnetic storm, while in the recovery phase, negative phases are pronounced at all latitudes. Maximum amplitudes of negative and <span class="hlt">positive</span> phases appear in the afternoon and post-dusk sectors during both main and recovery phases. Furthermore, dual-peak <span class="hlt">positive</span> phases in main phase and repeated negative phase during the recovery are found from BDS GEO <span class="hlt">observations</span>. The geomagnetic latitudes corresponding to the maximum disturbances during the main and recovery phases show large differences, but they are quasi-symmetrical between southern and northern hemispheres. No clear zonal propagation of traveling ionospheric disturbances is detected in the GNSS TEC disturbances at high and low latitudes. The thermospheric composition variations could be the dominant source of the <span class="hlt">observed</span> ionospheric storm effect from GUVI [O]/[N2] ratio data as well as storm-time electric fields. Our study demonstrates that the BDS (especially the GEO) <span class="hlt">observations</span> are an important data source to <span class="hlt">observe</span> ionospheric responses to the geomagnetic storm.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28134779','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28134779"><span>Geometric <span class="hlt">Positioning</span> for Satellite Imagery without Ground Control Points by Exploiting Repeated <span class="hlt">Observation</span>.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Ma, Zhenling; Wu, Xiaoliang; Yan, Li; Xu, Zhenliang</p> <p>2017-01-26</p> <p>With the development of space technology and the performance of remote sensors, high-resolution satellites are continuously launched by countries around the world. Due to high efficiency, large coverage and not being limited by the spatial regulation, satellite imagery becomes one of the important means to acquire geospatial information. This paper explores geometric processing using satellite imagery without ground control points (GCPs). The outcome of spatial triangulation is introduced for geo-<span class="hlt">positioning</span> as repeated <span class="hlt">observation</span>. Results from combining block adjustment with non-oriented new images indicate the feasibility of geometric <span class="hlt">positioning</span> with the repeated <span class="hlt">observation</span>. GCPs are a must when high accuracy is demanded in conventional block adjustment; the accuracy of direct georeferencing with repeated <span class="hlt">observation</span> without GCPs is superior to conventional forward intersection and even approximate to conventional block adjustment with GCPs. The conclusion is drawn that taking the existing oriented imagery as repeated <span class="hlt">observation</span> enhances the effective utilization of previous spatial triangulation achievement, which makes the breakthrough for repeated <span class="hlt">observation</span> to improve accuracy by increasing the base-height ratio and redundant <span class="hlt">observation</span>. Georeferencing tests using data from multiple sensors and platforms with the repeated <span class="hlt">observation</span> will be carried out in the follow-up research.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013evga.conf..217A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013evga.conf..217A"><span>VLBI <span class="hlt">Observations</span> of Geostationary Satellites</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Artz, T.; Nothnagel, A.; La Porta, L.</p> <p>2013-08-01</p> <p>For a consistent realization of a Global Geodetic <span class="hlt">Observing</span> System (GGOS), a proper tie between the individual global reference systems used in the analysis of space-geodetic <span class="hlt">observations</span> is a prerequisite. For instance, the link between the terrestrial, the celestial and the dynamic reference system of artificial Earth orbiters may be realized by Very Long O Baseline Interferometry (VLBI) <span class="hlt">observations</span> of one or several satellites. In the preparation phase for a dedicated satellite mission, one option to realize this is using a geostationary (GEO) satellite emitting a radio signal in X-<span class="hlt">Band</span> and/or S-<span class="hlt">Band</span> and, thus, imitating a quasar. In this way, the GEO satellite can be <span class="hlt">observed</span> by VLBI together with nearby quasars and the GEO orbit can, thus, be determined in a celestial reference frame. If the GEO satellite is, e.g., also equipped with a GNSS-type transmitter, a further tie between GNSS and VLBI may be realized. In this paper, a concept for the generation of a radio signal is shown. Furthermore, simulation studies for estimating the GEO <span class="hlt">position</span> are presented with a GEO satellite included in the VLBI schedule. VLBI group delay <span class="hlt">observations</span> are then simulated for the quasars as well as for the GEO satellite. The analysis of the simulated <span class="hlt">observations</span> shows that constant orbit changes are adequately absorbed by estimated orbit parameters. Furthermore, the post-fit residuals are comparable to those from real VLBI sessions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24832981','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24832981"><span>Effects of replacing free weights with elastic <span class="hlt">band</span> resistance in squats on trunk muscle activation.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Saeterbakken, Atle H; Andersen, Vidar; Kolnes, Maria K; Fimland, Marius S</p> <p>2014-11-01</p> <p>The purpose of this study was to assess the effects of adding elastic <span class="hlt">bands</span> to free-weight squats on the neuromuscular activation of core muscles. Twenty-five resistance trained women with 4.6 ± 2.1 years of resistance training experience participated in the study. In randomized order, the participants performed 6 repetition maximum in free-weight squats, with and without elastic <span class="hlt">bands</span> (i.e., matched relative intensity between exercises). During free-weight squats with elastic <span class="hlt">bands</span>, some of the free weights were replaced with 2 elastic <span class="hlt">bands</span> attached to the lowest part of the squat rack. Surface electromyography (EMG) activity was measured from the erector spinae, external oblique, and rectus abdominis, whereas a linear encoder measured the vertical displacement. The EMG activities were compared between the 2 lifting modalities for the whole repetition and separately for the eccentric, concentric, and upper and lower eccentric and concentric phases. In the upper (greatest stretch of the elastic <span class="hlt">band</span>), middle, and lower <span class="hlt">positions</span> in squats with elastic <span class="hlt">bands</span>, the resistance values were approximately 117, 105, and 93% of the free weight-only trial. Similar EMG activities were <span class="hlt">observed</span> for the 2 lifting modalities for the erector spinae (p = 0.112-0.782), external oblique (p = 0.225-0.977), and rectus abdominis (p = 0.315-0.729) in all analyzed phases. In conclusion, there were no effects on the muscle activity of trunk muscles of substituting some resistance from free weights with elastic <span class="hlt">bands</span> in the free-weight squat.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19840018452','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19840018452"><span>Catalog of infrared <span class="hlt">observations</span> including: Bibliography of infrared astronomy and index of infrared source <span class="hlt">positions</span></span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Gezari, D. Y.; Schmitz, M.; Mead, J. M.</p> <p>1984-01-01</p> <p>The Catalog of Infrared <span class="hlt">Observations</span> and its Far Infrared Supplement summarize all infrared astronomical <span class="hlt">observations</span> at infrared wavelengths published in the scientific literature between 1965 and 1982. The Catalog includes as appendices the Bibliography of infrared astronomy which keys <span class="hlt">observations</span> in the Catalog with the original journal references, and the index of infrared source <span class="hlt">positions</span> which gives source <span class="hlt">positions</span> for alphabetically listed sources in the Catalog. The Catalog data base contains over 85,000 <span class="hlt">observations</span> of about 10,000 infrared sources, of which about 2,000 have no known visible counterpart.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4276241','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4276241"><span>Emergency treatment of esophageal varix incarceration in the endoscope and ligation device during endoscopic variceal rubber <span class="hlt">band</span> ligation</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Zhao, Hong; Cheng, Jilin; Xu, Yahong; Lu, Cuili; Huang, Shaoping; Fan, Zhenyu; Shi, Yuxin</p> <p>2014-01-01</p> <p>Sclerotherapy and endoscopic esophageal variceal ligation (EVL) are commonly used to treat and prevent variceal bleeding. As of today, there has been no report on an unexpected incarceration of a varix hooked on with the <span class="hlt">bands</span> from the endoscopic EVL device. We recently experienced this emergency while using the 7-<span class="hlt">band</span> ring endoscopic EVL device (Boston Scientific Corp., Boston, MA) for prophylaxis of variceal bleeding. In this case, the varix body itself was accidently incarcerated in the crevice of the esophageal endoscope after highly negative pressure of absorption was applied on the endoscope. In this situation, using force to take out the gastroscope was not an option as it would tear the vein and cause massive hemorrhage. We were managed to ligate the varix with rubber <span class="hlt">bands</span> while releasing the incarceration. We <span class="hlt">observed</span> that ligation of the varix at the same <span class="hlt">position</span> using all seven ligation <span class="hlt">bands</span> resulted in disappearance of the targeted varix. The surrounding esophageal mucosa became smooth after the treatment. PMID:25550983</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017IJC....90..813B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017IJC....90..813B"><span>A robust nonlinear <span class="hlt">position</span> <span class="hlt">observer</span> for synchronous motors with relaxed excitation conditions</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Bobtsov, Alexey; Bazylev, Dmitry; Pyrkin, Anton; Aranovskiy, Stanislav; Ortega, Romeo</p> <p>2017-04-01</p> <p>A robust, nonlinear and globally convergent rotor <span class="hlt">position</span> <span class="hlt">observer</span> for surface-mounted permanent magnet synchronous motors was recently proposed by the authors. The key feature of this <span class="hlt">observer</span> is that it requires only the knowledge of the motor's resistance and inductance. Using some particular properties of the mathematical model it is shown that the problem of state <span class="hlt">observation</span> can be translated into one of estimation of two constant parameters, which is carried out with a standard gradient algorithm. In this work, we propose to replace this estimator with a new one called dynamic regressor extension and mixing, which has the following advantages with respect to gradient estimators: (1) the stringent persistence of excitation (PE) condition of the regressor is not necessary to ensure parameter convergence; (2) the latter is guaranteed requiring instead a non-square-integrability condition that has a clear physical meaning in terms of signal energy; (3) if the regressor is PE, the new <span class="hlt">observer</span> (like the old one) ensures convergence is exponential, entailing some robustness properties to the <span class="hlt">observer</span>; (4) the new estimator includes an additional filter that constitutes an additional degree of freedom to satisfy the non-square integrability condition. Realistic simulation results show significant performance improvement of the <span class="hlt">position</span> <span class="hlt">observer</span> using the new parameter estimator, with a less oscillatory behaviour and a faster convergence speed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/1408425','SCIGOV-STC'); return false;" href="https://www.osti.gov/servlets/purl/1408425"><span>Multicolor emission from intermediate <span class="hlt">band</span> semiconductor ZnO 1-xSe x</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Welna, M.; Baranowski, M.; Linhart, W. M.</p> <p></p> <p>Photoluminescence and photomodulated reflectivity measurements of ZnOSe alloys are used to demonstrate a splitting of the valence <span class="hlt">band</span> due to the <span class="hlt">band</span> anticrossing interaction between localized Se states and the extended valence <span class="hlt">band</span> states of the host ZnO matrix. A strong multiband emission associated with optical transitions from the conduction <span class="hlt">band</span> to lower E - and upper E + valence subbands has been <span class="hlt">observed</span> at room temperature. The composition dependence of the optical transition energies is well explained by the electronic <span class="hlt">band</span> structure calculated using the kp method combined with the <span class="hlt">band</span> anticrossing model. The <span class="hlt">observation</span> of the multiband emissionmore » is possible because of relatively long recombination lifetimes. Longer than 1 ns lifetimes for holes photoexcited to the lower valence subband offer a potential of using the alloy as an intermediate <span class="hlt">band</span> semiconductor for solar power conversion applications.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1408425-multicolor-emission-from-intermediate-band-semiconductor-zno1-xsex','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1408425-multicolor-emission-from-intermediate-band-semiconductor-zno1-xsex"><span>Multicolor emission from intermediate <span class="hlt">band</span> semiconductor ZnO 1-xSe x</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Welna, M.; Baranowski, M.; Linhart, W. M.; ...</p> <p>2017-03-13</p> <p>Photoluminescence and photomodulated reflectivity measurements of ZnOSe alloys are used to demonstrate a splitting of the valence <span class="hlt">band</span> due to the <span class="hlt">band</span> anticrossing interaction between localized Se states and the extended valence <span class="hlt">band</span> states of the host ZnO matrix. A strong multiband emission associated with optical transitions from the conduction <span class="hlt">band</span> to lower E - and upper E + valence subbands has been <span class="hlt">observed</span> at room temperature. The composition dependence of the optical transition energies is well explained by the electronic <span class="hlt">band</span> structure calculated using the kp method combined with the <span class="hlt">band</span> anticrossing model. The <span class="hlt">observation</span> of the multiband emissionmore » is possible because of relatively long recombination lifetimes. Longer than 1 ns lifetimes for holes photoexcited to the lower valence subband offer a potential of using the alloy as an intermediate <span class="hlt">band</span> semiconductor for solar power conversion applications.« less</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li class="active"><span>16</span></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_16 --> <div id="page_17" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li class="active"><span>17</span></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="321"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013JKPS...62.1587L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013JKPS...62.1587L"><span>Hyper-spectral imager of the visible <span class="hlt">band</span> for lunar <span class="hlt">observations</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Lim, Y.-M.; Choi, Y.-J.; Jo, Y.-S.; Lim, T.-H.; Ham, J.; Min, K. W.; Choi, Y.-W.</p> <p>2013-06-01</p> <p>A prototype hyper-spectral imager in the visible spectral <span class="hlt">band</span> was developed for the planned Korean lunar missions in the 2020s. The instrument is based on simple refractive optics that adopted a linear variable filter and an interline charge-coupled device. This prototype imager is capable of mapping the lunar surface at wavelengths ranging from 450 to 900 nm with a spectral resolution of ˜8 nm and selectable channels ranging from 5 to 252. The anticipated spatial resolution is 17.2 m from an altitude of 100 km with a swath width of 21 km</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20170003053','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20170003053"><span><span class="hlt">Band-to-Band</span> Misregistration of the Images of MODIS On-Board Calibrators and Its Impact to Calibration</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Wang, Zhipeng; Xiong, Xiaoxiong</p> <p>2017-01-01</p> <p>The MODIS instruments aboard Terra and Aqua satellites are radiometrically calibrated on-orbit with a set of onboard calibrators (OBC) including a solar diffuser (SD), a blackbody (BB) and a space view (SV) port through which the detectors can view the dark space. As a whisk-broom scanning spectroradiometer, thirty-six MODIS spectral <span class="hlt">bands</span> are assembled in the along-scan direction on four focal plane assemblies (FPA). These <span class="hlt">bands</span> capture images of the same target sequentially with the motion of a scan mirror. Then the images are co-registered on board by delaying appropriate <span class="hlt">band</span> dependent amount of time depending on the <span class="hlt">band</span> locations on the FPA. While this co-registration mechanism is functioning well for the "far field" remote targets such as Earth view (EV) scenes or the Moon, noticeable <span class="hlt">band-to-band</span> misregistration in the along-scan direction has been <span class="hlt">observed</span> for near field targets, in particular the OBCs. In this paper, the misregistration phenomenon is presented and analyzed. It is concluded that the root cause of the misregistration is that the rotating element of the instrument, the scan mirror, is displaced from the focus of the telescope primary mirror. The amount of the misregistration is proportional to the <span class="hlt">band</span> location on the FPA and is inversely proportional to the distance between the target and the scan mirror. The impact of this misregistration to the calibration of MODIS <span class="hlt">bands</span> is discussed. In particular, the calculation of the detector gain coefficient m1 of <span class="hlt">bands</span> 8-16 (412 nm 870 nm) is improved by up to 1.5% for Aqua MODIS.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017A%26A...603A..77H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017A%26A...603A..77H"><span>Simultaneous 183 GHz H2O maser and SiO <span class="hlt">observations</span> towards evolved stars using APEX SEPIA <span class="hlt">Band</span> 5</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Humphreys, E. M. L.; Immer, K.; Gray, M. D.; De Beck, E.; Vlemmings, W. H. T.; Baudry, A.; Richards, A. M. S.; Wittkowski, M.; Torstensson, K.; De Breuck, C.; Møller, P.; Etoka, S.; Olberg, M.</p> <p>2017-07-01</p> <p>Aims: The aim is to investigate the use of 183 GHz H2O masers for characterization of the physical conditions and mass loss process in the circumstellar envelopes of evolved stars. Methods: We used APEX SEPIA <span class="hlt">Band</span> 5 (an ALMA <span class="hlt">Band</span> 5 receiver on the APEX telescope) to <span class="hlt">observe</span> the 183 GHz H2O line towards two red supergiant (RSG) and three asymptotic giant branch (AGB) stars. Simultaneously, we <span class="hlt">observed</span> the J = 4-3 line for 28SiO v = 0, 1, 2 and 3, and for 29SiO v = 0 and 1. We compared the results with simulations and radiative transfer models for H2O and SiO, and examined data for the individual linear orthogonal polarizations. Results: We detected the 183 GHz H2O line towards all the stars with peak flux densities >100 Jy, including a new detection from VY CMa. Towards all five targets, the water line had indications of being caused by maser emission and had higher peak flux densities than for the SiO lines. The SiO lines appear to originate from both thermal and maser processes. Comparison with simulations and models indicate that 183 GHz maser emission is likely to extend to greater radii in the circumstellar envelopes than SiO maser emission and to similar or greater radii than water masers at 22, 321 and 325 GHz. We speculate that a prominent blue-shifted feature in the W Hya 183 GHz spectrum is amplifying the stellar continuum, and is located at a similar distance from the star as mainline OH maser emission. We note that the coupling of an SiO maser model to a hydrodynamical pulsating model of an AGB star yields qualitatively similar simulated results to the <span class="hlt">observations</span>. From a comparison of the individual polarizations, we find that the SiO maser linear polarization fraction of several features exceeds the maximum fraction allowed under standard maser assumptions and requires strong anisotropic pumping of the maser transition and strongly saturated maser emission. The low polarization fraction of the H2O maser however, fits with the expectation for a non</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3624814','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3624814"><span>Direct <span class="hlt">Band</span> Gap Wurtzite Gallium Phosphide Nanowires</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p></p> <p>2013-01-01</p> <p>The main challenge for light-emitting diodes is to increase the efficiency in the green part of the spectrum. Gallium phosphide (GaP) with the normal cubic crystal structure has an indirect <span class="hlt">band</span> gap, which severely limits the green emission efficiency. <span class="hlt">Band</span> structure calculations have predicted a direct <span class="hlt">band</span> gap for wurtzite GaP. Here, we report the fabrication of GaP nanowires with pure hexagonal crystal structure and demonstrate the direct nature of the <span class="hlt">band</span> gap. We <span class="hlt">observe</span> strong photoluminescence at a wavelength of 594 nm with short lifetime, typical for a direct <span class="hlt">band</span> gap. Furthermore, by incorporation of aluminum or arsenic in the GaP nanowires, the emitted wavelength is tuned across an important range of the visible light spectrum (555–690 nm). This approach of crystal structure engineering enables new pathways to tailor materials properties enhancing the functionality. PMID:23464761</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2011BAAS...43..002C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2011BAAS...43..002C"><span>Obituary: David L. <span class="hlt">Band</span> (1957-2009)</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Cominsky, Lynn</p> <p>2011-12-01</p> <p>David L. <span class="hlt">Band</span>, of Potomac Maryland, died on March 16, 2009 succumbing to a long battle with spinal cord cancer. His death at the age of 52 came as a shock to his many friends and colleagues in the physics and astronomy community. <span class="hlt">Band</span> showed an early interest and exceptional aptitude for physics, leading to his acceptance at the Massachusetts Institute of Technology as an undergraduate student in 1975. After graduating from MIT with an undergraduate degree in Physics, <span class="hlt">Band</span> continued as a graduate student in Physics at Harvard University. His emerging interest in Astrophysics led him to the Astronomy Department at the Harvard Smithsonian Center for Astrophysics (CfA), where he did his dissertation work with Jonathan Grindlay. His dissertation (1985) entitled "Non-thermal Radiation Mechanisms and Processes in SS433 and Active Galactic Nuclei" was "pioneering work on the physics of jets arising from black holes and models for their emission, including self-absorption, which previewed much to come, and even David's own later work on Gamma-ray Bursts," according to Grindlay who remained a personal friend and colleague of <span class="hlt">Band</span>'s. Following graduate school, <span class="hlt">Band</span> held postdoctoral <span class="hlt">positions</span> at the Lawrence Livermore Laboratory, the University of California at Berkeley and the Center for Astronomy and Space Sciences at the University of California San Diego where he worked on the BATSE experiment that was part of the Compton Gamma Ray Observatory (CGRO), launched in 1991. BATSE had as its main objective the study of cosmic gamma-ray bursts (GRBs) and made significant advances in this area of research. <span class="hlt">Band</span> became a world-renowned figure in the emerging field of GRB studies. He is best known for his widely-used analytic form of gamma-ray burst spectra known as the "<span class="hlt">Band</span> Function." After the CGRO mission ended, <span class="hlt">Band</span> moved to the Los Alamos National Laboratory where he worked mainly on classified research but continued to work on GRB energetics and spectra. When NASA planned</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1356148-strain-fields-induced-kink-band-propagation-cu-nb-nanolaminate-composites','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1356148-strain-fields-induced-kink-band-propagation-cu-nb-nanolaminate-composites"><span>Strain fields induced by kink <span class="hlt">band</span> propagation in Cu-Nb nanolaminate composites</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Nizolek, T. J.; Begley, M. R.; McCabe, R. J.; ...</p> <p>2017-07-01</p> <p>Kink <span class="hlt">band</span> formation is a common deformation mode for anisotropic materials and has been <span class="hlt">observed</span> in polymer matrix fiber composites, single crystals, geological formations, and recently in metallic nanolaminates. While numerous studies have been devoted to kink <span class="hlt">band</span> formation, the majority do not consider the often rapid and unstable process of kink <span class="hlt">band</span> propagation. In this paper, we take advantage of stable kink <span class="hlt">band</span> formation in Cu-Nb nanolaminates to quantitatively map the local strain fields surrounding a propagating kink <span class="hlt">band</span> during uniaxial compression. Kink <span class="hlt">bands</span> are <span class="hlt">observed</span> to initiate at specimen edges, propagate across the sample during a rising globalmore » stress, and induce extended strain fields in the non-kinked material surrounding the propagating kink <span class="hlt">band</span>. Finally, it is proposed that these stress/strain fields significantly contribute to the total energy dissipated during kinking and, analogous to crack tip stress/strain fields, influence the direction of kink propagation and therefore the kink <span class="hlt">band</span> inclination angle.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1334327-triaxial-band-structures-chirality-magnetic-rotation-la133','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1334327-triaxial-band-structures-chirality-magnetic-rotation-la133"><span>Triaxial-<span class="hlt">band</span> structures, chirality, and magnetic rotation in La 133</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Petrache, C. M.; Chen, Q. B.; Guo, S.; ...</p> <p>2016-12-05</p> <p>The structure of 133La has been investigated using the 116Cd( 22Ne,4pn) reaction and the Gammasphere array. Three new <span class="hlt">bands</span> of quadrupole transitions and one <span class="hlt">band</span> of dipole transitions are identified and the previously reported level scheme is revised and extended to higher spins. The <span class="hlt">observed</span> structures are discussed using the cranked Nilsson-Strutinsky formalism, covariant density functional theory, and the particle-rotor model. Triaxial configurations are assigned to all <span class="hlt">observed</span> <span class="hlt">bands</span>. For the high-spin <span class="hlt">bands</span> it is found that rotations around different axes can occur, depending on the configuration. The orientation of the angular momenta of the core and of themore » active particles is investigated, suggesting chiral rotation for two nearly degenerate dipole <span class="hlt">bands</span> and magnetic rotation for one dipole <span class="hlt">band</span>. As a result, it is shown that the h 11/2 neutron holes present in the configuration of the nearly degenerate dipole <span class="hlt">bands</span> have significant angular momentum components not only along the long axis but also along the short axis, contributing to the balance of the angular momentum components along the short and long axes and thus giving rise to a chiral geometry.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-sts059-s-074.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-sts059-s-074.html"><span>Color composite C-<span class="hlt">band</span> and L-<span class="hlt">band</span> image of Kilauea volcanoe on Hawaii</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>1994-04-15</p> <p>STS059-S-074 (15 April 1994) --- This color composite C-<span class="hlt">Band</span> and L-<span class="hlt">Band</span> image of the Kilauea volcano on the big island of Hawaii was acquired by the Spaceborne Imaging Radar-C and X-<span class="hlt">Band</span> Synthetic Aperture Radar (SIR-C/X-SAR) flying on the Space Shuttle Endeavour. The city of Hilo can be seen at the top. The image shows the different types of lava flows around the crater Pu'u O'o. Ash deposits which erupted in 1790 from the summit of Kilauea volcano show up as dark in this image, and fine details associated with lava flows which erupted in 1919 and 1974 can be seen to the south of the summit in an area called the Ka'u Desert. In addition, the other historic lava flows created in 1881 and 1984 from Mauna Loa volcano (out of view to the left of this image) can easily be seen despite the fact that the surrounding area is covered by forest. Such information will be used to map the extent of such flows, which can pose a hazard to the subdivisions of Hilo. Highway 11 is the linear feature running from Hilo to the Kilauea volcano. The Kilauea volcano has been almost continuously active for more than the last 11 years. Field teams that were on the ground specifically to support these radar <span class="hlt">observations</span> report that there was vigorous surface activity about 400 meters (one-quarter mile) inland from the coast. A moving lava flow about 200 meters (660 feet) in length was <span class="hlt">observed</span> at the time of the Shuttle over flight, raising the possibility that subsequent images taken during this mission will show changes in the landscape. SIR-C/X-SAR is part of NASA's Mission to Planet Earth (MTPE). SIR-C/X-SAR radars illuminate Earth with microwaves allowing detailed <span class="hlt">observations</span> at any time, regardless of weather or sunlight conditions. SIR-C/X-SAR uses three microwave wavelengths: L-<span class="hlt">Band</span> (24 cm), C-<span class="hlt">Band</span> (6 cm), and X-<span class="hlt">Band</span> (3 cm). The multi-frequency data will be used by the international scientific community to better understand the global environment and how it is changing. The SIR</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018JETPL.tmp...77V','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018JETPL.tmp...77V"><span>Graphite, graphene and the flat <span class="hlt">band</span> superconductivity</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Volovik, G. E.</p> <p>2018-04-01</p> <p>Superconductivity has been <span class="hlt">observed</span> in bilayer graphene [1,2]. The main factor, which determines the mechanism of the formation of this superconductivity is the "magic angle" of twist of two graphene layers, at which the electronic <span class="hlt">band</span> structure becomes nearly flat. The specific role played by twist and by the <span class="hlt">band</span> flattening, has been earlier suggested for explanations of the signatures of room-temperature superconductivity <span class="hlt">observed</span> in the highly oriented pyrolytic graphite (HOPG), when the quasi two-dimensional interfaces between the twisted domains are present. The interface contains the periodic array of misfit dislocations (analogs of the boundaries of the unit cell of the Moire superlattice in bilayer graphene), which provide the possible source of the flat <span class="hlt">band</span>. This demonstrates that it is high time for combination of the theoretical and experimental efforts in order to reach the reproducible room-temperature superconductivity in graphite or in similar real or artificial materials.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018JPSJ...87d3703T','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018JPSJ...87d3703T"><span>Multi-<span class="hlt">band</span> Electronic Structure of Ferromagnetic CeRuPO</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Takahashi, Masaya; Ootsuki, Daiki; Horio, Masafumi; Arita, Masashi; Namatame, Hirofumi; Taniguchi, Masaki; Saini, Naurang L.; Sugawara, Hitoshi; Mizokawa, Takashi</p> <p>2018-04-01</p> <p>We have studied the multi-<span class="hlt">band</span> electronic structure of ferromagnetic CeRuPO (TC = 15 K) by means of angle-resolved photoemission spectroscopy (ARPES). The ARPES results show that three hole <span class="hlt">bands</span> exist around the zone center and two of them cross the Fermi level (EF). Around the zone corner, two electron <span class="hlt">bands</span> are <span class="hlt">observed</span> and cross EF. These hole and electron <span class="hlt">bands</span>, which can be assigned to the Ru 4d <span class="hlt">bands</span>, are basically consistent with the <span class="hlt">band</span>-structure calculation including their orbital characters. However, one of the electron <span class="hlt">bands</span> with Ru 4d 3z2 - r2 character is strongly renormalized indicating correlation effect due to hybridization with the Ce 4f orbitals. The Ru 4d 3z2 - r2 <span class="hlt">band</span> changes across TC suggesting that the out-of-plane 3z2 - r2 orbital channel plays essential roles in the ferromagnetism.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20080005154','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20080005154"><span>Silicon micromachined broad <span class="hlt">band</span> light source</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>George, Thomas (Inventor); Jones, Eric (Inventor); Tuma, Margaret L. (Inventor); Eastwood, Michael (Inventor); Hansler, Richard (Inventor)</p> <p>2004-01-01</p> <p>A micro electromechanical system (MEMS) broad <span class="hlt">band</span> incandescent light source includes three layers: a top transmission window layer; a middle filament mount layer; and a bottom reflector layer. A tungsten filament with a spiral geometry is <span class="hlt">positioned</span> over a hole in the middle layer. A portion of the broad <span class="hlt">band</span> light from the heated filament is reflective off the bottom layer. Light from the filament and the reflected light of the filament are transmitted through the transmission window. The light source may operate at temperatures of 2500 K or above. The light source may be incorporated into an on board calibrator (OBC) for a spectrometer.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/1961620','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/1961620"><span>Sclera-directed knot technique for securing an encircling <span class="hlt">band</span> in retinal surgery.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Bartov, E; Ginsburg, L H; Ashkenazi, I; Treister, G</p> <p>1991-10-01</p> <p>The protruding ends of sutures used to secure the ends of the silicone rubber <span class="hlt">band</span> placed during many retinal surgical procedures may cause postsurgical irritation, since with presently used suturing techniques, the knot of the suture remains on top of the <span class="hlt">band</span>, facing the conjunctiva. We describe a suturing technique which, by inverting the <span class="hlt">band</span> when suturing its ends and then allowing the <span class="hlt">band</span> to return to its original <span class="hlt">position</span>, places the knot on the undersurface of the <span class="hlt">band</span>, against the sclera. Thus, no protruding suture ends are left facing the conjunctiva and the irritation resulting from such a protrusion is averted.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2002PhRvB..65p5115W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2002PhRvB..65p5115W"><span>Ab initio electronic structure calculations for metallic intermediate <span class="hlt">band</span> formation in photovoltaic materials</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wahnón, P.; Tablero, C.</p> <p>2002-04-01</p> <p>A metallic isolated <span class="hlt">band</span> in the middle of the <span class="hlt">band</span> gap of several III-V semiconductors has been predicted as photovoltaic materials with the possibility of providing substantially enhanced efficiencies. We have investigated the electronic <span class="hlt">band</span> structures and lattice constants of GanAsmM and GanPmM with M=Sc, Ti, V, and Cr, to identify whether this isolated <span class="hlt">band</span> is likely to exist by means of accurate calculations. For this task, we use the SIESTA program, an ab initio periodic density-functional method, fully self consistent in the local-density approximation. Norm-conserving, nonlocal pseudopotentials and confined linear combination of atomic orbitals have been used. We have carried out a case study of GanAsmTi and GanPmTi energy-<span class="hlt">band</span> structure including analyses of the effect of the basis set, fine k-point mesh to ensure numerical convergence, structural parameters, and generalized gradient approximation for exchange and correlation corrections. We find the isolated intermediate <span class="hlt">band</span> when one Ti atom replaces the <span class="hlt">position</span> of one As (or P) atom in the crystal structure. For this kind of compound we show that the intermediate <span class="hlt">band</span> relative <span class="hlt">position</span> inside the <span class="hlt">band</span> gap and width are sensitive to the dynamic relaxation of the crystal and the size of the basis set.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017JChPh.147v4104J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017JChPh.147v4104J"><span>Complex <span class="hlt">band</span> structure and electronic transmission eigenchannels</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jensen, Anders; Strange, Mikkel; Smidstrup, Søren; Stokbro, Kurt; Solomon, Gemma C.; Reuter, Matthew G.</p> <p>2017-12-01</p> <p>It is natural to characterize materials in transport junctions by their conductance length dependence, β. Theoretical estimations of β are made employing two primary theories: complex <span class="hlt">band</span> structure and density functional theory (DFT) Landauer transport. It has previously been shown that the β value derived from total Landauer transmission can be related to the β value from the smallest |ki| complex <span class="hlt">band</span>; however, it is an open question whether there is a deeper relationship between the two. Here we probe the details of the relationship between transmission and complex <span class="hlt">band</span> structure, in this case individual eigenchannel transmissions and different complex <span class="hlt">bands</span>. We present calculations of decay constants for the two most conductive states as determined by complex <span class="hlt">band</span> structure and standard DFT Landauer transport calculations for one semi-conductor and two molecular junctions. The molecular junctions show that both the length dependence of the total transmission and the individual transmission eigenvalues can be, almost always, found through the complex <span class="hlt">band</span> structure. The complex <span class="hlt">band</span> structure of the semi-conducting material, however, does not predict the length dependence of the total transmission but only of the individual channels, at some k-points, due to multiple channels contributing to transmission. We also <span class="hlt">observe</span> instances of vertical <span class="hlt">bands</span>, some of which are the smallest |ki| complex <span class="hlt">bands</span>, that do not contribute to transport. By understanding the deeper relationship between complex <span class="hlt">bands</span> and individual transmission eigenchannels, we can make a general statement about when the previously accepted wisdom linking transmission and complex <span class="hlt">band</span> structure will fail, namely, when multiple channels contribute significantly to the transmission.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://pubs.er.usgs.gov/publication/70159620','USGSPUBS'); return false;" href="https://pubs.er.usgs.gov/publication/70159620"><span>Landsat-4/5 <span class="hlt">Band</span> 6 relative radiometry</span></a></p> <p><a target="_blank" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p>Chander, Gyanesh; Helder, D.L.; Boncyk, Wayne C.</p> <p>2002-01-01</p> <p>Relative radiometric responses for the thematic mapper (TM) <span class="hlt">band</span> 6 data from Landsat-4 and Landsat-5 were analyzed, and an algorithm has been developed that significantly reduces the striping in <span class="hlt">Band</span> 6 images due to detector mismatch. The TM internal calibration system as originally designed includes a DC restore circuit, which acts as a feedback system designed to keep detector bias at a constant value. There is a strong indication that the DC restore circuitry implemented in <span class="hlt">Band</span> 6 does not function as it had been designed to. It operates as designed only during a portion of the calibration interval and not at all during acquisition of scene data. This renders the data acquired during the calibration shutter interval period virtually useless for correction of the individual responses of the four detectors in <span class="hlt">Band</span> 6. It was <span class="hlt">observed</span> and statistically quantified that the relative response of each of the detectors to the <span class="hlt">band</span> average is stable over the dynamic range and throughout the lifetime of the instrument. This allows an alternate approach to relative radiometric correction of TM <span class="hlt">Band</span> 6 images</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20020034944&hterms=Polycyclic+aromatic+hydrocarbons&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3DPolycyclic%2Baromatic%2Bhydrocarbons','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20020034944&hterms=Polycyclic+aromatic+hydrocarbons&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3DPolycyclic%2Baromatic%2Bhydrocarbons"><span>Assessment of the Polycyclic Aromatic Hydrocarbon-Diffuse Interstellar <span class="hlt">Band</span> Proposal</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Salama, Farid; Bakes, F.; Allamandola, L.; Tielens, A. G. G. M.; Witteborn, Fred C. (Technical Monitor)</p> <p>1995-01-01</p> <p>The potential link between neutral and/or ionized polycyclic aromatic hydrocarbons (PAHs) and the diffuse interstellar <span class="hlt">band</span> (DIB) carriers is examined. Based on the study of the general physical and chemical properties of PAHs, an assessment is made of their possible contribution to the DIB carriers. It is found that, under the conditions reigning in the diffuse interstellar medium, PAHs can be present in the form of neutral molecules as well as <span class="hlt">positive</span> and/or negative ions. The charge distribution of small PAHs is dominated, however, by two charge states at one time with compact PAHs present only in the neutral and cationic forms. Each PAH has a distinct spectral signature depending on its charge state. Moreover, the spectra of ionized PAHs are always clearly dominated by a single <span class="hlt">band</span> in the DIB spectral range. In the case of compact PAH ions, the strongest absorption <span class="hlt">band</span> is of type A (i.e., the <span class="hlt">band</span> is broad, falls in the high energy range of the spectrum, and possess a large oscillator strength), and seems to correlate with strong and broad DIBs. In the case of non-compact PAH ions, the strongest absorption <span class="hlt">band</span> is of type I (i.e., the <span class="hlt">band</span> is narrow, falls in the low energy range of the spectrum, and possess a small oscillator strength), and seems to correlate with weak and narrow DIBs. Potential molecular size and structure constraints for interstellar PAHs are derived by comparing known DIB characteristics to the spectroscopic properties of PAHs. It is found that: (i) Only neutral PAHs larger than about 30 carbon atoms could, if present, contribute to the DIBs. (ii) For compact PAHs, only ions with less than about 250 carbon atoms could, if present, contribute to the DIBs. (iii) The <span class="hlt">observed</span> distribution of the DIBs between strong/moderate and broad <span class="hlt">bands</span> on the one hand and weak and narrow <span class="hlt">bands</span> on the other hand can easily be interpreted in the context of the PAH proposal by a distribution between compact and non-compact PAH ions, respectively. A</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018PhRvC..97c4317S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018PhRvC..97c4317S"><span>Shell-model-like approach based on cranking covariant density functional theory: <span class="hlt">Band</span> crossing and shape evolution in 60Fe</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Shi, Z.; Zhang, Z. H.; Chen, Q. B.; Zhang, S. Q.; Meng, J.</p> <p>2018-03-01</p> <p>The shell-model-like approach is implemented to treat the cranking many-body Hamiltonian based on the covariant density functional theory including pairing correlations with exact particle number conservation. The self-consistency is achieved by iterating the single-particle occupation probabilities back to the densities and currents. As an example, the rotational structures <span class="hlt">observed</span> in the neutron-rich nucleus 60Fe are investigated and analyzed. Without introducing any ad hoc parameters, the bandheads, the rotational spectra, and the relations between the angular momentum and rotational frequency for the <span class="hlt">positive</span>-parity <span class="hlt">band</span> A and negative-parity <span class="hlt">bands</span> B and C are well reproduced. The essential role of the pairing correlations is revealed. It is found that for <span class="hlt">band</span> A, the <span class="hlt">band</span> crossing is due to the change of the last two occupied neutrons from the 1 f5 /2 signature partners to the 1 g9 /2 signature partners. For the two negative-parity signature partner <span class="hlt">bands</span> B and C, the <span class="hlt">band</span> crossings are due to the pseudocrossing between the 1 f7 /2 ,5 /2 and the 1 f5 /2 ,1 /2 orbitals. Generally speaking, the deformation parameters β for <span class="hlt">bands</span> A, B, and C decrease with rotational frequency. For <span class="hlt">band</span> A, the deformation jumps from β ≈0.19 to β ≈0.29 around the <span class="hlt">band</span> crossing. In comparison with its signature partner <span class="hlt">band</span> C, <span class="hlt">band</span> B exhibits appreciable triaxial deformation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5470930','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5470930"><span>Dual-Polarization <span class="hlt">Observations</span> of Slowly Varying Solar Emissions from a Mobile X-<span class="hlt">Band</span> Radar</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Gabella, Marco; Leuenberger, Andreas</p> <p>2017-01-01</p> <p>The radio noise that comes from the Sun has been reported in literature as a reference signal to check the quality of dual-polarization weather radar receivers for the S-<span class="hlt">band</span> and C-<span class="hlt">band</span>. In most cases, the focus was on relative calibration: horizontal and vertical polarizations were evaluated versus the reference signal mainly in terms of standard deviation of the difference. This means that the investigated radar receivers were able to reproduce the slowly varying component of the microwave signal emitted by the Sun. A novel method, aimed at the absolute calibration of dual-polarization receivers, has recently been presented and applied for the C-<span class="hlt">band</span>. This method requires the antenna beam axis to be pointed towards the center of the Sun for less than a minute. Standard deviations of the difference as low as 0.1 dB have been found for the Swiss radars. As far as the absolute calibration is concerned, the average differences were of the order of −0.6 dB (after noise subtraction). The method has been implemented on a mobile, X-<span class="hlt">band</span> radar, and this paper presents the successful results that were obtained during the 2016 field campaign in Payerne (Switzerland). Despite a relatively poor Sun-to-Noise ratio, the “small” (~0.4 dB) amplitude of the slowly varying emission was captured and reproduced; the standard deviation of the difference between the radar and the reference was ~0.2 dB. The absolute calibration of the vertical and horizontal receivers was satisfactory. After the noise subtraction and atmospheric correction a, the mean difference was close to 0 dB. PMID:28531164</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28531164','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28531164"><span>Dual-Polarization <span class="hlt">Observations</span> of Slowly Varying Solar Emissions from a Mobile X-<span class="hlt">Band</span> Radar.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Gabella, Marco; Leuenberger, Andreas</p> <p>2017-05-22</p> <p>The radio noise that comes from the Sun has been reported in literature as a reference signal to check the quality of dual-polarization weather radar receivers for the S-<span class="hlt">band</span> and C-<span class="hlt">band</span>. In most cases, the focus was on relative calibration: horizontal and vertical polarizations were evaluated versus the reference signal mainly in terms of standard deviation of the difference. This means that the investigated radar receivers were able to reproduce the slowly varying component of the microwave signal emitted by the Sun. A novel method, aimed at the absolute calibration of dual-polarization receivers, has recently been presented and applied for the C-<span class="hlt">band</span>. This method requires the antenna beam axis to be pointed towards the center of the Sun for less than a minute. Standard deviations of the difference as low as 0.1 dB have been found for the Swiss radars. As far as the absolute calibration is concerned, the average differences were of the order of -0.6 dB (after noise subtraction). The method has been implemented on a mobile, X-<span class="hlt">band</span> radar, and this paper presents the successful results that were obtained during the 2016 field campaign in Payerne (Switzerland). Despite a relatively poor Sun-to-Noise ratio, the "small" (~0.4 dB) amplitude of the slowly varying emission was captured and reproduced; the standard deviation of the difference between the radar and the reference was ~0.2 dB. The absolute calibration of the vertical and horizontal receivers was satisfactory. After the noise subtraction and atmospheric correction a, the mean difference was close to 0 dB.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012ATel.4457....1M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012ATel.4457....1M"><span>X-ray emission at a <span class="hlt">position</span> consistent with SN2009ip</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Margutti, R.; Soderberg, A.</p> <p>2012-10-01</p> <p>We <span class="hlt">observed</span> SN2009ip for a total of ~93 ks with Swift/XRT. We split the <span class="hlt">observation</span> into two epochs. The first epoch comprises data acquired between September 10th and October 1st, for a total of ~53 ks of exposure. No source is detected at the <span class="hlt">position</span> of the SN, with a 3 sigma upper limit of 3.3d-4 counts/sec in the 0.3-10 keV energy <span class="hlt">band</span> (a similar limit has been reported by Campana Atel #4444).</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li class="active"><span>17</span></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_17 --> <div id="page_18" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li class="active"><span>18</span></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="341"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/23745977','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/23745977"><span>Microleakage under orthodontic <span class="hlt">bands</span> cemented with nano-hydroxyapatite-modified glass ionomer.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Enan, Enas T; Hammad, Shaza M</p> <p>2013-11-01</p> <p>To estimate the in vivo effect of nano-hydroxyapatite (HA) modification of <span class="hlt">banding</span> glass-ionomer cement on microleakage under orthodontic <span class="hlt">bands</span>. Eighty noncarious premolars scheduled for extraction in 20 orthodontic patients were randomly divided into four groups. Grouping was based on the ratio of nano-HA (0%, 5%, 10%, 15% by weight) added to the luting glass-ionomer cement (GIC) Ketac-Cem, which was used for cementation of prefabricated micro-etched orthodontic <span class="hlt">bands</span>. Dye penetration method was used for microleakage evaluation at the cement-<span class="hlt">band</span> and cement-enamel interfaces. Statistical evaluation was performed with a Kruskal-Wallis test and a Mann-Whitney U-test, and a Bonferroni-adjusted significance level was calculated. <span class="hlt">Bands</span> cemented with conventional GIC showed the highest microleakage scores in comparison to those cemented with nano-HA-modified GIC. No significant difference was found between teeth <span class="hlt">banded</span> with 10% and 15% modified GIC. Modification of the <span class="hlt">banding</span> GIC with 15% nano-HA revealed a <span class="hlt">positive</span> effect on reducing microleakage around orthodontic <span class="hlt">bands</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017AGUFMSM11E..08C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017AGUFMSM11E..08C"><span>Magnetopause Standoff <span class="hlt">Position</span> Changes and Geosynchronous Orbit Crossings: Models and <span class="hlt">Observations</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Collado-Vega, Y. M.; Rastaetter, L.; Sibeck, D. G.</p> <p>2017-12-01</p> <p>The Earth's magnetopause is the boundary that mostly separates the solar wind with the Earth's magnetosphere. Its location has been studied and estimated via simulation models, <span class="hlt">observational</span> data and empirical models. This research aims to study the changes of the magnetopause standoff location due to different solar wind conditions using a combination of all the different methods. We will use the Run-On-Request capabilities within the MHD models available from the Community Coordinated Modeling Center (CCMC) at NASA Goddard Space Flight Center, specifically BATS-R-US (SWMF), OpenGGCM, LFM and GUMICS models. The magnetopause standoff <span class="hlt">position</span> prediction and response time to the solar wind changes will then be compared to results from available empirical models (e.g. Shue et al. 1998), and to THEMIS, Cluster, Geotail and MMS missions magnetopause crossing <span class="hlt">observations</span>. We will also use times of extreme solar wind conditions where magnetopause crossings have been <span class="hlt">observed</span> by the GOES satellites. Rigorous analysis/comparison of <span class="hlt">observations</span> and empirical models is critical in determining magnetosphere dynamics for model validation. This research goes also hand in hand with the efforts of the working group at the CCMC/LWS International Forum for Space Weather Capabilities Assessment workshop that aims to analyze different events to define metrics for model-data comparison. Preliminary results of this particular research show that there are some discrepancies between the MHD models standoff <span class="hlt">positions</span> of the dayside magnetopause for the same solar wind conditions that include an increase in solar wind dynamic pressure and a step function in the IMF Bz component. In cases of nominal solar wind conditions, it has been <span class="hlt">observed</span> that the models do mostly agree with the <span class="hlt">observational</span> data from the different satellite missions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015JMoSp.313....4U','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015JMoSp.313....4U"><span>Precise ro-vibrational analysis of molecular <span class="hlt">bands</span> forbidden in absorption: The ν8 +ν10 <span class="hlt">band</span> of the 12C2H4 molecule</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ulenikov, O. N.; Gromova, O. V.; Bekhtereva, E. S.; Kashirina, N. V.; Bauerecker, S.; Horneman, V.-M.</p> <p>2015-07-01</p> <p>The highly accurate (experimental accuracy in line <span class="hlt">positions</span> ∼ (1 - 2) ×10-4 cm-1) ro-vibrational spectrum of the ν8 +ν10 <span class="hlt">band</span> of the 12C2H4 molecule was recorded for the first time with high resolution Fourier transform spectrometry and analyzed in the region of 1650-1950 cm-1 using the Hamiltonian model which takes into account Coriolis resonance interactions between the studied ν8 +ν10 <span class="hlt">band</span>, which is forbidden in absorption, and the <span class="hlt">bands</span> ν4 +ν8 and ν7 +ν8 . About 1570 transitions belonging to the ν8 +ν10 <span class="hlt">band</span> were assigned in the experimental spectra with the maximum values of quantum numbers Jmax. = 35 and Kamax . = 18 . On that basis, a set of 38 vibrational, rotational, centrifugal distortion, and resonance interaction parameters was obtained from the fit. They reproduce values of 598 initial "experimental" ro-vibrational energy levels (<span class="hlt">positions</span> of about 1570 experimentally recorded and assigned transitions) with the rms error drms = 0.00045 cm-1 (drms = 0.00028 cm-1 when upper ro-vibrational energies obtained from blended and very weak transitions were deleted from the fit).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19990099703&hterms=Global+Positioning+System&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DThe%2BGlobal%2BPositioning%2BSystem','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19990099703&hterms=Global+Positioning+System&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DThe%2BGlobal%2BPositioning%2BSystem"><span><span class="hlt">Observing</span> Tropospheric Water Vapor by Radio Occultation using the Global <span class="hlt">Positioning</span> System</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Kursinski, E. R.; Hajj, G. A.; Hardy, K. R.; Romans, L. J.; Schofield, J. T.</p> <p>1995-01-01</p> <p>Given the importance of water vapor to weather, climate and hydrology, global humidity <span class="hlt">observations</span> from satellites are critical. At low latitudes, radio occultation <span class="hlt">observations</span> of Earth's atmosphere using the Global <span class="hlt">Positioning</span> System (GPS) satellites allow water vapor profiles to be retrieved with accuracies of 10 to 20% below 6 to 7 km altitude and approx. 5% or better within the boundary layer. GPS <span class="hlt">observations</span> provide a unique combination of accuracy, vertical resolution (less than or equal to 1 km) and insensitivity to cloud and aerosol particles that is well suited to <span class="hlt">observations</span> of the lower troposphere. These characteristics combined with the inherent stability of radio occultation <span class="hlt">observations</span> make it an excellent candidate for the measurement of long term trends.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016AGUFM.G31B1055U','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016AGUFM.G31B1055U"><span>An Investigation on the Contribution of GLONASS to the Precise Point <span class="hlt">Positioning</span> for Short Time <span class="hlt">Observations</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ulug, R.; Ozludemir, M. T.</p> <p>2016-12-01</p> <p>After 2011, through the modernization process of GLONASS, the number of satellites increased rapidly. This progress has made the GLONASS the only fully operational system alternative to GPS in point <span class="hlt">positioning</span>. So far, many researches have been conducted to investigate the contribution of GLONASS to point <span class="hlt">positioning</span> considering different methods such as Real Time Kinematic (RTK) and Precise Point <span class="hlt">Positioning</span> (PPP). The latter one, PPP, is a method that performs precise <span class="hlt">position</span> determination using a single GNSS receiver. PPP method has become very attractive since the early 2000s and it provided great advantages for engineering and scientific applications. However, PPP method needs at least 2 hours <span class="hlt">observation</span> time and the required <span class="hlt">observation</span> length may be longer depending on several factors, such as the number of satellites, satellite configuration etc. The more satellites, the less <span class="hlt">observation</span> time. Nevertheless the impact of the number of satellites included must be known very well. In this study, to determine the contribution of GLONASS on PPP, GLONASS satellite <span class="hlt">observations</span> were added one by one from 1 to 5 satellite in 2, 4 and 6 hours of <span class="hlt">observations</span>. For this purpose, the data collected at the IGS site ISTA was used. Data processing has been done for Day of Year (DOY) 197 in 2016. 24 hours GPS <span class="hlt">observations</span> have been processed by Bernese 5.2 PPP module and the output was selected as the reference while 2, 4 and 6 hours GPS and GPS/GLONASS <span class="hlt">observations</span> have been processed by magic GNSS PPP module. The results clearly showed that GPS/GLONASS <span class="hlt">observations</span> improved <span class="hlt">positional</span> accuracy, precision, dilution of precision and convergence to the reference coordinates. In this context, coordinate differences between 24 hours GPS <span class="hlt">observations</span> and 6 hours GPS/GLONASS <span class="hlt">observations</span> have been obtained as less than 2 cm.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22089701-rri-gbt-multi-band-receiver-motivation-design-development','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22089701-rri-gbt-multi-band-receiver-motivation-design-development"><span>RRI-GBT MULTI-<span class="hlt">BAND</span> RECEIVER: MOTIVATION, DESIGN, AND DEVELOPMENT</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Maan, Yogesh; Deshpande, Avinash A.; Chandrashekar, Vinutha</p> <p>2013-01-15</p> <p>We report the design and development of a self-contained multi-<span class="hlt">band</span> receiver (MBR) system, intended for use with a single large aperture to facilitate sensitive and high time-resolution <span class="hlt">observations</span> simultaneously in 10 discrete frequency <span class="hlt">bands</span> sampling a wide spectral span (100-1500 MHz) in a nearly log-periodic fashion. The development of this system was primarily motivated by need for tomographic studies of pulsar polar emission regions. Although the system design is optimized for the primary goal, it is also suited for several other interesting astronomical investigations. The system consists of a dual-polarization multi-<span class="hlt">band</span> feed (with discrete responses corresponding to the 10 bandsmore » pre-selected as relatively radio frequency interference free), a common wide-<span class="hlt">band</span> radio frequency front-end, and independent back-end receiver chains for the 10 individual sub-<span class="hlt">bands</span>. The raw voltage time sequences corresponding to 16 MHz bandwidth each for the two linear polarization channels and the 10 <span class="hlt">bands</span> are recorded at the Nyquist rate simultaneously. We present the preliminary results from the tests and pulsar <span class="hlt">observations</span> carried out with the Robert C. Byrd Green Bank Telescope using this receiver. The system performance implied by these results and possible improvements are also briefly discussed.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3746460','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3746460"><span>Dysphoric students show higher use of the <span class="hlt">observer</span> perspective in their retrieval of <span class="hlt">positive</span> versus negative autobiographical memories</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Nelis, Sabine; Debeer, Elise; Holmes, Emily A.; Raes, Filip</p> <p>2013-01-01</p> <p>Autobiographical memories are retrieved as images from either a field perspective or an <span class="hlt">observer</span> perspective. The <span class="hlt">observer</span> perspective is thought to dull emotion. <span class="hlt">Positive</span> affect is blunted in depressed mood. Consequently, are <span class="hlt">positive</span> events recalled from an <span class="hlt">observer</span> perspective in depressed mood? We investigated the relationship between memory vantage perspective and depressive symptoms in a student sample. Participants completed the Autobiographical Memory Test (AMT; Williams & Broadbent, 1986) and assessed the perspective accompanying each memory. The Beck Depression Inventory-II (BDI-II; Beck, Steer, & Brown, 1996) and the Responses to <span class="hlt">Positive</span> Affect questionnaire (RPA; Feldman, Joormann, & Johnson, 2008) were administered. The results showed a small <span class="hlt">positive</span> association between depressive symptoms and the use of an <span class="hlt">observer</span> perspective for <span class="hlt">positive</span> autobiographical memories, but not for negative memories. Furthermore, comparing a subgroup with clinically significant symptom levels (dysphoric students) with non-dysphoric individuals revealed that dysphoric students used an <span class="hlt">observer</span> perspective more for <span class="hlt">positive</span> memories compared with negative memories. This was not the case for non-dysphoric students. The <span class="hlt">observer</span> perspective in dysphorics was associated with a dampening cognitive style in response to <span class="hlt">positive</span> experiences. PMID:23083015</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://medlineplus.gov/ency/article/007388.htm','NIH-MEDLINEPLUS'); return false;" href="https://medlineplus.gov/ency/article/007388.htm"><span>Laparoscopic gastric <span class="hlt">banding</span></span></a></p> <p><a target="_blank" href="http://medlineplus.gov/">MedlinePlus</a></p> <p></p> <p></p> <p>... adjustable gastric <span class="hlt">banding</span>; Bariatric surgery - laparoscopic gastric <span class="hlt">banding</span>; Obesity - gastric <span class="hlt">banding</span>; Weight loss - gastric <span class="hlt">banding</span> ... gastric <span class="hlt">banding</span> is not a "quick fix" for obesity. It will greatly change your lifestyle. You must ...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19740057513&hterms=twilight&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dtwilight','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19740057513&hterms=twilight&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dtwilight"><span>Nitric oxide gamma and delta <span class="hlt">band</span> emission at twilight</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Feldman, P. D.; Takacs, P. Z.</p> <p>1974-01-01</p> <p>Nitric oxide twilight emission above 140 km in the gamma- and delta-<span class="hlt">bands</span> was <span class="hlt">observed</span> with a rocket-borne spectrophotometer. The relative intensity of the two <span class="hlt">band</span> systems indicates that the emission is produced predominantly by the chemiluminescent preassociation of oxygen and nitrogen atoms.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28464837','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28464837"><span>The correlation between malaria RDT (Paracheck pf.®) faint test <span class="hlt">bands</span> and microscopy in the diagnosis of malaria in Malawi.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Makuuchi, Ryoko; Jere, Sandy; Hasejima, Nobuchika; Chigeda, Thoms; Gausi, January</p> <p>2017-05-02</p> <p>Faint test <span class="hlt">bands</span> of Paracheck Pf.® are interpreted as malaria <span class="hlt">positive</span> according to world health organization (WHO) guideline. However if there are conspicuous number of faint test <span class="hlt">bands</span>, a performance of Paracheck Pf.® could be influenced depending on whether interpreting faint test <span class="hlt">bands</span> as malaria <span class="hlt">positive</span> or negative. Finding out the frequency and accurate interpretation of faint test <span class="hlt">bands</span> are important to prevent the overdiagnosis and drug resistance. A cross-sectional, descriptive study was conducted to find out the frequency of faint test <span class="hlt">bands</span> and evaluate the performance of Paracheck Pf.® by sensitivity, specificity, <span class="hlt">positive</span> predictive value (PPV), negative predictive value (NPV) and accuracy of diagnosis of Paracheck Pf.® using microscopy as the gold standard. 388 suspected patients with malaria in Malawi were recruited in this study. Malaria rapid diagnostic tests (RDTs) and microscopy were used and patients' information which includes age, sex, body temperature and signs or symptoms of malaria were recorded. Among all patients involved in the study, 29.1% (113/388) were found malaria <span class="hlt">positive</span> by RDT. Overall 5.4% (21/388) of all Paracheck Pf.® tests resulted in a "faint test <span class="hlt">band</span>" and 85.7% (18/21) corresponded with malaria negative by microscopy. Faint test <span class="hlt">bands</span> which corresponded with malaria <span class="hlt">positive</span> by microscopy were lower parasite density and there are no patients who showed definitive symptom of malaria, such as fever. When Paracheck Pf.® "faint test <span class="hlt">bands</span>" were classified as <span class="hlt">positive</span>, accuracy of diagnosis was 76.5% (95% CI 72%-80.7%) as compared to 80.4% (95% CI 76.1%-84.2%) when Paracheck Pf.® "faint test <span class="hlt">bands</span>" were classified as negative. This study shows that frequency of faint test <span class="hlt">bands</span> is 5.4% in all malaria RDTs. The accuracy of diagnosis was improved when faint test <span class="hlt">bands</span> were interpreted as malaria negative. However information and data obtained in this study may not be enough and more intensive research including a</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017PhRvM...1f1201K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017PhRvM...1f1201K"><span>Evolution of <span class="hlt">band</span> topology by competing <span class="hlt">band</span> overlap and spin-orbit coupling: Twin Dirac cones in Ba3SnO as a prototype</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kariyado, Toshikaze; Ogata, Masao</p> <p>2017-11-01</p> <p>We theoretically demonstrate how competition between <span class="hlt">band</span> inversion and spin-orbit coupling (SOC) results in nontrivial evolution of <span class="hlt">band</span> topology, taking antiperovskite Ba3SnO as a prototype material. A key <span class="hlt">observation</span> is that when the <span class="hlt">band</span> inversion dominates over SOC, there appear "twin" Dirac cones in the <span class="hlt">band</span> structure. Due to the twin Dirac cones, the <span class="hlt">band</span> shows highly peculiar structure in which the upper cone of one of the twin continuously transforms to the lower cone of the other. Interestingly, the relative size of the <span class="hlt">band</span> inversion and SOC is controlled in this series of antiperovskite A3E O by substitution of A (Ca, Sr, Ba) and/or E (Sn, Pb) atoms. Analysis of an effective model shows that the emergence of twin Dirac cones is general, which makes our argument a promising starting point for finding a singular <span class="hlt">band</span> structure induced by the competing <span class="hlt">band</span> inversion and SOC.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1415428-generation-highly-oblique-lower-band-chorus-via-nonlinear-three-wave-resonance','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1415428-generation-highly-oblique-lower-band-chorus-via-nonlinear-three-wave-resonance"><span>Generation of Highly Oblique Lower <span class="hlt">Band</span> Chorus Via Nonlinear Three-Wave Resonance</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Fu, Xiangrong; Gary, Stephen Peter; Reeves, Geoffrey D.; ...</p> <p>2017-09-05</p> <p>Chorus in the inner magnetosphere has been <span class="hlt">observed</span> frequently at geomagnetically active times, typically exhibiting a two-<span class="hlt">band</span> structure with a quasi-parallel lower <span class="hlt">band</span> and an upper <span class="hlt">band</span> with a broad range of wave normal angles. But recent <span class="hlt">observations</span> by Van Allen Probes confirm another type of lower <span class="hlt">band</span> chorus, which has a large wave normal angle close to the resonance cone angle. It has been proposed that these waves could be generated by a low-energy beam-like electron component or by temperature anisotropy of keV electrons in the presence of a low-energy plateau-like electron component. This paper, however, presents an alternativemore » mechanism for generation of this highly oblique lower <span class="hlt">band</span> chorus. Through a nonlinear three-wave resonance, a quasi-parallel lower <span class="hlt">band</span> chorus wave can interact with a mildly oblique upper <span class="hlt">band</span> chorus wave, producing a highly oblique quasi-electrostatic lower <span class="hlt">band</span> chorus wave. This theoretical analysis is confirmed by 2-D electromagnetic particle-in-cell simulations. Furthermore, as the newly generated waves propagate away from the equator, their wave normal angle can further increase and they are able to scatter low-energy electrons to form a plateau-like structure in the parallel velocity distribution. As a result, the three-wave resonance mechanism may also explain the generation of quasi-parallel upper <span class="hlt">band</span> chorus which has also been <span class="hlt">observed</span> in the magnetosphere.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20150011873','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20150011873"><span>A Novel Ku-<span class="hlt">Band/Ka-Band</span> and Ka-<span class="hlt">Band/E-Band</span> Multimode Waveguide Couplers for Power Measurement of Traveling-Wave Tube Amplifier Harmonic Frequencies</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Wintucky, Edwin G.; Simons, Rainee N.</p> <p>2015-01-01</p> <p>This paper presents the design, fabrication and test results for a novel waveguide multimode directional coupler (MDC). The coupler, fabricated from two dissimilar frequency <span class="hlt">band</span> waveguides, is capable of isolating power at the second harmonic frequency from the fundamental power at the output port of a traveling-wave tube (TWT) amplifier. Test results from proof-of-concept demonstrations are presented for a Ku-<span class="hlt">band/Ka-band</span> MDC and a Ka-<span class="hlt">band/E-band</span> MDC. In addition to power measurements at harmonic frequencies, a potential application of the MDC is in the design of a satellite borne beacon source for atmospheric propagation studies at millimeter-wave (mm-wave) frequencies (Ka-<span class="hlt">band</span> and E-<span class="hlt">band</span>).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://elibrary.unm.edu/sora/JFO/v053n04/p0342-p0351.pdf','USGSPUBS'); return false;" href="http://elibrary.unm.edu/sora/JFO/v053n04/p0342-p0351.pdf"><span>Techniques for trapping, aging, and <span class="hlt">banding</span> wintering canvasbacks</span></a></p> <p><a target="_blank" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p>Haramis, G.M.; Derleth, E.L.; McAuley, D.G.</p> <p>1982-01-01</p> <p>Techniques used to trap, <span class="hlt">band</span>, and determine age of Canvasbacks during winter on Chesapeake Bay are presented. Canvasbacks were captured with welded-wire traps baited with corn. Two trap designs were used and traps and trapping techniques are described. Ducks were dipnetted from traps and held in modified poultry crates that provided seclusion and ventilation and allowed birds to dry unsoiled. Carney's (1964) wing plumage methodology was found most efficient in determining age of Canvasbacks during large-scale <span class="hlt">bandings</span>. This technique was rapid and was easily taught to inexperienced personnel. In contrast, the cloacal technique could be performed efficiently only by experienced and skillful banders. <span class="hlt">Band</span> wear was <span class="hlt">observed</span> to vary widely on individual birds and rounding of <span class="hlt">bands</span> was recognized as an important technique in extending <span class="hlt">band</span> life. <span class="hlt">Bands</span> were placed upside down on the tarsus so that wear along the upper edge would be less likely to destroy <span class="hlt">band</span> numbers. In 5 winter seasons, over 17,000 Canvasbacks were captured. Mortality rate for the program was .3%.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015RScI...86a4703N','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015RScI...86a4703N"><span>Development of an S-<span class="hlt">band</span> cavity-type beam <span class="hlt">position</span> monitor for a high power THz free-electron laser</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Noh, Seon Yeong; Kim, Eun-San; Hwang, Ji-Gwang; Heo, A.; won Jang, Si; Vinokurov, Nikolay A.; Jeong, Young UK; Hee Park, Seong; Jang, Kyu-Ha</p> <p>2015-01-01</p> <p>A cavity-type beam <span class="hlt">position</span> monitor (BPM) has been developed for a compact terahertz (THz) free-electron laser (FEL) system and ultra-short pulsed electron Linac system at the Korea Atomic Energy Research Institute (KAERI). Compared with other types of BPMs, the cavity-type BPM has higher sensitivity and faster response time even at low charge levels. When electron beam passes through the cavity-type BPM, it excites the dipole mode of the cavity of which amplitude depends linearly on the beam offset from the center of the cavity. Signals from the BPM were measured as a function of the beam offset by using an oscilloscope. The microtron accelerator for the KAERI THz FEL produces the electron beam with an energy of 6.5 MeV and pulse length of 5 μs with a micropulse of 10-20 ps at the frequency of 2.801 GHz. The macropulse beam current is 40 mA. Because the microtron provides multi-bunch system, output signal would be the superposition of each single bunch. So high output signal can be obtained from superposition of each single bunch. The designed <span class="hlt">position</span> resolution of the cavity-type BPM in multi-bunch is submicron. Our cavity-type BPM is made of aluminum and vacuum can be maintained by indium sealing without brazing process, resulting in easy modification and cost saving. The resonance frequency of the cavity-type BPM is 2.803 GHz and the cavity-type BPM dimensions are 200 × 220 mm (length × height) with a pipe diameter of 38 mm. The measured <span class="hlt">position</span> sensitivity was 6.19 (mV/mm)/mA and the measured isolation between the X and Y axis was -39 dB. By measuring the thermal noise of system, <span class="hlt">position</span> resolution of the cavity-type BPM was estimated to be less than 1 μm. In this article, we present the test results of the S-<span class="hlt">band</span> cavity-type BPM and prove the feasibility of the beam <span class="hlt">position</span> measurement with high resolution using this device.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25638104','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25638104"><span>Development of an S-<span class="hlt">band</span> cavity-type beam <span class="hlt">position</span> monitor for a high power THz free-electron laser.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Noh, Seon Yeong; Kim, Eun-San; Hwang, Ji-Gwang; Heo, A; Jang, Si won; Vinokurov, Nikolay A; Jeong, Young U K; Park, Seong Hee; Jang, Kyu-Ha</p> <p>2015-01-01</p> <p>A cavity-type beam <span class="hlt">position</span> monitor (BPM) has been developed for a compact terahertz (THz) free-electron laser (FEL) system and ultra-short pulsed electron Linac system at the Korea Atomic Energy Research Institute (KAERI). Compared with other types of BPMs, the cavity-type BPM has higher sensitivity and faster response time even at low charge levels. When electron beam passes through the cavity-type BPM, it excites the dipole mode of the cavity of which amplitude depends linearly on the beam offset from the center of the cavity. Signals from the BPM were measured as a function of the beam offset by using an oscilloscope. The microtron accelerator for the KAERI THz FEL produces the electron beam with an energy of 6.5 MeV and pulse length of 5 μs with a micropulse of 10-20 ps at the frequency of 2.801 GHz. The macropulse beam current is 40 mA. Because the microtron provides multi-bunch system, output signal would be the superposition of each single bunch. So high output signal can be obtained from superposition of each single bunch. The designed <span class="hlt">position</span> resolution of the cavity-type BPM in multi-bunch is submicron. Our cavity-type BPM is made of aluminum and vacuum can be maintained by indium sealing without brazing process, resulting in easy modification and cost saving. The resonance frequency of the cavity-type BPM is 2.803 GHz and the cavity-type BPM dimensions are 200 × 220 mm (length × height) with a pipe diameter of 38 mm. The measured <span class="hlt">position</span> sensitivity was 6.19 (mV/mm)/mA and the measured isolation between the X and Y axis was -39 dB. By measuring the thermal noise of system, <span class="hlt">position</span> resolution of the cavity-type BPM was estimated to be less than 1 μm. In this article, we present the test results of the S-<span class="hlt">band</span> cavity-type BPM and prove the feasibility of the beam <span class="hlt">position</span> measurement with high resolution using this device.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22392327-development-band-cavity-type-beam-position-monitor-high-power-thz-free-electron-laser','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22392327-development-band-cavity-type-beam-position-monitor-high-power-thz-free-electron-laser"><span>Development of an S-<span class="hlt">band</span> cavity-type beam <span class="hlt">position</span> monitor for a high power THz free-electron laser</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Noh, Seon Yeong; Kim, Eun-San, E-mail: eskim1@knu.ac.kr; Hwang, Ji-Gwang</p> <p>2015-01-15</p> <p>A cavity-type beam <span class="hlt">position</span> monitor (BPM) has been developed for a compact terahertz (THz) free-electron laser (FEL) system and ultra-short pulsed electron Linac system at the Korea Atomic Energy Research Institute (KAERI). Compared with other types of BPMs, the cavity-type BPM has higher sensitivity and faster response time even at low charge levels. When electron beam passes through the cavity-type BPM, it excites the dipole mode of the cavity of which amplitude depends linearly on the beam offset from the center of the cavity. Signals from the BPM were measured as a function of the beam offset by using anmore » oscilloscope. The microtron accelerator for the KAERI THz FEL produces the electron beam with an energy of 6.5 MeV and pulse length of 5 μs with a micropulse of 10-20 ps at the frequency of 2.801 GHz. The macropulse beam current is 40 mA. Because the microtron provides multi-bunch system, output signal would be the superposition of each single bunch. So high output signal can be obtained from superposition of each single bunch. The designed <span class="hlt">position</span> resolution of the cavity-type BPM in multi-bunch is submicron. Our cavity-type BPM is made of aluminum and vacuum can be maintained by indium sealing without brazing process, resulting in easy modification and cost saving. The resonance frequency of the cavity-type BPM is 2.803 GHz and the cavity-type BPM dimensions are 200 × 220 mm (length × height) with a pipe diameter of 38 mm. The measured <span class="hlt">position</span> sensitivity was 6.19 (mV/mm)/mA and the measured isolation between the X and Y axis was −39 dB. By measuring the thermal noise of system, <span class="hlt">position</span> resolution of the cavity-type BPM was estimated to be less than 1 μm. In this article, we present the test results of the S-<span class="hlt">band</span> cavity-type BPM and prove the feasibility of the beam <span class="hlt">position</span> measurement with high resolution using this device.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5025745','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5025745"><span>Madelung and Hubbard interactions in polaron <span class="hlt">band</span> model of doped organic semiconductors</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Png, Rui-Qi; Ang, Mervin C.Y.; Teo, Meng-How; Choo, Kim-Kian; Tang, Cindy Guanyu; Belaineh, Dagmawi; Chua, Lay-Lay; Ho, Peter K.H.</p> <p>2016-01-01</p> <p>The standard polaron <span class="hlt">band</span> model of doped organic semiconductors predicts that density-of-states shift into the π–π* gap to give a partially filled polaron <span class="hlt">band</span> that pins the Fermi level. This picture neglects both Madelung and Hubbard interactions. Here we show using ultrahigh workfunction hole-doped model triarylamine–fluorene copolymers that Hubbard interaction strongly splits the singly-occupied molecular orbital from its empty counterpart, while Madelung (Coulomb) interactions with counter-anions and other carriers markedly shift energies of the frontier orbitals. These interactions lower the singly-occupied molecular orbital <span class="hlt">band</span> below the valence <span class="hlt">band</span> edge and give rise to an empty low-lying counterpart <span class="hlt">band</span>. The Fermi level, and hence workfunction, is determined by conjunction of the bottom edge of this empty <span class="hlt">band</span> and the top edge of the valence <span class="hlt">band</span>. Calculations are consistent with the <span class="hlt">observed</span> Fermi-level downshift with counter-anion size and the <span class="hlt">observed</span> dependence of workfunction on doping level in the strongly doped regime. PMID:27582355</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27376841','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27376841"><span><span class="hlt">Band</span> gap in tubular pillar phononic crystal plate.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Shu, Fengfeng; Liu, Yongshun; Wu, Junfeng; Wu, Yihui</p> <p>2016-09-01</p> <p>In this paper, a phononic crystal (PC) plate with tubular pillars is presented and investigated. The <span class="hlt">band</span> structures and mode displacement profiles are calculated by using finite element method. The result shows that a complete <span class="hlt">band</span> gap opens when the ratio of the pillar height to the plate thickness is about 1.6. However, for classic cylinder pillar structures, a <span class="hlt">band</span> gap opens when the ratio is equal or greater than 3. A tubular pillar design with a void room in it enhances acoustic multiple scattering and gives rise to the opening of the <span class="hlt">band</span> gap. In order to verify it, a PC structure with double tubular pillars different in size (one within the other) is introduced and a more than 2times <span class="hlt">band</span> gap enlargement is <span class="hlt">observed</span>. Furthermore, the coupling between the resonant mode and the plate mode around the <span class="hlt">band</span> gap is characterized, as well as the effect of the geometrical parameters on the <span class="hlt">band</span> gap. The behavior of such structure could be utilized to design a pillar PC with stronger structural stability and to enlarge <span class="hlt">band</span> gaps. Copyright © 2016 Elsevier B.V. All rights reserved.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27386331','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27386331"><span>Compact filtering monopole patch antenna with dual-<span class="hlt">band</span> rejection.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Kim, Sun-Woong; Choi, Dong-You</p> <p>2016-01-01</p> <p>In this paper, a compact ultra-wideband patch antenna with dual-<span class="hlt">band</span> rejection is proposed. The proposed antenna filters 3.3-3.8 GHz WiMAX and 5.15-5.85 GHz WLAN by respectively rejecting these <span class="hlt">bands</span> through a C-shaped slit and a λg/4 resonator. The λg/4 resonator is <span class="hlt">positioned</span> as a pair, centered around the microstrip line, and a C-type slit is inserted into an elliptical patch. The impedance bandwidth of the proposed antenna is 2.9-9.3 GHz, which satisfies the bandwidth for ultra-wideband communication systems. Further, the proposed antenna provides dual-<span class="hlt">band</span> rejection at two <span class="hlt">bands</span>: 3.2-3.85 and 4.7-6.03 GHz. The radiation pattern of the antenna is omnidirectional, and antenna gain is maintained constantly while showing -8.4 and -1.5 dBi at the two rejected <span class="hlt">bands</span>, respectively.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li class="active"><span>18</span></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_18 --> <div id="page_19" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li class="active"><span>19</span></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="361"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2009JPhD...42h5110O','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2009JPhD...42h5110O"><span>Electronic transport properties of Ti-impurity <span class="hlt">band</span> in Si</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Olea, J.; González-Díaz, G.; Pastor, D.; Mártil, I.</p> <p>2009-04-01</p> <p>In this paper we show that pulsed laser melted high dose implantation of Ti in Si, above the Mott transition, produces an impurity <span class="hlt">band</span> (IB) in this semiconductor. Using the van der Pauw method and Hall effect measurements we find strong laminated conductivity at the implanted layer and a temperature dependent decoupling between the Ti implanted layer (TIL) and the substrate. The conduction mechanism from the TIL to the substrate shows blocking characteristics that could be well explained through IB theory. Using the ATLAS code we can estimate the energetic <span class="hlt">position</span> of the IB at 0.36 eV from the conduction <span class="hlt">band</span>, the density of holes in this <span class="hlt">band</span> which is closely related to the Ti atomic density and the hole mobility in this <span class="hlt">band</span>. <span class="hlt">Band</span> diagrams of the structure at low and high temperatures are also simulated in the ATLAS framework. The simulation obtained is fully coherent with experimental results.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28256467','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28256467"><span>Antibacterial nanosilver coated orthodontic <span class="hlt">bands</span> with potential implications in dentistry.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Prabha, Rahul Damodaran; Kandasamy, Rajasigamani; Sivaraman, U Sajeev; Nandkumar, Maya A; Nair, Prabha D</p> <p>2016-10-01</p> <p>Fixed orthodontic treatment, an indispensable procedure in orthodontics, necessitates insertion of dental <span class="hlt">bands</span>. Insertion of <span class="hlt">band</span> material could also introduce a site of plaque retention. It was hypothesized that <span class="hlt">band</span> materials with slow-release antimicrobial properties could help in sustained infection control, prevention of dental plaque formation and further associated health risks. Considering the known antimicrobial proprieties of silver, a coating of silver nanoparticle (SNP) onto the stainless steel <span class="hlt">bands</span> was done and characterized for its beneficial properties in the prevention of plaque accumulation. Coatings of SNPs on conventional stainless steel dental <span class="hlt">bands</span> were prepared using thermal evaporation technology. The coated dental <span class="hlt">bands</span> were characterized for their physicochemical properties and evaluated for antimicrobial activity and biocompatibility. The physiochemical characterization of <span class="hlt">band</span> material both coated and uncoated was carried out using scanning electron microscope, energy dispersive spectroscopy, atomic force microscopyand contact angle test. Biocompatibility tests for coated <span class="hlt">band</span> material were carried using L929 mouse fibroblast cell culture and MTT [3-(4, 5-dimethyl thiazol-2-yl)-2, 5-diphenyl tetrazolium bromide] assay. Antimicrobial activity of coated <span class="hlt">band</span> material against Gram-<span class="hlt">positive</span> bacteria was tested. A stable and uniform coating of SNPs was obtained. The coated <span class="hlt">band</span> materials were biocompatible as well as possessed distinct antimicrobial activity. The SNP coated dental <span class="hlt">bands</span> could be potential antimicrobial dental <span class="hlt">bands</span> for future clinical use. Further studies need to be done to validate the efficiency of coated <span class="hlt">band</span> materials in oral environments.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010EGUGA..12.1743D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010EGUGA..12.1743D"><span>Compaction <span class="hlt">bands</span> in porous rocks: localization analysis using breakage mechanics</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Das, Arghya; Nguyen, Giang; Einav, Itai</p> <p>2010-05-01</p> <p> sensitive to the state of the matter (e.g. the initial porosity and grain size distribution). In our previous work (Nguyen and Einav, 2009) we showed that the breakage mechanics model is capable of capturing the experimentally <span class="hlt">observed</span> stress-strain behaviour of sandstones under conventional triaxial loading, along with the associated evolving grain size distribution. Here, these predictions are further improved through the inclusion of the additional pore-collapse parameter. Furthermore, localization analysis that is based on the loss of <span class="hlt">positive</span> definiteness of the determinant of the acoustic tensor (Issen and Rudnicki, 2000) is performed to determine the onset of compaction localization, as an indication of material failure. This analysis results in the prediction of the possible range of compaction <span class="hlt">band</span> orientations. The behaviour and onset of compaction localization of different sandstones are numerically predicted in well accordance with published experimental <span class="hlt">observations</span>. A parametric study is also carried out to emphasize the complementary effects of grain crushing and pore-collapse on the formation of compaction <span class="hlt">bands</span>. References Einav, I. (2007a), Breakage mechanics-Part I: Theory, J. Mechan. Phys. Sol. 55(6), 1274-1297. Einav, I. (2007b), Breakage mechanics-Part II: Modelling granular materials, J. Mech. Phys. Sol. 55(6), 1298- 1320. Issen, K.A., Rudnicki, J.W. (2000), Conditions for compaction <span class="hlt">bands</span> in porous rocks, J. Geophys. Res. Lett., 105, 21,529-21,536. Mollema, P.N., Antonellini, M.A. (1996), Compaction <span class="hlt">bands</span>: a structural analog for anti-mode I cracks in aeolian sandstone, Tectonophysics 267:209-228. Nguyen, G.D., Einav, I. (2009), The energetics of cataclasis based on breakage mechanics, Pure Appl. Geophys., 166(10), 1693 - 1724. Wong, T-F, Baud, P., Klein, E. (2001), Localized failure modes in a compactant porous rock, J. Geophys. Res. Lett., 28, 2521-2524.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017NuPhA.968...48J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017NuPhA.968...48J"><span>Intrinsic properties of high-spin <span class="hlt">band</span> structures in triaxial nuclei</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jehangir, S.; Bhat, G. H.; Sheikh, J. A.; Palit, R.; Ganai, P. A.</p> <p>2017-12-01</p> <p>The <span class="hlt">band</span> structures of 68,70Ge, 128,130,132,134Ce and 132,134,136,138Nd are investigated using the triaxial projected shell model (TPSM) approach. These nuclei depict forking of the ground-state <span class="hlt">band</span> into several s-<span class="hlt">bands</span> and in some cases, both the lowest two <span class="hlt">observed</span> s-<span class="hlt">bands</span> depict neutron or proton character. It was discussed in our earlier work that this anomalous behaviour can be explained by considering γ-<span class="hlt">bands</span> based on two-quasiparticle configurations. As the parent <span class="hlt">band</span> and the γ-<span class="hlt">band</span> built on it have the same intrinsic structure, g-factors of the two <span class="hlt">bands</span> are expected to be similar. In the present work, we have undertaken a detailed investigation of g-factors for the excited <span class="hlt">band</span> structures of the studied nuclei and the available data for a few high-spin states are shown to be in fair agreement with the predicted values.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010IEITC..93.1993S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010IEITC..93.1993S"><span>Multi-<span class="hlt">Band</span> Received Signal Strength Fingerprinting Based Indoor Location System</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sertthin, Chinnapat; Fujii, Takeo; Ohtsuki, Tomoaki; Nakagawa, Masao</p> <p></p> <p>This paper proposes a new multi-<span class="hlt">band</span> received signal strength (MRSS) fingerprinting based indoor location system, which employs the frequency diversity on the conventional single-<span class="hlt">band</span> received signal strength (RSS) fingerprinting based indoor location system. In the proposed system, the impacts of frequency diversity on the enhancements of <span class="hlt">positioning</span> accuracy are analyzed. Effectiveness of the proposed system is proved by experimental approach, which was conducted in non line-of-sight (NLOS) environment under the area of 103m2 at Yagami Campus, Keio University. WLAN access points, which simultaneously transmit dual-<span class="hlt">band</span> signal of 2.4 and 5.2GHz, are utilized as transmitters. Likewise, a dual-<span class="hlt">band</span> WLAN receiver is utilized as a receiver. Signal distances calculated by both Manhattan and Euclidean were classified by K-Nearest Neighbor (KNN) classifier to illustrate the performance of the proposed system. The results confirmed that Frequency diversity attributions of multi-<span class="hlt">band</span> signal provide accuracy improvement over 50% of the conventional single-<span class="hlt">band</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015AGUFMSA31D2360L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015AGUFMSA31D2360L"><span>Aurora Activities <span class="hlt">Observed</span> by SNPP VIIRS Day-Night <span class="hlt">Band</span> during St. Patrick's Day, 2015 G4 Level Geomagnetic Storm</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Liu, T. C.; Shao, X.; Cao, C.; Zhang, B.; Fung, S. F.; Sharma, S.</p> <p>2015-12-01</p> <p>A G4 level (severe) geomagnetic storm occurred on March 17 (St. Patrick's Day), 2015 and it is among the strongest geomagnetic storms of the current solar cycle (Solar Cycle 24). The storm is identified as due to the Coronal Mass Ejections (CMEs) which erupted on March 15 from Region 2297 of solar surface. During this event, the geomagnetic storm index Dst reached -223 nT and the geomagnetic aurora electrojet (AE) index increased and reached as high as >2200 nT with large amplitude fluctuations. Aurora occurred in both hemispheres. Ground auroral sightings were reported from Michigan to Alaska and as far south as southern Colorado. The Day Night <span class="hlt">Band</span> (DNB) of the Visible Infrared Imaging Radiometer Suite (VIIRS) onboard Suomi-NPP represents a major advancement in night time imaging capabilities. The DNB senses radiance that can span 7 orders of magnitude in one panchromatic (0.5-0.9 μm) reflective solar <span class="hlt">band</span> and provides imagery of clouds and other Earth features over illumination levels ranging from full sunlight to quarter moon. In this paper, DNB <span class="hlt">observations</span> of aurora activities during the St. Patrick's Day geomagnetic storm are analyzed. Aurora are <span class="hlt">observed</span> to evolve with salient features by DNB for orbital pass on the night side (~local time 1:30am) in both hemispheres. The radiance data from DNB <span class="hlt">observation</span> are collected at the night sides of southern and northern hemispheres and geo-located onto geomagnetic local time (MLT) coordinates. Regions of aurora during each orbital pass are identified through image processing by contouring radiance values and excluding regions with stray light near day-night terminator. The evolution of aurora are characterized with time series of the poleward and low latitude boundary of aurora, their latitude-span and area, peak radiance and total light emission of the aurora region in DNB <span class="hlt">observation</span>. These characteristic parameters are correlated with solar wind and geomagnetic index parameters.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018AtmRe.201..116L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018AtmRe.201..116L"><span>Intercomparison of attenuation correction algorithms for single-polarized X-<span class="hlt">band</span> radars</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Lengfeld, K.; Berenguer, M.; Sempere Torres, D.</p> <p>2018-03-01</p> <p>Attenuation due to liquid water is one of the largest uncertainties in radar <span class="hlt">observations</span>. The effects of attenuation are generally inversely proportional to the wavelength, i.e. <span class="hlt">observations</span> from X-<span class="hlt">band</span> radars are more affected by attenuation than those from C- or S-<span class="hlt">band</span> systems. On the other hand, X-<span class="hlt">band</span> radars can measure precipitation fields in higher temporal and spatial resolution and are more mobile and easier to install due to smaller antennas. A first algorithm for attenuation correction in single-polarized systems was proposed by Hitschfeld and Bordan (1954) (HB), but it gets unstable in case of small errors (e.g. in the radar calibration) and strong attenuation. Therefore, methods have been developed that restrict attenuation correction to keep the algorithm stable, using e.g. surface echoes (for space-borne radars) and mountain returns (for ground radars) as a final value (FV), or adjustment of the radar constant (C) or the coefficient α. In the absence of mountain returns, measurements from C- or S-<span class="hlt">band</span> radars can be used to constrain the correction. All these methods are based on the statistical relation between reflectivity and specific attenuation. Another way to correct for attenuation in X-<span class="hlt">band</span> radar <span class="hlt">observations</span> is to use additional information from less attenuated radar systems, e.g. the ratio between X-<span class="hlt">band</span> and C- or S-<span class="hlt">band</span> radar measurements. Lengfeld et al. (2016) proposed such a method based isotonic regression of the ratio between X- and C-<span class="hlt">band</span> radar <span class="hlt">observations</span> along the radar beam. This study presents a comparison of the original HB algorithm and three algorithms based on the statistical relation between reflectivity and specific attenuation as well as two methods implementing additional information of C-<span class="hlt">band</span> radar measurements. Their performance in two precipitation events (one mainly convective and the other one stratiform) shows that a restriction of the HB is necessary to avoid instabilities. A comparison with vertically pointing</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20170002526','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20170002526"><span>Second Epoch VLBA Calibrator Survey <span class="hlt">Observations</span> - VCS-II</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Gordon, David; Jacobs, Christopher; Beasley, Anthony; Peck, Alison; Gaume, Ralph; Charlot, Patrick; Fey, Alan; Ma, Chopo; Titov, Oleg; Boboltz, David</p> <p>2016-01-01</p> <p>Six very successful VLBA calibrator survey campaigns were run between 1994 and 2007 to build up a large list of compact radio sources with <span class="hlt">positions</span> precise enough for use as VLBI phase reference calibrators. We report on the results of a second epoch VLBA Calibrator Survey campaign (VCS-II) in which 2400 VCS sources were re-<span class="hlt">observed</span> at X and S <span class="hlt">bands</span> in order to improve the upcoming third realization of the International Celestial Reference Frame (ICRF3) as well as to improve their usefulness as VLBI phase reference calibrators. In this survey, some 2062 previously detected sources and 324 previously undetected sources were detected and revised <span class="hlt">positions</span> are presented. Average <span class="hlt">position</span> uncertainties for the reobserved sources were reduced from 1.14 and 1.98 mas to 0.24 and 0.41 mas in RA and Declination, respectively, or by nearly a factor of 5. Minimum detected flux values were approximately 15 and 28 mJy in X and S <span class="hlt">bands</span>, respectively, and median total fluxes are approximately 230 and 280 mJy. The vast majority of these sources are flat-spectrum sources, with approximately 82% having spectral indices greater than -0.5.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19940028802','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19940028802"><span>Two-axis antenna <span class="hlt">positioning</span> mechanism</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Herald, Michelle; Wai, Leilani C.</p> <p>1994-01-01</p> <p>The two-axis antenna <span class="hlt">positioning</span> mechanism (TAAPM) is used to <span class="hlt">position</span> three Ku-<span class="hlt">band</span> and one C-<span class="hlt">band</span> spot antennas on the INTELSAT 7 (I-7) spacecraft, which is a commercial telecommunications satellite purchased and operated by INTELSAT, an international consortium. The first I-7 was successfully launched on 22 Oct. 1993 from French Guiana on an Ariane launch vehicle. The TAAPM's on the first I-7 satellite successfully completed their in-orbit functional testing. The TAAPM was an entirely new design for Space Systems/Loral. This paper will describe the spacecraft/system requirements and application of the TAAPM and present the technical findings of TAAPM qualification and protoflight testing.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24783945','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24783945"><span>Direct imaging of <span class="hlt">band</span> profile in single layer MoS2 on graphite: quasiparticle energy gap, metallic edge states, and edge <span class="hlt">band</span> bending.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Zhang, Chendong; Johnson, Amber; Hsu, Chang-Lung; Li, Lain-Jong; Shih, Chih-Kang</p> <p>2014-05-14</p> <p>Using scanning tunneling microscopy and spectroscopy, we probe the electronic structures of single layer MoS2 on graphite. The apparent quasiparticle energy gap of single layer MoS2 is measured to be 2.15 ± 0.06 eV at 77 K, albeit a higher second conduction <span class="hlt">band</span> threshold at 0.2 eV above the apparent conduction <span class="hlt">band</span> minimum is also <span class="hlt">observed</span>. Combining it with photoluminescence studies, we deduce an exciton binding energy of 0.22 ± 0.1 eV (or 0.42 eV if the second threshold is use), a value that is lower than current theoretical predictions. Consistent with theoretical predictions, we directly <span class="hlt">observe</span> metallic edge states of single layer MoS2. In the bulk region of MoS2, the Fermi level is located at 1.8 eV above the valence <span class="hlt">band</span> maximum, possibly due to the formation of a graphite/MoS2 heterojunction. At the edge, however, we <span class="hlt">observe</span> an upward <span class="hlt">band</span> bending of 0.6 eV within a short depletion length of about 5 nm, analogous to the phenomena of Fermi level pinning of a 3D semiconductor by metallic surface states.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014Nanos...6.6531W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014Nanos...6.6531W"><span>2D XANES-XEOL mapping: <span class="hlt">observation</span> of enhanced <span class="hlt">band</span> gap emission from ZnO nanowire arrays</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wang, Zhiqiang; Guo, Xiaoxuan; Sham, Tsun-Kong</p> <p>2014-05-01</p> <p>Using 2D XANES-XEOL spectroscopy, it is found that the <span class="hlt">band</span> gap emission of ZnO nanowire arrays is substantially enhanced i.e. that the intensity ratio between the <span class="hlt">band</span> gap and defect emissions increases by more than an order of magnitude when the excitation energy is scanned across the O K-edge. Possible mechanisms are discussed.Using 2D XANES-XEOL spectroscopy, it is found that the <span class="hlt">band</span> gap emission of ZnO nanowire arrays is substantially enhanced i.e. that the intensity ratio between the <span class="hlt">band</span> gap and defect emissions increases by more than an order of magnitude when the excitation energy is scanned across the O K-edge. Possible mechanisms are discussed. Electronic supplementary information (ESI) available: XEOL spectra with different excitation energies. X-ray attenuation length vs. photon energy. Details of surface defects in ZnO NWs. The second O K-edge and Zn L-edge 2D XANES-XEOL maps. Comparison of the first and second TEY at O K-edge and Zn L-edge scans, respectively. Raman spectra of the ZnO NWs with different IBGE/IDE ratios. See DOI: 10.1039/c4nr01049c</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017SPIE10402E..0NS','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017SPIE10402E..0NS"><span>Crosstalk effect and its mitigation in Aqua MODIS middle wave infrared <span class="hlt">bands</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sun, Junqiang; Madhavan, Sriharsha; Wang, Menghua</p> <p>2017-09-01</p> <p>The MODerate-resolution Imaging Spectroradiometer (MODIS) is one of the primary instruments in the National Aeronautics and Space Administration (NASA) Earth <span class="hlt">Observing</span> System (EOS). The first MODIS instrument was launched in December 1999 on-board the Terra spacecraft. A follow on MODIS was launched on an afternoon orbit in 2002 and is aboard the Aqua spacecraft. Both MODIS instruments are very akin, has 36 <span class="hlt">bands</span>, among which <span class="hlt">bands</span> 20 to 25 are Middle Wave Infrared (MWIR) <span class="hlt">bands</span> covering a wavelength range from approximately 3.750 μm to 4.515 μm. It was found that there was severe contamination in these <span class="hlt">bands</span> early in mission but the effect has not been characterized and mitigated at the time. The crosstalk effect induces strong striping in the Earth View (EV) images and causes significant retrieval errors in the EV Brightness Temperature (BT) in these <span class="hlt">bands</span>. An algorithm using a linear approximation derived from on-orbit lunar <span class="hlt">observations</span> has been developed to correct the crosstalk effect and successfully applied to mitigate the effect in both Terra and Aqua MODIS Long Wave Infrared (LWIR) Photovoltaic (PV) <span class="hlt">bands</span>. In this paper, the crosstalk effect in the Aqua MWIR <span class="hlt">bands</span> is investigated and characterized by deriving the crosstalk coefficients using the scheduled Aqua MODIS lunar <span class="hlt">observations</span> for the MWIR <span class="hlt">bands</span>. It is shown that there are strong crosstalk contaminations among the five MWIR <span class="hlt">bands</span> and they also have significant crosstalk contaminations from Short Wave Infrared (SWIR) <span class="hlt">bands</span>. The crosstalk correction algorithm previously developed is applied to correct the crosstalk effect in these <span class="hlt">bands</span>. It is demonstrated that the crosstalk correction successfully reduces the striping in the EV images and improves the accuracy of the EV BT in the five <span class="hlt">bands</span> as was done similarly for LWIR PV <span class="hlt">bands</span>. The crosstalk correction algorithm should thus be applied to improve both the image quality and radiometric accuracy of the Aqua MODIS MWIR <span class="hlt">bands</span> Level 1B (L1B) products.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/19257619','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/19257619"><span><span class="hlt">Band</span>-selective filter in a zigzag graphene nanoribbon.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Nakabayashi, Jun; Yamamoto, Daisuke; Kurihara, Susumu</p> <p>2009-02-13</p> <p>Electric transport of a zigzag graphene nanoribbon through a steplike potential and a barrier potential is investigated by using the recursive Green's function method. In the case of the steplike potential, we demonstrate numerically that scattering processes obey a selection rule for the <span class="hlt">band</span> indices when the number of zigzag chains is even; the electrons belonging to the "even" ("odd") <span class="hlt">bands</span> are scattered only into the even (odd) <span class="hlt">bands</span> so that the parity of the wave functions is preserved. In the case of the barrier potential, by tuning the barrier height to be an appropriate value, we show that it can work as the "<span class="hlt">band</span>-selective filter", which transmits electrons selectively with respect to the indices of the <span class="hlt">bands</span> to which the incident electrons belong. Finally, we suggest that this selection rule can be <span class="hlt">observed</span> in the conductance by applying two barrier potentials.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4839723','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4839723"><span>Oxygen Isotope Variability within Nautilus Shell Growth <span class="hlt">Bands</span></span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p></p> <p>2016-01-01</p> <p>Nautilus is often used as an analogue for the ecology and behavior of extinct externally shelled cephalopods. Nautilus shell grows quickly, has internal growth <span class="hlt">banding</span>, and is widely believed to precipitate aragonite in oxygen isotope equilibrium with seawater. Pieces of shell from a wild-caught Nautilus macromphalus from New Caledonia and from a Nautilus belauensis reared in an aquarium were cast in epoxy, polished, and then imaged. Growth <span class="hlt">bands</span> were visible in the outer prismatic layer of both shells. The thicknesses of the <span class="hlt">bands</span> are consistent with previously reported daily growth rates measured in aquarium reared individuals. In situ analysis of oxygen isotope ratios using secondary ion mass spectrometry (SIMS) with 10 μm beam-spot size reveals inter- and intra-<span class="hlt">band</span> δ18O variation. In the wild-caught sample, a traverse crosscutting 45 growth <span class="hlt">bands</span> yielded δ18O values ranging 2.5‰, from +0.9 to -1.6 ‰ (VPDB), a range that is larger than that <span class="hlt">observed</span> in many serial sampling of entire shells by conventional methods. The maximum range within a single <span class="hlt">band</span> (~32 μm) was 1.5‰, and 27 out of 41 <span class="hlt">bands</span> had a range larger than instrumental precision (±2 SD = 0.6‰). The results from the wild individual suggest depth migration is recorded by the shell, but are not consistent with a simple sinusoidal, diurnal depth change pattern. To create the <span class="hlt">observed</span> range of δ18O, however, this Nautilus must have traversed a temperature gradient of at least ~12°C, corresponding to approximately 400 m depth change. Isotopic variation was also measured in the aquarium-reared sample, but the pattern within and between <span class="hlt">bands</span> likely reflects evaporative enrichment arising from a weekly cycle of refill and replacement of the aquarium water. Overall, this work suggests that depth migration behavior in ancient nektonic mollusks could be elucidated by SIMS analysis across individual growth <span class="hlt">bands</span>. PMID:27100183</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1346602-oxygen-isotope-variability-within-nautilus-shell-growth-bands','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1346602-oxygen-isotope-variability-within-nautilus-shell-growth-bands"><span>Oxygen isotope variability within Nautilus shell growth <span class="hlt">bands</span></span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Linzmeier, Benjamin J.; Kozdon, Reinhard; Peters, Shanan E.; ...</p> <p>2016-04-21</p> <p>Nautilus is often used as an analogue for the ecology and behavior of extinct externally shelled cephalopods. Nautilus shell grows quickly, has internal growth <span class="hlt">banding</span>, and is widely believed to precipitate aragonite in oxygen isotope equilibrium with seawater. Pieces of shell from a wild-caught Nautilus macromphalus from New Caledonia and from a Nautilus belauensis reared in an aquarium were cast in epoxy, polished, and then imaged. Growth <span class="hlt">bands</span> were visible in the outer prismatic layer of both shells. The thicknesses of the <span class="hlt">bands</span> are consistent with previously reported daily growth rates measured in aquarium reared individuals. In situ analysis ofmore » oxygen isotope ratios using secondary ion mass spectrometry (SIMS) with 10 μm beam-spot size reveals inter- and intra-<span class="hlt">band</span> δ 18O variation. In the wild-caught sample, a traverse crosscutting 45 growth <span class="hlt">bands</span> yielded δ 18O values ranging 2.5‰, from +0.9 to -1.6 ‰ (VPDB), a range that is larger than that <span class="hlt">observed</span> in many serial sampling of entire shells by conventional methods. The maximum range within a single <span class="hlt">band</span> (~32 μm) was 1.5‰, and 27 out of 41 <span class="hlt">bands</span> had a range larger than instrumental precision (±2 SD = 0.6‰). The results from the wild individual suggest depth migration is recorded by the shell, but are not consistent with a simple sinusoidal, diurnal depth change pattern. In addition, to create the <span class="hlt">observed</span> range of δ 18O, however, this Nautilus must have traversed a temperature gradient of at least ~12°C, corresponding to approximately 400 m depth change. Isotopic variation was also measured in the aquarium-reared sample, but the pattern within and between <span class="hlt">bands</span> likely reflects evaporative enrichment arising from a weekly cycle of refill and replacement of the aquarium water. Overall, this work suggests that depth migration behavior in ancient nektonic mollusks could be elucidated by SIMS analysis across individual growth <span class="hlt">bands</span>.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017CEAS....9..531V','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017CEAS....9..531V"><span>Ka-<span class="hlt">band</span> to L-<span class="hlt">band</span> frequency down-conversion based on III-V-on-silicon photonic integrated circuits</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Van Gasse, K.; Wang, Z.; Uvin, S.; De Deckere, B.; Mariën, J.; Thomassen, L.; Roelkens, G.</p> <p>2017-12-01</p> <p>In this work, we present the design, simulation and characterization of a frequency down-converter based on III-V-on-silicon photonic integrated circuit technology. We first demonstrate the concept using commercial discrete components, after which we demonstrate frequency conversion using an integrated mode-locked laser and integrated modulator. In our experiments, five channels in the Ka-<span class="hlt">band</span> (27.5-30 GHz) with 500 MHz bandwidth are down-converted to the L-<span class="hlt">band</span> (1.5 GHz). The breadboard demonstration shows a conversion efficiency of - 20 dB and a flat response over the 500 MHz bandwidth. The simulation of a fully integrated circuit indicates that a <span class="hlt">positive</span> conversion gain can be obtained on a millimeter-sized photonic integrated circuit.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/21455104-near-infrared-thermal-emission-from-tres-ks-band-detection-band-upper-limit-depth-secondary-eclipse','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/21455104-near-infrared-thermal-emission-from-tres-ks-band-detection-band-upper-limit-depth-secondary-eclipse"><span>NEAR-INFRARED THERMAL EMISSION FROM TrES-3b: A Ks-<span class="hlt">BAND</span> DETECTION AND AN H-<span class="hlt">BAND</span> UPPER LIMIT ON THE DEPTH OF THE SECONDARY ECLIPSE</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Croll, Bryce; Jayawardhana, Ray; Fortney, Jonathan J.</p> <p>2010-08-01</p> <p>We present H- and Ks-<span class="hlt">band</span> photometry bracketing the secondary eclipse of the hot Jupiter TrES-3b using the Wide-field Infrared Camera on the Canada-France-Hawaii Telescope. We detect the secondary eclipse of TrES-3b with a depth of 0.133{sup +0.018}{sub -0.016}% in the Ks <span class="hlt">band</span> (8{sigma})-a result that is in sharp contrast to the eclipse depth reported by de Mooij and Snellen. We do not detect its thermal emission in the H <span class="hlt">band</span>, but place a 3{sigma} limit of 0.051% on the depth of the secondary eclipse in this <span class="hlt">band</span>. A secondary eclipse of this depth in Ks requires very efficient day-to-nightside redistributionmore » of heat and nearly isotropic reradiation, a conclusion that is in agreement with longer wavelength, mid-infrared Spitzer <span class="hlt">observations</span>. Our 3{sigma} upper limit on the depth of our H-<span class="hlt">band</span> secondary eclipse also argues for very efficient redistribution of heat and suggests that the atmospheric layer probed by these <span class="hlt">observations</span> may be well homogenized. However, our H-<span class="hlt">band</span> upper limit is so constraining that it suggests the possibility of a temperature inversion at depth, or an absorbing molecule, such as methane, that further depresses the emitted flux at this wavelength. The combination of our near-infrared measurements and those obtained with Spitzer suggests that TrES-3b displays a near-isothermal dayside atmospheric temperature structure, whose spectrum is well approximated by a blackbody. We emphasize that our strict H-<span class="hlt">band</span> limit is in stark disagreement with the best-fit atmospheric model that results from longer wavelength <span class="hlt">observations</span> only, thus highlighting the importance of near-infrared <span class="hlt">observations</span> at multiple wavelengths, in addition to those returned by Spitzer in the mid-infrared, to facilitate a comprehensive understanding of the energy budgets of transiting exoplanets.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28951053','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28951053"><span>Additional <span class="hlt">band</span> broadening of peptides in the first size-exclusion chromatographic dimension of an automated stop-flow two-dimensional high performance liquid chromatography.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Xu, Jucai; Sun-Waterhouse, Dongxiao; Qiu, Chaoying; Zhao, Mouming; Sun, Baoguo; Lin, Lianzhu; Su, Guowan</p> <p>2017-10-27</p> <p>The need to improve the peak capacity of liquid chromatography motivates the development of two-dimensional analysis systems. This paper presented a fully automated stop-flow two-dimensional liquid chromatography system with size exclusion chromatography followed by reversed phase liquid chromatography (SEC×RPLC) to efficiently separate peptides. The effects of different stop-flow operational parameters (stop-flow time, peak parking <span class="hlt">position</span>, number of stop-flow periods and column temperature) on <span class="hlt">band</span> broadening in the first dimension (1 st D) SEC column were quantitatively evaluated by using commercial small proteins and peptides. Results showed that the effects of peak parking <span class="hlt">position</span> and the number of stop-flow periods on <span class="hlt">band</span> broadening were relatively small. Unlike stop-flow analysis of large molecules with a long running time, additional <span class="hlt">band</span> broadening was evidently <span class="hlt">observed</span> for small molecule analytes due to the relatively high effective diffusion coefficient (D eff ). Therefore, shorter analysis time and lower 1 st D column temperature were suggested for analyzing small molecules. The stop-flow two-dimensional liquid chromatography (2D-LC) system was further tested on peanut peptides and an evidently improved resolution was <span class="hlt">observed</span> for both stop-flow heart-cutting and comprehensive 2D-LC analysis (in spite of additional <span class="hlt">band</span> broadening in SEC). The stop-flow SEC×RPLC, especially heart-cutting analysis with shorter analysis time and higher 1 st D resolution for selected fractions, offers a promising approach for efficient analysis of complex samples. Copyright © 2017 Elsevier B.V. All rights reserved.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/29740259','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/29740259"><span>Dilatancy induced ductile-brittle transition of shear <span class="hlt">band</span> in metallic glasses.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Zeng, F; Jiang, M Q; Dai, L H</p> <p>2018-04-01</p> <p>Dilatancy-generated structural disordering, an inherent feature of metallic glasses (MGs), has been widely accepted as the physical mechanism for the primary origin and structural evolution of shear <span class="hlt">banding</span>, as well as the resultant shear failure. However, it remains a great challenge to determine, to what degree of dilatation, a shear <span class="hlt">banding</span> will evolve into a runaway shear failure. In this work, using in situ acoustic emission monitoring, we probe the dilatancy evolution at the different stages of individual shear <span class="hlt">band</span> in MGs that underwent severely plastic deformation by the controlled cutting technology. A scaling law is revealed that the dilatancy in a shear <span class="hlt">band</span> is linearly related to its evolution degree. A transition from ductile-to-brittle shear <span class="hlt">bands</span> is <span class="hlt">observed</span>, where the formers dominate stable serrated flow, and the latter lead to a runaway instability (catastrophe failure) of serrated flow. To uncover the underlying mechanics, we develop a theoretical model of shear-<span class="hlt">band</span> evolution dynamics taking into account an atomic-scale deformation process. Our theoretical results agree with the experimental <span class="hlt">observations</span>, and demonstrate that the atomic-scale volume expansion arises from an intrinsic shear-<span class="hlt">band</span> evolution dynamics. Importantly, the onset of the ductile-brittle transition of shear <span class="hlt">banding</span> is controlled by a critical dilatation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018RSPSA.47470836Z','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018RSPSA.47470836Z"><span>Dilatancy induced ductile-brittle transition of shear <span class="hlt">band</span> in metallic glasses</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Zeng, F.; Jiang, M. Q.; Dai, L. H.</p> <p>2018-04-01</p> <p>Dilatancy-generated structural disordering, an inherent feature of metallic glasses (MGs), has been widely accepted as the physical mechanism for the primary origin and structural evolution of shear <span class="hlt">banding</span>, as well as the resultant shear failure. However, it remains a great challenge to determine, to what degree of dilatation, a shear <span class="hlt">banding</span> will evolve into a runaway shear failure. In this work, using in situ acoustic emission monitoring, we probe the dilatancy evolution at the different stages of individual shear <span class="hlt">band</span> in MGs that underwent severely plastic deformation by the controlled cutting technology. A scaling law is revealed that the dilatancy in a shear <span class="hlt">band</span> is linearly related to its evolution degree. A transition from ductile-to-brittle shear <span class="hlt">bands</span> is <span class="hlt">observed</span>, where the formers dominate stable serrated flow, and the latter lead to a runaway instability (catastrophe failure) of serrated flow. To uncover the underlying mechanics, we develop a theoretical model of shear-<span class="hlt">band</span> evolution dynamics taking into account an atomic-scale deformation process. Our theoretical results agree with the experimental <span class="hlt">observations</span>, and demonstrate that the atomic-scale volume expansion arises from an intrinsic shear-<span class="hlt">band</span> evolution dynamics. Importantly, the onset of the ductile-brittle transition of shear <span class="hlt">banding</span> is controlled by a critical dilatation.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li class="active"><span>19</span></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_19 --> <div id="page_20" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li class="active"><span>20</span></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="381"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018JAP...123k5701A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018JAP...123k5701A"><span>Heterostructures with diffused interfaces: Luminescent technique for ascertainment of <span class="hlt">band</span> alignment type</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Abramkin, D. S.; Gutakovskii, A. K.; Shamirzaev, T. S.</p> <p>2018-03-01</p> <p>The experimental ascertainment of <span class="hlt">band</span> alignment type for semiconductor heterostructures with diffused interfaces is discussed. A method based on the analysis of the spectral shift of photoluminescence (PL) <span class="hlt">band</span> with excitation density (Pex) that takes into account state filling and <span class="hlt">band</span> bending effects on the PL <span class="hlt">band</span> shift is developed. It is shown that the shift of PL <span class="hlt">band</span> maximum <span class="hlt">position</span> is proportional to ℏωmax ˜ (Ue + Uh).ln(Pex) + b.Pex1/3, where Ue (Uh) are electron (hole) Urbach energy tail, and parameter b characterizes the effect of <span class="hlt">band</span> bending or is equal to zero for heterostructures with type-II or type-I <span class="hlt">band</span> alignment, respectively. The method was approved with InAs/AlAs, GaAs/AlAs, GaSb/AlAs, and AlSb/AlAs heterostructures containing quantum wells.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5579558','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5579558"><span>Dual-<span class="hlt">Band</span> <span class="hlt">Band</span>-Pass Filter with Fixed Low <span class="hlt">Band</span> and Fluidically-Tunable High <span class="hlt">Band</span></span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Park, Eiyong; Lim, Daecheon</p> <p>2017-01-01</p> <p>In this work, we present a dual-<span class="hlt">band</span> <span class="hlt">band</span>-pass filter with fixed low-<span class="hlt">band</span> resonant frequency and tunable high-<span class="hlt">band</span> resonant frequency. The proposed filter consists of two split-ring resonators (SRRs) with a stub and microfluidic channels. The lower resonant frequency is determined by the length of the SRR alone, whereas the higher resonant frequency is determined by the lengths of the SRR and the stub. Using this characteristic, we fix the lower resonant frequency by fixing the SRR length and tune the higher resonant frequency by controlling the stub length by injecting liquid metal in the microfluidic channel. We fabricated the filter on a Duroid substrate. The microfluidic channel was made from polydimethylsiloxane (PDMS), and eutectic gallium–indium (EGaIn) was used as the liquid metal. This filter operates in two states—with, and without, the liquid metal. In the state without the liquid metal, the filter has resonant frequencies at 1.85 GHz and 3.06 GHz, with fractional bandwidths of 4.34% and 2.94%, respectively; and in the state with the liquid metal, it has resonant frequencies at 1.86 GHz and 2.98 GHz, with fractional bandwidths of 4.3% and 2.95%, respectively. PMID:28813001</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20140011182','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20140011182"><span>Uncertainty Quantification of GEOS-5 L-<span class="hlt">band</span> Radiative Transfer Model Parameters Using Bayesian Inference and SMOS <span class="hlt">Observations</span></span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>DeLannoy, Gabrielle J. M.; Reichle, Rolf H.; Vrugt, Jasper A.</p> <p>2013-01-01</p> <p>Uncertainties in L-<span class="hlt">band</span> (1.4 GHz) radiative transfer modeling (RTM) affect the simulation of brightness temperatures (Tb) over land and the inversion of satellite-<span class="hlt">observed</span> Tb into soil moisture retrievals. In particular, accurate estimates of the microwave soil roughness, vegetation opacity and scattering albedo for large-scale applications are difficult to obtain from field studies and often lack an uncertainty estimate. Here, a Markov Chain Monte Carlo (MCMC) simulation method is used to determine satellite-scale estimates of RTM parameters and their posterior uncertainty by minimizing the misfit between long-term averages and standard deviations of simulated and <span class="hlt">observed</span> Tb at a range of incidence angles, at horizontal and vertical polarization, and for morning and evening overpasses. Tb simulations are generated with the Goddard Earth <span class="hlt">Observing</span> System (GEOS-5) and confronted with Tb <span class="hlt">observations</span> from the Soil Moisture Ocean Salinity (SMOS) mission. The MCMC algorithm suggests that the relative uncertainty of the RTM parameter estimates is typically less than 25 of the maximum a posteriori density (MAP) parameter value. Furthermore, the actual root-mean-square-differences in long-term Tb averages and standard deviations are found consistent with the respective estimated total simulation and <span class="hlt">observation</span> error standard deviations of m3.1K and s2.4K. It is also shown that the MAP parameter values estimated through MCMC simulation are in close agreement with those obtained with Particle Swarm Optimization (PSO).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013DPS....4540203E','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013DPS....4540203E"><span>Understanding Asteroid Disruptions Using Very Young Dust <span class="hlt">Bands</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Espy Kehoe, Ashley J.; Kehoe, T. J.; Colwell, J. E.; Dermott, S. F.</p> <p>2013-10-01</p> <p>Zodiacal dust <span class="hlt">bands</span> are structures that result from the dynamical sculpting of the dust particles released in the catastrophic disruption of an asteroid. Partial dust <span class="hlt">bands</span> are the recently discovered younger siblings of the dust <span class="hlt">bands</span>, ones that are still forming and due to very recent disruptions within the last few hundred thousand years. During the early stages of formation, these structures retain information on the original catastrophic disruptions that produced them (since the dust has not yet been lost or significantly altered by orbital or collisional decay). The first partial dust <span class="hlt">band</span>, at about 17 degrees latitude, was revealed using a very precise method of co-adding the IRAS data set. We have shown that these partial dust <span class="hlt">bands</span> exhibit structure consistent with a forming <span class="hlt">band</span>, can be used to constrain the original size distribution of the dust produced in the catastrophic disruption of an asteroid, and these very young structures also allow a much better estimate of the total amount of dust released in the disruption. In order to interpret the <span class="hlt">observations</span> and constrain the parameters of the dust injected into the cloud following an asteroid disruption, we have developed detailed models of the dynamical evolution of the dust that makes up the <span class="hlt">band</span>. We model the dust velocity distribution resulting from the initial impact and then track the orbital evolution of the dust under the effects of gravitational perturbations from all the planets as well as radiative forces of Poynting-Robertson drag, solar wind drag and radiation pressure and use these results to produce maps of the thermal emission. Through the comparison of our newly completed dynamical evolution models with the coadded <span class="hlt">observations</span>, we can put constraints on the parameters of dust producing the <span class="hlt">band</span>. We confirm the source of the <span class="hlt">band</span> as the very young Emilkowalski cluster ( <250,000 years; Nesvorny et al., 2003) and present our most recent estimates of the size-distribution and cross</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017PhRvB..95g5302H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017PhRvB..95g5302H"><span><span class="hlt">Band</span> alignment of semiconductors and insulators using dielectric-dependent hybrid functionals: Toward high-throughput evaluation</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hinuma, Yoyo; Kumagai, Yu; Tanaka, Isao; Oba, Fumiyasu</p> <p>2017-02-01</p> <p>The <span class="hlt">band</span> alignment of prototypical semiconductors and insulators is investigated using first-principles calculations. A dielectric-dependent hybrid functional, where the nonlocal Fock exchange mixing is set at the reciprocal of the static electronic dielectric constant and the exchange correlation is otherwise treated as in the Perdew-Burke-Ernzerhof (PBE0) hybrid functional, is used as well as the Heyd-Scuseria-Ernzerhof (HSE06) hybrid and PBE semilocal functionals. In addition, these hybrid functionals are applied non-self-consistently to accelerate calculations. The systems considered include C and Si in the diamond structure, BN, AlP, AlAs, AlSb, GaP, GaAs, InP, ZnS, ZnSe, ZnTe, CdS, CdSe, and CdTe in the zinc-blende structure, MgO in the rocksalt structure, and GaN and ZnO in the wurtzite structure. Surface <span class="hlt">band</span> <span class="hlt">positions</span> with respect to the vacuum level, i.e., ionization potentials and electron affinities, and <span class="hlt">band</span> offsets at selected zinc-blende heterointerfaces are evaluated as well as <span class="hlt">band</span> gaps. The non-self-consistent approach speeds up hybrid functional calculations by an order of magnitude, while it is shown using HSE06 that the resultant <span class="hlt">band</span> gaps and surface <span class="hlt">band</span> <span class="hlt">positions</span> are similar to the self-consistent results. The dielectric-dependent hybrid functional improves the <span class="hlt">band</span> gaps and surface <span class="hlt">band</span> <span class="hlt">positions</span> of wide-gap systems over HSE06. The interfacial <span class="hlt">band</span> offsets are predicted with a similar degree of precision. Overall, the performance of the dielectric-dependent hybrid functional is comparable to the G W0 approximation based on many-body perturbation theory in the prediction of <span class="hlt">band</span> gaps and alignments for most systems. The present results demonstrate that the dielectric-dependent hybrid functional, particularly when applied non-self-consistently, is promising for applications to systematic calculations or high-throughput screening that demand both computational efficiency and sufficient accuracy.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22685142-clinically-observed-discrepancy-between-image-based-log-based-mlc-positions','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22685142-clinically-observed-discrepancy-between-image-based-log-based-mlc-positions"><span>A clinically <span class="hlt">observed</span> discrepancy between image-based and log-based MLC <span class="hlt">positions</span></span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Neal, Brian, E-mail: bpn2p@virginia.edu; Ahmed, Mahmoud; Kathuria, Kunal</p> <p>2016-06-15</p> <p>Purpose: To present a clinical case in which real-time intratreatment imaging identified an multileaf collimator (MLC) leaf to be consistently deviating from its programmed and logged <span class="hlt">position</span> by >1 mm. Methods: An EPID-based exit-fluence dosimetry system designed to prevent gross delivery errors was used to capture cine during treatment images. The author serendipitously visually identified a suspected MLC leaf displacement that was not otherwise detected. The leaf <span class="hlt">position</span> as recorded on the EPID images was measured and log-files were analyzed for the treatment in question, the prior day’s treatment, and for daily MLC test patterns acquired on those treatment days.more » Additional standard test patterns were used to quantify the leaf <span class="hlt">position</span>. Results: Whereas the log-file reported no difference between planned and recorded <span class="hlt">positions</span>, image-based measurements showed the leaf to be 1.3 ± 0.1 mm medial from the planned <span class="hlt">position</span>. This offset was confirmed with the test pattern irradiations. Conclusions: It has been clinically <span class="hlt">observed</span> that log-file derived leaf <span class="hlt">positions</span> can differ from their actual <span class="hlt">position</span> by >1 mm, and therefore cannot be considered to be the actual leaf <span class="hlt">positions</span>. This cautions the use of log-based methods for MLC or patient quality assurance without independent confirmation of log integrity. Frequent verification of MLC <span class="hlt">positions</span> through independent means is a necessary precondition to trust log-file records. Intratreatment EPID imaging provides a method to capture departures from MLC planned <span class="hlt">positions</span>.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2006epsc.conf..189J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2006epsc.conf..189J"><span>Analysis of Mars surface hydration through the MEx/OMEGA <span class="hlt">observation</span> of the 3 μm absorption <span class="hlt">band</span>.</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jouglet, D.; Poulet, F.; Bibring, J. P.; Langevin, Y.; Gondet, B.; Milliken, R. E.; Mustard, J. F.</p> <p></p> <p>The near infrared Mars surface global mapping done by OMEGA gives the first opportunity to study the global and detailed characteristics of the 3µm hydration absorption <span class="hlt">band</span> on Mars surface. This feature is indistinctly due to bending and stretching vibrations of water bound in minerals or adsorbed at their surface, and of hydroxyl groups (for a review, see e.g. [1] or [2]). Its study may give new elements to determine the geologic and climatic past of Mars, and may put new constrain about the current water cycle of Mars. OMEGA data are processed in a pipeline that converts raw data to radiance, removes atmospheric effects and gets I/F. Specific data reduction scheme has been developed to assess temperature of OMEGA spectra at 5 µm and to remove their thermal part so as to get the albedo from 1.µm to 5.1µm ([2]). Two methods, the Integrated <span class="hlt">Band</span> Depth and the water content based on comparison with laboratory measures of Yen et al. ([3]), have been used to assess the 3µm <span class="hlt">band</span> depth. These two methods where applied to OMEGA spectra acquired at a nominal calibration level and not exhibiting water ice features. This corresponds to approximately 35 million spectra ([2]). The data processed show the presence of this absorption feature overall the Martian surface, which could be explained by the presence of adsorbed water up to 1% water mass percentage ([4]) and by rinds or coating resulting from weathering (see e.g. [5] or [6]). A possible increase of hydration with albedo is discussed so as to discriminate between the albedo-dependence of the method and hydration variations. Terrains enriched in phyllosilicates ([7]), sulfates ([8]) or hydroxides exhibit an increased hydration at 3 µm. This terrains show that the 3 µm <span class="hlt">band</span> can bring additional information about composition, for example by <span class="hlt">observing</span> a variation in the shape of the <span class="hlt">band</span>. A decrease of hydration with elevation is <span class="hlt">observed</span> on the processed data independently of the value of albedo. This correlation</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1393003-experimental-observation-incoherent-coherent-crossover-orbital-dependent-band-renormalization-iron-chalcogenide-superconductors','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1393003-experimental-observation-incoherent-coherent-crossover-orbital-dependent-band-renormalization-iron-chalcogenide-superconductors"><span>Experimental <span class="hlt">observation</span> of incoherent-coherent crossover and orbital-dependent <span class="hlt">band</span> renormalization in iron chalcogenide superconductors</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Liu, Z. K.; Yi, M.; Zhang, Y.; ...</p> <p>2015-12-22</p> <p>The level of electronic correlation has been one of the key questions in understanding the nature of superconductivity. Among the iron-based superconductors, the iron chalcogenide family exhibits the strongest electron correlations. To gauge the correlation strength, we performed a systematic angle-resolved photoemission spectroscopy study on the iron chalcogenide series Fe 1+ySe xTe 1-x (0 < x < 0.59), a model system with the simplest structure. Our measurement reveals an incoherent-to-coherent crossover in the electronic structure as the selenium ratio increases and the system evolves from a weakly localized to a more itinerant state. Furthermore, we found that the effective massmore » of <span class="hlt">bands</span> dominated by the d xy orbital character significantly decreases with increasing selenium ratio, as compared to the d xz/d yz orbital-dominated <span class="hlt">bands</span>. The orbital-dependent change in the correlation level agrees with theoretical calculations on the <span class="hlt">band</span> structure renormalization, and may help to understand the onset of superconductivity in Fe 1+ySe xTe 1-x.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017AGUFM.A13D2093W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017AGUFM.A13D2093W"><span>Sensitivity Study of IROE Cloud Retrievals Using VIIRS M-<span class="hlt">Bands</span> and Combined VIIRS/CrIS IR <span class="hlt">Observations</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wang, C.; Platnick, S. E.; Meyer, K.; Ackerman, S. A.; Holz, R.; Heidinger, A.</p> <p>2017-12-01</p> <p>The Visible Infrared Imaging Radiometer Suite (VIIRS) on board the Suomi-NPP spacecraft is considered as the next generation of instrument providing operational moderate resolution imaging capabilities after the Moderate Resolution Imaging Spectroradiometer (MODIS) on Terra and Aqua. However, cloud-top property (CTP) retrieval algorithms designed for the two instruments cannot be identical because of the absence of CO2 <span class="hlt">bands</span> on VIIRS. In this study, we conduct a comprehensive sensitivity study of cloud retrievals utilizing a IR-Optimal Estimation (IROE) based algorithm. With a fast IR radiative transfer model, the IROE simultaneously retrieves cloud-top height (CTH), cloud optical thickness (COT), cloud effective radius (CER) and corresponding uncertainties using a set of IR <span class="hlt">bands</span>. Three retrieval runs are implemented for this sensitivity study: retrievals using 1) three native VIIRS M-<span class="hlt">Bands</span> at 750m resolution (8.5-, 11-, and 12-μm), 2) three native VIIRS M-<span class="hlt">Bands</span> with spectrally integrated CO2 <span class="hlt">bands</span> from the Cross-Track Infrared Sounder (CrIS), and 3) six MODIS IR <span class="hlt">bands</span> (8.5-, 11-, 12-, 13.3-, 13.6-, and 13.9-μm). We select a few collocated MODIS and VIIRS granules for pixel-level comparison. Furthermore, aggregated daily and monthly cloud properties from the three runs are also compared. It shows that, the combined VIIRS/CrIS run agrees well with the MODIS-only run except for pixels near cloud edges. The VIIRS-only run is close to its counterparts when clouds are optically thick. However, for optically thin clouds, the VIIRS-only run can be readily influenced by the initial guess. Large discrepancies and uncertainties can be found for optically thin clouds from the VIIRS-only run.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3833734','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3833734"><span><span class="hlt">Banded</span> karyotype of the Konya wild sheep (Ovis orientalis anatolica Valenciennes, 1856) from Turkey</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Arslan, Atilla; Zima, Jan</p> <p>2011-01-01</p> <p>Abstract Thekaryotype, C-<span class="hlt">banding</span>, and nucleoar organizer regions (NORs) of eight specimens ofKonya wild sheepfrom Turkey were examined. The complement included six large metacentric autosomes, 46 acrocentric autosomes of decreasing size, a medium-sized acrocentric X chromosome, and a small bi-armed Y chromosome (the diploid chromosome number 2n=54, the number of autosomal arms NFa=58, the number of chromosome arms NF=61). G-<span class="hlt">banding</span> allowed reliable identification of all the chromosome pairs and the pairing of homologous elements. All the autosomes possessed distinct centromeric or pericentromeric C-<span class="hlt">positive</span> <span class="hlt">bands</span>. The X chromosome had a pericentromeric C-<span class="hlt">positive</span> <span class="hlt">band</span>, and the Y chromosome was entirely C-heterochromatic. The NORs were located in the terminal regions of the long arms of three metacentric and two acrocentric autosomes. The karyotype of the Konya wild sheep and its <span class="hlt">banding</span> patterns are quite similar to chromosome complement reported in domestic sheep and European mouflon. PMID:24260621</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012AGUFM.H24E..04C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012AGUFM.H24E..04C"><span>Airborne Active and Passive L-<span class="hlt">Band</span> <span class="hlt">Observations</span> in Soil Moisture Active Passive Validation Experiment 2012 (SMAPVEX12)</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Colliander, A.; Yueh, S. H.; Chazanoff, S.; Jackson, T. J.; McNairn, H.; Bullock, P.; Wiseman, G.; Berg, A. A.; Magagi, R.; Njoku, E. G.</p> <p>2012-12-01</p> <p>NASA's (National Aeronautics and Space Administration) Soil Moisture Active Passive (SMAP) Mission is scheduled for launch in October 2014. The objective of the mission is global mapping of soil moisture and freeze/thaw state. Merging of active and passive L-<span class="hlt">band</span> <span class="hlt">observations</span> of the mission will enable unprecedented combination of accuracy, resolution, coverage and revisit-time for soil moisture and freeze/thaw state retrieval. For pre-launch algorithm development and validation the SMAP project and NASA coordinated a field campaign named as SMAPVEX12 (Soil Moisture Active Passive Validation Experiment 2012) together with Agriculture and Agri-Food Canada in the vicinity of Winnipeg, Canada in June-July, 2012. The main objective of SMAPVEX12 was acquisition of data record that features long-time series with varying soil moisture and vegetation conditions (for testing the application of time-series approach) over aerial domain of multiple parallel lines (for spatial disaggregation studies). The coincident active and passive L-<span class="hlt">band</span> data were acquired using the Passive Active L-<span class="hlt">band</span> System (PALS), which is an airborne radiometer and radar developed for testing L-<span class="hlt">band</span> retrieval algorithms. For SMAPVEX12 PALS was installed on a Twin Otter aircraft. The flight plan included flights at two altitudes. The higher altitude was used to map the whole experiment domain and the lower altitude was used to obtain measurements over a specific set of field sites. The spatial resolution (and swath) of the radar and radiometer from low altitude was about 600 m and from high altitude about 1500 m. The PALS acquisitions were complemented with high resolution (~10 m) L-<span class="hlt">band</span> SAR measurements carried out by UAVSAR instrument on-board G-III aircraft. The campaign ran from June 7 until July 19. The PALS instrument conducted 17 brightness temperature and backscatter measurement flights and the UAVSAR conducted 14 backscatter measurement flights. The airborne data acquisition was supported by</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/19206638','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/19206638"><span><span class="hlt">Band</span>-filling of solution-synthesized CdS nanowires.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Puthussery, James; Lan, Aidong; Kosel, Thomas H; Kuno, Masaru</p> <p>2008-02-01</p> <p>The <span class="hlt">band</span> edge optical characterization of solution-synthesized CdS nanowires (NWs) is described. Investigated wires are made through a solution-liquid-solid approach that entails the use of low-melting bimetallic catalyst particles to seed NW growth. Resulting diameters are approximately 14 nm, and lengths exceed 1 microm. Ensemble diameter distributions are approximately 13%, with corresponding intrawire diameter variations of approximately 5%. High-resolution transmission electron micrographs show that the wires are highly crystalline and have the wurtzite structure with growth along at least two directions: [0001] and [1010]. <span class="hlt">Band</span> edge emission is <span class="hlt">observed</span> with estimated quantum yields between approximately 0.05% and 1%. Complementary photoluminescence excitation spectra show structure consistent with the linear absorption. Carrier cooling dynamics are subsequently examined through ensemble lifetime and transient differential absorption measurements. The former reveals unexpectedly long <span class="hlt">band</span> edge decays that extend beyond tens of nanoseconds. The latter indicates rapid intraband carrier cooling on time scales of 300-400 fs. Subsequent recovery at the <span class="hlt">band</span> edge contains significant Auger contributions at high intensities which are usurped by other, possibly surface-related, carrier relaxation pathways at lower intensities. Furthermore, an unusual intensity-dependent transient broadening is seen, connected with these long decays. The effect likely stems from <span class="hlt">band</span>-filling on the basis of an analysis of <span class="hlt">observed</span> spectral shifts and line widths.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2011CorRe..30..473C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2011CorRe..30..473C"><span>Selective feeding by coral reef fishes on coral lesions associated with brown <span class="hlt">band</span> and black <span class="hlt">band</span> disease</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Chong-Seng, K. M.; Cole, A. J.; Pratchett, M. S.; Willis, B. L.</p> <p>2011-06-01</p> <p>Recent studies have suggested that corallivorous fishes may be vectors for coral disease, but the extent to which fishes actually feed on and thereby potentially transmit coral pathogens is largely unknown. For this study, in situ video <span class="hlt">observations</span> were used to assess the level to which fishes fed on diseased coral tissues at Lizard Island, northern Great Barrier Reef. Surveys conducted at multiple locations around Lizard Island revealed that coral disease prevalence, especially of brown <span class="hlt">band</span> disease (BrB), was higher in lagoon and backreef locations than in exposed reef crests. Accordingly, video cameras were deployed in lagoon and backreef habitats to record feeding by fishes during 1-h periods on diseased sections of each of 44 different coral colonies. Twenty-five species from five fish families (Blennidae, Chaetodontidae, Gobiidae, Labridae and Pomacentridae) were <span class="hlt">observed</span> to feed on infected coral tissues of staghorn species of Acropora that were naturally infected with black <span class="hlt">band</span> disease (BBD) or brown <span class="hlt">band</span> disease (BrB). Collectively, these fishes took an average of 18.6 (±5.6 SE) and 14.3 (±6.1 SE) bites per hour from BBD and BrB lesions, respectively. More than 40% (408/948 bites) and nearly 25% (314/1319 bites) of bites were <span class="hlt">observed</span> on lesions associated with BBD and BrB, respectively, despite these <span class="hlt">bands</span> each representing only about 1% of the substratum available. Moreover, many corallivorous fishes ( Labrichthys unilineatus, Chaetodon aureofasciatus, C. baronessa, C. lunulatus, C. trifascialis, Cheiloprion labiatus) selectively targeted disease lesions over adjacent healthy coral tissues. These findings highlight the important role that reef fishes may play in the dynamics of coral diseases, either as vectors for the spread of coral disease or in reducing coral disease progression through intensive and selective consumption of diseased coral tissues.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/23938497','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/23938497"><span>Narrow-<span class="hlt">band</span> generation in random distributed feedback fiber laser.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Sugavanam, Srikanth; Tarasov, Nikita; Shu, Xuewen; Churkin, Dmitry V</p> <p>2013-07-15</p> <p>Narrow-<span class="hlt">band</span> emission of spectral width down to ~0.05 nm line-width is achieved in the random distributed feedback fiber laser employing narrow-<span class="hlt">band</span> fiber Bragg grating or fiber Fabry-Perot interferometer filters. The <span class="hlt">observed</span> line-width is ~10 times less than line-width of other demonstrated up to date random distributed feedback fiber lasers. The random DFB laser with Fabry-Perot interferometer filter provides simultaneously multi-wavelength and narrow-<span class="hlt">band</span> (within each line) generation with possibility of further wavelength tuning.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22518917-first-infrared-band-strengths-amorphous-co-sub-overlooked-component-interstellar-ices','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22518917-first-infrared-band-strengths-amorphous-co-sub-overlooked-component-interstellar-ices"><span>FIRST INFRARED <span class="hlt">BAND</span> STRENGTHS FOR AMORPHOUS CO{sub 2}, AN OVERLOOKED COMPONENT OF INTERSTELLAR ICES</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Gerakines, Perry A.; Hudson, Reggie L., E-mail: Reggie.Hudson@NASA.gov</p> <p>2015-08-01</p> <p>Solid carbon dioxide (CO{sub 2}) has long been recognized as a component of both interstellar and solar system ices, but a recent literature search has revealed significant qualitative and quantitative discrepancies in the laboratory spectra on which the abundances of extraterrestrial CO{sub 2} are based. Here we report new infrared (IR) spectra of amorphous CO{sub 2}-ice along with <span class="hlt">band</span> intensities (<span class="hlt">band</span> strengths) of four mid-IR absorptions, the first such results in the literature. A possible thickness dependence for amorphous-CO{sub 2} IR <span class="hlt">band</span> shapes and <span class="hlt">positions</span> also is investigated, and the three discordant reports of amorphous CO{sub 2} spectra in themore » literature are addressed. Applications of our results are discussed with an emphasis on laboratory investigations and results from astronomical <span class="hlt">observations</span>. A careful comparison with earlier work shows that the IR spectra calculated from several databases for CO{sub 2} ices, all ices being made near 10 K, are not for amorphous CO{sub 2}, but rather for crystalline CO{sub 2} or crystalline-amorphous mixtures.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018JMP....59e2103K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018JMP....59e2103K"><span>On <span class="hlt">observation</span> of <span class="hlt">position</span> in quantum theory</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kryukov, A.</p> <p>2018-05-01</p> <p>Newtonian and Schrödinger dynamics can be formulated in a physically meaningful way within the same Hilbert space framework. This fact was recently used to discover an unexpected relation between classical and quantum motions that goes beyond the results provided by the Ehrenfest theorem. A formula relating the normal probability distribution and the Born rule was also found. Here the dynamical mechanism responsible for the latter formula is proposed and applied to measurements of macroscopic and microscopic systems. A relationship between the classical Brownian motion and the diffusion of state on the space of states is discovered. The role of measuring devices in quantum theory is investigated in the new framework. It is shown that the so-called collapse of the wave function is not measurement specific and does not require a "concentration" near the eigenstates of the measured <span class="hlt">observable</span>. Instead, it is explained by the common diffusion of a state over the space of states under interaction with the apparatus and the environment. This in turn provides us with a basic reason for the definite <span class="hlt">position</span> of macroscopic bodies in space.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4495810','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4495810"><span>RefMoB, a Reflectivity Feature Model-Based Automated Method for Measuring Four Outer Retinal Hyperreflective <span class="hlt">Bands</span> in Optical Coherence Tomography</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Ross, Douglas H.; Clark, Mark E.; Godara, Pooja; Huisingh, Carrie; McGwin, Gerald; Owsley, Cynthia; Litts, Katie M.; Spaide, Richard F.; Sloan, Kenneth R.; Curcio, Christine A.</p> <p>2015-01-01</p> <p>Purpose. To validate a model-driven method (RefMoB) of automatically describing the four outer retinal hyperreflective <span class="hlt">bands</span> revealed by spectral-domain optical coherence tomography (SDOCT), for comparison with histology of normal macula; to report thickness and <span class="hlt">position</span> of <span class="hlt">bands</span>, particularly <span class="hlt">band</span> 2 (ellipsoid zone [EZ], commonly called IS/OS). Methods. Foveal and superior perifoveal scans of seven SDOCT volumes of five individuals aged 28 to 69 years with healthy maculas were used (seven eyes for validation, five eyes for measurement). RefMoB determines <span class="hlt">band</span> thickness and <span class="hlt">position</span> by a multistage procedure that models reflectivities as a summation of Gaussians. <span class="hlt">Band</span> thickness and <span class="hlt">positions</span> were compared with those obtained by manual evaluators for the same scans, and compared with an independent published histological dataset. Results. Agreement among manual evaluators was moderate. Relative to manual evaluation, RefMoB reported reduced thickness and vertical shifts in <span class="hlt">band</span> <span class="hlt">positions</span> in a <span class="hlt">band</span>-specific manner for both simulated and empirical data. In foveal and perifoveal scans, <span class="hlt">band</span> 1 was thick relative to the anatomical external limiting membrane, <span class="hlt">band</span> 2 aligned with the outer one-third of the anatomical IS ellipsoid, and <span class="hlt">band</span> 3 (IZ, interdigitation of retinal pigment epithelium and photoreceptors) was cleanly delineated. Conclusions. RefMoB is suitable for automatic description of the location and thickness of the four outer retinal hyperreflective <span class="hlt">bands</span>. Initial results suggest that <span class="hlt">band</span> 2 aligns with the outer ellipsoid, thus supporting its recent designation as EZ. Automated and objective delineation of <span class="hlt">band</span> 3 will help investigations of structural biomarkers of dark-adaptation changes in aging. PMID:26132776</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27779317','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27779317"><span>Adhesives for fixed orthodontic <span class="hlt">bands</span>.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Millett, Declan T; Glenny, Anne-Marie; Mattick, Rye Cr; Hickman, Joy; Mandall, Nicky A</p> <p>2016-10-25</p> <p>Orthodontic treatment involves using fixed or removable appliances (dental braces) to correct the <span class="hlt">positions</span> of teeth. It has been shown that the quality of treatment result obtained with fixed appliances is much better than with removable appliances. Fixed appliances are, therefore, favoured by most orthodontists for treatment. The success of a fixed orthodontic appliance depends on the metal attachments (brackets and <span class="hlt">bands</span>) being attached securely to the teeth so that they do not become loose during treatment. Brackets are usually attached to the front and side teeth, whereas <span class="hlt">bands</span> (metal rings that go round the teeth) are more commonly used on the back teeth (molars). A number of adhesives are available to attach <span class="hlt">bands</span> to teeth and it is important to understand which group of adhesives bond most reliably, as well as reducing or preventing dental decay during the treatment period. To evaluate the effectiveness of the adhesives used to attach <span class="hlt">bands</span> to teeth during fixed appliance treatment, in terms of:(1) how often the <span class="hlt">bands</span> come off during treatment; and(2) whether they protect the <span class="hlt">banded</span> teeth against decay during fixed appliance treatment. The following electronic databases were searched: Cochrane Oral Health's Trials Register (searched 2 June 2016), Cochrane Central Register of Controlled Trials (CENTRAL; 2016, Issue 5) in the Cochrane Library (searched 2 June 2016), MEDLINE Ovid (1946 to 2 June 2016) and EMBASE Ovid (1980 to 2 June 2016). We searched ClinicalTrials.gov and the World Health Organization International Clinical Trials Registry Platform for ongoing trials. No restrictions were placed on the language or date of publication when searching the electronic databases. Randomised and controlled clinical trials (RCTs and CCTs) (including split-mouth studies) of adhesives used to attach orthodontic <span class="hlt">bands</span> to molar teeth were selected. Patients with full arch fixed orthodontic appliance(s) who had <span class="hlt">bands</span> attached to molars were included. All review authors</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19880036224&hterms=swans&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DTitle%26N%3D0%26No%3D30%26Ntt%3Dswans','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19880036224&hterms=swans&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DTitle%26N%3D0%26No%3D30%26Ntt%3Dswans"><span>Study of the isotopic features of Swan <span class="hlt">bands</span> in comets</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Krishna Swamy, K. S.</p> <p>1987-01-01</p> <p>It is shown from a detailed statistical equilibrium calculation of the (C-12)(C-13) molecule that the interpretation of the <span class="hlt">observed</span> intensities of Swan <span class="hlt">bands</span> of the normal and the isotopic molecule of C2 in terms of the abundance ratio of C-12 and C-13 is a reasonable one. The synthetic profile of some isotopic features in the (0.0) Swan <span class="hlt">band</span> is compared with the <span class="hlt">observed</span> profiles for comet West.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19800037389&hterms=1082&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3D%2526%25231082','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19800037389&hterms=1082&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3D%2526%25231082"><span>Temperature dependence of intensities of the 8-12 micron <span class="hlt">bands</span> of CFCl3</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Nanes, R.; Silvaggio, P. M.; Boese, R. W.</p> <p>1980-01-01</p> <p>The absolute intensities of the 8-12 micron <span class="hlt">bands</span> from Freon 11 (CFCl3) were measured at temperatures of 294 and 216 K. Intensities of the <span class="hlt">bands</span> centered at 798, 847, 934, and 1082 per cm are all <span class="hlt">observed</span> to depend on temperature. The temperature dependence for the 847 and 1082 per cm fundamental regions is attributed to underlying hot <span class="hlt">bands</span>; for the nu2 + nu5 combination <span class="hlt">band</span> (934 per cm), the <span class="hlt">observed</span> temperature dependence is in close agreement with theoretical prediction. The implication of these results on atmospheric IR remote-sensing is briefly discussed.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li class="active"><span>20</span></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_20 --> <div id="page_21" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li class="active"><span>21</span></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="401"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://pubs.er.usgs.gov/publication/70044136','USGSPUBS'); return false;" href="https://pubs.er.usgs.gov/publication/70044136"><span>Applications of spectral <span class="hlt">band</span> adjustment factors (SBAF) for cross-calibration</span></a></p> <p><a target="_blank" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p>Chander, Gyanesh</p> <p>2013-01-01</p> <p>To monitor land surface processes over a wide range of temporal and spatial scales, it is critical to have coordinated <span class="hlt">observations</span> of the Earth's surface acquired from multiple spaceborne imaging sensors. However, an integrated global <span class="hlt">observation</span> framework requires an understanding of how land surface processes are seen differently by various sensors. This is particularly true for sensors acquiring data in spectral <span class="hlt">bands</span> whose relative spectral responses (RSRs) are not similar and thus may produce different results while <span class="hlt">observing</span> the same target. The intrinsic offsets between two sensors caused by RSR mismatches can be compensated by using a spectral <span class="hlt">band</span> adjustment factor (SBAF), which takes into account the spectral profile of the target and the RSR of the two sensors. The motivation of this work comes from the need to compensate the spectral response differences of multispectral sensors in order to provide a more accurate cross-calibration between the sensors. In this paper, radiometric cross-calibration of the Landsat 7 Enhanced Thematic Mapper Plus (ETM+) and the Terra Moderate Resolution Imaging Spectroradiometer (MODIS) sensors was performed using near-simultaneous <span class="hlt">observations</span> over the Libya 4 pseudoinvariant calibration site in the visible and near-infrared spectral range. The RSR differences of the analogous ETM+ and MODIS spectral <span class="hlt">bands</span> provide the opportunity to explore, understand, quantify, and compensate for the measurement differences between these two sensors. The cross-calibration was initially performed by comparing the top-of-atmosphere (TOA) reflectances between the two sensors over their lifetimes. The average percent differences in the long-term trends ranged from $-$5% to $+$6%. The RSR compensated ETM+ TOA reflectance (ETM+$^{ast}$) measurements were then found to agree with MODIS TOA reflectance to within 5% for all <span class="hlt">bands</span> when Earth <span class="hlt">Observing</span>-1 Hy- erion hyperspectral data were used to produce the SBAFs. These differences were later</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19940020905','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19940020905"><span>Catalog of Infrared <span class="hlt">Observations</span>, Third Edition</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Gezari, Daniel Y.; Schmitz, Marion; Pitts, Patricia S.; Mead, Jaylee M.</p> <p>1993-01-01</p> <p>The Far Infrared Supplement contains a subset of the data in the full Catalog of Infrared <span class="hlt">Observations</span> (all <span class="hlt">observations</span> at wavelengths greater than 4.6 microns). The Catalog of Infrared <span class="hlt">Observations</span> (CIO), NASA RP-1294, is a compilation of infrared astronomical <span class="hlt">observational</span> data obtained from an extensive literature search of scientific journals and major astronomical catalogs and surveys. The literature search is complete for years 1965 through 1990 in this Third Edition. The Catalog contains about 210,000 <span class="hlt">observations</span> of roughly 20,000 individual sources and supporting appendices. The expanded Third Edition contains coded IRAS 4-<span class="hlt">band</span> data for all CIO sources detected by IRAS. The appendices include an atlas of infrared source <span class="hlt">positions</span> (also included in this volume), two bibliographies of Catalog listings, and an atlas of infrared spectral ranges. The complete CIO database is available to qualified users in printed, microfiche, and magnetic-tape formats.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22036835-photonic-band-structures-two-dimensional-magnetized-plasma-photonic-crystals','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22036835-photonic-band-structures-two-dimensional-magnetized-plasma-photonic-crystals"><span>Photonic <span class="hlt">band</span> structures of two-dimensional magnetized plasma photonic crystals</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Qi, L.</p> <p></p> <p>By using modified plane wave method, photonic <span class="hlt">band</span> structures of the transverse electric polarization for two types of two-dimensional magnetized plasma photonic crystals are obtained, and influences of the external magnetic field, plasma density, and dielectric materials on the dispersion curves are studied, respectively. Results show that two areas of flat <span class="hlt">bands</span> appear in the dispersion curves due to the role of external magnetic field, and the higher frequencies of the up and down flat <span class="hlt">bands</span> are corresponding to the right-circled and left-circled cutoff frequencies, respectively. Adjusting external magnetic field and plasma density can not only control <span class="hlt">positions</span> of themore » flat <span class="hlt">bands</span>, but also can control the location and width of the local gap; increasing relative dielectric constant of the dielectric materials makes omni-direction gaps appear.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25176363','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25176363"><span>Fresh and aged human lymphocyte metaphase slides are equally usable for GTG <span class="hlt">banding</span>.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Sajjad, Naheed; Haque, Sayedul; SBurney, Syed Intesar; Shahid, Syed Muhammad; Zehra, Sitwat; Azhar, Abid</p> <p>2014-09-01</p> <p>The identification of chromosomes for routine cytogenetic analysis is based on quality of metaphases and good <span class="hlt">banding</span> pattern. Fresh slides of human lymphocytes have been shown to produce good <span class="hlt">bands</span> for the identification of chromosomes morphology. G-<span class="hlt">bands</span> by Trypsin using Giemsa (GTG) <span class="hlt">banding</span> of aged slides is generally considered hard to get desired <span class="hlt">band</span> pattern of chromosomes persistently. The current study is focused on GTG <span class="hlt">banding</span> of aged slides. A total of 340 subjects including 290 primary infertile and 50 fertile were selected. The blood samples were drawn aseptically for cytogenetic analysis. Lymphocytes were cultured and GTG <span class="hlt">banding</span> was done on 1440 glass slides. Giemsa trypsin <span class="hlt">banding</span> of aged slides were done by adjusting average trypsin time for each month according to the slide age and metaphase concentration. Correlation analyses showed a significant and <span class="hlt">positive</span> correlation between slide ageing and trypsin pre-treatment time. The results of this study suggest that, the fresh and aged human lymphocyte metaphases are equally usable for GTG <span class="hlt">banding</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012EGUGA..1410873P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012EGUGA..1410873P"><span>Composition of <span class="hlt">bands</span> in Argadnel Regio, Europa: Implications for Volcanic Resurfacing.</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Prockter, L. M.; Shirley, J. H.; Dalton, J. B.; Kamp, L. W.</p> <p>2012-04-01</p> <p><span class="hlt">Bands</span> on Europa are dark or grey features which formed as a result of the pulling apart of cracks in Europa's surface, allowing new cryovolcanic material to be emplaced into the newly formed gaps. <span class="hlt">Bands</span> have been shown to be sites of extensive resurfacing, and appear to have brightened over time, although the exact cause is not known. Thus the relative albedo of a <span class="hlt">band</span> can be used as a proxy for age, as has been <span class="hlt">observed</span> on Europa's surface, where the darkest <span class="hlt">bands</span> crosscut, and are therefore younger than, lighter, or "grey" <span class="hlt">bands</span>. We here combine Galileo Near-Infrared Mapping Spectrometer (NIMS) and Solid State Imager (SSI) data, using the methods of Shirley et al., [2010], to determine the surface compositions and water ice grain sizes of dark and grey <span class="hlt">bands</span> in Europa's anti-Jovian Argadnel Regio, and to understand their relative histories. Preliminary results show that the total amount of hydrated salts modeled in the grey <span class="hlt">bands</span> tends to be less than that seen in the dark <span class="hlt">bands</span> (from ~19 to ~38% and ~38 to 47% respectively). One dark <span class="hlt">band</span> contains hydrated sulfuric acid which is >5% lower than that of the surrounding ridged plains, as well as only 9% water ice of small grain size. These <span class="hlt">observations</span> are interpreted as evidence that this <span class="hlt">band</span> has been less processed by radiolysis, and so is relatively young or has been recently resurfaced. Relatively larger ice grain sizes are <span class="hlt">observed</span> in the grey <span class="hlt">bands</span>, as might be expected if they are older than the dark <span class="hlt">bands</span>, and all the <span class="hlt">bands</span> contain less large-grained ice than the surrounding ridged plains, thought to be the oldest unit on Europa's surface. We also find a wedge-shaped <span class="hlt">band</span> that exhibits a different composition across its northern part, and appears to have undergone resurfacing as the result of the formation of a large, shallow trough that cuts diagonally across the <span class="hlt">band</span>. We speculate that this resurfacing could be due to processes such as (1) the removal of frost due to surface shaking during the tectonic</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013EGUGA..1511980L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013EGUGA..1511980L"><span>Studying Big Planets with Small Telescopes: The z'-<span class="hlt">Band</span> Occultation of WASP-19b <span class="hlt">Observed</span> with EulerCam and TRAPPIST</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Lendl, Monika; Gillon, Michael; Queloz, Didier</p> <p>2013-04-01</p> <p>Transiting planets have opened up a window to the detailed study of extrasolar planets as their orbital orientation allows the measurement of the planet/star radius and flux ratios. From the <span class="hlt">observation</span> of planetary transits and occultations at different wavelengths we can gain insights into the planets temperature, atmospheric composition, energy redistribution and albedo. In order to contribute to the characterization of planetary atmospheres, it is necessary to obtain high precision measurements of planetary transits and occultations as the signals of interest have amplitudes of typically 100 ppm. We use two dedicated instruments, EulerCam at the 1.2m Euler-Swiss telescope and the 0.6m TRAPPIST telescope for the in-depth study of transiting planets through time resolution photometry. While single lightcurves from 1m class telescopes typically reach photometric precisions of around 1mmag, we obtain very high accuracy on the transit and occultation shape by not relying on single <span class="hlt">observations</span> but collecting larger samples of lightcurves. In this framework, we have performed an extensive <span class="hlt">observing</span> campaign on the Hot Jupiter WASP-19b collecting over 60 hours of <span class="hlt">observations</span> with EulerCam and TRAPPIST. The data cover 14 transits and 10 occultations of WASP-19b. We demonstrate how the attainable photometric precision and accuracy of the derived parameters can be greatly improved by combining an increasing number of lightcurves as instrumental and stellar effects can be identified and accounted for. We report the detection of the occultation of WASP-19b in the z'-<span class="hlt">band</span>. This measurement is one of only a handful of exoplanet occultations detected from the ground at wavelengths shorter than 1μm , and so far the only one obtained from the ground using 1m class telescopes. Our value adds to an ensemble of occultation measurements for this planet, and is indicative of an Oxygen-dominated chemistry. From our sample of transits, we measure the transit depth to a precision of</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015JGRD..12011536D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015JGRD..12011536D"><span>Mesoscale kinematics derived from X-<span class="hlt">band</span> Doppler radar <span class="hlt">observations</span> of convective versus stratiform precipitation and comparison with GPS radiosonde profiles</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Deshpande, Sachin M.; Dhangar, N.; Das, S. K.; Kalapureddy, M. C. R.; Chakravarty, K.; Sonbawne, S.; Konwar, M.</p> <p>2015-11-01</p> <p>Single Doppler analysis techniques known as velocity azimuth display (VAD) and volume velocity processing (VVP) are used to analyze kinematics of mesoscale flow such as horizontal wind and divergence using X-<span class="hlt">band</span> Doppler weather radar <span class="hlt">observations</span>, for selected cases of convective, stratiform, and shallow cloud systems near tropical Indian sites Pune (18.58°N, 73.92°E, above sea level (asl) 560 m) and Mandhardev (18.51°N, 73.85°E, asl 1297 m). The vertical profiles of horizontal wind estimated from radar VVP/VAD methods agree well with GPS radiosonde profiles, with the low-level jet at about 1.5 km during monsoon season well depicted in both. The vertical structure and temporal variability of divergence and reflectivity profiles are indicative of the dynamical and microphysical characteristics of shallow convective, deep convective, and stratiform cloud systems. In shallow convective systems, vertical development of reflectivity profiles is limited below 5 km. In deep convective systems, reflectivity values as large as 55 dBZ were <span class="hlt">observed</span> above freezing level. The stratiform system shows the presence of a reflectivity bright <span class="hlt">band</span> (~35 dBZ) near the melting level. The diagnosed vertical profiles of divergence in convective and stratiform systems are distinct. In shallow convective conditions, convergence was seen below 4 km with divergence above. Low-level convergence and upper level divergence are <span class="hlt">observed</span> in deep convective profiles, while stratiform precipitation has midlevel convergence present between lower level and upper level divergence. The divergence profiles in stratiform precipitation exhibit intense shallow layers of "melting convergence" at 0°C level, near 4.5 km altitude, with a steep gradient on the both sides of the peak. The level of nondivergence in stratiform situations is lower than that in convective situations. These <span class="hlt">observed</span> vertical structures of divergence are largely indicative of latent heating profiles in the atmosphere, an</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018AAS...23135411C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018AAS...23135411C"><span>The VLA Low-<span class="hlt">band</span> Ionosphere and Transient Experiment (VLITE)</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Clarke, Tracy; Peters, Wendy; Brisken, Walter; Giacintucci, Simona; Kassim, Namir; Polisensky, Emil; Helmboldt, Joseph; Richards, Emily E.; Erickson, Alan; Ray, Paul S.; Kerr, Matthew T.; Deneva, Julia; Coburn, William; Huber, Robert; Long, Jeff</p> <p>2018-01-01</p> <p>The VLA Low-<span class="hlt">band</span> Ionosphere and Transient Experiment (VLITE, http://vlite.nrao.edu/ ) is a commensal low-frequency <span class="hlt">observing</span> system that has been operational on the National Radio Astronomy Observatory's Karl G. Jansky Very Large Array (VLA) since late 2014. The separate optical paths of the prime-focus sub-GHz dipole feeds and the Cassegrain-focus 1-50 GHz feeds allow both systems to operate simultaneously with independent correlators. The initial 2.5 years of VLITE operation provided real-time correlation of 10 antennas across the 320-384 MHz <span class="hlt">band</span> with a total <span class="hlt">observing</span> time approaching 12,000 hours. During the summer of 2017, VLITE was upgraded to a total of 16 antennas (more than doubling the number of baselines) with enhanced correlator capabilities to enable correlation of the on-the-fly <span class="hlt">observing</span> mode being used for the new NRAO VLA Sky Survey (VLASS).We present an overview of the VLITE system, including highlights of the complexities of a commensal <span class="hlt">observing</span> program, sparse-array challenges, and scientific capabilities from our science-ready data pipeline. In the longer term, we seek a path to broadband expansion across all VLA antennas to develop a powerful new LOw <span class="hlt">Band</span> Observatory (LOBO).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018AdSpR..61..823S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018AdSpR..61..823S"><span>VLBI <span class="hlt">observations</span> to the APOD satellite</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sun, Jing; Tang, Geshi; Shu, Fengchun; Li, Xie; Liu, Shushi; Cao, Jianfeng; Hellerschmied, Andreas; Böhm, Johannes; McCallum, Lucia; McCallum, Jamie; Lovell, Jim; Haas, Rüdiger; Neidhardt, Alexander; Lu, Weitao; Han, Songtao; Ren, Tianpeng; Chen, Lue; Wang, Mei; Ping, Jinsong</p> <p>2018-02-01</p> <p>The APOD (Atmospheric density detection and Precise Orbit Determination) is the first LEO (Low Earth Orbit) satellite in orbit co-located with a dual-frequency GNSS (GPS/BD) receiver, an SLR reflector, and a VLBI X/S dual <span class="hlt">band</span> beacon. From the overlap statistics between consecutive solution arcs and the independent validation by SLR measurements, the orbit <span class="hlt">position</span> deviation was below 10 cm before the on-board GNSS receiver got partially operational. In this paper, the focus is on the VLBI <span class="hlt">observations</span> to the LEO satellite from multiple geodetic VLBI radio telescopes, since this is the first implementation of a dedicated VLBI transmitter in low Earth orbit. The practical problems of tracking a fast moving spacecraft with current VLBI ground infrastructure were solved and strong interferometric fringes were obtained by cross-correlation of APOD carrier and DOR (Differential One-way Ranging) signals. The precision in X-<span class="hlt">band</span> time delay derived from 0.1 s integration time of the correlator output is on the level of 0.1 ns. The APOD <span class="hlt">observations</span> demonstrate encouraging prospects of co-location of multiple space geodetic techniques in space, as a first prototype.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010AAS...21543320P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010AAS...21543320P"><span>The K-<span class="hlt">Band</span> Quasar Luminosity Function from an SDSS and UKIDSS Matched Catalog</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Peth, Michael; Ross, N. P.; Schneider, D. P.</p> <p>2010-01-01</p> <p>We match the 1,015,082 quasars from the Sloan Digital Sky Survey (SDSS) DR6 Photometric Quasar catalog to the UKIRT Infrared Digital Sky Survey (UKIDSS) Large Area Survey (LAS) DR3 to produce a catalog of 130,827 objects with optical (ugriz) and infrared (YJHK) measurements over an area of 1,200 sq. deg. A matching radius of 1'’ is used; the <span class="hlt">positional</span> standard deviations of SDSS DR6 quasars and UKIDSS LAS is δRA = 0.137'’ and δDec = 0.131''. The catalog contains 74,351 K-<span class="hlt">band</span> detections and 42,133 objects have coverage in all four NIR <span class="hlt">bands</span>. In addition to the catalog, we present optical and NIR color-redshift and color-color plots. The photometric vs. spectroscopic redshift plots demonstrate how unreliable high reported photometric redshifts can be. This forces us to focus on z4.6 quasars are compared to our highest redshift objects. The giK color-color plot demonstrates that stellar contamination only affects a small sample of the objects. Distributions for Y,J,H,K and i-<span class="hlt">bands</span> reveal insights into the flux limits in each magnitude. We investigate the distribution of redshifts from different data sets and investigate the legitimacy of certain measured photometric redshift regions. For in-depth analysis, we focus on the 300 sq. deg area equatorial SDSS region designated as Stripe 82. We measure the <span class="hlt">observed</span> K-<span class="hlt">band</span> quasar luminosity function (QLF) for a subset of 9,872, z<2.2 objects. We find the shape of the K-<span class="hlt">band</span> QLF is very similar to that of the optical QLF, over the considered redshift ranges. Our calculated K-<span class="hlt">Band</span> QLFs broadly match previous optical QLFs calculated from the SDSS and 2SLAQ QSO surveys and should provide important constraints linking unobscured optical quasars to Mid-Infrared detected, dusty and obscured AGNs at high-redshift.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.jstor.org/stable/3798230','USGSPUBS'); return false;" href="http://www.jstor.org/stable/3798230"><span>Reward <span class="hlt">banding</span> to determine reporting rate of recovered mourning dove <span class="hlt">bands</span></span></a></p> <p><a target="_blank" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p>Tomlinson, R.E.</p> <p>1968-01-01</p> <p>Reward <span class="hlt">bands</span> placed on the other leg of certain regularly <span class="hlt">banded</span> immature mourning doves (Zenaidura macroura) were used to develop information on reporting rates of recovered dove <span class="hlt">bands</span>. Reports from 15 widely separated sections of the United States showed considerable variation in recovery rate of doves both with and without reward <span class="hlt">bands</span>. The overall percentages of <span class="hlt">banded</span> doves that were reported as recovered were 9.69% for those with reward <span class="hlt">bands</span> and 3.83% for controls. The bandreporting rate for states influenced by publicity was 66%; that for states not influenced was 32%.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018BSRSL..87..321A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018BSRSL..87..321A"><span>Multi-<span class="hlt">band</span> optical variability studies of Blazars</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Agarwal, Aditi</p> <p>2018-04-01</p> <p>To search for optical variability on a wide range of timescales, we have carried out photometric monitoring of a dozen blazars. CCD magnitudes in B, V, R and I pass-<span class="hlt">bands</span> were determined for > 10,000f new optical <span class="hlt">observations</span> from 300 nights made during 2011 – 2016, with an average length of 4 h each, using seven optical telescopes: four in Bulgaria, one in Greece, and two in India. We measured multiband optical flux and colour variations on diverse timescales. Blazar variability studies helped us in understanding their nature and extreme conditions within the emission region. To explain possible physical causes of the <span class="hlt">observed</span> spectral variability, we also investigated spectral energy distributions using B, V, R, I, J and K pass-<span class="hlt">band</span> data.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24135149','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24135149"><span>Cellular mechanics of germ <span class="hlt">band</span> retraction in Drosophila.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Lynch, Holley E; Crews, Sarah M; Rosenthal, Brett; Kim, Elliott; Gish, Robert; Echiverri, Karl; Hutson, M Shane</p> <p>2013-12-15</p> <p>Germ <span class="hlt">band</span> retraction involves a dramatic rearrangement of the tissues on the surface of the Drosophila embryo. As germ <span class="hlt">band</span> retraction commences, one tissue, the germ <span class="hlt">band</span>, wraps around another, the amnioserosa. Through retraction the two tissues move cohesively as the highly elongated cells of the amnioserosa contract and the germ <span class="hlt">band</span> moves so it is only on one side of the embryo. To understand the mechanical drivers of this process, we designed a series of laser ablations that suggest a mechanical role for the amnioserosa. First, we find that during mid retraction, segments in the curve of the germ <span class="hlt">band</span> are under anisotropic tension. The largest tensions are in the direction in which the amnioserosa contracts. Second, ablating one lateral flank of the amnioserosa reduces the <span class="hlt">observed</span> force anisotropy and leads to retraction failures. The other intact flank of amnioserosa is insufficient to drive retraction, but can support some germ <span class="hlt">band</span> cell elongation and is thus not a full phenocopy of ush mutants. Another ablation-induced failure in retraction can phenocopy mys mutants, and does so by targeting amnioserosa cells in the same region where the mutant fails to adhere to the germ <span class="hlt">band</span>. We conclude that the amnioserosa must play a key, but assistive, mechanical role that aids uncurling of the germ <span class="hlt">band</span>. © 2013 Elsevier Inc. All rights reserved.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3856716','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3856716"><span>Cellular Mechanics of Germ <span class="hlt">Band</span> Retraction in Drosophila</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Lynch, Holley E.; Crews, Sarah M.; Rosenthal, Brett; Kim, Elliott; Gish, Robert; Echiverri, Karl; Hutson, M. Shane</p> <p>2013-01-01</p> <p>Germ <span class="hlt">band</span> retraction involves a dramatic rearrangement of the tissues on the surface of the Drosophila embryo. As germ <span class="hlt">band</span> retraction commences, one tissue, the germ <span class="hlt">band</span>, wraps around another, the amnioserosa. Through retraction the two tissues move cohesively as the highly elongated cells of the amnioserosa contract and the germ <span class="hlt">band</span> moves so it is only on one side of the embryo. To understand the mechanical drivers of this process, we designed a series of laser ablations that suggest a mechanical role for the amnioserosa. First, we find that during mid retraction, segments in the curve of the germ <span class="hlt">band</span> are under anisotropic tension. The largest tensions are in the direction in which the amnioserosa contracts. Second, ablating one lateral flank of the amnioserosa reduces the <span class="hlt">observed</span> force anisotropy and leads to retraction failures. The other intact flank of amnioserosa is insufficient to drive retraction, but can support some germ <span class="hlt">band</span> cell elongation and is thus not a full phenocopy of ush mutants. Another ablation-induced failure in retraction can phenocopy mys mutants, and does so by targeting amnioserosa cells in the same region where the mutant fails to adhere to the germ <span class="hlt">band</span>. We conclude that the amnioserosa must play a key, but assistive, mechanical role that aids uncurling of the germ <span class="hlt">band</span>. PMID:24135149</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018AIPC.1953c0097P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018AIPC.1953c0097P"><span><span class="hlt">Observation</span> of shift in <span class="hlt">band</span> gap with annealing in hydrothermally synthesized TiO2-thin films</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Pawar, Vani; Jha, Pardeep K.; Singh, Prabhakar</p> <p>2018-05-01</p> <p>Anatase TiO2 thin films were synthesized by hydrothermal method. The films were fabricated on a glass substrate by spin coating unit and annealed at 500 °C for 2 hours in ambient atmosphere. The effect of annealing on microstructure and optical properties of TiO2 thin films namely, just deposited and annealed thin film were investigated. The XRD data confirms the tetragonal crystalline structure of the films with space group I41/amd. The surface morphology suggests that TiO2 particles are almost homogeneous in size and annealing of the film affect the grain growth of the particles. The <span class="hlt">band</span> gap energy increases from 2.81 to 3.34 eV. On the basis of our <span class="hlt">observation</span>, it can be concluded that the annealing of TiO2 thin films enhances the absorption range and it may find potential application in the field of solar cells.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013PhDT........77O','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013PhDT........77O"><span>Hydrologic applications of GPS site-<span class="hlt">position</span> <span class="hlt">observations</span> in the Western U.S</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ouellette, Karli J.</p> <p></p> <p>Permanent Global <span class="hlt">Positioning</span> System (GPS) networks have been established around the globe for a variety of uses, most notably to monitor the activity of fault lines and tectonic plate motion. A model for utilizing GPS as a tool for hydrologic monitoring is also developed. First, <span class="hlt">observations</span> of the recent movement of the land surface throughout California by the Scripps Orbit and Permanent Array Center (SOPAC) GPS network are explored. Significant seasonal cycles and long term trends are related to historical <span class="hlt">observations</span> of land subsidence. The pattern of deformation throughout the state appears to be caused by the occurrence of poroelastic deformation of the aquifer in the Central Valley, and elastic crustal loading by surface water and the winter snowpack in the Sierra Nevada Mountains. The result is a sort of teeter-totter motion between the Valley and the mountains where the Valley sinks in the dry season while the mountains lift, and the mountains sink in the wet season while the Valley lifts. Next, the elastic crustal deformation caused by the winter snowpack is explored more thoroughly at 6 high elevations throughout the Western United States. Expected annual deformation as a result of thermoelastic and snow water equivalent are calculated using SNOTEL <span class="hlt">observations</span> and an elastic half-space model. The results demonstrate the dominance of snow loading on the seasonal vertical land surface deformation at all 6 GPS stations. The model is then reversed and applied to the GPS vertical site-<span class="hlt">position</span> <span class="hlt">observations</span> in order to predict snow water equivalent. The results are compared to SNOTEL <span class="hlt">observations</span> of snow water equivalent and soil moisture. The study concludes that GPS site-<span class="hlt">position</span> <span class="hlt">observations</span> are able to predict variations in snow water equivalent and soil moisture with good accuracy. Then a model which incorporates both elastic crustal loading and poroelastic deformation was used to predict groundwater storage variations at 54 GPS stations throughout the</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20170005641','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20170005641"><span>Satellite Communications for Unmanned Aircraft C2 Links: C-<span class="hlt">Band</span>, Ku-<span class="hlt">Band</span> and Ka-<span class="hlt">Band</span></span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Kerczewski, Robert J.; Wilson, Jeffrey D.; Bishop, William D.</p> <p>2016-01-01</p> <p>Unmanned aircraft (UA) that require access to controlled (or non-segregated) airspace require a highly reliable and robust command and control (C2) link, operating over protected aviation spectrum. While operating within radio line-of-sight (LOS) UA can make use of air-to-ground C2 links to terrestrial stations. When operating beyond LOS (BLOS) where a group of networked terrestrial stations does not exist to provide effective BLOS coverage, a satellite communications link is required. Protected aviation spectrum for satellite C2 links has only recently been allocated in <span class="hlt">bands</span> where operational satellites exist. A previously existing C-<span class="hlt">Band</span> allocation covers a <span class="hlt">bands</span> where there are currently no operational satellites. The new allocations, within the Fixed Satellite Service <span class="hlt">bands</span> at Ku and Ka-<span class="hlt">Bands</span> will not be finalized until 2023 due to the need for the development of standards and technical decisions on the operation of UA satellite C2 links within these <span class="hlt">bands</span>. This paper provides an overview of BLOS satellite C2 links, some of the conditions which will need to be met for the operation of such links, and a look at some aspects of spectrum sharing which may constrain these operations.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010JNav...63..527K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010JNav...63..527K"><span>Locata Performance Evaluation in the Presence of Wide- and Narrow-<span class="hlt">Band</span> Interference</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Khan, Faisal A.; Rizos, Chris; Dempster, Andrew G.</p> <p></p> <p>Classically difficult <span class="hlt">positioning</span> environments often call for augmentation technology to assist the GPS, or more generally the Global Navigation Satellite System (GNSS) technology. The ground-based ranging technology offers augmentation, and even replacement, to GPS in such environments. However, like any other system relying on wireless technology, a Locata <span class="hlt">positioning</span> network also faces issues in the presence of RF interference (RFI). This problem is magnified due to the fact that Locata operates in the licence-free 2·4 GHz Industrial, Scientific and Medical (ISM) <span class="hlt">band</span>. The licence-free nature of this <span class="hlt">band</span> attracts a much larger number of devices using a wider range of signal types than for licensed <span class="hlt">bands</span>, resulting in elevation of the noise floor. Also, harmonics from out-of-<span class="hlt">band</span> signals can act as potential interferers. WiFi devices operating in this <span class="hlt">band</span> have been identified as the most likely potential interferer, due partially to their use of the whole ISM <span class="hlt">band</span>, but also because Locata applications often also may use a wireless network. This paper evaluates the performance of Locata in the presence of both narrow- and wide-<span class="hlt">band</span> interfering signals. Effects of received interference on both raw measurements and final solutions are reported and analysed. Test results show that Locata performance degrades in the presence of received interference. It is also identified that high levels of received interference can affect Locata carriers even if the interference is not in co-frequency situation with the affected carrier. Finally, Locata characteristics have been identified which can be exploited to mitigate RFI issues.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3058943','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3058943"><span>Disturbances in the <span class="hlt">positioning</span>, proliferation, and apoptosis of neural progenitors contribute to subcortical <span class="hlt">band</span> heterotopia formation</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Fitzgerald, MP; Covio, M; Lee, KS</p> <p>2011-01-01</p> <p>Cortical malformations are commonly associated with intractable epilepsy and other developmental disorders. Our studies utilize the tish rat, a spontaneously occurring genetic model of subcortical <span class="hlt">band</span> heterotopia (SBH) associated with epilepsy, to evaluate the developmental events underlying SBH formation in the neocortex. Our results demonstrate that Pax6+ and Tbr2+ progenitors are mislocalized in tish+/− and tish−/− neocortex throughout neurogenesis. In addition, mislocalized tish−/− progenitors possess a longer cell cycle than wildtype or normally-<span class="hlt">positioned</span> tish−/− progenitors, owing to a lengthened G2+M+G1 time. This mislocalization is not associated with adherens junction breakdown or loss of radial glial polarity in the ventricular zone, as assessed by immunohistochemistry against phalloidin (to identify F-actin), aPKC-λ, and Par3. However, vimentin immunohistochemistry indicates that the radial glial scaffold is disrupted in the region of the tish−/− heterotopia. Moreover, lineage tracing experiments using in utero electroporation in tish−/− neocortex demonstrate that mislocalized progenitors do not retain contact with the ventricular surface and that ventricular/subventricular zone progenitors produce neurons that migrate into both the heterotopia and cortical plate. Taken together, these findings define a series of developmental errors contributing to SBH formation that differs fundamentally from a primary error in neuronal migration. PMID:21145942</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010ApJ...718..920C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010ApJ...718..920C"><span>Near-infrared Thermal Emission from TrES-3b: A Ks-<span class="hlt">band</span> Detection and an H-<span class="hlt">band</span> Upper Limit on the Depth of the Secondary Eclipse</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Croll, Bryce; Jayawardhana, Ray; Fortney, Jonathan J.; Lafrenière, David; Albert, Loic</p> <p>2010-08-01</p> <p>We present H- and Ks-<span class="hlt">band</span> photometry bracketing the secondary eclipse of the hot Jupiter TrES-3b using the Wide-field Infrared Camera on the Canada-France-Hawaii Telescope. We detect the secondary eclipse of TrES-3b with a depth of 0.133+0.018 -0.016% in the Ks <span class="hlt">band</span> (8σ)—a result that is in sharp contrast to the eclipse depth reported by de Mooij & Snellen. We do not detect its thermal emission in the H <span class="hlt">band</span>, but place a 3σ limit of 0.051% on the depth of the secondary eclipse in this <span class="hlt">band</span>. A secondary eclipse of this depth in Ks requires very efficient day-to-nightside redistribution of heat and nearly isotropic reradiation, a conclusion that is in agreement with longer wavelength, mid-infrared Spitzer <span class="hlt">observations</span>. Our 3σ upper limit on the depth of our H-<span class="hlt">band</span> secondary eclipse also argues for very efficient redistribution of heat and suggests that the atmospheric layer probed by these <span class="hlt">observations</span> may be well homogenized. However, our H-<span class="hlt">band</span> upper limit is so constraining that it suggests the possibility of a temperature inversion at depth, or an absorbing molecule, such as methane, that further depresses the emitted flux at this wavelength. The combination of our near-infrared measurements and those obtained with Spitzer suggests that TrES-3b displays a near-isothermal dayside atmospheric temperature structure, whose spectrum is well approximated by a blackbody. We emphasize that our strict H-<span class="hlt">band</span> limit is in stark disagreement with the best-fit atmospheric model that results from longer wavelength <span class="hlt">observations</span> only, thus highlighting the importance of near-infrared <span class="hlt">observations</span> at multiple wavelengths, in addition to those returned by Spitzer in the mid-infrared, to facilitate a comprehensive understanding of the energy budgets of transiting exoplanets. Based on <span class="hlt">observations</span> obtained with WIRCam, a joint project of CFHT, Taiwan, Korea, Canada, France, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li class="active"><span>21</span></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_21 --> <div id="page_22" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li class="active"><span>22</span></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li><a href="#" onclick='return showDiv("page_24");'>24</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="421"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20000072482&hterms=Polycyclic+aromatic+hydrocarbons&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3DPolycyclic%2Baromatic%2Bhydrocarbons','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20000072482&hterms=Polycyclic+aromatic+hydrocarbons&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3DPolycyclic%2Baromatic%2Bhydrocarbons"><span>Spatial Variation of the 3.29 and 3.40 Micron Emission <span class="hlt">Bands</span> Within Reflection Nebulae and The Photochemical Evolution of Methylated Polycyclic Aromatic Hydrocarbons</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Joblin, C.; Tielens, A. G. G. M.; Allamandola, L. J.; Geballe, T. R.</p> <p>1996-01-01</p> <p>Spectra of 3 microns emission features have been obtained at several <span class="hlt">positions</span> within the reflection nebulae NGC 1333 SVS3 and NGC 2023. Strong variations of the relative intensities of the 3.29 microns feature and its most prominent satellite <span class="hlt">band</span> at 3.40 microns are found. It is shown that: (1) the 3.40 microns <span class="hlt">band</span> is too intense with respect to the 3.29 microns <span class="hlt">band</span> at certain <span class="hlt">positions</span> to arise from hot <span class="hlt">band</span> emission alone, (2) the 3.40 microns <span class="hlt">band</span> can be reasonably well matched by new laboratory spectra of gas-phase polycyclic aromatic hydrocarbons (PAHs) with alkyl (-CH3) side groups, and (3) the variations in the 3.40 microns to 3.29 microns <span class="hlt">band</span> intensity ratios are consistent with the photochemical erosion of alkylated PAHs. We conclude that the 3.40 microns emission feature is attributable to -CH3 side groups on PAH molecules. We predict a value of 0.5 for the peak intensity ratio of the 3.40 and 3.29 microns emission <span class="hlt">bands</span> from free PAHs in the diffuse interstellar medium, which would correspond to a proportion of one methyl group for four peripheral hydrogens. We also compare the 3 microns spectrum of the proto-planetary nebula IRAS 05341 + 0852 with the spectrum of the planetary nebula IRAS 21282 + 5050. We suggest that a photochemical evolution of the initial aliphatic and aromatic hydrocarbon mixture formed in the outflow is responsible for the changes <span class="hlt">observed</span> in the 3 microns emission spectra of these objects.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20040090012&hterms=Polycyclic+aromatic+hydrocarbons&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3DPolycyclic%2Baromatic%2Bhydrocarbons','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20040090012&hterms=Polycyclic+aromatic+hydrocarbons&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3DPolycyclic%2Baromatic%2Bhydrocarbons"><span>Spatial variation of the 3.29 and 3.40 micron emission <span class="hlt">bands</span> within reflection nebulae and the photochemical evolution of methylated polycyclic aromatic hydrocarbons</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Joblin, C.; Tielens, A. G.; Allamandola, L. J.; Geballe, T. R.</p> <p>1996-01-01</p> <p>Spectra of 3 micrometers emission features have been obtained at several <span class="hlt">positions</span> within the reflection nebulae NGC 1333 SVS3 and NGC 2023. Strong variations of the relative intensities of the 3.29 micrometers feature and its most prominent satellite <span class="hlt">band</span> at 3.40 micrometers are found. It is shown that (i) the 3.40 micrometers <span class="hlt">band</span> is too intense with respect to the 3.29 micrometers <span class="hlt">band</span> at certain <span class="hlt">positions</span> to arise from hot <span class="hlt">band</span> emission alone, (ii) the 3.40 micrometers <span class="hlt">band</span> can be reasonably well matched by new laboratory spectra of gas-phase polycyclic aromatic hydrocarbons (PAHs) with alkyl (-CH3) side groups, and (iii) the variations in the 3.40 micrometers to 3.29 micrometers <span class="hlt">band</span> intensity ratios are consistent with the photochemical erosion of alkylated PAHs. We conclude that the 3.40 micrometers emission feature is attributable to -CH3 side groups on PAH molecules. We predict a value of 0.5 for the peak intensity ratio of the 3.40 and 3.29 micrometers emission <span class="hlt">bands</span> from free PAHs in the diffuse interstellar medium, which would correspond to a proportion of one methyl group for four peripheral hydrogens. We also compare the 3 micrometers spectrum of the proto-planetary nebula IRAS 05341+0852 with the spectrum of the planetary nebula IRAS 21282+5050. We suggest that a photochemical evolution of the initial aliphatic and aromatic hydrocarbon mixture formed in the outflow is responsible for the changes <span class="hlt">observed</span> in the 3 micrometers emission spectra of these objects.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018JPhD...51r5102C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018JPhD...51r5102C"><span>Reconfigurable dual-<span class="hlt">band</span> metamaterial antenna based on liquid crystals</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Che, Bang-Jun; Meng, Fan-Yi; Lyu, Yue-Long; Wu, Qun</p> <p>2018-05-01</p> <p>In this paper, a novel reconfigurable dual-<span class="hlt">band</span> metamaterial antenna with a continuous beam that is electrically steered in backward to forward directions is first proposed by employing a liquid crystal (LC)-loaded tunable extended composite right-/left-handed (E-CRLH) transmission line (TL). The frequency-dependent property of the E-CRLH TL is analyzed and a compact unit cell based on the nematic LC is proposed to realize the tunable dual <span class="hlt">band</span> characteristics. The phase constant of the proposed unit cell can be dynamically continuously tuned from negative to <span class="hlt">positive</span> values in two operating <span class="hlt">bands</span> by changing the bias voltage of the loaded LC material. A resulting dual <span class="hlt">band</span> fixed-frequency beam steering property has been predicted by numerical simulations and experimentally verified. The measured results show that the fabricated reconfigurable antenna features an electrically controlled continuous beam steering from backward  ‑16° to forward  +13° at 7.2 GHz and backward  ‑9° to forward  +17° at 9.4 GHz, respectively. This electrically controlled beam steering range turns out to be competitive with the previously reported single <span class="hlt">band</span> reconfigurable antennas. Besides, the measured and simulated results of the proposed reconfigurable dual-<span class="hlt">band</span> metamaterial antenna are in good agreement.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012AGUFM.H23C1379D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012AGUFM.H23C1379D"><span>Posterior uncertainty of GEOS-5 L-<span class="hlt">band</span> radiative transfer model parameters and brightness temperatures after calibration with SMOS <span class="hlt">observations</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>De Lannoy, G. J.; Reichle, R. H.; Vrugt, J. A.</p> <p>2012-12-01</p> <p>Simulated L-<span class="hlt">band</span> (1.4 GHz) brightness temperatures are very sensitive to the values of the parameters in the radiative transfer model (RTM). We assess the optimum RTM parameter values and their (posterior) uncertainty in the Goddard Earth <span class="hlt">Observing</span> System (GEOS-5) land surface model using <span class="hlt">observations</span> of multi-angular brightness temperature over North America from the Soil Moisture Ocean Salinity (SMOS) mission. Two different parameter estimation methods are being compared: (i) a particle swarm optimization (PSO) approach, and (ii) an MCMC simulation procedure using the differential evolution adaptive Metropolis (DREAM) algorithm. Our results demonstrate that both methods provide similar "optimal" parameter values. Yet, DREAM exhibits better convergence properties, resulting in a reduced spread of the posterior ensemble. The posterior parameter distributions derived with both methods are used for predictive uncertainty estimation of brightness temperature. This presentation will highlight our model-data synthesis framework and summarize our initial findings.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20120010450','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20120010450"><span>Dichroic Filter for Separating W-<span class="hlt">Band</span> and Ka-<span class="hlt">Band</span></span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Epp, Larry W.; Durden, Stephen L.; Jamnejad, Vahraz; Long, Ezra M.; Sosnowski, John B.; Higuera, Raymond J.; Chen, Jacqueline C.</p> <p>2012-01-01</p> <p>The proposed Aerosol/Cloud/Ecosystems (ACEs) mission development would advance cloud profiling radar from that used in CloudSat by adding a 35-GHz (Ka-<span class="hlt">band</span>) channel to the 94-GHz (W-<span class="hlt">band</span>) channel used in CloudSat. In order to illuminate a single antenna, and use CloudSat-like quasi-optical transmission lines, a spatial diplexer is needed to add the Ka-<span class="hlt">band</span> channel. A dichroic filter separates Ka-<span class="hlt">band</span> from W-<span class="hlt">band</span> by employing advances in electrical discharge machining (EDM) and mode-matching analysis techniques developed and validated for designing dichroics for the Deep Space Network (DSN), to develop a preliminary design that both met the requirements of frequency separation and mechanical strength. First, a mechanical prototype was built using an approximately 102-micron-diameter EDM process, and tolerances of the hole dimensions, wall thickness, radius, and dichroic filter thickness measured. The prototype validated the manufacturing needed to design a dichroic filter for a higher-frequency usage than previously used in the DSN. The initial design was based on a Ka-<span class="hlt">band</span> design, but thicker walls are required for mechanical rigidity than one obtains by simply scaling the Ka-<span class="hlt">band</span> dichroic filter. The resulting trade of hole dimensions for mechanical rigidity (wall thickness) required electrical redesign of the hole dimensions. Updates to existing codes in the linear solver decreased the analysis time using mode-matching, enabling the electrical design to be realized quickly. This work is applicable to missions and instruments that seek to extend W-<span class="hlt">band</span> cloud profiling measurements to other frequencies. By demonstrating a dichroic filter that passes W-<span class="hlt">band</span>, but reflects a lower frequency, this opens up the development of instruments that both compare to and enhance CloudSat.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016EGUGA..18.5236L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016EGUGA..18.5236L"><span>Precisely determined the surface displacement by the ionospheric mitigation using the L-<span class="hlt">band</span> SAR Interferometry over Mt.Baekdu</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Lee, Won-Jin; Jung, Hyung-Sup; Park, Sun-Cheon; Lee, Duk Kee</p> <p>2016-04-01</p> <p>Mt. Baekdu (Changbaishan in Chinese) is located on the border between China and North Korea. It has recently attracted the attention of volcanic unrest during 2002-2005. Many researchers have applied geophysical approaches to detect magma system of beneath Mt.Baekdu such as leveling, Global <span class="hlt">Positioning</span> System (GPS), gases analysis, seismic analysis, etc. Among them, deformation measuring instruments are important tool to evaluate for volcanism. In contrast to GPS or other deformation measuring instruments, Synthetic Aperture Radar Interferometry (InSAR) has provided high resolution of 2-D surface displacement from remote sensed data. However, Mt. Baekdu area has disturbed by decorrelation on interferogram because of wide vegetation coverage. To overcome this limitation, L-<span class="hlt">band</span> system of long wavelength is more effective to detect surface deformation. In spite of this advantage, L-<span class="hlt">band</span> can surfer from more severe ionospheric phase distortions than X- or C- <span class="hlt">band</span> system because ionospheric phase distortions are inverse proportion to the radar frequency. Recently, Multiple Aperture Interferometry (MAI) based ionospheric phase distortions mitigation method have proposed and investigated. We have applied this technique to the Mt.Baekdu area to measure surface deformation precisely using L-<span class="hlt">band</span> Advanced Land <span class="hlt">Observing</span> Satellite-1(ALOS-1) Phased Array type L-<span class="hlt">band</span> Synthetic Aperture Radar(PALSAR) data acquiring from 2006 to 2011.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=1447507','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=1447507"><span><span class="hlt">Band</span> structures of TiO2 doped with N, C and B*</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Xu, Tian-Hua; Song, Chen-Lu; Liu, Yong; Han, Gao-Rong</p> <p>2006-01-01</p> <p>This study on the <span class="hlt">band</span> structures and charge densities of nitrogen (N)-, carbon (C)- and boron (B)-doped titanium dioxide (TiO2) by first-principles simulation with the CASTEP code (Segall et al., 2002) showed that the three 2p <span class="hlt">bands</span> of impurity atom are located above the valence-<span class="hlt">band</span> maximum and below the Ti 3d <span class="hlt">bands</span>, and that along with the decreasing of impurity atomic number, the fluctuations become more intensive. We cannot <span class="hlt">observe</span> obvious <span class="hlt">band</span>-gap narrowing in our result. Therefore, the cause of absorption in visible light might be the isolated impurity atom 2p states in <span class="hlt">band</span>-gap rather than the <span class="hlt">band</span>-gap narrowing. PMID:16532532</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20070035137','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20070035137"><span>Soil Moisture Retrieval During a Corn Growth Cycle using L-<span class="hlt">band</span> (1.6 GHz) Radar <span class="hlt">Observations</span></span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Joseph, Alicia T.; vanderVelde, Rogier; O'Neill, Peggy E.; Lang, Roger; Gish, Tim</p> <p>2007-01-01</p> <p>New opportunities for large-scale soil moisture monitoring will emerge with the launch of two low frequency (L-<span class="hlt">band</span> 1.4 GHz) radiometers: the Aquarius mission in 2009 and the Soil Moisture and Ocean Salinity (SMOS) mission in 2008. Soil moisture is an important land surface variable affecting water and heat exchanges between atmosphere, land surface and deeper ground water reservoirs. The data products from these sensors provide valuable information in a range of climate and hydrologic applications (e.g., numecal weather prediction, drought monitoring, flood forecasting, water resources management, etc.). This paper describes a unique data set that was collected during a field campaign at OPE^ (Optimizing Production Inputs for Economic and Environmental Enhancements) site in Beltsville, Maryland throughout the eompj2ete corn growing in 2002. This investigation describes a simple methodology to correct active microwave <span class="hlt">observations</span> for vegetation effects, which could potentially be implemented in a global soil moisture monitoring algorithm. The methodology has been applied to radar <span class="hlt">observation</span> collected during the entire corn growth season and validation against ground measurements showed that the top 5-cm soil moisture can be retrieved with an accuracy up to 0.033 [cu cm/cu cm] depending on the sensing configuration.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19940017111','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19940017111"><span>Using parallel <span class="hlt">banded</span> linear system solvers in generalized eigenvalue problems</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Zhang, Hong; Moss, William F.</p> <p>1993-01-01</p> <p>Subspace iteration is a reliable and cost effective method for solving <span class="hlt">positive</span> definite <span class="hlt">banded</span> symmetric generalized eigenproblems, especially in the case of large scale problems. This paper discusses an algorithm that makes use of two parallel <span class="hlt">banded</span> solvers in subspace iteration. A shift is introduced to decompose the <span class="hlt">banded</span> linear systems into relatively independent subsystems and to accelerate the iterations. With this shift, an eigenproblem is mapped efficiently into the memories of a multiprocessor and a high speed-up is obtained for parallel implementations. An optimal shift is a shift that balances total computation and communication costs. Under certain conditions, we show how to estimate an optimal shift analytically using the decay rate for the inverse of a <span class="hlt">banded</span> matrix, and how to improve this estimate. Computational results on iPSC/2 and iPSC/860 multiprocessors are presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24999245','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24999245"><span>Multiple sclerosis patients lacking oligoclonal <span class="hlt">bands</span> in the cerebrospinal fluid have less global and regional brain atrophy.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Ferreira, Daniel; Voevodskaya, Olga; Imrell, Kerstin; Stawiarz, Leszek; Spulber, Gabriela; Wahlund, Lars-Olof; Hillert, Jan; Westman, Eric; Karrenbauer, Virginija Danylaité</p> <p>2014-09-15</p> <p>To investigate whether multiple sclerosis (MS) patients with and without cerebrospinal fluid (CSF) oligoclonal immunoglobulin G <span class="hlt">bands</span> (OCB) differ in brain atrophy. Twenty-eight OCB-negative and thirty-five OCB-<span class="hlt">positive</span> patients were included. Larger volumes of total CSF and white matter (WM) lesions; smaller gray matter (GM) volume in the basal ganglia, diencephalon, cerebellum, and hippocampus; and smaller WM volume in corpus callosum, periventricular-deep WM, brainstem, and cerebellum, were <span class="hlt">observed</span> in OCB-<span class="hlt">positives</span>. OCB-negative patients, known to differ genetically from OCB-<span class="hlt">positives</span>, are characterized by less global and regional brain atrophy. This finding supports the notion that OCB-negative MS patients may represent a clinically relevant MS subgroup. Copyright © 2014 Elsevier B.V. All rights reserved.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016AGUFM.G41B1034C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016AGUFM.G41B1034C"><span>Broad-<span class="hlt">Band</span> Analysis of Polar Motion Excitations</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Chen, J.</p> <p>2016-12-01</p> <p>Earth rotational changes, i.e. polar motion and length-of-day (LOD), are driven by two types of geophysical excitations: 1) mass redistribution within the Earth system, and 2) angular momentum exchange between the solid Earth (more precisely the crust) and other components of the Earth system. Accurate quantification of Earth rotational excitations has been difficult, due to the lack of global-scale <span class="hlt">observations</span> of mass redistribution and angular momentum exchange. The over 14-years time-variable gravity measurements from the Gravity Recovery and Climate Experiment (GRACE) have provided a unique means for quantifying Earth rotational excitations from mass redistribution in different components of the climate system. Comparisons between <span class="hlt">observed</span> Earth rotational changes and geophysical excitations estimated from GRACE, satellite laser ranging (SLR) and climate models show that GRACE-derived excitations agree remarkably well with polar motion <span class="hlt">observations</span> over a broad-<span class="hlt">band</span> of frequencies. GRACE estimates also suggest that accelerated polar region ice melting in recent years and corresponding sea level rise have played an important role in driving long-term polar motion as well. With several estimates of polar motion excitations, it is possible to estimate broad-<span class="hlt">band</span> noise variance and noise power spectra in each, given reasonable assumptions about noise independence. Results based on GRACE CSR RL05 solutions clearly outperform other estimates with the lowest noise levels over a broad <span class="hlt">band</span> of frequencies.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19910035431&hterms=petroleum&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dpetroleum','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19910035431&hterms=petroleum&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dpetroleum"><span>The <span class="hlt">observation</span> of spectral variation indicative of porphyrin biomarkers in reflectance spectra of source rock - The application of remote sensing technology to petroleum geochemistry</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Holden, Peter Newhall; Gaffey, Michael J.</p> <p>1990-01-01</p> <p>The spectral signature of porphyrin compounds, considered to be biomarkers of depositional environment and thermal maturity, have been identified in reflectance spectra of oil shales. The key <span class="hlt">bands</span> identified, in order of intensity, are the Soret (0.40 microns), alpha (0.57 microns), and beta (0.53 microns) <span class="hlt">bands</span>. The <span class="hlt">observed</span> <span class="hlt">bands</span> represent the composite spectral signature of all porphyrin compounds present in the sample and, therefore, change <span class="hlt">position</span> and intensity in accordance with changes in porphyrin chemistry.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24484540','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24484540"><span>Use of a three-<span class="hlt">band</span> HRP2/pLDH combination rapid diagnostic test increases diagnostic specificity for falciparum malaria in Ugandan children.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Hawkes, Michael; Conroy, Andrea L; Opoka, Robert O; Namasopo, Sophie; Liles, W Conrad; John, Chandy C; Kain, Kevin C</p> <p>2014-02-01</p> <p>Rapid diagnostic tests (RDTs) for malaria provide a practical alternative to light microscopy for malaria diagnosis in resource-limited settings. Three-<span class="hlt">band</span> RDTs incorporating two parasite antigens may have enhanced diagnostic specificity, relative to two-<span class="hlt">band</span> RDTs with a single parasite antigen (typically histidine-rich protein 2 [HRP2]). Phase 1: 2,000 children, two months to five years of age, admitted to a referral hospital in Jinja, Uganda, with acute febrile illness were enrolled. A WHO highly rated three-<span class="hlt">band</span> RDT was compared to light microscopy of thick peripheral blood films read by local expert microscopists.Phase 2: the three-<span class="hlt">band</span> RDT was used as a screening tool for inclusion of patients in a clinical trial, and subjects with three <span class="hlt">positive</span> RDT <span class="hlt">bands</span> were tested by microscopy using blood samples drawn in parallel. Discordant results were adjudicated by PCR. Phase 1: 1,648 children had both a RDT and peripheral blood smear performed. The specificity of a RDT with all three <span class="hlt">bands</span> <span class="hlt">positive</span> was 82% (95% CI: 79-85%) compared to 62% (95% CI: 59-66%) for HRP2 alone. The sensitivity was 88% (95% CI: 85-89%) and 94% (95% CI: 92-95%) for three-<span class="hlt">band</span> <span class="hlt">positive</span> RDT and HRP2 antigen, respectively. 119 patients (7.2%) had a <span class="hlt">positive</span> HRP2 <span class="hlt">band</span>, but negative parasite lactate dehydrogenase (pLHD) <span class="hlt">band</span> and negative peripheral smear, and 72 (61%) of these had received pre-treatment with anti-malarials, suggesting a false <span class="hlt">positive</span> HRP2 result (p = 0.002).Phase 2: the <span class="hlt">positive</span> predictive value (PPV) of the three-<span class="hlt">band</span> RDT was 94% (95% CI 89%-97%) using microscopy as the reference standard. However, microscopy-discordant results were shown to be <span class="hlt">positive</span> for P. falciparum by PCR in all cases, suggesting that the PPV was in fact higher. The pLDH antigen on three-<span class="hlt">band</span> RDTs, used in combination with HRP2, provides added diagnostic specificity for malaria parasitaemia and may be useful to distinguish acute infection from recently treated infection. In situations where</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/23062670','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/23062670"><span>Tension <span class="hlt">band</span> wiring of the olecranon: is it really a dynamic principle of osteosynthesis?</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Brink, P R G; Windolf, M; de Boer, P; Brianza, S; Braunstein, V; Schwieger, K</p> <p>2013-04-01</p> <p>The tension <span class="hlt">band</span> principle as applied to transverse olecranon fractures fixed by tension <span class="hlt">band</span> wiring is based on the premise that distraction forces on the outer cortex of the ulna during elbow flexion are converted to compression forces on the articular surface of the olecranon at the fracture site. In view of some clinical outcomes, where hardware failure and secondary dislocations occur, the question arises if the dynamic compression theory is correct. Compressive forces during active flexion and extension after tension <span class="hlt">band</span> wiring of a transverse osteotomy of the olecranon were measured in 6 fresh frozen human cadaveric models using a pressure-sensor in the osteotomy gap. We could collect 30 measurements during active flexion and 30 during active extension. Active flexion did not cause any compressive forces in the osteotomy gap. Extension with the humerus in an upright <span class="hlt">position</span> and the elbow actively extended causes some compression (0.37-0.51 MPa) at the articular surface comparing with active flexion (0.2 MPa) due to gravity forces. Posterior, there was no significant pressure difference <span class="hlt">observed</span> (0.41-0.45 versus 0.36-0.32 MPa) between active flexion and extension. The tension <span class="hlt">band</span> wiring principle only exists during active extension in a range of 30-120° of flexion of the elbow. Postoperative exercise programs should be modified in order to prevent loss of compression at the fracture site of transverse olecranon fractures, treated with tension <span class="hlt">band</span> wiring when the elbow is mobilised. Copyright © 2012 Elsevier Ltd. All rights reserved.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.dtic.mil/docs/citations/ADA412962','DTIC-ST'); return false;" href="http://www.dtic.mil/docs/citations/ADA412962"><span>C (G)-<span class="hlt">Band</span> & X (I) - <span class="hlt">Band</span> Noncoherent Radar Transponder Performance Specification Standard</span></a></p> <p><a target="_blank" href="http://www.dtic.mil/">DTIC Science & Technology</a></p> <p></p> <p>2002-04-01</p> <p>TRAINING RANGE NEVADA TEST SITE STANDARD 262-02 ELECTRONIC TRAJECTORY MEASUREMENTS GROUP C (G) – <span class="hlt">BAND</span> & X (I) – <span class="hlt">BAND</span> NONCOHERENT RADAR...Date 00 Apr 2002 Report Type N/A Dates Covered (from... to) - Title and Subtitle C (G)-<span class="hlt">Band</span> & X (I) - <span class="hlt">Band</span> Noncoherent Radar Transponder...Number of Pages 157 i STANDARD 262-02 C (G) – <span class="hlt">BAND</span> & X (I) – <span class="hlt">BAND</span> NONCOHERENT RADAR TRANSPONDER PERFORMANCE SPECIFICATION STANDARD APRIL 2002 Prepared by</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1344110-superconducting-transitions-flat-band-systems','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1344110-superconducting-transitions-flat-band-systems"><span>Superconducting transitions in flat-<span class="hlt">band</span> systems</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Iglovikov, V. I.; Hébert, F.; Grémaud, B.; ...</p> <p>2014-09-11</p> <p>The physics of strongly correlated quantum particles within a flat <span class="hlt">band</span> was originally explored as a route to itinerant ferromagnetism and, indeed, a celebrated theorem by Lieb rigorously establishes that the ground state of the repulsive Hubbard model on a bipartite lattice with unequal number of sites in each sublattice must have nonzero spin S at half-filling. Recently, there has been interest in Lieb geometries due to the possibility of novel topological insulator, nematic, and Bose-Einstein condensed (BEC) phases. In this paper, we extend the understanding of the attractive Hubbard model on the Lieb lattice by using Determinant Quantum Montemore » Carlo to study real space charge and pair correlation functions not addressed by the Lieb theorems. Specifically, our results show unusual charge and charge transfer signatures within the flat <span class="hlt">band</span>, and a reduction in pairing order at ρ = 2/3 and ρ = 4/3, the points at which the flat <span class="hlt">band</span> is first occupied and then completely filled. Lastly, we compare our results to the case of flat <span class="hlt">bands</span> in the Kagome lattice and demonstrate that the behavior <span class="hlt">observed</span> in the two cases is rather different.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20150000880','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20150000880"><span>Studying NASA's Transition to Ka-<span class="hlt">Band</span> Communications for Low Earth Orbit</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Chelmins, David; Reinhart, Richard; Mortensen, Dale; Welch, Bryan; Downey, Joseph; Evans, Mike</p> <p>2014-01-01</p> <p>As the S-<span class="hlt">band</span> spectrum becomes crowded, future space missions will need to consider moving command and telemetry services to Ka-<span class="hlt">band</span>. NASAs Space Communications and Navigation (SCaN) Testbed provides a software-defined radio (SDR) platform that is capable of supporting investigation of this service transition. The testbed contains two S-<span class="hlt">band</span> SDRs and one Ka-<span class="hlt">band</span> SDR. Over the past year, SCaN Testbed has demonstrated Ka-<span class="hlt">band</span> communications capabilities with NASAs Tracking and Data Relay Satellite System (TDRSS) using both open- and closed-loop antenna tracking profiles. A number of technical areas need to be addressed for successful transition to Ka-<span class="hlt">band</span>. The smaller antenna beamwidth at Ka-<span class="hlt">band</span> increases the criticality of antenna pointing, necessitating closed loop tracking algorithms and new techniques for received power estimation. Additionally, the antenna pointing routines require enhanced knowledge of spacecraft <span class="hlt">position</span> and attitude for initial acquisition, versus an S-<span class="hlt">band</span> antenna. Ka-<span class="hlt">band</span> provides a number of technical advantages for bulk data transfer. Unlike at S-<span class="hlt">band</span>, a larger bandwidth may be available for space missions, allowing increased data rates. The potential for high rate data transfer can also be extended for direct-to-ground links through use of variable or adaptive coding and modulation. Specific examples of Ka-<span class="hlt">band</span> research from SCaN Testbeds first year of operation will be cited, such as communications link performance with TDRSS, and the effects of truss flexure on antenna pointing.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20140016968','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20140016968"><span>Studying NASA's Transition to Ka-<span class="hlt">Band</span> Communications for Low Earth Orbit</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Chelmins, David T.; Reinhart, Richard C.; Mortensen, Dale; Welch, Bryan; Downey, Joseph; Evans, Michael</p> <p>2014-01-01</p> <p>As the S-<span class="hlt">band</span> spectrum becomes crowded, future space missions will need to consider moving command and telemetry services to Ka-<span class="hlt">band</span>. NASA's Space Communications and Navigation (SCaN) Testbed provides a software-defined radio (SDR) platform that is capable of supporting investigation of this service transition. The testbed contains two S-<span class="hlt">band</span> SDRs and one Ka-<span class="hlt">band</span> SDR. Over the past year, SCaN Testbed has demonstrated Ka-<span class="hlt">band</span> communications capabilities with NASAs Tracking and Data Relay Satellite System (TDRSS) using both open- and closed-loop antenna tracking profiles. A number of technical areas need to be addressed for successful transition to Ka-<span class="hlt">band</span>. The smaller antenna beamwidth at Ka-<span class="hlt">band</span> increases the criticality of antenna pointing, necessitating closed loop tracking algorithms and new techniques for received power estimation. Additionally, the antenna pointing routines require enhanced knowledge of spacecraft <span class="hlt">position</span> and attitude for initial acquisition, versus an S-<span class="hlt">band</span> antenna. Ka-<span class="hlt">band</span> provides a number of technical advantages for bulk data transfer. Unlike at S-<span class="hlt">band</span>, a larger bandwidth may be available for space missions, allowing increased data rates. The potential for high rate data transfer can also be extended for direct-to-ground links through use of variable or adaptive coding and modulation. Specific examples of Ka-<span class="hlt">band</span> research from SCaN Testbeds first year of operation will be cited, such as communications link performance with TDRSS, and the effects of truss flexure on antenna pointing.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/1444096','SCIGOV-STC'); return false;" href="https://www.osti.gov/servlets/purl/1444096"><span>Tunable dual-<span class="hlt">band</span> graphene-based infrared reflectance filter</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Goldflam, Michael D.; Ruiz, Isaac; Howell, Stephen W.</p> <p></p> <p>Here, we experimentally demonstrated an actively tunable optical filter that controls the amplitude of reflected long-wave-infrared light in two separate spectral regions concurrently. Our device exploits the dependence of the excitation energy of plasmons in a continuous and unpatterned sheet of graphene on the Fermi-level, which can be controlled via conventional electrostatic gating. The filter enables simultaneous modification of two distinct spectral <span class="hlt">bands</span> whose <span class="hlt">positions</span> are dictated by the device geometry and graphene plasmon dispersion. Within these <span class="hlt">bands</span>, the reflected amplitude can be varied by over 15% and resonance <span class="hlt">positions</span> can be shifted by over 90 cm –1. Electromagnetic simulationsmore » verify that tuning arises through coupling of incident light to graphene plasmons by a grating structure. Importantly, the tunable range is determined by a combination of graphene properties, device structure, and the surrounding dielectrics, which dictate the plasmon dispersion. Thus, the underlying design shown here is applicable across a broad range of infrared frequencies.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/29715819','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/29715819"><span>Tunable dual-<span class="hlt">band</span> graphene-based infrared reflectance filter.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Goldflam, Michael D; Ruiz, Isaac; Howell, Stephen W; Wendt, Joel R; Sinclair, Michael B; Peters, David W; Beechem, Thomas E</p> <p>2018-04-02</p> <p>We experimentally demonstrated an actively tunable optical filter that controls the amplitude of reflected long-wave-infrared light in two separate spectral regions concurrently. Our device exploits the dependence of the excitation energy of plasmons in a continuous and unpatterned sheet of graphene on the Fermi-level, which can be controlled via conventional electrostatic gating. The filter enables simultaneous modification of two distinct spectral <span class="hlt">bands</span> whose <span class="hlt">positions</span> are dictated by the device geometry and graphene plasmon dispersion. Within these <span class="hlt">bands</span>, the reflected amplitude can be varied by over 15% and resonance <span class="hlt">positions</span> can be shifted by over 90 cm -1 . Electromagnetic simulations verify that tuning arises through coupling of incident light to graphene plasmons by a grating structure. Importantly, the tunable range is determined by a combination of graphene properties, device structure, and the surrounding dielectrics, which dictate the plasmon dispersion. Thus, the underlying design shown here is applicable across a broad range of infrared frequencies.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li class="active"><span>22</span></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li><a href="#" onclick='return showDiv("page_24");'>24</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_22 --> <div id="page_23" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li class="active"><span>23</span></li> <li><a href="#" onclick='return showDiv("page_24");'>24</a></li> <li><a href="#" onclick='return showDiv("page_25");'>25</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="441"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1444096-tunable-dual-band-graphene-based-infrared-reflectance-filter','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1444096-tunable-dual-band-graphene-based-infrared-reflectance-filter"><span>Tunable dual-<span class="hlt">band</span> graphene-based infrared reflectance filter</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Goldflam, Michael D.; Ruiz, Isaac; Howell, Stephen W.; ...</p> <p>2018-03-23</p> <p>Here, we experimentally demonstrated an actively tunable optical filter that controls the amplitude of reflected long-wave-infrared light in two separate spectral regions concurrently. Our device exploits the dependence of the excitation energy of plasmons in a continuous and unpatterned sheet of graphene on the Fermi-level, which can be controlled via conventional electrostatic gating. The filter enables simultaneous modification of two distinct spectral <span class="hlt">bands</span> whose <span class="hlt">positions</span> are dictated by the device geometry and graphene plasmon dispersion. Within these <span class="hlt">bands</span>, the reflected amplitude can be varied by over 15% and resonance <span class="hlt">positions</span> can be shifted by over 90 cm –1. Electromagnetic simulationsmore » verify that tuning arises through coupling of incident light to graphene plasmons by a grating structure. Importantly, the tunable range is determined by a combination of graphene properties, device structure, and the surrounding dielectrics, which dictate the plasmon dispersion. Thus, the underlying design shown here is applicable across a broad range of infrared frequencies.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018JQSRT.211..172A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018JQSRT.211..172A"><span>High accuracy line <span class="hlt">positions</span> of the ν1 fundamental <span class="hlt">band</span> of 14N216O</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>AlSaif, Bidoor; Lamperti, Marco; Gatti, Davide; Laporta, Paolo; Fermann, Martin; Farooq, Aamir; Lyulin, Oleg; Campargue, Alain; Marangoni, Marco</p> <p>2018-05-01</p> <p>The ν1 fundamental <span class="hlt">band</span> of N2O is examined by a novel spectrometer that relies on the frequency locking of an external-cavity quantum cascade laser around 7.8 μm to a near-infrared Tm:based frequency comb at 1.9 μm. Due to the large tunability, nearly 70 lines in the 1240-1310 cm-1 range of the ν1 <span class="hlt">band</span> of N2O, from P(40) to R(31), are for the first time measured with an absolute frequency calibration and an uncertainty from 62 to 180 kHz, depending on the line. Accurate values of the spectroscopic constants of the upper state are derived from a fit of the line centers (rms ≈ 4.8 × 10-6 cm-1 or 144 kHz). The ν1 transitions presently measured in a Doppler regime validate high accuracy predictions based on sub-Doppler measurements of the ν3 and ν3-ν1 transitions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2002AGUFM.T71E1217S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2002AGUFM.T71E1217S"><span>Deformation <span class="hlt">Bands</span> in an Exhumed Oil Reservoir, Corona del Mar, California, USA</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sample, J.; Woods, S.; Bender, E.; Loveall, M.</p> <p>2002-12-01</p> <p>Deformation <span class="hlt">bands</span> in coarse-grained sandstones are commonly narrow zones of reduced porosity that restrict migration of fluids. Deformation <span class="hlt">bands</span> are known from core <span class="hlt">observations</span> and outcrop studies, but we present for the first time results from an exhumed oil reservoir. The deformation <span class="hlt">bands</span> occur in a poorly consolidated, oil-bearing sandstone of the Miocene Monterey Formation, within the active, right-slip Newport-Inglewood fault zone (NIFZ). The deformation <span class="hlt">bands</span> crop out as resistant ribs and fins in a very coarse-grained sandstone comprising mainly quartz and feldspar detritus. Deformation <span class="hlt">bands</span> strike 323°, similar to the NIFZ, and dip variably (N = 113). There are three clusters of dips within the main set: 88NE, 60NE, and 47SW. A fourth cluster has an orientation of 353 °, 70W. Although the kinematic history is complex, steep <span class="hlt">bands</span> generally are youngest. Deformation <span class="hlt">bands</span> exhibit both normal and right-slip separations, but net slip was rarely possible to determine. The deformation <span class="hlt">bands</span> are closely spaced. They formed by porosity reduction and locally cataclasis. Most deformation <span class="hlt">bands</span> are oil-free, indicating formation before oil migration, and that they were barriers to flow. There are at least two modes of oil-bearing <span class="hlt">bands</span>: 1) <span class="hlt">bands</span> with oil in pore spaces; and 2) <span class="hlt">bands</span> containing oil in small open pockets, especially lining the edges of <span class="hlt">bands</span>. Case 1 suggests that porosity reduction did not completely preclude oil penetration or that at least some <span class="hlt">band</span> formation occurred after oil migration. Case 2 is consistent with reactivation of <span class="hlt">bands</span> as tensional features, perhaps late in the evolution of the reservoir. Other evidence for late-stage tensional deformation during oil migration includes the presence of young sandstone dikes and bitumen veins up to 7 cm in width lined with euhedral quartz. The relationships <span class="hlt">observed</span> at Corona del Mar are generally consistent with deformation <span class="hlt">bands</span> acting as barriers to flow, but clearly deformation <span class="hlt">bands</span> can be</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018ISPAr42.3.1085L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018ISPAr42.3.1085L"><span>Sharpending of the Vnir and SWIR <span class="hlt">Bands</span> of the Wide <span class="hlt">Band</span> Spectral Imager Onboard Tiangong-II Imagery Using the Selected <span class="hlt">Bands</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Liu, Q.; Li, X.; Liu, G.; Huang, C.; Li, H.; Guan, X.</p> <p>2018-04-01</p> <p>The Tiangong-II space lab was launched at the Jiuquan Satellite Launch Center of China on September 15, 2016. The Wide <span class="hlt">Band</span> Spectral Imager (WBSI) onboard the Tiangong-II has 14 visible and near-infrared (VNIR) spectral <span class="hlt">bands</span> covering the range from 403-990 nm and two shortwave infrared (SWIR) <span class="hlt">bands</span> covering the range from 1230-1250 nm and 1628-1652 nm respectively. In this paper the selected <span class="hlt">bands</span> are proposed which aims at considering the closest spectral similarities between the VNIR with 100 m spatial resolution and SWIR <span class="hlt">bands</span> with 200 m spatial resolution. The evaluation of Gram-Schmidt transform (GS) sharpening techniques embedded in ENVI software is presented based on four types of the different low resolution pan <span class="hlt">band</span>. The experimental results indicated that the VNIR <span class="hlt">band</span> with higher CC value with the raw SWIR <span class="hlt">Band</span> was selected, more texture information was injected the corresponding sharpened SWIR <span class="hlt">band</span> image, and at that time another sharpened SWIR <span class="hlt">band</span> image preserve the similar spectral and texture characteristics to the raw SWIR <span class="hlt">band</span> image.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018JGRA..123.3063C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018JGRA..123.3063C"><span>ISUAL-<span class="hlt">Observed</span> Blue Luminous Events: The Associated Sferics</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Chou, Jung-Kuang; Hsu, Rue-Ron; Su, Han-Tzong; Chen, Alfred Bing-Chih; Kuo, Cheng-Ling; Huang, Sung-Ming; Chang, Shu-Chun; Peng, Kang-Ming; Wu, Yen-Jung</p> <p>2018-04-01</p> <p>The blue luminous events (BLEs) recorded by ISUAL (Imager of Sprites and Upper Atmospheric Lightning) radiate unambiguous middle ultraviolet to blue emissions (230-450 nm) but contain dim red emissions (623-754 nm). The BLE appears to be dot-like on one ISUAL image with an integration time of 29 ms. A few BLEs develop upward into blue jets/starters or type II gigantic jets (GJs). The associated sferics of the BLEs in the extremely low frequency to very low frequency <span class="hlt">band</span> and in the low-frequency <span class="hlt">band</span> exhibit similar patterns to the narrow bipolar events (NBEs) identified in the very low frequency and low-frequency <span class="hlt">band</span>. The ISUAL BLEs are conjectured to be the accompanied light emissions of the NBEs. Both upward and downward propagating current obtained from the associated sferics of the BLEs have been found. The source heights of the six BLEs related to negative NBEs are estimated in the range of 16.2-17.8 km. These six events are suggested to occur between the upper <span class="hlt">positive</span> charge layer and the negative screen charge layer on the top of the normally electrified thunderstorm. The six blue starters, one blue jet, and one type II GJ are inferred to be <span class="hlt">positive</span> upward discharges from their associated sferics in the extremely low frequency to very low frequency <span class="hlt">band</span>. Based on the simultaneous radio and optical <span class="hlt">observations</span>, a NBE is conjectured to be the initiation discharge with rapidly flowing current within the thunderstorm, while a blue jet/starter or a type II GJ is suggested to be the ensuing discharge with slowly varying current propagating upward from the thunderstorm.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015A%26A...580A..76G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015A%26A...580A..76G"><span>Astrometric <span class="hlt">positions</span> for 18 irregular satellites of giant planets from 23 years of <span class="hlt">observations</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gomes-Júnior, A. R.; Assafin, M.; Vieira-Martins, R.; Arlot, J.-E.; Camargo, J. I. B.; Braga-Ribas, F.; da Silva Neto, D. N.; Andrei, A. H.; Dias-Oliveira, A.; Morgado, B. E.; Benedetti-Rossi, G.; Duchemin, Y.; Desmars, J.; Lainey, V.; Thuillot, W.</p> <p>2015-08-01</p> <p>Context. The irregular satellites of the giant planets are believed to have been captured during the evolution of the solar system. Knowing their physical parameters, such as size, density, and albedo is important for constraining where they came from and how they were captured. The best way to obtain these parameters are <span class="hlt">observations</span> in situ by spacecrafts or from stellar occultations by the objects. Both techniques demand that the orbits are well known. Aims: We aimed to obtain good astrometric <span class="hlt">positions</span> of irregular satellites to improve their orbits and ephemeris. Methods: We identified and reduced <span class="hlt">observations</span> of several irregular satellites from three databases containing more than 8000 images obtained between 1992 and 2014 at three sites (Observatório do Pico dos Dias, Observatoire de Haute-Provence, and European Southern Observatory - La Silla). We used the software Platform for Reduction of Astronomical Images Automatically (PRAIA) to make the astrometric reduction of the CCD frames. The UCAC4 catalog represented the International Celestial Reference System in the reductions. Identification of the satellites in the frames was done through their ephemerides as determined from the SPICE/NAIF kernels. Some procedures were followed to overcome missing or incomplete information (coordinates, date), mostly for the older images. Results: We managed to obtain more than 6000 <span class="hlt">positions</span> for 18 irregular satellites: 12 of Jupiter, 4 of Saturn, 1 of Uranus (Sycorax), and 1 of Neptune (Nereid). For some satellites the number of obtained <span class="hlt">positions</span> is more than 50% of what was used in earlier orbital numerical integrations. Conclusions: Comparison of our <span class="hlt">positions</span> with recent JPL ephemeris suggests there are systematic errors in the orbits for some of the irregular satellites. The most evident case was an error in the inclination of Carme. <span class="hlt">Position</span> tables are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19800017026','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19800017026"><span>Shuttle Ku-<span class="hlt">band</span> and S-<span class="hlt">band</span> communications implementation study</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Dodds, J. G.; Huth, G. K.; Nilsen, P. W.; Polydoros, A.; Simon, M. K.; Weber, C. L.</p> <p>1980-01-01</p> <p>Various aspects of the shuttle orbiter S-<span class="hlt">band</span> network communication system, the S-<span class="hlt">band</span> payload communication system, and the Ku-<span class="hlt">band</span> communication system are considered. A method is proposed for obtaining more accurate S-<span class="hlt">band</span> antenna patterns of the actual shuttle orbiter vehicle during flight because the preliminary antenna patterns using mock-ups are not realistic that they do not include the effects of additional appendages such as wings and tail structures. The Ku-<span class="hlt">band</span> communication system is discussed especially the TDRS antenna pointing accuracy with respect to the orbiter and the modifications required and resulting performance characteristics of the convolutionally encoded high data rate return link to maintain bit synchronizer lock on the ground. The TDRS user constraints on data bit clock jitter and data asymmetry on unbalanced QPSK with noisy phase references are included. The S-<span class="hlt">band</span> payload communication system study is outlined including the advantages and experimental results of a peak regulator design built and evaluated by Axiomatrix for the bent-pipe link versus the existing RMS-type regulator. The nominal sweep rate for the deep-space transponder of 250 Hz/s, and effects of phase noise on the performance of a communication system are analyzed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012ChPhB..21e4101Z','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012ChPhB..21e4101Z"><span>Dual-<span class="hlt">band</span> frequency selective surface with large <span class="hlt">band</span> separation and stable performance</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Zhou, Hang; Qu, Shao-Bo; Peng, Wei-Dong; Lin, Bao-Qin; Wang, Jia-Fu; Ma, Hua; Zhang, Jie-Qiu; Bai, Peng; Wang, Xu-Hua; Xu, Zhuo</p> <p>2012-05-01</p> <p>A new technique of designing a dual-<span class="hlt">band</span> frequency selective surface with large <span class="hlt">band</span> separation is presented. This technique is based on a delicately designed topology of L- and Ku-<span class="hlt">band</span> microwave filters. The two <span class="hlt">band</span>-pass responses are generated by a capacitively-loaded square-loop frequency selective surface and an aperture-coupled frequency selective surface, respectively. A Faraday cage is located between the two frequency selective surface structures to eliminate undesired couplings. Based on this technique, a dual-<span class="hlt">band</span> frequency selective surface with large <span class="hlt">band</span> separation is designed, which possesses large <span class="hlt">band</span> separation, high selectivity, and stable performance under various incident angles and different polarizations.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016ApPhA.122...70B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016ApPhA.122...70B"><span>Electronic <span class="hlt">band</span> structure and Shubnikov-de Haas effect in two-dimensional semimetallic InAs/GaSb nanostructure superlattice</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Boutramine, Abderrazak; Nafidi, Abdelhakim; Barkissy, Driss; El-Frikhe, Es-Said; Charifi, Hicham; Elanique, Abdellatif; Chaib, Hassan</p> <p>2016-02-01</p> <p>We have investigated the <span class="hlt">band</span> structure E( d = d 1 + d 2), E( k z) and E( k p), respectively, as a function of the SL period, d, in the growth direction and in plan of InAs( d 1 = 160 Å)/GaSb( d 2 = 105 Å) type II superlattice, performed in the envelope function formalism with the valence <span class="hlt">band</span> offset, Λ, of 510 meV at 4.2 K. For the ratio d 1/ d 2 = 1.52, d and Λ dependence of the SL energy <span class="hlt">band</span> gap show that the semiconductor-to-semimetal transition takes place at d c = 173 Å and Λ c = 463 meV. Therefore, this sample is semimetallic. The <span class="hlt">position</span> of the Fermi level, E F = 500.2 meV, indicates n type conductivity. The spectra of energy, E( k z, k p), show a negative <span class="hlt">band</span> gap of -48.3 meV. The cutoff wavelength | λ c| = 25.7 µm indicates that this sample can be used as a far-infrared detector. Further, we have interpreted the minima of the magnetoresistance oscillations, Shubnikov-de Haas effect, <span class="hlt">observed</span> by D. M. Symons et al.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.ars.usda.gov/research/publications/publication/?seqNo115=257635','TEKTRAN'); return false;" href="http://www.ars.usda.gov/research/publications/publication/?seqNo115=257635"><span>L <span class="hlt">band</span> brightness temperature <span class="hlt">observations</span> over a corn canopy during the entire growth cycle</span></a></p> <p><a target="_blank" href="https://www.ars.usda.gov/research/publications/find-a-publication/">USDA-ARS?s Scientific Manuscript database</a></p> <p></p> <p></p> <p>During a field campaign covering the 2002 corn growing season, a dual polarized tower mounted L-<span class="hlt">band</span> (1.4 GHz) radiometer (LRAD) provided brightness temperature (T¬B) measurements at preset intervals, incidence and azimuth angles. These radiometer measurements were supported by an extensive characte...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1998AIPC..429..285D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1998AIPC..429..285D"><span>Shear <span class="hlt">band</span> formation in plastic bonded explosive (PBX)</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Dey, T. N.; Johnson, J. N.</p> <p>1998-07-01</p> <p>Adiabatic shear <span class="hlt">bands</span> can be a source of ignition and lead to detonation. At low to moderate deformation rates, 10-1000 s-1, two other mechanisms can also give rise to shear <span class="hlt">bands</span>. These mechanisms are: 1) softening caused by micro-cracking and 2) a constitutive response with a non-associated flow rule as is <span class="hlt">observed</span> in granular material such as soil. Brittle behavior at small strains and the granular nature of HMX suggest that PBX-9501 constitutive behavior may be similar to sand. A constitutive model for the first of these mechanisms is studied in a series of calculations. This viscoelastic constitutive model for PBX-9501 softens via a statistical crack model. A sand model is used to provide a non-associated flow rule and detailed results will be reported elsewhere. Both models generate shear <span class="hlt">band</span> formation at 1-2% strain at nominal strain rates at and below 1000 s-1. Shear <span class="hlt">band</span> formation is suppressed at higher strain rates. Both mechanisms may accelerate the formation of adiabatic shear <span class="hlt">bands</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/979197-multi-quasiparticle-gamma-band-structure-neutron-deficient-ce-nd-isotopes','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/979197-multi-quasiparticle-gamma-band-structure-neutron-deficient-ce-nd-isotopes"><span>Multi-Quasiparticle Gamma-<span class="hlt">Band</span> Structure in Neutron-Deficient Ce and Nd Isotopes</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Sheikh, Javid; Bhat, G. H.; Palit, R.</p> <p>2009-01-01</p> <p>The newly developed multi-quasiparticle triaxial projected shell-model approach is employed to study the high-spin <span class="hlt">band</span> structures in neutron-deficient even-even Ce and Nd isotopes. It is <span class="hlt">observed</span> that gamma <span class="hlt">bands</span> are built on each intrinsic configuration of the triaxial mean-field deformation. Due to the fact that a triaxial configuration is a superposition of several K states, the projection from these states results in several low-lying <span class="hlt">bands</span> originating from the same intrinsic configuration. This generalizes the well-known concept of the surface gamma oscillation in deformed nuclei based on the ground state to gamma <span class="hlt">bands</span> built on multi-quasiparticle configurations. This new feature providesmore » an alternative explanation on the <span class="hlt">observation</span> of two I=10 aligning states in ^{134}Ce and both exhibiting a neutron character.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/26057035','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/26057035"><span>CPM Signals for Satellite Navigation in the S and C <span class="hlt">Bands</span>.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Xue, Rui; Sun, Yanbo; Zhao, Danfeng</p> <p>2015-06-05</p> <p>Frequency allocations in the L <span class="hlt">band</span> suitable for global navigation satellite system (GNSS) services are getting crowded and system providers face an ever tougher job when they try to bring in new signals and services while maintaining radio frequency compatibility. With the successive opening of the S and C <span class="hlt">bands</span> to GNSS service, the multi-<span class="hlt">band</span> combined navigation is predicted to become a key technology for future high-precision <span class="hlt">positioning</span> navigation systems, and a single modulation scheme satisfying the requirements in each <span class="hlt">band</span> is a promising solution for reducing user terminal complexity. A universal modulation scheme based on the continuous phase modulation (CPM) family suitable for the above <span class="hlt">bands</span>' demands is proposed. Moreover, this paper has put forward two specific CPM signals for the S and C <span class="hlt">bands</span>, respectively. Then the proposed modulation schemes, together with existing candidates, are comprehensively evaluated. Simulation results show that the proposed CPM signals can not only satisfy the constraint condition of compatibility in different <span class="hlt">bands</span> well and reduce user terminal complexity, but also provide superior performance in terms of tracking accuracy, multi-path mitigation and anti-jamming compared to other candidate modulation schemes.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22280620-fine-structure-red-luminescence-band-undoped-gan','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22280620-fine-structure-red-luminescence-band-undoped-gan"><span>Fine structure of the red luminescence <span class="hlt">band</span> in undoped GaN</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Reshchikov, M. A., E-mail: mreshchi@vcu.edu; Usikov, A.; Saint-Petersburg National Research University of Information Technologies, Mechanics and Optics, 49 Kronverkskiy Ave., 197101 Saint Petersburg</p> <p>2014-01-20</p> <p>Many point defects in GaN responsible for broad photoluminescence (PL) <span class="hlt">bands</span> remain unidentified. Their presence in thick GaN layers grown by hydride vapor phase epitaxy (HVPE) detrimentally affects the material quality and may hinder the use of GaN in high-power electronic devices. One of the main PL <span class="hlt">bands</span> in HVPE-grown GaN is the red luminescence (RL) <span class="hlt">band</span> with a maximum at 1.8 eV. We <span class="hlt">observed</span> the fine structure of this <span class="hlt">band</span> with a zero-phonon line (ZPL) at 2.36 eV, which may help to identify the related defect. The shift of the ZPL with excitation intensity and the temperature-related transformation of the RLmore » <span class="hlt">band</span> fine structure indicate that the RL <span class="hlt">band</span> is caused by transitions from a shallow donor (at low temperature) or from the conduction <span class="hlt">band</span> (above 50 K) to an unknown deep acceptor having an energy level 1.130 eV above the valence <span class="hlt">band</span>.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1996JMoSp.175..354W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1996JMoSp.175..354W"><span>The ν 1<span class="hlt">Band</span> System of H-CC-CN (Cyanoacetylene)</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Winther, F.; Klee, S.; Mellau, G.; Naı̈m, S.; Mbosei, L.; Fayt, A.</p> <p>1996-02-01</p> <p>The ν1<span class="hlt">band</span> system of cyanoacetylene (H-CC-CN) has been <span class="hlt">observed</span> with an effective resolution of 0.006 cm-1. ν1= 3327.37085(3) cm-1,B1= 0.15149762(2) cm-1,D1= 1.8065(3) × 10-8cm-1. Several hot <span class="hlt">bands</span> from the statesv5= 1,v6= 1,v7= 1, 2 (l= 0 and 2), 3 (l= 1 and 3), and 4 (l= 0 and 2),v6=v7= 1 (l= 0 and 2), andv6= 1 andv7= 2 (l= 3) have also been <span class="hlt">observed</span> and analyzed. Many <span class="hlt">bands</span> show strong local perturbations due to interactions with states which are combinations of the modes 4, 5, 6, and 7. These perturbing states are also described quantitatively, and rovibrational constants are given.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017FrMat...4...25B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017FrMat...4...25B"><span>Indentation-Induced Shear <span class="hlt">Band</span> Formation in Thin-Film Multilayers</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Bigelow, Shannon; Shen, Yu-Lin</p> <p>2017-08-01</p> <p>We report an exploratory investigation into the cause of shear <span class="hlt">band</span> formation in multilayer thin-films subject to nanoindentation. The material system considered here is composed of alternating aluminum (Al) and silicon carbide (SiC) nanolayers, atop a silicon (Si) substrate. Finite element models are developed in an attempt to reproduce the shear <span class="hlt">banding</span> phenomenon <span class="hlt">observed</span> experimentally. By introducing strain softening into the material model for the hard SiC layers, shear <span class="hlt">bands</span> can be seen to emerge from the indentation site in the finite element analysis. Broad implications, along with possible directions for future work, are discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/882798','SCIGOV-STC'); return false;" href="https://www.osti.gov/servlets/purl/882798"><span>Impurity-<span class="hlt">Band</span> Model for GaP1-xNx</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Fluegel, B.; Zhang, Y.; Geisz, J. F.</p> <p>2005-11-01</p> <p>Low-temperature absorption studies on free-standing GaP1-xNx films provide direct experimental evidence that the host conduction-<span class="hlt">band</span> minimum (CBM) near X1C does not plunge downward with increased nitrogen doping, contrary to what has been suggested recently; rather, it remains stationary for x up to 0.1%. This fact, combined with the results of earlier studies of the CBM at ..GAMMA.. and conduction-<span class="hlt">band</span> edge near L, confirms that the giant bandgap lowering <span class="hlt">observed</span> in GaP1-xNx results from a CBM that evolves purely from nitrogen impurity <span class="hlt">bands</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016A%26A...595A.104A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016A%26A...595A.104A"><span>Sunspot <span class="hlt">positions</span>, areas, and group tilt angles for 1611-1631 from <span class="hlt">observations</span> by Christoph Scheiner</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Arlt, R.; Senthamizh Pavai, V.; Schmiel, C.; Spada, F.</p> <p>2016-11-01</p> <p>Aims: Digital images of <span class="hlt">observations</span> printed in the books Rosa Ursina sive solis and Prodromus pro sole mobili by Christoph Scheiner, as well as the drawings from Scheiner's letters to Marcus Welser, are analysed to obtain information on the <span class="hlt">positions</span> and sizes of sunspots that appeared before the Maunder minimum. Methods: In most cases, the given orientation of the ecliptic is used to set up the heliographic coordinate system for the drawings. <span class="hlt">Positions</span> and sizes are measured manually on screen. Very early drawings have no indication of their orientation. A rotational matching using common spots of adjacent days is used in some cases, while in other cases, the assumption that images were aligned with a zenith-horizon coordinate system appeared to be the most probable. Results: In total, 8167 sunspots were measured. A distribution of sunspot latitudes versus time (butterfly diagram) is obtained for Scheiner's <span class="hlt">observations</span>. The <span class="hlt">observations</span> of 1611 are very inaccurate, the drawings of 1612 have at least an indication of their orientation, while the remaining part of the spot <span class="hlt">positions</span> from 1618-1631 have good to very good accuracy. We also computed 697 tilt angles of apparently bipolar sunspot groups <span class="hlt">observed</span> in the period 1618-1631. We find that the average tilt angle of nearly 4 degrees is not significantly different from 20th-century values. Data on the sunspot <span class="hlt">position</span> and area are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/595/A104</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/29795946','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/29795946"><span>Is the Factor <span class="hlt">Observed</span> in Investigations on the Item-<span class="hlt">Position</span> Effect Actually the Difficulty Factor?</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Schweizer, Karl; Troche, Stefan</p> <p>2018-02-01</p> <p>In confirmatory factor analysis quite similar models of measurement serve the detection of the difficulty factor and the factor due to the item-<span class="hlt">position</span> effect. The item-<span class="hlt">position</span> effect refers to the increasing dependency among the responses to successively presented items of a test whereas the difficulty factor is ascribed to the wide range of item difficulties. The similarity of the models of measurement hampers the dissociation of these factors. Since the item-<span class="hlt">position</span> effect should theoretically be independent of the item difficulties, the statistical ex post manipulation of the difficulties should enable the discrimination of the two types of factors. This method was investigated in two studies. In the first study, Advanced Progressive Matrices (APM) data of 300 participants were investigated. As expected, the factor thought to be due to the item-<span class="hlt">position</span> effect was <span class="hlt">observed</span>. In the second study, using data simulated to show the major characteristics of the APM data, the wide range of items with various difficulties was set to zero to reduce the likelihood of detecting the difficulty factor. Despite this reduction, however, the factor now identified as item-<span class="hlt">position</span> factor, was <span class="hlt">observed</span> in virtually all simulated datasets.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018AIPC.1942i0031T','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018AIPC.1942i0031T"><span><span class="hlt">Bands</span> dispersion and charge transfer in β-BeH2</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Trivedi, D. K.; Galav, K. L.; Joshi, K. B.</p> <p>2018-04-01</p> <p>Predictive capabilities of ab-initio method are utilised to explore <span class="hlt">bands</span> dispersion and charge transfer in β-BeH2. Investigations are carried out using the linear combination of atomic orbitals method at the level of density functional theory. The crystal structure and related parameters are settled by coupling total energy calculations with the Murnaghan equation of state. Electronic <span class="hlt">bands</span> dispersion from PBE-GGA is reported. The PBE-GGA, and PBE0 hybrid functional, show that β-BeH2 is a direct gap semiconductor with 1.18 and 2.40 eV <span class="hlt">band</span> gap. The <span class="hlt">band</span> gap slowly decreases with pressure and beyond l00 GPa overlap of conduction and valence <span class="hlt">bands</span> at the r point is <span class="hlt">observed</span>. Charge transfer is studied by means of Mullikan population analysis.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li class="active"><span>23</span></li> <li><a href="#" onclick='return showDiv("page_24");'>24</a></li> <li><a href="#" onclick='return showDiv("page_25");'>25</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_23 --> <div id="page_24" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li class="active"><span>24</span></li> <li><a href="#" onclick='return showDiv("page_25");'>25</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="461"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2011ATel.3804....1M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2011ATel.3804....1M"><span>Swift <span class="hlt">observations</span> of SN2011it</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Margutti, R.; Soderberg, A. M.; Milisavljevic, D.</p> <p>2011-12-01</p> <p>SN2011it has been recently classified as a broad-line type-Ic supernova (Tomasella, CBET 2938). A Swift-ToO was executed to <span class="hlt">observe</span> the field of SN2011it starting from 2011-12-08T00:22:48 UT, with the primary aim to constrain the off-axis X-ray emission from the SN. No X-ray source is detected at the optical <span class="hlt">position</span> of the transient with a 3 sigma upper limit of 2.4d-3 cts/s in the 0.3-10 keV energy <span class="hlt">band</span> (total exposure= 8.3 ks).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20140012047','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20140012047"><span>Physical Characterization of Warm Spitzer-<span class="hlt">observed</span> Near-Earth Objects</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Thomas, Cristina A.; Emery, Joshua P.; Trilling, David E.; Delbo, Marco; Hora, Joseph L.; Mueller, Michael</p> <p>2014-01-01</p> <p>Near-infrared spectroscopy of Near-Earth Objects (NEOs) connects diagnostic spectral features to specific surface mineralogies. The combination of spectroscopy with albedos and diameters derived from thermal infrared <span class="hlt">observations</span> can increase the scientific return beyond that of the individual datasets. For instance, some taxonomic classes can be separated into distinct compositional groupings with albedo and different mineralogies with similar albedos can be distinguished with spectroscopy. To that end, we have completed a spectroscopic <span class="hlt">observing</span> campaign to complement the ExploreNEOs Warm Spitzer program that obtained albedos and diameters of nearly 600 NEOs (Trilling et al., 2010). The spectroscopy campaign included visible and near-infrared <span class="hlt">observations</span> of ExploreNEOs targets from various observatories. Here we present the results of <span class="hlt">observations</span> using the low-resolution prism mode (approx. 0.7-2.5 microns) of the SpeX instrument on the NASA Infrared Telescope Facility (IRTF). We also include near-infrared <span class="hlt">observations</span> of Explore-NEOs targets from the MIT-UH-IRTF Joint Campaign for Spectral Reconnaissance. Our dataset includes near-infrared spectra of 187 ExploreNEOs targets (125 <span class="hlt">observations</span> of 92 objects from our survey and 213 <span class="hlt">observations</span> of 154 objects from the MIT survey). We identify a taxonomic class for each spectrum and use <span class="hlt">band</span> parameter analysis to investigate the mineralogies for the S-, Q-, and V-complex objects. Our analysis suggests that for spectra that contain near-infrared data but lack the visible wavelength region, the Bus-DeMeo system misidentifies some S-types as Q-types. We find no correlation between spectral <span class="hlt">band</span> parameters and ExploreNEOs albedos and diameters. We investigate the correlations of phase angle with <span class="hlt">band</span> area ratio and near-infrared spectral slope. We find slightly negative <span class="hlt">Band</span> Area Ratio (BAR) correlations with phase angle for Eros and Ivar, but a <span class="hlt">positive</span> BAR correlation with phase angle for Ganymed.The results of our</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018AIPC.1942e0111S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018AIPC.1942e0111S"><span>Determination of shift in energy of <span class="hlt">band</span> edges and <span class="hlt">band</span> gap of ZnSe spherical quantum dot</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Siboh, Dutem; Kalita, Pradip Kumar; Sarma, Jayanta Kumar; Nath, Nayan Mani</p> <p>2018-04-01</p> <p>We have determined the quantum confinement induced shifts in energy of <span class="hlt">band</span> edges and <span class="hlt">band</span> gap with respect to size of ZnSe spherical quantum dot employing an effective confinement potential model developed in our earlier communication "arXiv:1705.10343". We have also performed phenomenological analysis of our theoretical results in comparison with available experimental data and <span class="hlt">observe</span> a very good agreement in this regard. Phenomenological success achieved in this regard confirms validity of the confining potential model as well as signifies the capability and applicability of the ansatz for the effective confining potential to have reasonable information in the study of real nano-structured spherical systems.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016AGUFMMR43A..01E','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016AGUFMMR43A..01E"><span>Structural and diagenetic evolution of deformation <span class="hlt">bands</span> in contractional and extensional tectonic regimes</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Eichhubl, P.; O'Brien, C. M.; Elliott, S. J.</p> <p>2016-12-01</p> <p>Mechanisms of brittle deformation of sediments and sedimentary rock change with burial because of increasing confining stress, change in pore fluid chemical and temperature conditions, and diagenetic state. In the field, these changes are <span class="hlt">observed</span> in a transition from early non-cataclastic to later cataclastic deformation <span class="hlt">bands</span> and to joint-based structures. Jurassic eolian sandstones in the San Rafael monocline and adjacent San Rafael Desert region, Utah, allow comparison of deformation <span class="hlt">band</span> structures and their diagenetic attributes in contractional and extensional tectonic settings in close proximity. In the Entrada and Navajo Sandstones, we <span class="hlt">observe</span> up to six generations of deformation <span class="hlt">bands</span>, with earliest non-cataclastic <span class="hlt">bands</span> having diffuse boundaries to host rock, and short and irregular traces. Later <span class="hlt">bands</span> are cataclastic, more sharply defined, with long and straight traces. Cataclastic <span class="hlt">bands</span> in the San Rafael monocline are interpreted to form as reverse faults during progressive rotation of the steeply dipping fold limb, resulting in an array of <span class="hlt">bands</span> of varying dip. <span class="hlt">Bands</span> in the San Rafael Desert form as normal faults with a narrower dip range. Although structural characteristics of <span class="hlt">bands</span> differ in extensional and contractional tectonic regimes, cataclastic <span class="hlt">bands</span> in either regime have comparable amount of porosity loss and quartz cementation indicating that tectonic regime does not influence <span class="hlt">band</span> diagenesis. Abundance of quartz cement in <span class="hlt">bands</span>, determined by point counting of SEM images, increases from earlier to later generations of <span class="hlt">bands</span> and, within a single generation, with increasing slip along the <span class="hlt">band</span>, reaching up to 24% of <span class="hlt">band</span> volume. This trend is attributed to an increase in cataclasis with increasing host rock cementation and confining stress during burial, and, within the same generation, with increasing slip. Porosity loss by cementation tends to dominate over porosity loss by mechanical compaction. These findings demonstrate that quartz</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20150014246','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20150014246"><span>Antarctic Analog for Dilational <span class="hlt">Bands</span> on Europa</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hurford, T. A.; Brunt, K. M.</p> <p>2014-01-01</p> <p>Europa's surface shows signs of extension, which is revealed as lithospheric dilation expressed along ridges, dilational <span class="hlt">bands</span> and ridged <span class="hlt">bands</span>. Ridges, the most common tectonic feature on Europa, comprise a central crack flanked by two raised banks a few hundred meters high on each side. Together these three classes may represent a continuum of formation. In Tufts' Dilational Model ridge formation is dominated by daily tidal cycling of a crack, which can be superimposed with regional secular dilation. The two sources of dilation can combine to form the various <span class="hlt">band</span> morphologies <span class="hlt">observed</span>. New GPS data along a rift on the Ross Ice Shelf, Antarctica is a suitable Earth analog to test the framework of Tufts' Dilational Model. As predicted by Tufts' Dilational Model, tensile failures in the Ross Ice Shelf exhibit secular dilation, upon which a tidal signal can be seen. From this analog we conclude that Tufts' Dilational Model for Europan ridges and <span class="hlt">bands</span> may be credible and that the secular dilation is most likely from a regional source and not tidally driven.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014AAS...22334818G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014AAS...22334818G"><span>High Resolution Active Optics <span class="hlt">Observations</span> from the Kepler Follow-up <span class="hlt">Observation</span> Program</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gautier, Thomas N.; Ciardi, D. R.; Marcy, G. W.; Hirsch, L.</p> <p>2014-01-01</p> <p>The ground based follow-up <span class="hlt">observation</span> program for candidate exoplanets discovered with the Kepler observatory has supported a major effort for high resolution imaging of candidate host stars using adaptive optics wave-front correction (AO), speckle imaging and lucky imaging. These images allow examination of the sky as close as a few tenths of an arcsecond from the host stars to detect background objects that might be the source of the Kepler transit signal instead of the host star. This poster reports on the imaging done with AO cameras on the Keck, Palomar 5m and Shane 3m (Lick Observatory) which have been used to obtain high resolution images of over 500 Kepler Object of Interest (KOI) exoplanet candidate host stars. All <span class="hlt">observations</span> were made at near infrared wavelengths in the J, H and K <span class="hlt">bands</span>, mostly using the host target star as the AO guide star. Details of the sensitivity to background objects actually attained by these <span class="hlt">observations</span> and the number of background objects discovered are presented. Implications to the false <span class="hlt">positive</span> rate of the Kepler candidates are discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20120011659','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20120011659"><span>NIMBUS: A Near-Infrared Multi-<span class="hlt">Band</span> Ultraprecise Spectroimager for SOFIA</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>McElwain, Michael W.; Mandell, Avi; Woodgate, Bruce E.; Spiegel, David S.; Madhusudhan, Nikku; Amatucci, Edward; Blake, Cullen; Budinoff, Jason; Burgasser, Adam; Burrows, Adam; <a style="text-decoration: none; " href="javascript:void(0); " onClick="displayelement('author_20120011659'); toggleEditAbsImage('author_20120011659_show'); toggleEditAbsImage('author_20120011659_hide'); "> <img style="display:inline; width:12px; height:12px; " src="images/arrow-up.gif" width="12" height="12" border="0" alt="hide" id="author_20120011659_show"> <img style="width:12px; height:12px; display:none; " src="images/arrow-down.gif" width="12" height="12" border="0" alt="hide" id="author_20120011659_hide"></p> <p>2012-01-01</p> <p>We present a new and innovative near-infrared multi-<span class="hlt">band</span> ultraprecise spectroimager (NIMBUS) for SOFIA. This instrument will enable many exciting <span class="hlt">observations</span> in the new age of precision astronomy. This optical design splits the beam into 8 separate spectral bandpasses, centered around key molecular <span class="hlt">bands</span> from 1 to 4 microns. Each spectral channel has a wide field of view for simultaneous <span class="hlt">observations</span> of a reference star that can decorrelate time-variable atmospheric and optical assembly effects, allowing the instrument to achieve ultraprecise photometry for a wide variety of astrophysical sources</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018A%26A...614A..28L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018A%26A...614A..28L"><span>The EDIBLES survey II. The detectability of C60+ <span class="hlt">bands</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Lallement, R.; Cox, N. L. J.; Cami, J.; Smoker, J.; Fahrang, A.; Elyajouri, M.; Cordiner, M. A.; Linnartz, H.; Smith, K. T.; Ehrenfreund, P.; Foing, B. H.</p> <p>2018-06-01</p> <p>Gas phase spectroscopic laboratory experiments for the buckminsterfullerene cation C60+ have resulted in accurate rest wavelengths for five C60+ transitions that have been compared with diffuse interstellar <span class="hlt">bands</span> (DIBs) in the near infra-red. Detecting these in astronomical spectra is difficult because of the strong contamination of ground-based spectra by atmospheric water vapor, to the presence of weak and shallow stellar lines and/or blending with other weak DIBs. The detection of the two strong <span class="hlt">bands</span> has been claimed by several teams, and the three additional and weaker <span class="hlt">bands</span> have been detected in a few sources. Certain recent papers have argued against the identification of C60+ based on spectral analyses claiming (i) a large variation in the ratio of the equivalent widths of the 9632 and 9577 Å <span class="hlt">bands</span>, (ii) a large redshift of the 9632 Å <span class="hlt">band</span> for the Orion star HD 37022, and (iii) the non-detection of the weaker 9428 Å DIB. Here we address these three points: (i) We show that the model stellar line correction for the 9632 Å DIB overestimates the difference between the strengths of the lines in giant and dwarf star spectra, casting doubts on the conclusions about the ratio variability. (ii) Using high quality stellar spectra from the ESO Diffuse Interstellar <span class="hlt">Bands</span> Large Exploration Survey (EDIBLES), recorded with the ESO/Paranal Ultraviolet Echelle Spectrograph (UVES) in about the same atmospheric conditions, we find no wavelength shift in the 9632 Å <span class="hlt">band</span> toward HD 37022. (iii) Using EDIBLES spectra and data from the Echelle SpectroPolarimetric Device for the <span class="hlt">Observation</span> of Stars (ESPaDOnS) at CFHT we show that the presence of a weak 9428 Å <span class="hlt">band</span> cannot be ruled out, even in the same <span class="hlt">observations</span> that a previous study claimed it was not present.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018Freq...72..237M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018Freq...72..237M"><span>Wideband Bandpass Filter with High Selectivity and an Adjustable Notched-<span class="hlt">band</span> Adopting a Multi-mode Resonator</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ma, Xing-Bing; Jiang, Ting</p> <p>2018-04-01</p> <p>A wideband bandpass filter (BPF) with an adjustable notched-<span class="hlt">band</span> and high selectivity is proposed. The proposed BPF consists of a multi-mode resonator (MMR), two λ/2 resonators, and I/O feed lines with 50 ohm characteristic impedance. The MMR, connected as a whole by a wide stub, is composed of one I-shaped resonator and two open-loop resonators. Tightly coupling is built between MMR and λ/2 resonators. I/O feed lines are directly connected with two λ/2 resonators, respectively. Due to the use of tapped-line coupling, one transmission zero (TZ) is formed near low-edge of aim passband. High-edge of passband with one attendant TZ can be tuned to desired location by adjusting bottom-side <span class="hlt">position</span> of used wide stub or bottom-side length of I-shaped resonator in MMR. The top-side length of I-shaped resonator is applied to improve upper stopband performance and shift undesired resonant mode of MMR near high-edge of aim passband to proper frequency point. The notched-<span class="hlt">band</span> in aim passband is dominated by top-side <span class="hlt">position</span> of wide stub in MMR. Good agreement is <span class="hlt">observed</span> between simulated and measured results.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24734845','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24734845"><span>Secular trends in Cherokee cranial morphology: Eastern vs Western <span class="hlt">bands</span>.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Sutphin, Rebecca; Ross, Ann H; Jantz, Richard L</p> <p>2014-01-01</p> <p>The research objective was to examine if secular trends can be identified for cranial data commissioned by Boas in 1892, specifically for cranial breadth and cranial length of the Eastern and Western <span class="hlt">band</span> Cherokee who experienced environmental hardships. Multiple regression analysis was used to test the degree of relationship between each of the cranial measures: cranial length, cranial breadth and cephalic index, along with predictor variables (year-of-birth, location, sex, admixture); the model revealed a significant difference for all craniometric variables. Additional regression analysis was performed with smoothing Loess plots to <span class="hlt">observe</span> cranial length and cranial breadth change over time (year-of-birth) separately for Eastern and Western Cherokee <span class="hlt">band</span> females and males born between 1783-1874. This revealed the Western and Eastern <span class="hlt">bands</span> show a decrease in cranial length over time. Eastern <span class="hlt">band</span> individuals maintain a relatively constant head breadth, while Western <span class="hlt">Band</span> individuals show a sharp decline beginning around 1860. These findings support negative secular trend occurring for both Cherokee <span class="hlt">bands</span> where the environment made a detrimental impact; this is especially marked with the Western Cherokee <span class="hlt">band</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20060044151&hterms=ionosphere&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3Dionosphere','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20060044151&hterms=ionosphere&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3Dionosphere"><span>Impact of the Ionosphere on an L-<span class="hlt">band</span> Space Based Radar</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Chapin, Elaine; Chan, Samuel F.; Chapman, Bruce D.; Chen, Curtis W.; Martin, Jan M.; Michel, Thierry R.; Muellerschoen, Ronald J.; Pi, Xiaoqing; Rosen, Paul A.</p> <p>2006-01-01</p> <p>We have quantified the impact that the ionosphere would have on a L-<span class="hlt">band</span> interferometric Synthetic Aperture Radar (SAR) mission using a combination of simulation, modeling, Global <span class="hlt">Positioning</span> System (GPS) data collected during the last solar maximum, and existing spaceborne SAR data. We conclude that, except for high latitude scintillation related effects, the ionosphere will not significantly impact the performance of an L-<span class="hlt">band</span> InSAR mission in an appropriate orbit. We evaluated the strength of the ionospheric irregularities using GPS scintillation data collected at Fairbanks, Alaska and modeled the impact of these irregularities on azimuth resolution, azimuth displacement, peak sidelobe ratio (PSLR), and integrated sidelobe ratio (ISLR). Although we predict that less than 5% of auroral zone data would show scintillation related artifacts, certain sites imaged near the equinoxes could be effected up to 25% of the time because the frequency of occurrence of scintillation is a strong function of season and local time of day. Our examination of ionospheric artifacts <span class="hlt">observed</span> in InSAR data has revealed that the artifacts occur primarily in the polar cap data, not auroral zone data as was previously thought.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2008ApJ...688..583H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2008ApJ...688..583H"><span>Deep L'- and M-<span class="hlt">band</span> Imaging for Planets around Vega and epsilon Eridani</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Heinze, A. N.; Hinz, Philip M.; Kenworthy, Matthew; Miller, Douglas; Sivanandam, Suresh</p> <p>2008-11-01</p> <p>We have obtained deep adaptive optics (AO) images of Vega and epsilon Eri to search for planetary mass companions. We <span class="hlt">observed</span> at the MMT in the L' (3.8 μm) and M (4.8 μm) <span class="hlt">bands</span> using Clio, a recently commissioned imager optimized for these wavelengths. <span class="hlt">Observing</span> at these long wavelengths represents a departure from the H <span class="hlt">band</span> (1.65 μm) more commonly used for AO imaging searches for extrasolar planets. The long wavelengths offer better predicted planet/star flux ratios and cleaner (higher Strehl) AO images at the cost of lower diffraction-limited resolution and higher sky background. We have not detected any planets or planet candidates around Vega or epsilon Eri. We report the sensitivities obtained around both stars, which correspond to upper limits on any planetary companions which may exist. The sensitivities of our L'- and M-<span class="hlt">band</span> <span class="hlt">observations</span> are comparable to those of the best H-regime <span class="hlt">observations</span> of these stars. For epsilon Eri, our M-<span class="hlt">band</span> <span class="hlt">observations</span> deliver considerably better sensitivity to close-in planets than any previously published results, and we show that the M <span class="hlt">band</span> is by far the best wavelength choice for attempts at ground-based AO imaging of the known planet epsilon Eri b. The Clio camera itself, with MMTAO, may be capable of detecting epsilon Eri b at its 2010 apastron, given a multinight <span class="hlt">observing</span> campaign. Clio appears to be the only currently existing AO imager that has a realistic possibility of detecting epsilon Eri b. <span class="hlt">Observations</span> reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1327598-asymmetric-band-flipping-time-flight-neutron-diffraction-data','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1327598-asymmetric-band-flipping-time-flight-neutron-diffraction-data"><span>Asymmetric <span class="hlt">band</span> flipping for time-of-flight neutron diffraction data</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Whitfield, Pamela S.; Coelho, Alan A.</p> <p>2016-08-24</p> <p>Charge flipping with powder diffraction data is known to produce a result more reliably with high-resolution data,i.e.visible reflections at smalldspacings. This data are readily accessible with the neutron time-of-flight technique but the assumption that negative scattering density is nonphysical is no longer valid where elements with negative scattering lengths are present. The concept of <span class="hlt">band</span> flipping was introduced in the literature, where a negative threshold is used in addition to a <span class="hlt">positive</span> threshold during the flipping. But, it was not tested with experimental data at the time. Finallly, <span class="hlt">band</span> flipping has been implemented inTOPAStogether with the <span class="hlt">band</span> modification of low-densitymore » elimination and tested with experimental powder and Laue single-crystal neutron data.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20010073720&hterms=alfalfa&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Dalfalfa','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20010073720&hterms=alfalfa&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Dalfalfa"><span>Ground-Based Passive Microwave Remote Sensing <span class="hlt">Observations</span> of Soil Moisture at S and L <span class="hlt">Band</span> with Insight into Measurement Accuracy</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Laymon, Charles A.; Crosson, William L.; Jackson, Thomas J.; Manu, Andrew; Tsegaye, Teferi D.; Soman, V.; Arnold, James E. (Technical Monitor)</p> <p>2001-01-01</p> <p>Accurate estimates of spatially heterogeneous algorithm variables and parameters are required in determining the spatial distribution of soil moisture using radiometer data from aircraft and satellites. A ground-based experiment in passive microwave remote sensing of soil moisture was conducted in Huntsville, Alabama from July 1-14, 1996 to study retrieval algorithms and their sensitivity to variable and parameter specification. With high temporal frequency <span class="hlt">observations</span> at S and L <span class="hlt">band</span>, we were able to <span class="hlt">observe</span> large scale moisture changes following irrigation and rainfall events, as well as diurnal behavior of surface moisture among three plots, one bare, one covered with short grass and another covered with alfalfa. The L <span class="hlt">band</span> emitting depth was determined to be on the order of 0-3 or 0-5 cm below 0.30 cubic centimeter/cubic centimeter with an indication of a shallower emitting depth at higher moisture values. Surface moisture behavior was less apparent on the vegetated plots than it was on the bare plot because there was less moisture gradient and because of difficulty in determining vegetation water content and estimating the vegetation b parameter. Discrepancies between remotely sensed and gravimetric, soil moisture estimates on the vegetated plots point to an incomplete understanding of the requirements needed to correct for the effects of vegetation attenuation. Quantifying the uncertainty in moisture estimates is vital if applications are to utilize remotely-sensed soil moisture data. Computations based only on the real part of the complex dielectric constant and/or an alternative dielectric mixing model contribute a relatively insignificant amount of uncertainty to estimates of soil moisture. Rather, the retrieval algorithm is much more sensitive to soil properties, surface roughness and biomass.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013JGRD..11813338Z','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013JGRD..11813338Z"><span>Anomalous phenomena in Schumann resonance <span class="hlt">band</span> <span class="hlt">observed</span> in China before the 2011 magnitude 9.0 Tohoku-Oki earthquake in Japan</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Zhou, Hongjuan; Zhou, Zhiquan; Qiao, Xiaolin; Yu, Haiyan</p> <p>2013-12-01</p> <p>anomalous phenomena in the Schumann resonance (SR) <span class="hlt">band</span>, possibly associated with the Tohoku-Oki earthquake (EQ), are studied based on the ELF <span class="hlt">observations</span> at two stations in China. The anomaly appeared on 8 March, 3 days prior to the main shock, and was characterized by an increase in the intensity at frequencies from the first mode to the fourth mode in both magnetic field components, different from the <span class="hlt">observations</span> in Japan before large EQs in Taiwan. The abnormal behaviors of the north-south and east-west magnetic field components primarily appeared at 0000-0900 UT and 0200-0900 UT on 8 March, respectively. The finite difference time domain numerical method is applied to model the impact of seismic process on the ELF radio propagation. A partially uniform knee model of the vertical conductivity profile suggested by V. C. Mushtak is used to model the day-night asymmetric Earth-ionosphere cavity, and a locally EQ-induced disturbance model of the atmospheric conductivity is introduced. The atmospheric conductivity is assumed to increase around the epicenter according to the localized enhancement of total electron content in the ionosphere. It is concluded that the SR anomalous phenomena before the Tohoku-Oki EQ have much to do with the excited sources located at South America and Asia and also with the localized distribution of the disturbed conductivity. This work is a further confirmation of the relationship of SR anomalies with large EQs and has further concluded that the distortions in the SR <span class="hlt">band</span> before large EQs may be caused by the irregularities located over the shock epicenter in the Earth-ionosphere cavity by numerical method.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20020028399&hterms=solar+intensity+measurement&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3Dsolar%2Bintensity%2Bmeasurement','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20020028399&hterms=solar+intensity+measurement&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3Dsolar%2Bintensity%2Bmeasurement"><span>Measurements of <span class="hlt">Band</span> Intensities, Herman-Wallis Parameters, and Self-Broadening Line-Widths of the 30011 - 00001 and 30014 - 00001 <span class="hlt">Bands</span> of CO2 at 6503 cm(exp -1) and 6076 cm(exp -1)</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Giver, L. P.; Brown, L. R.; Wattson, R. B.; Spencer, M. N.; Chackerian, C., Jr.; Strawa, Anthony W. (Technical Monitor)</p> <p>1995-01-01</p> <p>Rotationless <span class="hlt">band</span> intensities and Herman-Wallis parameters are listed in HITRAN tabulations for several hundred CO2 overtone-combination <span class="hlt">bands</span>. These parameters are based on laboratory measurements when available, and on DND calculations for the unmeasured <span class="hlt">bands</span>. The DND calculations for the Fermi interacting nv(sub 1) + v(sub 3) polyads show the a(sub 2) Herman-Wallis parameter varying smoothly from a negative value for the first member of the polyad to a <span class="hlt">positive</span> value for the final member. Measurements of the v(sub 1) + v(sub 3) dyad are consistent with the DND calculations for the a(sub 2) parameter, as are our recent measurements of the 4v(sub 1) + v(sub 3) pentad. However, the measurement-based values in the HITRAN tables for the 2v(sub 1) + v(sub 3) triad and the 3v(sub 1) + v(sub 3) tetrad do not support the DND calculated values for the a(sub 2) parameters. We therefore decided to make new measurements to improve some of these intensity parameters. With the McMath FTS at Kitt Peak National Observatory/National Solar Observatory we recorded several spectra of the. 4000 to 8000 cm(exp -1) region of pure CO2 at 0.011 cm(exp -1) resolution using the 6 meter White absorption cell. The signal/noise and absorbance of the first and fourth <span class="hlt">bands</span> of the 3v(sub 1) + v(sub 3) tetrad of C-12O-16 were ideal on these spectra for measuring line intensities and broadening widths. Our selfbroadening results agree with the HITRAN parameterization, while our measurements of the rotationless <span class="hlt">band</span> intensities are about 15% less than the HITRAN values. We find a negative value of a(sub 2) for the 30011-00001 <span class="hlt">band</span> and a <span class="hlt">positive</span> value for the 30014-00001 <span class="hlt">band</span>, whereas the HITRAN values of a(sub 2) are <span class="hlt">positive</span> for all four tetrad <span class="hlt">bands</span>. Our a(sub 1) and a(sub 2) Herman-Wallis parameters are closer to DND calculated values than the 1992 HITRAN values for both the 30011-00001 and the 30014-00001 <span class="hlt">band</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2005APS..MARV14002E','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2005APS..MARV14002E"><span>Interface <span class="hlt">band</span> alignment in high-k gate stacks</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Eric, Bersch; Hartlieb, P.</p> <p>2005-03-01</p> <p>In order to successfully implement alternate high-K dielectric materials into MOS structures, the interface properties of MOS gate stacks must be better understood. Dipoles that may form at the metal/dielectric and dielectric/semiconductor interfaces make the <span class="hlt">band</span> offsets difficult to predict. We have measured the conduction and valence <span class="hlt">band</span> densities of states for a variety MOS stacks using in situ using inverse photoemission (IPE) and photoemission spectroscopy (PES), respectively. Results obtained from clean and metallized (with Ru or Al) HfO2/Si, SiO2/Si and mixed silicate films will be presented. IPE indicates a shift of the conduction <span class="hlt">band</span> minimum (CBM) to higher energy (i.e. away from EF) with increasing SiO2. The effect of metallization on the location of <span class="hlt">band</span> edges depends upon the metal species. The addition of N to the dielectrics shifts the CBM in a way that is thickness dependent. Possible mechanisms for these <span class="hlt">observed</span> effects will be discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22310942-band-gap-engineering-graphene-using-na-sup-ions','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22310942-band-gap-engineering-graphene-using-na-sup-ions"><span><span class="hlt">Band</span> gap engineering for graphene by using Na{sup +} ions</span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Sung, S. J.; Lee, P. R.; Kim, J. G.</p> <p>2014-08-25</p> <p>Despite the noble electronic properties of graphene, its industrial application has been hindered mainly by the absence of a stable means of producing a <span class="hlt">band</span> gap at the Dirac point (DP). We report a new route to open a <span class="hlt">band</span> gap (E{sub g}) at DP in a controlled way by depositing <span class="hlt">positively</span> charged Na{sup +} ions on single layer graphene formed on 6H-SiC(0001) surface. The doping of low energy Na{sup +} ions is found to deplete the π* <span class="hlt">band</span> of graphene above the DP, and simultaneously shift the DP downward away from Fermi energy indicating the opening of E{sub g}.more » The <span class="hlt">band</span> gap increases with increasing Na{sup +} coverage with a maximum E{sub g}≥0.70 eV. Our core-level data, C 1s, Na 2p, and Si 2p, consistently suggest that Na{sup +} ions do not intercalate through graphene, but produce a significant charge asymmetry among the carbon atoms of graphene to cause the opening of a <span class="hlt">band</span> gap. We thus provide a reliable way of producing and tuning the <span class="hlt">band</span> gap of graphene by using Na{sup +} ions, which may play a vital role in utilizing graphene in future nano-electronic devices.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20130001913','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20130001913"><span><span class="hlt">Observations</span> of C-<span class="hlt">Band</span> Brightness Temperature and Ocean Surface Wind Speed and Rain Rate in Hurricanes Earl And Karl (2010)</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Miller, Timothy; James, Mark; Roberts, Brent J.; Biswax, Sayak; Uhlhorn, Eric; Black, Peter; Linwood Jones, W.; Johnson, Jimmy; Farrar, Spencer; Sahawneh, Saleem</p> <p>2012-01-01</p> <p>Ocean surface emission is affected by: a) Sea surface temperature. b) Wind speed (foam fraction). c) Salinity After production of calibrated Tb fields, geophysical fields wind speed and rain rate (or column) are retrieved. HIRAD utilizes NASA Instrument Incubator Technology: a) Provides unique <span class="hlt">observations</span> of sea surface wind, temp and rain b) Advances understanding & prediction of hurricane intensity c) Expands Stepped Frequency Microwave Radiometer capabilities d) Uses synthetic thinned array and RFI mitigation technology of Lightweight Rain Radiometer (NASA Instrument Incubator) Passive Microwave C-<span class="hlt">Band</span> Radiometer with Freq: 4, 5, 6 & 6.6 GHz: a) Version 1: H-pol for ocean wind speed, b) Version 2: dual ]pol for ocean wind vectors. Performance Characteristics: a) Earth Incidence angle: 0deg - 60deg, b) Spatial Resolution: 2-5 km, c) Swath: approx.70 km for 20 km altitude. <span class="hlt">Observational</span> Goals: WS 10 - >85 m/s RR 5 - > 100 mm/hr.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/20960488','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/20960488"><span>Oligoclonal <span class="hlt">bands</span> in cerebrospinal fluid in patients with Tourette's syndrome.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Wenzel, Claudia; Wurster, Ulrich; Müller-Vahl, Kirsten R</p> <p>2011-02-01</p> <p>Since a postinfectious or autoimmune etiology is suggested to be involved in the pathogenesis of Tourette's syndrome (TS), we investigated oligoclonal <span class="hlt">bands</span> (OB) of immunoglobulin G (IgG) in cerebrospinal fluid (CSF), indicating a humoral immune response in the central nervous system. CSF examinations including isoelectric focusing to analyze the presence of OB were performed in 21 TS patients [17 men/4 women, mean age = 29 ± 12 (SD) years]. Isoelectric focusing showed the presence of <span class="hlt">positive</span> OB in 6, borderline <span class="hlt">bands</span> in 2, and serum and CSF <span class="hlt">bands</span> ("mirrored pattern") in another 2 patients. Clinical data did not correlate with CSF findings. Thus, 38% (8 of 21) of our patients exhibited pathological CSF <span class="hlt">bands</span>. Since none of them suffered from another disease known to be associated with OB, our results suggest an association with the pathogenesis of TS itself and point to an involvement of immunological mechanisms in TS pathology. Copyright © 2010 Movement Disorder Society.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li class="active"><span>24</span></li> <li><a href="#" onclick='return showDiv("page_25");'>25</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_24 --> <div id="page_25" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li><a href="#" onclick='return showDiv("page_24");'>24</a></li> <li class="active"><span>25</span></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="481"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012AGUFMOS21D1785P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012AGUFMOS21D1785P"><span>Sensor-centric calibration and characterization of the VIIRS Ocean Color <span class="hlt">bands</span> using Suomi NPP operational data</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Pratt, P.</p> <p>2012-12-01</p> <p>Ocean color <span class="hlt">bands</span> on VIIRS span the visible spectrum and include two NIR <span class="hlt">bands</span>. There are sixteen detectors per <span class="hlt">band</span> and two HAM (Half-angle mirror) sides giving a total of thirty two independent systems. For each scan, thirty two hundred pixels are collected and each has a fixed specific optical path and a dynamic <span class="hlt">position</span> relative to the earth geoid. For a given calibration target where scene variation is minimized, sensor characteristics can be <span class="hlt">observed</span>. This gives insight into the performance and calibration of the instrument from a sensor-centric perspective. Calibration of the blue <span class="hlt">bands</span> is especially challenging since there are few blue targets on land. An ocean region called the South Pacific Gyre (SPG) was chosen for its known stability and large area to serve as a calibration target for this investigation. Thousands of pixels from every granule that views the SPG are collected daily through an automated system and tabulated along with the detector, HAM and scan <span class="hlt">position</span>. These are then collated and organized in a sensor-centric set of tables. The data are then analyzed by slicing by each variable and then plotted in a number of ways over time. Trends in the data show that the VIIRS sensor is largely behaving as expected according to heritage data and also reveals weaknesses where additional characterization of the sensor is possible. This work by Northrop Grumman NPP CalVal Team is supporting the VIIRS on-orbit calibration and validation teams for the sensor and ocean color as well as providing scientists interested in performing ground truth with results that show which detectors and scan angles are the most reliable over time. This novel approach offers a comprehensive sensor-centric on-orbit characterization of the VIIRS instrument on the NASA Suomi NPP mission.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/22346599','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/22346599"><span>CAROLS: a new airborne L-<span class="hlt">band</span> radiometer for ocean surface and land <span class="hlt">observations</span>.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Zribi, Mehrez; Pardé, Mickael; Boutin, Jacquline; Fanise, Pascal; Hauser, Daniele; Dechambre, Monique; Kerr, Yann; Leduc-Leballeur, Marion; Reverdin, Gilles; Skou, Niels; Søbjærg, Sten; Albergel, Clement; Calvet, Jean Christophe; Wigneron, Jean Pierre; Lopez-Baeza, Ernesto; Rius, Antonio; Tenerelli, Joseph</p> <p>2011-01-01</p> <p>The "Cooperative Airborne Radiometer for Ocean and Land Studies" (CAROLS) L-<span class="hlt">Band</span> radiometer was designed and built as a copy of the EMIRAD II radiometer constructed by the Technical University of Denmark team. It is a fully polarimetric and direct sampling correlation radiometer. It is installed on board a dedicated French ATR42 research aircraft, in conjunction with other airborne instruments (C-<span class="hlt">Band</span> scatterometer-STORM, the GOLD-RTR GPS system, the infrared CIMEL radiometer and a visible wavelength camera). Following initial laboratory qualifications, three airborne campaigns involving 21 flights were carried out over South West France, the Valencia site and the Bay of Biscay (Atlantic Ocean) in 2007, 2008 and 2009, in coordination with in situ field campaigns. In order to validate the CAROLS data, various aircraft flight patterns and maneuvers were implemented, including straight horizontal flights, circular flights, wing and nose wags over the ocean. Analysis of the first two campaigns in 2007 and 2008 leads us to improve the CAROLS radiometer regarding isolation between channels and filter bandwidth. After implementation of these improvements, results show that the instrument is conforming to specification and is a useful tool for Soil Moisture and Ocean Salinity (SMOS) satellite validation as well as for specific studies on surface soil moisture or ocean salinity.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018FrMat...5....8M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018FrMat...5....8M"><span>Experimental <span class="hlt">observation</span> of a large low-frequency <span class="hlt">band</span> gap in a polymer waveguide</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Miniaci, Marco; Mazzotti, Matteo; Radzieński, Maciej; Kherraz, Nesrine; Kudela, Pawel; Ostachowicz, Wieslaw; Morvan, Bruno; Bosia, Federico; Pugno, Nicola M.</p> <p>2018-02-01</p> <p>The quest for large and low frequency <span class="hlt">band</span> gaps is one of the principal objectives pursued in a number of engineering applications, ranging from noise absorption to vibration control, to seismic wave abatement. For this purpose, a plethora of complex architectures (including multi-phase materials) and multi-physics approaches have been proposed in the past, often involving difficulties in their practical realization. To address this issue, in this work we propose an easy-to-manufacture design able to open large, low frequency complete Lamb <span class="hlt">band</span> gaps exploiting a suitable arrangement of masses and stiffnesses produced by cavities in a monolithic material. The performance of the designed structure is evaluated by numerical simulations and confirmed by Scanning Laser Doppler Vibrometer (SLDV) measurements on an isotropic polyvinyl chloride plate in which a square ring region of cross-like cavities is fabricated. The full wave field reconstruction clearly confirms the ability of even a limited number of unit cell rows of the proposed design to efficiently attenuate Lamb waves. In addition, numerical simulations show that the structure allows to shift of the central frequency of the BG through geometrical modifications. The design may be of interest for applications in which large BGs at low frequencies are required.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1407026-coulomb-excitation-isomeric-band','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1407026-coulomb-excitation-isomeric-band"><span>Coulomb excitation of the K π= 8⁻ isomeric <span class="hlt">band</span> in 178Hf</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Napiorkovsk, P. J.; Srebrny, J.; Czosnyka, T.; ...</p> <p>2001-12-01</p> <p>The Coulomb excitation experiment on the 178Hf was performed using 650 MeV beam of 136Xe. The first <span class="hlt">observation</span> of discrete transitions in the K π = 8 - isomeric <span class="hlt">band</span>. Coulomb excited from K π = 0+ ground state, is reported. The possible mechanisms of El coupling of the ground state <span class="hlt">band</span> and the isomeric <span class="hlt">band</span> is discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://pubs.er.usgs.gov/publication/5224838','USGSPUBS'); return false;" href="https://pubs.er.usgs.gov/publication/5224838"><span>Temporal patterns of apparent leg <span class="hlt">band</span> retention in North American geese</span></a></p> <p><a target="_blank" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p>Zimmerman, Guthrie S.; Kendall, William L.; Moser, Timothy J.; White, Gary C.; Doherty, Paul F.</p> <p>2009-01-01</p> <p>An important assumption of mark?recapture studies is that individuals retain their marks, which has not been assessed for goose reward <span class="hlt">bands</span>. We estimated aluminum leg <span class="hlt">band</span> retention probabilities and modeled how <span class="hlt">band</span> retention varied with <span class="hlt">band</span> type (standard vs. reward <span class="hlt">band</span>), <span class="hlt">band</span> age (1-40 months), and goose characteristics (species and size class) for Canada (Branta canadensis), cackling (Branta hutchinsii), snow (Chen caerulescens), and Ross?s (Chen rossii) geese that field coordinators double-leg <span class="hlt">banded</span> during a North American goose reward <span class="hlt">band</span> study (N = 40,999 individuals from 15 populations). We conditioned all models in this analysis on geese that were encountered with >1 leg <span class="hlt">band</span> still attached (n = 5,747 dead recoveries and live recaptures). Retention probabilities for standard aluminum leg <span class="hlt">bands</span> were high (estimate of 0.9995, SE = 0.001) and constant over 1-40 months. In contrast, apparent retention probabilities for reward <span class="hlt">bands</span> demonstrated an interactive relationship between 5 size and species classes (small cackling, medium Canada, large Canada, snow, and Ross?s geese). In addition, apparent retention probabilities for each of the 5 classes varied quadratically with time, being lower immediately after <span class="hlt">banding</span> and at older age classes. The differential retention probabilities among <span class="hlt">band</span> type (reward vs. standard) that we <span class="hlt">observed</span> suggests that 1) models estimating reporting probability should incorporate differential <span class="hlt">band</span> loss if it is nontrivial, 2) goose managers should consider the costs and benefits of double-<span class="hlt">banding</span> geese on an operational basis, and 3) the United States Geological Survey Bird <span class="hlt">Banding</span> Lab should modify protocols for receiving recovery data.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017JAP...122a4502J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017JAP...122a4502J"><span><span class="hlt">Band-to-band</span> tunneling in Γ valley for Ge source lateral tunnel field effect transistor: Thickness scaling</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jain, Prateek; Rastogi, Priyank; Yadav, Chandan; Agarwal, Amit; Chauhan, Yogesh Singh</p> <p>2017-07-01</p> <p>The direct and indirect valleys in Germanium (Ge) are separated by a very small offset, which opens up the prospect of direct tunneling in the Γ valley of an extended Ge source tunnel field effect transistor (TFET). We explore the impact of thickness scaling of extended Ge source lateral TFET on the <span class="hlt">band</span> to <span class="hlt">band</span> tunneling (BTBT) current. The Ge source is extended inside the gate by 2 nm to confine the tunneling in Ge only. We <span class="hlt">observe</span> that as the thickness is scaled, the <span class="hlt">band</span> alignment at the Si/Ge heterojunction changes significantly, which results in an increase in Ge to Si BTBT current. Based on density functional calculations, we first obtain the <span class="hlt">band</span> structure parameters (bandgap, effective masses, etc.) for the Ge and Si slabs of varying thickness, and these are then used to obtain the thickness dependent Kane's BTBT tunneling parameters. We find that electrostatics improves as the thickness is reduced in the ultra-thin Ge film ( ≤ 10 nm). The ON current degrades as we scale down in thickness; however, the subthreshold slope ( S S AVG ) improves remarkably with thickness scaling due to subsurface BTBT. We predict that 8 nm thin devices offer the best option for optimized ON current and S S AVG .</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016GeoRL..43.2343G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016GeoRL..43.2343G"><span>Generation of multiband chorus by lower <span class="hlt">band</span> cascade in the Earth's magnetosphere</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gao, Xinliang; Lu, Quanming; Bortnik, Jacob; Li, Wen; Chen, Lunjin; Wang, Shui</p> <p>2016-03-01</p> <p>Chorus waves are intense electromagnetic whistler mode emissions in the magnetosphere, typically falling into two distinct frequency <span class="hlt">bands</span>: a lower <span class="hlt">band</span> (0.1-0.5fce) and an upper <span class="hlt">band</span> (0.5-0.8fce) with a power gap at about 0.5fce. In this letter, with the Time History of Events and Macroscale Interactions during Substorms satellite, we <span class="hlt">observed</span> two special chorus events, which are called as multiband chorus because upper <span class="hlt">band</span> chorus is located at harmonics of lower <span class="hlt">band</span> chorus. We propose a new potential generation mechanism for multiband chorus, which is called as lower <span class="hlt">band</span> cascade. In this scenario, a density mode with a frequency equal to that of lower <span class="hlt">band</span> chorus is generated by the ponderomotive effect (inhomogeneity of the electric amplitude) along the wave vector, and then upper <span class="hlt">band</span> chorus with the frequency twice that of lower <span class="hlt">band</span> chorus is generated through wave-wave couplings between lower <span class="hlt">band</span> chorus and the density mode. The mechanism provides a new insight into the evolution of whistler mode chorus in the Earth's magnetosphere.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4142109','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4142109"><span><span class="hlt">Banding</span> of NMR-derived Methyl Order Parameters: Implications for Protein Dynamics</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Sharp, Kim A.; Kasinath, Vignesh; Wand, A. Joshua</p> <p>2014-01-01</p> <p>Our understanding of protein folding, stability and function has begun to more explicitly incorporate dynamical aspects. Nuclear magnetic resonance has emerged as a powerful experimental method for obtaining comprehensive site-resolved insight into protein motion. It has been <span class="hlt">observed</span> that methyl-group motion tends to cluster into three “classes” when expressed in terms of the popular Lipari-Szabo model-free squared generalized order parameter. Here the origins of the three classes or <span class="hlt">bands</span> in the distribution of order parameters are examined. As a first step, a Bayesian based approach, which makes no a priori assumption about the existence or number of <span class="hlt">bands</span>, is developed to detect the <span class="hlt">banding</span> of O2axis values derived either from NMR experiments or molecular dynamics simulations. The analysis is applied to seven proteins with extensive molecular dynamics simulations of these proteins in explicit water to examine the relationship between O2 and fine details of the motion of methyl bearing side chains. All of the proteins studied display <span class="hlt">banding</span>, with some subtle differences. We propose a very simple yet plausible physical mechanism for <span class="hlt">banding</span>. Finally, our Bayesian method is used to analyze the measured distributions of methyl group motions in the catabolite activating protein and several of its mutants in various liganded states and discuss the functional implications of the <span class="hlt">observed</span> <span class="hlt">banding</span> to protein dynamics and function. PMID:24677353</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22649059-su-clinically-observed-discrepancy-between-image-based-log-based-mlc-position','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22649059-su-clinically-observed-discrepancy-between-image-based-log-based-mlc-position"><span>SU-F-T-469: A Clinically <span class="hlt">Observed</span> Discrepancy Between Image-Based and Log- Based MLC <span class="hlt">Position</span></span></a></p> <p><a target="_blank" href="http://www.osti.gov/search">DOE Office of Scientific and Technical Information (OSTI.GOV)</a></p> <p>Neal, B; Ahmed, M; Siebers, J</p> <p>2016-06-15</p> <p>Purpose: To present a clinical case which challenges the base assumption of log-file based QA, by showing that the actual <span class="hlt">position</span> of a MLC leaf can suddenly deviate from its programmed and logged <span class="hlt">position</span> by >1 mm as <span class="hlt">observed</span> with real-time imaging. Methods: An EPID-based exit-fluence dosimetry system designed to prevent gross delivery errors was used in cine mode to capture portal images during treatment. Visual monitoring identified an anomalous MLC leaf pair gap not otherwise detected by the automatic <span class="hlt">position</span> verification. The <span class="hlt">position</span> of the erred leaf was measured on EPID images and log files were analyzed for themore » treatment in question, the prior day’s treatment, and for daily MLC test patterns acquired on those treatment days. Additional standard test patterns were used to quantify the leaf <span class="hlt">position</span>. Results: Whereas the log file reported no difference between planned and recorded <span class="hlt">positions</span>, image-based measurements showed the leaf to be 1.3±0.1 mm medial from the planned <span class="hlt">position</span>. This offset was confirmed with the test pattern irradiations. Conclusion: It has been clinically <span class="hlt">observed</span> that log-file derived leaf <span class="hlt">positions</span> can differ from their actual <span class="hlt">positions</span> by >1 mm, and therefore cannot be considered to be the actual leaf <span class="hlt">positions</span>. This cautions the use of log-based methods for MLC or patient quality assurance without independent confirmation of log integrity. Frequent verification of MLC <span class="hlt">positions</span> through independent means is a necessary precondition to trusting log file records. Intra-treatment EPID imaging provides a method to capture departures from MLC planned <span class="hlt">positions</span>. Work was supported in part by Varian Medical Systems.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/FR-2010-03-04/pdf/2010-4562.pdf','FEDREG'); return false;" href="https://www.gpo.gov/fdsys/pkg/FR-2010-03-04/pdf/2010-4562.pdf"><span>75 FR 9850 - Tank Level Probing Radars in the Frequency <span class="hlt">Band</span> 77-81 GHz</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collection.action?collectionCode=FR">Federal Register 2010, 2011, 2012, 2013, 2014</a></p> <p></p> <p>2010-03-04</p> <p>... National Radio Astronomy Observatory (NRAO) states that it would not object to the Ohmart/VEGA waiver if it Frequency <span class="hlt">Band</span> of Operation. Authorized operations in the 77-81 GHz <span class="hlt">band</span> currently include radio astronomy... operations in this <span class="hlt">band</span> would have on authorized services. Regarding radio astronomy, the Commission <span class="hlt">observes</span>...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://pubs.er.usgs.gov/publication/70030948','USGSPUBS'); return false;" href="https://pubs.er.usgs.gov/publication/70030948"><span>Simulation and <span class="hlt">observations</span> of annual density <span class="hlt">banding</span> in skeletons of Montastraea (Cnidaria: Scleractinia) growing under thermal stress associated with ocean warming</span></a></p> <p><a target="_blank" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p>Worum, F.P.; Carricart-Ganivet, J. P.; Benson, L.; Golicher, D.</p> <p>2007-01-01</p> <p>We present a model of annual density <span class="hlt">banding</span> in skeletons of Montastraea coral species growing under thermal stress associated with an ocean-warming scenario. The model predicts that at sea-surface temperatures (SSTs) <29??C, high-density <span class="hlt">bands</span> (HDBs) are formed during the warmest months of the year. As temperature rises and oscillates around the optimal calcification temperature, an annual doublet in the HDB (dHDB) occurs that consists of two narrow HDBs. The presence of such dHDBs in skeletons of Montastraea species is a clear indication of thermal stress. When all monthly SSTs exceed the optimal calcification temperature, HDBs form during the coldest, not the warmest, months of the year. In addition, a decline in mean-annual calcification rate also occurs during this period of elevated SST. A comparison of our model results with annual density patterns <span class="hlt">observed</span> in skeletons of M. faveolata and M. franksi, collected from several localities in the Mexican Caribbean, indicates that elevated SSTs are already resulting in the presence of dHDBs as a first sign of thermal stress, which occurs even without coral bleaching. ?? 2007, by the American Society of Limnology and Oceanography, Inc.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19830025015','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19830025015"><span>Assessment of Thematic Mapper <span class="hlt">band-to-band</span> registration by the block correlation method</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Card, D. H.; Wrigley, R. C.; Mertz, F. C.; Hall, J. R.</p> <p>1983-01-01</p> <p>Rectangular blocks of pixels from one <span class="hlt">band</span> image were statistically correlated against blocks centered on identical pixels from a second <span class="hlt">band</span> image. The block pairs were shifted in pixel increments both vertically and horizontally with respect to each other and the correlation coefficient to the maximum correlation was taken as the best estimate of registration error for each block pair. For the <span class="hlt">band</span> combinations of the Arkansas scene studied, the misregistration of TM spectral <span class="hlt">bands</span> within the noncooled focal plane lie well within the 0.2 pixel target specification. Misregistration between the middle IR <span class="hlt">bands</span> is well within this specification also. The thermal IR <span class="hlt">band</span> has an apparent misregistration with TM <span class="hlt">band</span> 7 of approximately 3 pixels in each direction. The TM <span class="hlt">band</span> 3 has a misregistration of approximately 0.2 pixel in the across-scan direction and 0.5 pixel in the along-scan direction, with both TM <span class="hlt">bands</span> 5 and 7.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19850013433&hterms=correlation+coefficient&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3Dcorrelation%2Bcoefficient','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19850013433&hterms=correlation+coefficient&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3Dcorrelation%2Bcoefficient"><span>Assessment of Thematic Mapper <span class="hlt">Band-to-band</span> Registration by the Block Correlation Method</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Card, D. H.; Wrigley, R. C.; Mertz, F. C.; Hall, J. R.</p> <p>1985-01-01</p> <p>Rectangular blocks of pixels from one <span class="hlt">band</span> image were statistically correlated against blocks centered on identical pixels from a second <span class="hlt">band</span> image. The block pairs were shifted in pixel increments both vertically and horizontally with respect to each other and the correlation coefficient to the maximum correlation was taken as the best estimate of registration error for each block pair. For the <span class="hlt">band</span> combinations of the Arkansas scene studied, the misregistration of TM spectral <span class="hlt">bands</span> within the noncooled focal plane lie well within the 0.2 pixel target specification. Misregistration between the middle IR <span class="hlt">bands</span> is well within this specification also. The thermal IR <span class="hlt">band</span> has an apparent misregistration with TM <span class="hlt">band</span> 7 of approximately 3 pixels in each direction. The TM <span class="hlt">band</span> 3 has a misregistration of approximately 0.2 pixel in the across-scan direction and 0.5 pixel in the along-scan direction, with both TM <span class="hlt">bands</span> 5 and 7.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/21503853','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/21503853"><span>Biocompatibility of orthodontic <span class="hlt">bands</span> following exposure to dental plaque.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Hornikel, Sandra; Erbe, Christina; Schmidtmann, Irene; Wehrbein, Heiner</p> <p>2011-03-01</p> <p>The aim of this study was to assess the biocompatibility of orthodontic <span class="hlt">bands</span> following exposure to the human oral environment. Cell adherence and cell morphology of gingival fibroblasts grown on 32 orthodontic <span class="hlt">bands</span> were tested. The <span class="hlt">bands</span> were in place intraorally for 6 to 37 months. We <span class="hlt">observed</span> cell adherence in 76% of the previously plaque-free surfaces. Cell morphology was 50% spherical and 50% elongated. The surfaces that had had plaque attached demonstrated cell adherence in 84% of the given areas; those cells were spherical in 42% and elongated in 58%. We conclude that individual oral hygiene habits during orthodontic treatment seem to have no effect on the biocompatibility of orthodontic <span class="hlt">bands</span>, as we failed to discern a difference in either cell adherence or cell morphology in areas with and without prior plaque attachment.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27787351','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27787351"><span>Utilization of <span class="hlt">Positive</span> and Negative Controls to Examine Comorbid Associations in <span class="hlt">Observational</span> Database Studies.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Desai, Jigar R; Hyde, Craig L; Kabadi, Shaum; St Louis, Matthew; Bonato, Vinicius; Katrina Loomis, A; Galaznik, Aaron; Berger, Marc L</p> <p>2017-03-01</p> <p>Opportunities to leverage <span class="hlt">observational</span> data for precision medicine research are hampered by underlying sources of bias and paucity of methods to handle resulting uncertainty. We outline an approach to account for bias in identifying comorbid associations between 2 rare genetic disorders and type 2 diabetes (T2D) by applying a <span class="hlt">positive</span> and negative control disease paradigm. Association between 10 common and 2 rare genetic disorders [Hereditary Fructose Intolerance (HFI) and α-1 antitrypsin deficiency] and T2D was compared with the association between T2D and 7 negative control diseases with no established relationship with T2D in 4 <span class="hlt">observational</span> databases. Negative controls were used to estimate how much bias and variance existed in datasets when no effect should be <span class="hlt">observed</span>. Unadjusted association for common and rare genetic disorders and T2D was <span class="hlt">positive</span> and variable in magnitude and distribution in all 4 databases. However, association between negative controls and T2D was 200% greater than expected indicating the magnitude and confidence intervals for comorbid associations are sensitive to systematic bias. A meta-analysis using this method demonstrated a significant association between HFI and T2D but not for α-1 antitrypsin deficiency. For <span class="hlt">observational</span> studies, when covariate data are limited or ambiguous, <span class="hlt">positive</span> and negative controls provide a method to account for the broadest level of systematic bias, heterogeneity, and uncertainty. This provides greater confidence in assessing associations between diseases and comorbidities. Using this approach we were able to demonstrate an association between HFI and T2D. Leveraging real-world databases is a promising approach to identify and corroborate potential targets for precision medicine therapies.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20000073297&hterms=forest+trees&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3Dforest%2Btrees','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20000073297&hterms=forest+trees&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3Dforest%2Btrees"><span>Passive Microwave Measurements Over Conifer Forests at L-<span class="hlt">Band</span> and C-<span class="hlt">Band</span></span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>LeVine, D. M.; Lang, R.; Chauhan, N.; Kim, E.; Bidwell, S.; Goodberlet, M.; Haken, M.; deMatthaeis, P.</p> <p>2000-01-01</p> <p>Measurements have been made at L-<span class="hlt">band</span> and C-<span class="hlt">band</span> over conifer forests in Virginia to study the response of passive microwave instruments to biomass and soil moisture. A series of aircraft measurements were made in July, August and November, 1999 over relatively homogenous conifer forests of varying biomass. Three radiometers participated in these measurements. These were: 1) the L-<span class="hlt">band</span> radiometer ESTAR, a horizontally polarized synthetic aperture radiometer which has been used extensively in past measurements of soil moisture; 2) the L-<span class="hlt">band</span> radiometer SLFMR, a vertically polarized cross-track scanner which has been used successfully in the past for mapping sea surface salinity; and 3) The ACMR, a new C-<span class="hlt">band</span> radiometer which operates at V- and H-polarization and in the configuration for these experiments did not scan. All three radiometers were flown on the NASA P-3 aircraft based at the Goddard Space Flight Center's Wallops Flight Facility. The ESTAR and SLFMR were mounted in the bomb bay of the P-3 and imaged across track whereas the ACMR was mounted to look aft at 54 degrees up from nadir. Data was collected at altitudes of 915 meters and 457 meters. The forests consisted of relatively homogeneous "managed" stands of conifer located near Waverly, Virginia. This is a relatively flat area about 30 miles southeast of Richmond, VA with numerous stands of trees being grown for the forestry industry. The stands selected for study consisted of areas of regrowth and mature stands of pine. In addition, a small stand of very large trees was <span class="hlt">observed</span>. Soil moisture sampling was done in each stand during the aircraft over flights. Data was collected on July 7, August 27, November 15 and November 30, 1999. Measurements were made with ESTAR on all days. The ACMR flew on the summer missions and the SLFMR was present only on the August 27 flight. Soil moisture varied from quite dry on July 7 to quite moist on November 30 (which was shortly after a period of rain). The microwave</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016AGUFM.P53C2217L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016AGUFM.P53C2217L"><span><span class="hlt">Positioning</span> for the Chang'E-3 lander and rover using Earth-based <span class="hlt">Observations</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Li, P.; Huang, Y.; Hu, X.; Shengqi, C.</p> <p>2016-12-01</p> <p>The Chinese first lunar lander, Chang'E-3, performed a lunar soft-landing on 14 Dec, 2013. Precise <span class="hlt">positioning</span> for the lander and rover was the most important precondition and guarantee for a successful lunar surface exploration. In this study, first, the tracking system, measurement models and <span class="hlt">positioning</span> method are discussed in detail. Second, the location of the CE-3 lander was determined: 44.1206°N, -19.5124°E, -2632 m (altitude was relative to the assumed lunar surface with a height of 1737.4 km), and the analysis showed the VLBI Very Long Base Interferometry data were able to significantly improve the <span class="hlt">positioning</span> accuracy. Furthermore, the <span class="hlt">positioning</span> error was evaluated in various ways; the result was better than 50 m. Finally, the relative <span class="hlt">positioning</span> of the rover and lander using earth-based <span class="hlt">observations</span> was studied and compared with the optical <span class="hlt">positioning</span> method using photographs taken by the lander and rover. The method applied in this study was not limited by the visible range of the lander, and the relative <span class="hlt">positioning</span> accuracy did not decrease as the distance between the lander and rover increased. The results indicated that under the current tracking and measuring conditions, the relative <span class="hlt">positioning</span> accuracy was about 100 m using the same beam VLBI group delay data with ns nanosecond level noise. Furthermore, using the same beam VLBI phase delay data with ps picosecond level noise it was possible to significantly improve the relative <span class="hlt">positioning</span> accuracy to the order of 1 m.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20090032049','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20090032049"><span>Progressive <span class="hlt">Band</span> Selection</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Fisher, Kevin; Chang, Chein-I</p> <p>2009-01-01</p> <p>Progressive <span class="hlt">band</span> selection (PBS) reduces spectral redundancy without significant loss of information, thereby reducing hyperspectral image data volume and processing time. Used onboard a spacecraft, it can also reduce image downlink time. PBS prioritizes an image's spectral <span class="hlt">bands</span> according to priority scores that measure their significance to a specific application. Then it uses one of three methods to select an appropriate number of the most useful <span class="hlt">bands</span>. Key challenges for PBS include selecting an appropriate criterion to generate <span class="hlt">band</span> priority scores, and determining how many <span class="hlt">bands</span> should be retained in the reduced image. The image's Virtual Dimensionality (VD), once computed, is a reasonable estimate of the latter. We describe the major design details of PBS and test PBS in a land classification experiment.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20170003532&hterms=improvement+products&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dimprovement%2Bproducts','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20170003532&hterms=improvement+products&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dimprovement%2Bproducts"><span>Calibration Improvements in the Detector-to-Detector Differences for the MODIS Ocean Color <span class="hlt">Bands</span></span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Li, Yonghong; Angal, Amit; Wu, Aisheng; Geng, Xu; Link, Daniel; Xiong, Xiaoxiong</p> <p>2016-01-01</p> <p>The Moderate Resolution Imaging Spectroradiometer (MODIS), a major instrument within NASAs Earth <span class="hlt">Observation</span> System missions, has operated for over 16 and 14 years onboard the Terra and Aqua satellites, respectively. Its reflective solar <span class="hlt">bands</span> (RSB) covering a spectral range from 0.4 to 2.1 micrometers are primarily calibrated using the on-board solar diffuser(SD), with its on-orbit degradation monitored using the Solar Diffuser Stability Monitor. RSB calibrations are supplemented by near-monthly lunar measurements acquired from the instruments space-view port. Nine <span class="hlt">bands</span> (<span class="hlt">bands</span> 8-16) in the visible to near infrared spectral range from 0.412 to 0.866 micrometers are primarily used for ocean color <span class="hlt">observations</span>.During a recent reprocessing of ocean color products, performed by the NASA Ocean Biology Processing Group, detector-to-detector differences of up to 1.5% were <span class="hlt">observed</span> in <span class="hlt">bands</span> 13-16 of Terra MODIS. This paper provides an overview of the current approach to characterize the MODIS detector-to-detector differences. An alternative methodology was developed to mitigate the <span class="hlt">observed</span> impacts for <span class="hlt">bands</span> 13-16. The results indicated an improvement in the detector residuals and in turn are expected to improve the MODIS ocean color products. This paper also discusses the limitations,subsequent enhancements, and the improvements planned for future MODIS calibration collections.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017APS..MARY26012M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017APS..MARY26012M"><span>Sensitivity of gap symmetry to an incipient <span class="hlt">band</span>: Application to iron based superconductors</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Mishra, Vivek; Scalapino, Douglas; Maier, Thomas</p> <p></p> <p><span class="hlt">Observation</span> of high temperature superconductivity in iron-based superconductors with a submerged hole <span class="hlt">band</span> has attracted wide interest. A spin fluctuation mediated pairing mechanism has been proposed as a possible explanation for the high transition temperatures <span class="hlt">observed</span> in these systems. Here we discuss the importance of the submerged <span class="hlt">band</span> in the context of the gap symmetry. We show that the incipient <span class="hlt">band</span> can lead to an attractive pairing interaction and thus have significant effects on the pairing symmetry. We propose a framework to include the effect of the incipient <span class="hlt">band</span> in the standard multi-orbital spin-fluctuation theories which are widely used for studying various iron-based superconductors. Research sponsored by the Laboratory Directed Research and Development Program of Oak Ridge National Laboratory, managed by UT-Battelle, LLC, for the U. S. Department of Energy.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li><a href="#" onclick='return showDiv("page_24");'>24</a></li> <li class="active"><span>25</span></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_25 --> <div class="footer-extlink text-muted" style="margin-bottom:1rem; text-align:center;">Some links on this page may take you to non-federal websites. 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