Sample records for albeit ultraviolet bright

  1. Extreme Ultraviolet Explorer Bright Source List

    NASA Technical Reports Server (NTRS)

    Malina, Roger F.; Marshall, Herman L.; Antia, Behram; Christian, Carol A.; Dobson, Carl A.; Finley, David S.; Fruscione, Antonella; Girouard, Forrest R.; Hawkins, Isabel; Jelinsky, Patrick

    1994-01-01

    Initial results from the analysis of the Extreme Ultraviolet Explorer (EUVE) all-sky survey (58-740 A) and deep survey (67-364 A) are presented through the EUVE Bright Source List (BSL). The BSL contains 356 confirmed extreme ultraviolet (EUV) point sources with supporting information, including positions, observed EUV count rates, and the identification of possible optical counterparts. One-hundred twenty-six sources have been detected longward of 200 A.

  2. An Ultraviolet/Optical Atlas of Bright Galaxies

    NASA Astrophysics Data System (ADS)

    Marcum, Pamela M.; O'Connell, Robert W.; Fanelli, Michael N.; Cornett, Robert H.; Waller, William H.; Bohlin, Ralph C.; Neff, Susan G.; Roberts, Morton S.; Smith, Andrew M.; Cheng, K.-P.; Collins, Nicholas R.; Hennessy, Gregory S.; Hill, Jesse K.; Hill, Robert S.; Hintzen, Paul; Landsman, Wayne B.; Ohl, Raymond G.; Parise, Ronald A.; Smith, Eric P.; Freedman, Wendy L.; Kuchinski, Leslie E.; Madore, Barry; Angione, Ronald; Palma, Christopher; Talbert, Freddie; Stecher, Theodore P.

    2001-02-01

    We present wide-field imagery and photometry of 43 selected nearby galaxies of all morphological types at ultraviolet and optical wavelengths. The ultraviolet (UV) images, in two broad bands at 1500 and 2500 Å, were obtained using the Ultraviolet Imaging Telescope (UIT) during the Astro-1 Spacelab mission. The UV images have ~3" resolution, and the comparison sets of ground-based CCD images (in one or more of B, V, R, and Hα) have pixel scales and fields of view closely matching the UV frames. The atlas consists of multiband images and plots of UV/optical surface brightness and color profiles. Other associated parameters, such as integrated photometry and half-light radii, are tabulated. In an appendix, we discuss the sensitivity of different wavebands to a galaxy's star formation history in the form of ``history weighting functions'' and emphasize the importance of UV observations as probes of evolution during the past 10-1000 Myr. We find that UV galaxy morphologies are usually significantly different from visible band morphologies as a consequence of spatially inhomogeneous stellar populations. Differences are quite pronounced for systems in the middle range of Hubble types, Sa through Sc, but less so for ellipticals or late-type disks. Normal ellipticals and large spiral bulges are fainter and more compact in the UV. However, they typically exhibit smooth UV profiles with far-UV/optical color gradients which are larger than any at optical/IR wavelengths. The far-UV light in these cases is probably produced by extreme horizontal branch stars and their descendants in the dominant, low-mass, metal-rich population. The cool stars in the large bulges of Sa and Sb spirals fade in the UV while hot OB stars in their disks brighten, such that their Hubble classifications become significantly later. In the far-UV, early-type spirals often appear as peculiar, ringlike systems. In some spiral disks, UV-bright structures closely outline the spiral pattern; in others, the

  3. Bright high-repetition-rate source of narrowband extreme-ultraviolet harmonics beyond 22 eV

    PubMed Central

    Wang, He; Xu, Yiming; Ulonska, Stefan; Robinson, Joseph S.; Ranitovic, Predrag; Kaindl, Robert A.

    2015-01-01

    Novel table-top sources of extreme-ultraviolet light based on high-harmonic generation yield unique insight into the fundamental properties of molecules, nanomaterials or correlated solids, and enable advanced applications in imaging or metrology. Extending high-harmonic generation to high repetition rates portends great experimental benefits, yet efficient extreme-ultraviolet conversion of correspondingly weak driving pulses is challenging. Here, we demonstrate a highly-efficient source of femtosecond extreme-ultraviolet pulses at 50-kHz repetition rate, utilizing the ultraviolet second-harmonic focused tightly into Kr gas. In this cascaded scheme, a photon flux beyond ≈3 × 1013 s−1 is generated at 22.3 eV, with 5 × 10−5 conversion efficiency that surpasses similar harmonics directly driven by the fundamental by two orders-of-magnitude. The enhancement arises from both wavelength scaling of the atomic dipole and improved spatio-temporal phase matching, confirmed by simulations. Spectral isolation of a single 72-meV-wide harmonic renders this bright, 50-kHz extreme-ultraviolet source a powerful tool for ultrafast photoemission, nanoscale imaging and other applications. PMID:26067922

  4. Ultraviolet Imaging Telescope images of the reflection nebula NGC 7023 - Derivation of ultraviolet scattering properties of dust grains

    NASA Technical Reports Server (NTRS)

    Witt, Adolf N.; Petersohn, Jens K.; Bohlin, Ralph C.; O'Connell, Robert W.; Roberts, Morton S.; Smith, Andrew M.; Stecher, Theodore P.

    1992-01-01

    The Ultraviolet Imaging Telescope as part of the Astro-1 mission, was used to obtain high-resolution surface brightness distribution data in six ultraviolet wavelength bands for the bright reflection nebula NGC 7023. From the quantitative comparison of the measured surface brightness gradients ratios of nebular to stellar flux, and detail radial surface brightness profiles with corresponding data from the visible, two major conclusions results: (1) the scattering in the near- and far-ultraviolet in this nebula is more strongly forward-directed than in the visible; (2) the dust albedo in the ultraviolet for wavelengths not less than 140 nm is identical to that in the visible, with the exception of the 220 nm bump in the extinction curve. In the wavelengths region of the bump, the albedo is reduced by 25 to 30 percent in comparison with wavelengths regions both shorter and longer. This lower albedo is expected, if the bump is a pure absorption feature.

  5. An ultraviolet imager to study bright UV sources

    NASA Astrophysics Data System (ADS)

    Mathew, Joice; Prakash, Ajin; Sarpotdar, Mayuresh; Sreejith, A. G.; Safonova, Margarita; Murthy, Jayant

    2016-07-01

    We have designed and developed a compact ultraviolet imaging payload to y on a range of possible platforms such as high altitude balloon experiments, cubesats, space missions, etc. The primary science goals are to study the bright UV sources (mag < 10) and also to look for transients in the Near UV (200 - 300 nm) domain. Our first choice is to place this instrument on a spacecraft going to the Moon as part of the Indian entry into Google lunar X-Prize competition. The major constraints for the instrument are, it should be lightweight (< 2Kg), compact (length < 50cm) and cost effective. The instrument is an 80 mm diameter Cassegrain telescope with a field of view of around half a degree designated for UV imaging. In this paper we will discuss about the various science cases that can be performed by having observations with the instrument on different platforms. We will also describe the design, development and the current state of implementation of the instrument. This includes opto-mechanical and electrical design of the instrument. We have adopted an all spherical optical design which would make the system less complex to realize and a cost effective solution compared to other telescope configuration. The structural design has been chosen in such a way that it will ensure that the instrument could withstand all the launch load vibrations. An FPGA based electronics board is used for the data acquisition, processing and CCD control. We will also brie y discuss about the hardware implementation of the detector interface and algorithms for the detector readout and data processing.

  6. Bright Points and Subflares in Ultraviolet Lines and X-Rays

    NASA Technical Reports Server (NTRS)

    Rovira, M.; Schmieder, B.; Demoulin, P.; Simnett, G. M.; Hagyard, M. J.; Reichmann, E.; Reichmann, E.; Tandberg-Hanssen, E.

    1999-01-01

    We have analyzed an active region which was observed in H.alpha (Multichannel Subtractive Double Pass Spectrograph), in UV lines (SMM/UVSP), and in X-rays (SMM/HXIS). In this active region there were only a few subflares and many small bright points visible in UV and in X-rays. Using an extrapolation based on the Fourier transform, we have computed magnetic field lines connecting different photospheric magnetic polarities from ground-based magnetograms. Along the magnetic inversion lines we find two different zones: (1) a high-shear region (> 70 deg) where subflares occur, and (2) a low-shear region along the magnetic inversion line where UV bright points are observed. In these latter regions the magnetic topology is complex with a mixture of polarities. According to the velocity field observed in the Si IV lamda.1402 line and the extrapolation of the magnetic field, we notice that each UV bright point is consistent with emission from low-rising loops with downflows at both ends. We notice some hard X-ray emissions above the bright-point regions with temperatures up to 8 x 10(exp 6) K, which suggests some induced reconnection due to continuous emergence of new flux. This reconnection is also enhanced by neighboring subflares.

  7. Giant Low Surface Brightness Galaxies

    NASA Astrophysics Data System (ADS)

    Mishra, Alka; Kantharia, Nimisha G.; Das, Mousumi

    2018-04-01

    In this paper, we present radio observations of the giant low surface brightness (LSB) galaxies made using the Giant Metrewave Radio Telescope (GMRT). LSB galaxies are generally large, dark matter dominated spirals that have low star formation efficiencies and large HI gas disks. Their properties suggest that they are less evolved compared to high surface brightness galaxies. We present GMRT emission maps of LSB galaxies with an optically-identified active nucleus. Using our radio data and archival near-infrared (2MASS) and near-ultraviolet (GALEX) data, we studied morphology and star formation efficiencies in these galaxies. All the galaxies show radio continuum emission mostly associated with the centre of the galaxy.

  8. ASASSN-15LH: A SUPERLUMINOUS ULTRAVIOLET REBRIGHTENING OBSERVED BY SWIFT AND HUBBLE

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

    Brown, Peter J.; Yang, Yi; Wang, Lifan

    2016-09-01

    We present and discuss ultraviolet and optical photometry from the Ultraviolet/Optical Telescope, X-ray limits from the X-Ray Telescope on Swift, and imaging polarimetry and ultraviolet/optical spectroscopy with the Hubble Space Telescope , all from observations of ASASSN-15lh. It has been classified as a hydrogen-poor superluminous supernova (SLSN I), making it more luminous than any other supernova observed. ASASSN-15lh is not detected in the X-rays in individual or co-added observations. From the polarimetry we determine that the explosion was only mildly asymmetric. We find the flux of ASASSN-15lh to increase strongly into the ultraviolet, with an ultraviolet luminosity 100 times greatermore » than the hydrogen-rich, ultraviolet-bright SLSN II SN 2008es. We find that objects as bright as ASASSN-15lh are easily detectable beyond redshifts of ∼4 with the single-visit depths planned for the Large Synoptic Survey Telescope. Deep near-infrared surveys could detect such objects past a redshift of ∼20, enabling a probe of the earliest star formation. A late rebrightening—most prominent at shorter wavelengths—is seen about two months after the peak brightness, which is itself as bright as an SLSN. The ultraviolet spectra during the rebrightening are dominated by the continuum without the broad absorption or emission lines seen in SLSNe or tidal disruption events (TDEs) and the early optical spectra of ASASSN-15lh. Our spectra show no strong hydrogen emission, showing only Ly α absorption near the redshift previously found by optical absorption lines of the presumed host. The properties of ASASSN-15lh are extreme when compared to either SLSNe or TDEs.« less

  9. Ultraviolet brightness of celestial targets for Apollo 17

    NASA Technical Reports Server (NTRS)

    Fastie, W. G.

    1972-01-01

    An evaluation of the ultraviolet flux from the stars expected in the various inertial-hold pointing directions and PTC scans during the Apollo 17 mission is presented. These directions and PTC scan poles for the nominal mission are listed. The methodology used in evaluating the flux, and the individual targets themselves is explained.

  10. Observations of the Ultraviolet Spectra of Carbon White Dwarfs

    NASA Technical Reports Server (NTRS)

    Wagner, G. A.

    1982-01-01

    Strong ultraviolet carbon lines were detected in additional white DC (continuous visual spectra) dwarfs using the IUE. These lines are not seen in the ultraviolet spectrum of the cool DC star Stein 2051 B. The bright DA white dwarf LB 3303 has a strong unidentified absorption near lambda 1400.

  11. Brightness and magnetic evolution of solar coronal bright points

    NASA Astrophysics Data System (ADS)

    Ugarte-Urra, I.

    2004-12-01

    This thesis presents a study of the brightness and magnetic evolution of several Extreme ultraviolet (EUV) coronal bright points (hereafter BPs). BPs are loop-like features of enhanced emission in the coronal EUV and X-ray images of the Sun, that are associated to the interaction of opposite photospheric magnetic polarities with magnetic fluxes of ≈1018 - 1019 Mx. The study was carried out using several instruments on board the Solar and Heliospheric Observatory (SOHO): the Extreme Ultraviolet Imager (EIT), the Coronal Diagnostic Spectrometer (CDS) and the Michelson Doppler Imager (MDI), supported by the high resolution imaging from the Transition Region And Coronal Explorer (TRACE). The results confirm that, down to 1'' (i.e. ~715 km) resolution, BPs are made of small loops with lengths of ~6 Mm and cross-sections of ~2 Mm. The loops are very dynamic, evolving in time scales as short as 1 - 2 minutes. This is reflected in a highly variable EUV response with fluctuations highly correlated in spectral lines at transition region temperatures (in the range 3.2x10^4 - 3.5x10^5 K), but not always at coronal temperatures. A wavelet analysis of the intensity variations reveals, for the first time, the existence of quasi-periodic oscillations with periods ranging 400 -- 1000 s, in the range of periods characteristic of the chromospheric network. The link between BPs and network bright points is discussed, as well as the interpretation of the oscillations in terms of global acoustic modes of closed magnetic structures. A comparison of the magnetic flux evolution of the magnetic polarities to the EUV flux changes is also presented. Throughout their lifetime, the intrinsic EUV emission of BPs is found to be dependent on the total magnetic flux of the polarities. In short time scales, co-spatial and co-temporal TRACE and MDI images, reveal the signature of heating events that produce sudden EUV brightenings simultaneous to magnetic flux cancellations. This is interpreted in

  12. The ultraviolet-bright stars of Omega Centauri, M3, and M13

    NASA Technical Reports Server (NTRS)

    Landsman, Wayne B.; O'Connell, Robert W.; Whitney, Jonathan H.; Bohlin, Ralph C.; Hill, Robert S.; Maran, Stephen P.; Parise, Ronald A.; Roberts, Morton S.; Smith, Andrew A.; Stecher, Theodore P.

    1992-01-01

    Two new UV-bright stars detected within 2 arcmin of the center of Omega Cen are spectroscopically investigated with the short-wavelength spectrograph of the IUE. The IUE spectra of the UV-bright stars UIT-1 and UIT-2 in the core of Omega Cen superficially resemble those of Population I mid-B stars. The absorption lines of the core UV-bright stars are significantly weaker than in Population I stars, consistent with their membership in the cluster. Synthetic spectra calculated from low-metallicity Kurucz model stellar atmospheres are compared with the spectra. These objects are insufficiently luminous to be classical hydrogen-burning post-AGB stars. They may be evolved hot horizontal branch stars which have been brightened by more than 3 mag since leaving the zero-age horizontal branch. It is inferred from the spectra and luminosity of the core UV-bright stars that similar objects could provide the source of the UV light in elliptical galaxies.

  13. Resonances in the Photoionization Cross Sections of Atomic Nitrogen Shape the Far-ultraviolet Spectrum of the Bright Star in 47 Tucanae

    NASA Astrophysics Data System (ADS)

    Dixon, William V.; Chayer, Pierre

    2013-08-01

    The far-ultraviolet spectrum of the Bright Star (B8 III) in 47 Tuc (NGC 104) shows a remarkable pattern: it is well fit by local thermodynamic equilibrium models at wavelengths longer than Lyβ, but at shorter wavelengths it is fainter than the models by a factor of two. A spectrum of this star obtained with the Far Ultraviolet Spectroscopic Explorer shows broad absorption troughs with sharp edges at 995 and 1010 Å and a deep absorption feature at 1072 Å none of which are predicted by the models. We find that these features are caused by resonances in the photoionization cross sections of the first and second excited states of atomic nitrogen (2s 2 2p 3 2 D 0 and 2 P 0). Using cross sections from the Opacity Project, we can reproduce these features, but only if we use the cross sections at their full resolution, rather than the resonance-averaged cross sections usually employed to model stellar atmospheres. These resonances are strongest in stellar atmospheres with enhanced nitrogen and depleted carbon abundances, a pattern typical of post-asymptotic giant branch stars.

  14. A survey of ultraviolet interstellar absorption lines

    NASA Technical Reports Server (NTRS)

    Bohlin, R. C.; Jenkins, E. B.; Spitzer, L., Jr.; York, D. G.; Hill, J. K.; Savage, B. D.; Snow, T. P., Jr.

    1983-01-01

    A telescope-spectrometer on the Copernicus spacecraft made possible the measurement of many ultraviolet absorption lines produced by the interstellar gas. The present survey provides data on ultraviolet absorption lines in the spectra of 88 early-type stars. The stars observed are divided into four classes, including reddened stars, unreddened bright stars, moderately reddened bright stars, and unreddened and moderately reddened faint stars. Data are presented for equivalent width, W, radial velocity V, and rms line width, D, taking into account some 10 to 20 lines of N I, O I, Si II, P II, S II, Cl I, Cl II, Mn II, Fe II, Ni II, Cu II, and H2. The data are based on multiple scans for each line. Attention is given to details of observations, the data reduction procedure, and the computation of equivalent width, mean velocity, and velocity dispersion.

  15. Far-ultraviolet imagery of the Orion Nebula

    NASA Technical Reports Server (NTRS)

    Carruthers, G. R.; Opal, C. B.

    1977-01-01

    Two electrographic cameras carried on a sounding rocket have yielded useful-resolution far-ultraviolet (1000-2000 A) imagery of the Orion Nebula. The brightness distribution in the images is consistent with a primary source which is due to scattering of starlight by dust grains, although an emission-line contribution, particularly in the fainter outer regions, is not ruled out. The results are consistent with an albedo of the dust grains that is high in the far-ultraviolet and which increases toward shorter wavelengths below 1230 A.

  16. The ASAS-SN Bright Supernova Catalog – II. 2015

    DOE PAGES

    Holoien, T. W. -S.; Brown, J. S.; Stanek, K. Z.; ...

    2017-01-16

    Here, this paper presents information for all supernovae discovered by the All-Sky Automated Survey for SuperNovae (ASAS-SN) during 2015, its second full year of operations. The same information is presented for bright (mV ≤ 17), spectroscopically confirmed supernovae discovered by other sources in 2015. As with the first ASAS-SN bright supernova catalogue, we also present redshifts and near-ultraviolet through infrared magnitudes for all supernova host galaxies in both samples. Combined with our previous catalogue, this work comprises a complete catalogue of 455 supernovae from multiple professional and amateur sources, allowing for population studies that were previously impossible. This is themore » second of a series of yearly papers on bright supernovae and their hosts from the ASAS-SN team.« less

  17. The ASAS-SN Bright Supernova Catalog – II. 2015

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

    Holoien, T. W. -S.; Brown, J. S.; Stanek, K. Z.

    Here, this paper presents information for all supernovae discovered by the All-Sky Automated Survey for SuperNovae (ASAS-SN) during 2015, its second full year of operations. The same information is presented for bright (mV ≤ 17), spectroscopically confirmed supernovae discovered by other sources in 2015. As with the first ASAS-SN bright supernova catalogue, we also present redshifts and near-ultraviolet through infrared magnitudes for all supernova host galaxies in both samples. Combined with our previous catalogue, this work comprises a complete catalogue of 455 supernovae from multiple professional and amateur sources, allowing for population studies that were previously impossible. This is themore » second of a series of yearly papers on bright supernovae and their hosts from the ASAS-SN team.« less

  18. Bright Loops at 171

    NASA Technical Reports Server (NTRS)

    2007-01-01

    STEREO was able to capture bright loops in exquisite detail as they were arcing above an active region (May 26, 2007) over an 18 hour period. What we are actually seeing are charged particles spinning along magnetic field lines that extend above the Sun's surface. Active regions are areas of intense magnetic activity and often the source of solar storms. In fact, the clip ends with a flourish in which a small coronal mass ejection (CME) blows out into space. This is from the STEREO Ahead spacecraft at the 171 Angstroms wavelength in extreme ultraviolet light.

  19. An Ultraviolet and Near-Infrared View of NGC 4214: A Starbursting Core Embedded in a Low Surface Brightness Disk

    NASA Astrophysics Data System (ADS)

    Fanelli, Michael N.; Waller, William W.; Smith, Denise A.; Freedman, Wendy L.; Madore, Barry; Neff, Susan G.; O'Connell, Robert W.; Roberts, Morton S.; Bohlin, Ralph; Smith, Andrew M.; Stecher, Theodore P.

    1997-05-01

    During the Astro-2 Spacelab mission in 1995 March, the Ultraviolet Imaging Telescope (UIT) obtained far-UV (λ = 1500 Å) imagery of the nearby Sm/Im galaxy NGC 4214. The UIT images have a spatial resolution of ~3" and a limiting surface brightness, μ1500 > 25 mag arcsec-2, permitting detailed investigation of the intensity and spatial distribution of the young, high-mass stellar component. These data provide the first far-UV imagery covering the full spatial extent of NGC 4214. Comparison with a corresponding I-band image reveals the presence of a starbursting core embedded in an extensive low surface brightness disk. In the far-UV (FUV), NGC 4214 is resolved into several components: a luminous, central knot; an inner region (r <~ 2.5 kpc) with ~15 resolved sources embedded in bright, diffuse emission; and a population of fainter knots extending to the edge of the optically defined disk (r ~ 5 kpc). The FUV light, which traces recent massive star formation, is observed to be more centrally concentrated than the I-band light, which traces the global stellar population. The FUV radial light profile is remarkably well represented by an R1/4 law, providing evidence that the centrally concentrated massive star formation in NGC 4214 is the result of an interaction, possibly a tidal encounter, with a dwarf companion(s). The brightest FUV source produces ~8% of the global FUV luminosity. This unresolved source, corresponding to the Wolf-Rayet knot described by Sargent & Filippenko, is located at the center of the FUV light distribution, giving NGC 4214 an active galactic nucleus-like morphology. Another strong source is present in the I band, located 19" west, 10" north of the central starburst knot, with no FUV counterpart. The I-band source may be the previously unrecognized nucleus of NGC 4214 or an evolved star cluster with an age greater than ~200 Myr. The global star formation rate derived from the total FUV flux is consistent with rates derived using data at other

  20. Brightness and magnetic evolution of solar coronal bright points

    NASA Astrophysics Data System (ADS)

    Ugarte Urra, Ignacio

    This thesis presents a study of the brightness and magnetic evolution of several Extreme ultraviolet (EUV) coronal bright points (hereafter BPs). The study was carried out using several instruments on board the Solar and Heliospheric Observatory, supported by the high resolution imaging from the Transition Region And Coronal Explorer. The results confirm that, down to 1" resolution, BPs are made of small loops with lengths of [approximate]6 Mm and cross-sections of ≈2 Mm. The loops are very dynamic, evolving in time scales as short as 1 - 2 minutes. This is reflected in a highly variable EUV response with fluctuations highly correlated in spectral lines at transition region temperatures, but not always at coronal temperatures. A wavelet analysis of the intensity variations reveals the existence of quasi-periodic oscillations with periods ranging 400--1000s, in the range of periods characteristic of the chromospheric network. The link between BPs and network bright points is discussed, as well as the interpretation of the oscillations in terms of global acoustic modes of closed magnetic structures. A comparison of the magnetic flux evolution of the magnetic polarities to the EUV flux changes is also presented. Throughout their lifetime, the intrinsic EUV emission of BPs is found to be dependent on the total magnetic flux of the polarities. In short time scales, co-spatial and co-temporal coronal images and magnetograms, reveal the signature of heating events that produce sudden EUV brightenings simultaneous to magnetic flux cancellations. This is interpreted in terms of magnetic reconnection events. Finally, a electron density study of six coronal bright points produces values of ≈1.6×10 9 cm -3 , closer to active region plasma than to quiet Sun. The analysis of a large coronal loop (half length of 72 Mm) introduces the discussion on the prospects of future plasma diagnostics of BPs with forthcoming solar missions.

  1. The ASAS-SN bright supernova catalogue - III. 2016

    NASA Astrophysics Data System (ADS)

    Holoien, T. W.-S.; Brown, J. S.; Stanek, K. Z.; Kochanek, C. S.; Shappee, B. J.; Prieto, J. L.; Dong, Subo; Brimacombe, J.; Bishop, D. W.; Bose, S.; Beacom, J. F.; Bersier, D.; Chen, Ping; Chomiuk, L.; Falco, E.; Godoy-Rivera, D.; Morrell, N.; Pojmanski, G.; Shields, J. V.; Strader, J.; Stritzinger, M. D.; Thompson, Todd A.; Woźniak, P. R.; Bock, G.; Cacella, P.; Conseil, E.; Cruz, I.; Fernandez, J. M.; Kiyota, S.; Koff, R. A.; Krannich, G.; Marples, P.; Masi, G.; Monard, L. A. G.; Nicholls, B.; Nicolas, J.; Post, R. S.; Stone, G.; Wiethoff, W. S.

    2017-11-01

    This catalogue summarizes information for all supernovae discovered by the All-Sky Automated Survey for SuperNovae (ASAS-SN) and all other bright (mpeak ≤ 17), spectroscopically confirmed supernovae discovered in 2016. We then gather the near-infrared through ultraviolet magnitudes of all host galaxies and the offsets of the supernovae from the centres of their hosts from public data bases. We illustrate the results using a sample that now totals 668 supernovae discovered since 2014 May 1, including the supernovae from our previous catalogues, with type distributions closely matching those of the ideal magnitude limited sample from Li et al. This is the third of a series of yearly papers on bright supernovae and their hosts from the ASAS-SN team.

  2. Unveiling the Low Surface Brightness Stellar Peripheries of Galaxies

    NASA Astrophysics Data System (ADS)

    Ferguson, Annette M. N.

    2018-01-01

    The low surface brightness peripheral regions of galaxies contain a gold mine of information about how minor mergers and accretions have influenced their evolution over cosmic time. Enormous stellar envelopes and copious amounts of faint tidal debris are natural outcomes of the hierarchical assembly process and the search for and study of these features, albeit highly challenging, offers the potential for unrivalled insight into the mechanisms of galaxy growth. Over the last two decades, there has been burgeoning interest in probing galaxy outskirts using resolved stellar populations. Wide-field surveys have uncovered vast tidal debris features and new populations of very remote globular clusters, while deep Hubble Space Telescope photometry has provided exquisite star formation histories back to the earliest epochs. I will highlight some recent results from studies within and beyond the Local Group and conclude by briefly discussing the great potential of future facilities, such as JWST, Euclid, LSST and WFIRST, for major breakthroughs in low surface brightness galaxy periphery science.

  3. Apollo-16 far-ultraviolet spectra in the Large Magellanic Cloud

    NASA Technical Reports Server (NTRS)

    Carruthers, G. R.; Page, T.

    1977-01-01

    Spectra in the wavelength ranges from 900 to 1600 A and 1050 to 1600 A of some OB associations in the Large Magellanic Cloud were obtained from the lunar surface by the Apollo-16 far-ultraviolet camera/spectrograph on April 22, 1972. The observed spectral distributions appear consistent with a stellar model having an effective temperature of 30,000 K, reddened by E(B-V) = 0.3, and characterized by the average far-ultraviolet extinction curve of Bless and Savage (1972). However, the absolute intensity of the far-ultraviolet spectrum of the associations NGC 2050 and 2055 seems somewhat too bright in comparison with ground-based photometry.

  4. Three-Dimensional Structure and Evolution of Extreme-Ultraviolet Bright Points Observed by STEREO/SECCHI/EUVI

    NASA Technical Reports Server (NTRS)

    Kwon, Ryun Young; Chae, Jongchul; Davila, Joseph M.; Zhang, Jie; Moon, Yong-Jae; Poomvises, Watanachak; Jones, Shaela I.

    2012-01-01

    We unveil the three-dimensional structure of quiet-Sun EUV bright points and their temporal evolution by applying a triangulation method to time series of images taken by SECCHI/EUVI on board the STEREO twin spacecraft. For this study we examine the heights and lengths as the components of the three-dimensional structure of EUV bright points and their temporal evolutions. Among them we present three bright points which show three distinct changes in the height and length: decreasing, increasing, and steady. We show that the three distinct changes are consistent with the motions (converging, diverging, and shearing, respectively) of their photospheric magnetic flux concentrations. Both growth and shrinkage of the magnetic fluxes occur during their lifetimes and they are dominant in the initial and later phases, respectively. They are all multi-temperature loop systems which have hot loops (approx. 10(exp 6.2) K) overlying cooler ones (approx 10(exp 6.0) K) with cool legs (approx 10(exp 4.9) K) during their whole evolutionary histories. Our results imply that the multi-thermal loop system is a general character of EUV bright points. We conclude that EUV bright points are flaring loops formed by magnetic reconnection and their geometry may represent the reconnected magnetic field lines rather than the separator field lines.

  5. Far-Ultraviolet Observations of Outflows from Infrared-Luminous Galaxies

    NASA Astrophysics Data System (ADS)

    Leitherer, Claus; Chandar, Rupali; Tremonti, Christy A.; Wofford, Aida

    2013-03-01

    We have obtained ultraviolet spectra between 1150 and 1450 Å of four ultraviolet-bright, infrared-luminous starburst galaxies. Our selected sight-lines towards the starburst nuclei probe the conditions in the starburst-driven outflows. We detect outflowing gas with velocities of up to ˜900 km s-1. It is likely that the outflows are a major source of metal enrichment of the galaxies' halos. The mass outflow rates of several tens of M⊙ yr-1 are similar to the star-formation rates. The outflows may quench star formation and ultimately regulate the starburst.

  6. Ultraviolet spectrophotometry from Gemini 11 of stars in Orion

    NASA Technical Reports Server (NTRS)

    Morgan, T. H.; Spear, G. G.; Kondo, Y.; Henize, K. G.

    1975-01-01

    Ultraviolet spectrophotometry in the wavelength region 2600-3600 A is reported for the bright early-type stars beta, eta, gamma, delta, iota, epsilon, sigma, zeta, and kappa Ori. The results are in good agreement with other observations, and, with the possible exception of the supergiants, are in good agreement with recent line-blanketed model atmospheres. There is evidence that the supergiants possess a small ultraviolet deficiency shortward of 3000 A relative to main-sequence stars of similar spectral type. The most extreme example of this phenomenon is the star kappa Ori.

  7. Investigation of ultraviolet fluxes of normal and peculiar stars

    NASA Technical Reports Server (NTRS)

    Deutschman, W. A.; Schild, R. E.

    1974-01-01

    Data from Project Celescope, a program that photographed the ultraviolet sky, in order to study several problems in current astrophysics are analyzed. Two star clusters, the Pleiades and the Hyades, reveal differences between the two that we are unable to explain simply from their differences in chemical abundance, rotation, or reddening. Data for Orion show large scatter, which appears to be in the sense that the Orion stars are too faint for their ground-based photometry. Similarly, many supergiants in the association Sco OB1 are too faint in the ultraviolet, but the ultraviolet brightness appears to be only poorly correlated with spectral type. Ultraviolet Celescope data for several groups of peculiar stars have also been analyzed. The strong He I stars are too faint in the ultraviolet, possibly owing to enhancement of O II continuous opacity due to oxygen overabundance. The Be stars appear to have ultraviolet colors normal for their MK spectral types. The P Cygni stars are considerably fainter than main-sequence stars of comparable spectral type, probably owing, at least in part, to line blocking by resonance lines of multiply ionized light metals. The Wolf-Rayet stars have ultraviolet color temperatures of O stars.

  8. International Ultraviolet Explorer (IUE) ultraviolet spectral atlas of selected astronomical objects

    NASA Technical Reports Server (NTRS)

    Wu, Chi-Chao; Reichert, Gail A.; Ake, Thomas B.; Boggess, Albert; Holm, Albert V.; Imhoff, Catherine L.; Kondo, Yoji; Mead, Jaylee M.; Shore, Steven N.

    1992-01-01

    The IUE Ultraviolet Spectral Atlas of Selected Astronomical Objects (or 'the Atlas'), is based on the data that were available in the IUE archive in 1986, and is intended to be a quick reference for the ultraviolet spectra of many categories of astronomical objects. It shows reflected sunlight from the Moon, planets, and asteroids, and also shows emission from comets. Comprehensive compilations of UV spectra for main sequence, subgiant, giant, bright giant, and supergiant stars are published elsewhere. This Atlas contains the spectra for objects occupying other areas of the Hertzsprung-Russell diagram: pre-main sequence stars, chemically peculiar stars, pulsating variables, subluminous stars, and Wolf-Rayet stars. This Atlas also presents phenomena such as the chromospheric and transition region emissions from late-type stars; composite spectra of stars, gas streams, accretion disks and gas envelopes of binary systems; the behavior of gas ejecta shortly after the outburst of novac and supernovac; and the H II regions, planetary nebulae, and supernova remnants. Population 2 stars, globular clusters, and luminous stars in the Magellanic Clouds, M31, and M33, are also included in this publication. Finally, the Atlas gives the ultraviolet spectra of galaxies of different Hubble types and of active galaxies.

  9. Synchronized observations of bright points from the solar photosphere to the corona

    NASA Astrophysics Data System (ADS)

    Tavabi, Ehsan

    2018-05-01

    One of the most important features in the solar atmosphere is the magnetic network and its relationship to the transition region (TR) and coronal brightness. It is important to understand how energy is transported into the corona and how it travels along the magnetic field lines between the deep photosphere and chromosphere through the TR and corona. An excellent proxy for transportation is the Interface Region Imaging Spectrograph (IRIS) raster scans and imaging observations in near-ultraviolet (NUV) and far-ultraviolet (FUV) emission channels, which have high time, spectral and spatial resolutions. In this study, we focus on the quiet Sun as observed with IRIS. The data with a high signal-to-noise ratio in the Si IV, C II and Mg II k lines and with strong emission intensities show a high correlation with TR bright network points. The results of the IRIS intensity maps and dopplergrams are compared with those of the Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI) instruments onboard the Solar Dynamical Observatory (SDO). The average network intensity profiles show a strong correlation with AIA coronal channels. Furthermore, we applied simultaneous observations of the magnetic network from HMI and found a strong relationship between the network bright points in all levels of the solar atmosphere. These features in the network elements exhibited regions of high Doppler velocity and strong magnetic signatures. Plenty of corona bright points emission, accompanied by the magnetic origins in the photosphere, suggest that magnetic field concentrations in the network rosettes could help to couple the inner and outer solar atmosphere.

  10. Ultraviolet photometry from the Orbiting Astronomical Observatory. XXXII - An atlas of ultraviolet stellar spectra

    NASA Technical Reports Server (NTRS)

    Code, A. D.; Meade, M. R.

    1979-01-01

    Ultraviolet stellar fluxes are presented in graphs and tables for 164 bright stars in the spectral region from 1200 to 3600 A. The spectra represent a subset of OAO 2 spectrometer data on file at the National Space Science Data Center. The monochromatic flux is given in units of erg per (sq cm-s-A) with a spectral resolution of about 22 A in the region from 3600 to 1850 A and of approximately 12 A in the region from 1850 to 1160 A.

  11. The ASAS-SN bright supernova catalogue – III. 2016

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

    Holoien, T. W. -S.; Brown, J. S.; Stanek, K. Z.

    In this catalogue we summarize information for all supernovae discovered by the All-Sky Automated Survey for SuperNovae (ASAS-SN) and all other bright (m peak ≤ 17), spectroscopically confirmed supernovae discovered in 2016. We then gather the near-infrared through ultraviolet magnitudes of all host galaxies and the offsets of the supernovae from the centres of their hosts from public data bases. We illustrate the results using a sample that now totals 668 supernovae discovered since 2014 May 1, including the supernovae from our previous catalogues, with type distributions closely matching those of the ideal magnitude limited sample from Li et al.more » This is then the third of a series of yearly papers on bright supernovae and their hosts from the ASAS-SN team.« less

  12. The ASAS-SN bright supernova catalogue – III. 2016

    DOE PAGES

    Holoien, T. W. -S.; Brown, J. S.; Stanek, K. Z.; ...

    2017-08-18

    In this catalogue we summarize information for all supernovae discovered by the All-Sky Automated Survey for SuperNovae (ASAS-SN) and all other bright (m peak ≤ 17), spectroscopically confirmed supernovae discovered in 2016. We then gather the near-infrared through ultraviolet magnitudes of all host galaxies and the offsets of the supernovae from the centres of their hosts from public data bases. We illustrate the results using a sample that now totals 668 supernovae discovered since 2014 May 1, including the supernovae from our previous catalogues, with type distributions closely matching those of the ideal magnitude limited sample from Li et al.more » This is then the third of a series of yearly papers on bright supernovae and their hosts from the ASAS-SN team.« less

  13. Prospects for Near Ultraviolet Astronomical Observations from the Lunar Surface — LUCI

    NASA Astrophysics Data System (ADS)

    Mathew, J.; Kumar, B.; Sarpotdar, M.; Suresh, A.; Nirmal, K.; Sreejith, A. G.; Safonova, M.; Murthy, J.; Brosch, N.

    2018-04-01

    We have explored the prospects for UV observations from the lunar surface and developed a UV telescope (LUCI-Lunar Ultraviolet Cosmic Imager) to put on the Moon, with the aim to detect bright UV transients such as SNe, novae, TDE, etc.

  14. Bright point study. [of solar corona

    NASA Technical Reports Server (NTRS)

    Tang, F.; Harvey, K.; Bruner, M.; Kent, B.; Antonucci, E.

    1982-01-01

    Transition region and coronal observations of bright points by instruments aboard the Solar Maximum Mission and high resolution photospheric magnetograph observations on September 11, 1980 are presented. A total of 31 bipolar ephemeral regions were found in the photosphere from birth in 9.3 hours of combined magnetograph observations from three observatories. Two of the three ephemeral regions present in the field of view of the Ultraviolet Spectrometer-Polarimeter were observed in the C IV 1548 line. The unobserved ephemeral region was determined to be the shortest-lived (2.5 hr) and lowest in magnetic flux density (13G) of the three regions. The Flat Crystal Spectrometer observed only low level signals in the O VIII 18.969 A line, which were not statistically significant to be positively identified with any of the 16 ephemeral regions detected in the photosphere. In addition, the data indicate that at any given time there lacked a one-to-one correspondence between observable bright points and photospheric ephemeral regions, while more ephemeral regions were observed than their counterparts in the transition region and the corona.

  15. STEREOSCOPIC DETERMINATION OF HEIGHTS OF EXTREME ULTRAVIOLET BRIGHT POINTS USING DATA TAKEN BY SECCHI/EUVI ABOARD STEREO

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

    Kwon, Ryun-Young; Chae, Jongchul; Zhang Jie

    2010-05-01

    We measure the heights of EUV bright points (BPs) above the solar surface by applying a stereoscopic method to the data taken by the Solar TErrestrial RElations Observatory/SECCHI/Extreme UltraViolet Imager (EUVI). We have developed a three-dimensional reconstruction method for point-like features such as BPs using the simple principle that the position of a point in the three-dimensional space is specified as the intersection of two lines of sight. From a set of data consisting of EUVI 171 A, 195 A, 284 A, and 304 A images taken on 11 days arbitrarily selected during a period of 14 months, we havemore » identified and analyzed 210 individual BPs that were visible on all four passband images and smaller than 30 Mm. The BPs seen in the 304 A images have an average height of 4.4 Mm, and are often associated with the legs of coronal loops. In the 171 A, 195 A, and 284 A images the BPs appear loop-shaped, and have average heights of 5.1, 6.7, and 6.1 Mm, respectively. Moreover, there is a tendency that overlying loops are filled with hotter plasmas. The average heights of BPs in 171 A, 195 A, and 284 A passbands are roughly twice the corresponding average lengths. Our results support the notion that an EUV BP represents a system of small loops with temperature stratification like flaring loops, being consistent with the magnetic reconnection origin.« less

  16. Improving Assessment of Lifetime Solar Ultraviolet Radiation Exposure in Epidemiologic Studies: Comparison of Ultraviolet Exposure Assessment Methods in a Nationwide United States Occupational Cohort.

    PubMed

    Little, Mark P; Tatalovich, Zaria; Linet, Martha S; Fang, Michelle; Kendall, Gerald M; Kimlin, Michael G

    2018-06-13

    Solar ultraviolet radiation is the primary risk factor for skin cancers and sun-related eye disorders. Estimates of individual ambient ultraviolet irradiance derived from ground-based solar measurements and from satellite measurements have rarely been compared. Using self-reported residential history from 67,189 persons in a nationwide occupational US radiologic technologists cohort, we estimated ambient solar irradiance using data from ground-based meters and noontime satellite measurements. The mean distance-moved from city of longest residence in childhood increased from 137.6 km at ages 13-19 to 870.3 km at ages ≥65, with corresponding increases in absolute latitude-difference moved. At ages 20/40/60/80, the Pearson/Spearman correlation coefficients of ground-based and satellite-derived solar potential ultraviolet exposure, using irradiance and cumulative radiant-exposure metrics, were high (=0.87-0.92). There was also moderate correlation (Pearson/Spearman correlation coefficients=0.51-0.60) between irradiance at birth and at last-known address, for ground-based and satellite data. Satellite-based lifetime estimates of ultraviolet radiation were generally 14-15% lower than ground-based estimates, albeit with substantial uncertainties, possibly because ground-based estimates incorporate fluctuations in cloud and ozone, which are incompletely incorporated in the single noontime satellite-overpass ultraviolet value. If confirmed elsewhere, the findings suggest that ground-based estimates may improve exposure-assessment accuracy and potentially provide new insights into ultraviolet-radiation-disease relationships in epidemiologic studies. This article is protected by copyright. All rights reserved. This article is protected by copyright. All rights reserved.

  17. Far-ultraviolet stellar photometry: A field in Orion

    NASA Astrophysics Data System (ADS)

    Schmidt, Edward G.; Carruthers, George R.

    1993-12-01

    Far-ultraviolet photometry for 625 objects in Orion is presented. These data were extracted from electrographic camera images obtained during sounding rocket flights in 1975 and 1982. The 1975 images were centered close to the belt of Orion while the 1982 images were centered approximately 9 deg further north. One hundred and fifty stars fell in the overlapping region and were observed with both cameras. Sixty-eight percent of the objects were tentatively identified with known stars using the SIMBAD database while another 24% are blends of objects too close together to separate with our resolution. As in previous studies, the majority of the identified ultraviolet sources are early-type stars. However, there are a significant number for which no such identification was possible, and we suggest that these are interesting objects which should be further investigated. Seven stars were found which were bright in the ultraviolet but faint in the visible. We suggest that some of these are nearby white dwarfs.

  18. The Magnetic Evolution of Coronal Hole Bright Points

    NASA Astrophysics Data System (ADS)

    He, Y.; Muglach, K.

    2017-12-01

    Space weather refers to the state of the heliosphere and the geospace environment that are caused primarily by solar activity. Coronal mass ejections and flares originate in active regions and filaments close to the solar surface and can cause geomagnetic storms and solar energetic particles events, which can damage both spacecraft and ground-based systems that are critical for society's well-being. Coronal bright points are small-scale magnetic regions on the sun that seem to be similar to active regions, but are about an order of magnitude smaller. Due to their shorter lifetime, the complete evolutionary cycle of these mini active regions can be studied, from the time they appear in extreme-ultraviolet (EUV) images to the time they fade. We are using data from the Solar Dynamics Observatory (SDO) to study both the coronal EUV flux and the photospheric magnetic field and compare them to activities of the coronal bright point.

  19. Vehicle/Atmosphere Interaction Glows: Far Ultraviolet, Visible, and Infrared

    NASA Technical Reports Server (NTRS)

    Swenson, G.

    1999-01-01

    Spacecraft glow information has been gathered from a number of spacecraft including Atmospheric and Dynamic satellites, and Space Shuttles (numerous flights) with dedicated pallet flow observations on STS-39 (DOD) and STS-62 (NASA). In addition, a larger number of laboratory experiments with low energy oxygen beam studies have made important contributions to glow understanding. The following report provides information on three engineering models developed for spacecraft glow including the far ultraviolet to ultraviolet (1400-4000 A), and infrared (0.9-40 microns) spectral regions. The models include effects resulting from atmospheric density/altitude, spacecraft temperature, spacecraft material, and ram angle. Glow brightness would be predicted as a function of distance from surfaces for all wavelengths.

  20. Skylab experiment SO73: Gegenschein/zodiacal light. [electrophotometry of surface brightness and polarization

    NASA Technical Reports Server (NTRS)

    Weinberg, J. L.

    1976-01-01

    A 10 color photoelectric polarimeter was used to measure the surface brightness and polarization associated with zodiacal light, background starlight, and spacecraft corona during each of the Skylab missions. Fixed position and sky scanning observations were obtained during Skylab missions SL-2 and SL-3 at 10 wavelenghts between 4000A and 8200A. Initial results from the fixed-position data are presented on the spacecraft corona and on the polarized brightness of the zodiacal light. Included among the fixed position regions that were observed are the north celestial pole, south ecliptic pole, two regions near the north galactic pole, and 90 deg from the sun in the ecliptic. The polarized brightness of the zodiacal light was found to have the color of the sun at each of these positions. Because previous observations found the total brightness to have the color of the sun from the near ultraviolet out to 2.4 micrometers, the degree of polarization of the zodiacal light is independent of wavelength from 4000A to 8200A.

  1. International Ultraviolet Explorer observations of the peculiar variable spectrum of the eclipsing binary R Arae

    NASA Technical Reports Server (NTRS)

    Mccluskey, G. E.; Kondo, Y.

    1983-01-01

    The eclipsing binary system R Arae = HD 149730 is a relatively bright southern system with an orbital period of about 4.4 days. It is a single-lined spectroscopic binary. The spectral class of the primary component is B9 Vp. The system was included in a study of mass flow and evolution in close binary systems using the International Ultraviolet Explorer satellite (IUE). Four spectra in the wavelength range from 1150 to 1900 A were obtained with the far-ultraviolet SWP camera, and six spectra in the range from 1900 to 3200 range were obtained with the mid-ultraviolet LWR camera. The close binary R Arae exhibits very unusual ultraviolet spectra. It appears that no other close binary system, observed with any of the orbiting satellites, shows outside-eclipse ultraviolet continuum flux variations of this nature.

  2. HUBBLE IDENTIFIES SOURCE OF ULTRAVIOLET LIGHT IN AN OLD GALAXY

    NASA Technical Reports Server (NTRS)

    2002-01-01

    Hubble Space Telescope's exquisite resolution has allowed astronomers to resolve, for the first time, hot blue stars deep inside an elliptical galaxy. The swarm of nearly 8,000 blue stars resembles a blizzard of snowflakes near the core (lower right) of the neighboring galaxy M32, located 2.5 million light-years away in the constellation Andromeda. Hubble confirms that the ultraviolet light comes from a population of extremely hot helium-burning stars at a late stage in their lives. Unlike the Sun, which burns hydrogen into helium, these old stars exhausted their central hydrogen long ago, and now burn helium into heavier elements. The observations, taken in October 1998, were made with the camera mode of the Space Telescope Imaging Spectrograph (STIS) in ultraviolet light. The STIS field of view is only a small portion of the entire galaxy, which is 20 times wider on the sky. For reference, the full moon is 70 times wider than the STIS field-of-view. The bright center of the galaxy was placed on the right side of the image, allowing fainter stars to be seen on the left side of the image. These results are to be published in the March 1, 2000 issue of The Astrophysical Journal. Thirty years ago, the first ultraviolet observations of elliptical galaxies showed that they were surprisingly bright when viewed in ultraviolet light. Before those pioneering UV observations, old groups of stars were assumed to be relatively cool and thus extremely faint in the ultraviolet. Over the years since the initial discovery of this unexpected ultraviolet light, indirect evidence has accumulated that it originates in a population of old, but hot, helium-burning stars. Now Hubble provides the first direct visual evidence. Nearby elliptical galaxies are thought to be relatively simple galaxies comprised of old stars. Because they are among the brightest objects in the Universe, this simplicity makes them useful for tracing the evolution of stars and galaxies. Credits: NASA and Thomas

  3. Extreme ultraviolet explorer satellite observation of Jupiter's Io plasma torus

    NASA Technical Reports Server (NTRS)

    Hall, D. T; Gladstone, G. R.; Moos, H. W.; Bagenal, F.; Clarke, J. T.; Feldman, P. D.; Mcgrath, M. A.; Schneider, N. M.; Shemansky, D. E.; Strobel, D. F.

    1994-01-01

    We present the first Extreme Ultraviolet Explorer (EUVE) satellite observation of the Jupiter system, obtained during the 2 day period 1993 March 30 through April 1, which shows a rich emission-line spectrum from the Io plasma torus spanning wavelengths 370 to 735 A. The emission features correspond primarily to known multiplets of oxygen and sulfur ions, but a blended feature near 372 A is a plausible Na II transition. The summed detected energy flux of (7.2 +/- 0.2) x 10(exp -11) ergs/sq cm(s) corresponds to a radiated power of approximately equal to 4 x 10(exp 11) W in this spectral range. All ansa emissions show a distinct dawn-dusk brightness asymmetry and the measured dusk/dawn ratio of the bright S III lambda-680 feature is 2.3 +/- 0.3, significantly larger than the ratio measured by the Voyager spacecraft ultraviolet (UV) instruments. A preliminary estimate of ion partitioning indicates that the oxygen/sulfur ion ratio is approximately equal to 2, compared to the value approximately equal to 1.3 measured by Voyager, and that (Na(+))/(e) greater than 0.01.

  4. A study of the feasibility of ultraviolet spectrometry for cometary missions

    NASA Technical Reports Server (NTRS)

    Feldman, P. D.

    1979-01-01

    Ultraviolet spectra fo the comet West obtained by sounding rocket experiments in 1976 are reproduced and interpreted in order to estimate the expected brightness of the emission features and determine the spatial extent of these features for the proposed Halley Flyby/Tempel 2 rendezvous and the possible Halley or Encke flybys close to perihelion. A coma model was constructed and evaluated for the physical condition of candidate targets such as heliocentric distance, gas production, and composition. In addition to brightness profiles, the neutral and ion densities of the principal species are also dervied. The brightness profiles can be used to determine the feasibility of utilizing the space telescope to provide supporting observations during the mission. Basic parameters identified are spectral range, wavelength resolution, spatial resolution, sensitivity and dynamic range, rejection of scattered light, and integration or accumulation time.

  5. Absolute measurement of undulator radiation in the extreme ultraviolet

    NASA Astrophysics Data System (ADS)

    Maezawa, H.; Mitani, S.; Suzuki, Y.; Kanamori, H.; Tamamushi, S.; Mikuni, A.; Kitamura, H.; Sasaki, T.

    1983-04-01

    The spectral brightness of undulator radiation emitted by the model PMU-1 incorporated in the SOR-RING, the dedicated synchrotron radiation source in Tokyo, has been studied in the extreme ultraviolet region from 21.6 to 72.9 eV as a function of the electron energy γ, the field parameter K, and the angle of observation ϴ in the absolute scale. A series of measurements covering the first and the second harmonic component of undulator radiation was compared with the fundamental formula λ n= {λ 0}/{2nγ 2}( {1+K 2}/{2}+γϴ 2 and the effects of finite emittance were studied. The brightness at the first peak was smaller than the theoretical value, while an enhanced second harmonic component was observed.

  6. A Search for Low Surface Brightness Galaxies in the Ultraviolet with GALEX

    NASA Astrophysics Data System (ADS)

    Wyder, Ted K.; GALEX Science Team

    2006-12-01

    Low surface brightness (LSB) galaxies have traditionally been difficult to detect at visible wavelengths due to their low contrast with the night sky and their low numbers per deg2. We describe a new search for LSB galaxies using UV images from the Galaxy Evolution Explorer (GALEX) satellite. The images are from the GALEX Medium Imaging Survey targeting mainly areas of the sky within the Sloan Digital Sky Survey (SDSS) footprint. Due to the UV sky background at high Galactic latitudes reaching levels of only approximately 28 mag arcsec-2 as well as the relatively large sky coverage from GALEX, we can potentially search for LSB galaxies that would be difficult to detect optically.After first convolving the images with a suitable kernel, we select a diameter limited set of objects which we then inspect manually in order to remove image artifacts and other spurious detections. Red galaxies that have high optical surface brightness can be identified using either the ratio of far-UV to near-UV flux or via comparison to SDSS images. We quantify our selection limits using a set of artificial galaxy tests. Our goal is to find blue, ultra-LSB galaxies that would be virtually undetectable in large optical imaging surveys. GALEX is a NASA Small Explorer, launched in April 2003. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission.

  7. The first Extreme Ultraviolet Explorer source catalog

    NASA Technical Reports Server (NTRS)

    Bowyer, S.; Lieu, R.; Lampton, M.; Lewis, J.; Wu, X.; Drake, J. J.; Malina, R. F.

    1994-01-01

    The Extreme Ultraviolet Explorer (EUVE) has conducted an all-sky survey to locate and identify point sources of emission in four extreme ultraviolet wavelength bands centered at approximately 100, 200, 400, and 600 A. A companion deep survey of a strip along half the ecliptic plane was simultaneously conducted. In this catalog we report the sources found in these surveys using rigorously defined criteria uniformly applied to the data set. These are the first surveys to be made in the three longer wavelength bands, and a substantial number of sources were detected in these bands. We present a number of statistical diagnostics of the surveys, including their source counts, their sensitivites, and their positional error distributions. We provide a separate list of those sources reported in the EUVE Bright Source List which did not meet our criteria for inclusion in our primary list. We also provide improved count rate and position estimates for a majority of these sources based on the improved methodology used in this paper. In total, this catalog lists a total of 410 point sources, of which 372 have plausible optical ultraviolet, or X-ray identifications, which are also listed.

  8. Ultraviolet Spectra of Comets Observed with the International Ultraviolet Explorer Satellite Observatory.

    NASA Astrophysics Data System (ADS)

    Weaver, Harold Anthony, Jr.

    Ultraviolet spectra of seven comets observed with the International Ultraviolet Explorer (IUE) satellite are presented. Observations of comet Bradfield (1979 X) made in early 1980 allow a comprehensive study of the production of water by this comet. By comparing the observations to the predictions of two water models of the coma (Haser and vectorial), it is determined that these measurements support the idea of a comet composed principally of water ice. The vaporization of the water has a rather unexpected heliocentric variation, decreasing as r('-3.7) over the entire range of observations. Atomic carbon is relatively abundant in the coma of comet Bradfield; the production rate of carbon is roughly 5-10% of the water production rate. Analysis of the spatial brightness profiles of the strongest atomic carbon emission does not reveal the identity of the source of the observed carbon, but the data are apparently inconsistent with a photodissociation source that is either CO or CO(,2). A comparison of the ultraviolet spectrum of periodic comet Encke, recorded by the IUE between 1980 October 24 and November 5, with similar spectra of short and long period comets shows the gaseous composition of P/Encke to be virtually identical to that of the other comets. If P/Encke is indeed the remains of a once giant comet, this similarity implies a homogeneous structure for the cometary ice nucleus. The OH(0,0) band brightness distribution shows a spatial variation similar to the visible fan-shaped image of the comet. Comets P/Tuttle (1980h), P/Stephan-Oterma (1980g), and Meier (1980q) were observed during November-December 1980 with IUE, while comets P/Borrelly (1980i) and Panther (1980u) were observed with IUE on 6 March 1981. The spectra of these comets are compared with those of comets Bradfield (1979 X) and P/Encke, as well as with each other. In order to simplify the interpretation of the data and to minimize the dependence upon a specific model, the spectra are compared at

  9. Energy-exchange collisions of dark-bright-bright vector solitons.

    PubMed

    Radhakrishnan, R; Manikandan, N; Aravinthan, K

    2015-12-01

    We find a dark component guiding the practically interesting bright-bright vector one-soliton to two different parametric domains giving rise to different physical situations by constructing a more general form of three-component dark-bright-bright mixed vector one-soliton solution of the generalized Manakov model with nine free real parameters. Moreover our main investigation of the collision dynamics of such mixed vector solitons by constructing the multisoliton solution of the generalized Manakov model with the help of Hirota technique reveals that the dark-bright-bright vector two-soliton supports energy-exchange collision dynamics. In particular the dark component preserves its initial form and the energy-exchange collision property of the bright-bright vector two-soliton solution of the Manakov model during collision. In addition the interactions between bound state dark-bright-bright vector solitons reveal oscillations in their amplitudes. A similar kind of breathing effect was also experimentally observed in the Bose-Einstein condensates. Some possible ways are theoretically suggested not only to control this breathing effect but also to manage the beating, bouncing, jumping, and attraction effects in the collision dynamics of dark-bright-bright vector solitons. The role of multiple free parameters in our solution is examined to define polarization vector, envelope speed, envelope width, envelope amplitude, grayness, and complex modulation of our solution. It is interesting to note that the polarization vector of our mixed vector one-soliton evolves in sphere or hyperboloid depending upon the initial parametric choices.

  10. IRAS surface brightness maps of reflection nebulae in the Pleiades

    NASA Technical Reports Server (NTRS)

    Castelaz, Michael W.; Werner, M. W.; Sellgren, K.

    1987-01-01

    Surface brightness maps at 12, 25, 60, and 100 microns were made of a 2.5 deg x 2.5 deg area of the reflection nebulae in the Pleiades by coadding IRAS scans of this region. Emission is seen surrounding 17 Tau, 20 Tau, 23 Tau, and 25 Tau in all four bands, coextensive with the visible reflection nebulosity, and extending as far as 30 arcminutes from the illuminating stars. The infrared energy distributions of the nebulae peak in the 100 micron band, but up to 40 percent of the total infrared power lies in the 12 and 25 micron bands. The brightness of the 12 and 25 micron emission and the absence of temperature gradients at these wavelengths are inconsistent with the predictions of equilibrium thermal emission models. The emission at these wavelengths appears to be the result of micron nonequilibrium emission from very small grains, or from molecules consisting of 10-100 carbon atoms, which have been excited by ultraviolet radiation from the illuminating stars.

  11. Ultraviolet Imaging Telescope ultraviolet images - Large-scale structure, H II regions, and extinction in M81

    NASA Technical Reports Server (NTRS)

    Hill, Jesse K.; Bohlin, Ralph C.; Cheng, Kwang-Ping; Hintzen, Paul M. N.; Landsman, Wayne B.; Neff, Susan G.; O'Connell, Robert W.; Roberts, Morton S.; Smith, Andrew M.; Smith, Eric P.

    1992-01-01

    The study employs UV images of M81 obtained by the Ultraviolet Imaging Telescope (UIT) during the December 1990 Astro-1 spacelab mission to determine 2490- and 1520-A fluxes from 46 H II regions and global surface brightness profiles. Comparison photometry in the V band is obtained from a ground-based CCD image. UV radial profiles show bulge and exponential disk components, with a local decrease in disk surface brightness inside the inner Lindblad Resonance about 4 arcmin from the nucleus. The V profile shows typical bulge plus exponential disk structure, with no local maximum in the disk. There is little change of UV color across the disk, although there is a strong gradient in the bulge. Observed m152-V colors of the H II regions are consistent with model spectra for young clusters, after dereddening using Av determined from m249-V and the Galactic extinction curve. The value of Av, so determined, is 0.4 mag greater on the average than Av derived from radio continuum and H-alpha fluxes.

  12. The ultraviolet reflectance of Enceladus: Implications for surface composition

    NASA Astrophysics Data System (ADS)

    Hendrix, Amanda R.; Hansen, Candice J.; Holsclaw, Greg M.

    2010-04-01

    The reflectance of Saturn's moon Enceladus has been measured at far ultraviolet (FUV) wavelengths (115-190 nm) by Cassini's Ultraviolet Imaging Spectrograph (UVIS). At visible and near infrared (VNIR) wavelengths Enceladus' reflectance spectrum is very bright, consistent with a surface composed primarily of H 2O ice. At FUV wavelengths, however, Enceladus is surprisingly dark - darker than would be expected for pure water ice. Previous analyses have focused on the VNIR spectrum, comparing it to pure water ice (Cruikshank, D.P., Owen, T.C., Dalle Ore, C., Geballe, T.R., Roush, T.L., de Bergh, C., Sandford, S.A., Poulet, F., Benedix, G.K., Emery, J.P. [2005] Icarus, 175, 268-283) or pure water ice plus a small amount of NH 3 (Emery, J.P., Burr, D.M., Cruikshank, D.P., Brown, R.H., Dalton, J.B. [2005] Astron. Astrophys., 435, 353-362) or NH 3 hydrate (Verbiscer, A.J., Peterson, D.E., Skrutskie, M.F., Cushing, M., Helfenstein, P., Nelson, M.J., Smith, J.D., Wilson, J.C. [2006] Icarus, 182, 211-223). We compare Enceladus' FUV spectrum to existing laboratory measurements of the reflectance spectra of candidate species, and to spectral models. We find that the low FUV reflectance of Enceladus can be explained by the presence of a small amount of NH 3 and a small amount of a tholin in addition to H 2O ice on the surface. The presence of these three species (H 2O, NH 3, and a tholin) appears to satisfy not only the low FUV reflectance and spectral shape, but also the middle-ultraviolet to visible wavelength brightness and spectral shape. We expect that ammonia in the Enceladus plume is transported across the surface to provide a global coating.

  13. The GALEX/S4G Surface Brightness and Color Profiles Catalog. I. Surface Photometry and Color Gradients of Galaxies

    NASA Astrophysics Data System (ADS)

    Bouquin, Alexandre Y. K.; Gil de Paz, Armando; Muñoz-Mateos, Juan Carlos; Boissier, Samuel; Sheth, Kartik; Zaritsky, Dennis; Peletier, Reynier F.; Knapen, Johan H.; Gallego, Jesús

    2018-02-01

    We present new spatially resolved surface photometry in the far-ultraviolet (FUV) and near-ultraviolet (NUV) from images obtained by the Galaxy Evolution Explorer (GALEX) and IRAC1 (3.6 μm) photometry from the Spitzer Survey of Stellar Structure in Galaxies (S4G). We analyze the radial surface brightness profiles μ FUV, μ NUV, and μ [3.6], as well as the radial profiles of (FUV ‑ NUV), (NUV ‑ [3.6]), and (FUV ‑ [3.6]) colors in 1931 nearby galaxies (z < 0.01). The analysis of the 3.6 μm surface brightness profiles also allows us to separate the bulge and disk components in a quasi-automatic way and to compare their light and color distribution with those predicted by the chemo-spectrophotometric models for the evolution of galaxy disks of Boissier & Prantzos. The exponential disk component is best isolated by setting an inner radial cutoff and an upper surface brightness limit in stellar mass surface density. The best-fitting models to the measured scale length and central surface brightness values yield distributions of spin and circular velocity within a factor of two of those obtained via direct kinematic measurements. We find that at a surface brightness fainter than μ [3.6] = 20.89 mag arcsec‑2, or below 3 × 108 M ⊙ kpc‑2 in stellar mass surface density, the average specific star formation rate (sSFR) for star-forming and quiescent galaxies remains relatively flat with radius. However, a large fraction of GALEX Green Valley galaxies show a radial decrease in sSFR. This behavior suggests that an outside-in damping mechanism, possibly related to environmental effects, could be testimony of an early evolution of galaxies from the blue sequence of star-forming galaxies toward the red sequence of quiescent galaxies.

  14. Differential responses to high- and low-dose ultraviolet-B stress in tobacco Bright Yellow-2 cells

    PubMed Central

    Takahashi, Shinya; Kojo, Kei H.; Kutsuna, Natsumaro; Endo, Masaki; Toki, Seiichi; Isoda, Hiroko; Hasezawa, Seiichiro

    2015-01-01

    Ultraviolet (UV)-B irradiation leads to DNA damage, cell cycle arrest, growth inhibition, and cell death. To evaluate the UV-B stress–induced changes in plant cells, we developed a model system based on tobacco Bright Yellow-2 (BY-2) cells. Both low-dose UV-B (low UV-B: 740 J m−2) and high-dose UV-B (high UV-B: 2960 J m−2) inhibited cell proliferation and induced cell death; these effects were more pronounced at high UV-B. Flow cytometry showed cell cycle arrest within 1 day after UV-B irradiation; neither low- nor high-UV-B–irradiated cells entered mitosis within 12 h. Cell cycle progression was gradually restored in low-UV-B–irradiated cells but not in high-UV-B–irradiated cells. UV-A irradiation, which activates cyclobutane pyrimidine dimer (CPD) photolyase, reduced inhibition of cell proliferation by low but not high UV-B and suppressed high-UV-B–induced cell death. UV-B induced CPD formation in a dose-dependent manner. The amounts of CPDs decreased gradually within 3 days in low-UV-B–irradiated cells, but remained elevated after 3 days in high-UV-B–irradiated cells. Low UV-B slightly increased the number of DNA single-strand breaks detected by the comet assay at 1 day after irradiation, and then decreased at 2 and 3 days after irradiation. High UV-B increased DNA fragmentation detected by the terminal deoxynucleotidyl transferase dUTP nick end labeling assay 1 and 3 days after irradiation. Caffeine, an inhibitor of ataxia telangiectasia mutated (ATM) and ataxia telangiectasia and Rad3-related (ATR) checkpoint kinases, reduced the rate of cell death in high-UV-B–irradiated cells. Our data suggest that low-UV-B–induced CPDs and/or DNA strand-breaks inhibit DNA replication and proliferation of BY-2 cells, whereas larger contents of high-UV-B–induced CPDs and/or DNA strand-breaks lead to cell death. PMID:25954287

  15. The Variability of Atmospheric Deuterium Brightness at Mars: Evidence for Seasonal Dependence

    NASA Astrophysics Data System (ADS)

    Mayyasi, Majd; Clarke, John; Bhattacharyya, Dolon; Deighan, Justin; Jain, Sonal; Chaffin, Michael; Thiemann, Edward; Schneider, Nick; Jakosky, Bruce

    2017-10-01

    The enhanced ratio of deuterium to hydrogen on Mars has been widely interpreted as indicating the loss of a large column of water into space, and the hydrogen content of the upper atmosphere is now known to be highly variable. The variation in the properties of both deuterium and hydrogen in the upper atmosphere of Mars is indicative of the dynamical processes that produce these species and propagate them to altitudes where they can escape the planet. Understanding the seasonal variability of D is key to understanding the variability of the escape rate of water from Mars. Data from a 15 month observing campaign, made by the Mars Atmosphere and Volatile Evolution Imaging Ultraviolet Spectrograph high-resolution echelle channel, are used to determine the brightness of deuterium as observed at the limb of Mars. The D emission is highly variable, with a peak in brightness just after southern summer solstice. The trends of D brightness are examined against extrinsic as well as intrinsic sources. It is found that the fluctuations in deuterium brightness in the upper atmosphere of Mars (up to 400 km), corrected for periodic solar variations, vary on timescales that are similar to those of water vapor fluctuations lower in the atmosphere (20-80 km). The observed variability in deuterium may be attributed to seasonal factors such as regional dust storm activity and subsequent circulation lower in the atmosphere.

  16. The far-ultraviolet emission spectrum of the K2 III star, Arcturus.

    NASA Technical Reports Server (NTRS)

    Moos, H. W.; Rottman, G. J.

    1972-01-01

    A moderate-resolution far-ultraviolet spectrum of the K2 IIIp star Arcturus, obtained with a rocket-borne spectrometer, shows chromospheric emission features. Hydrogen L-alpha and O I (1303 A) are clearly identified. The O I (1304 A) stellar surface brightness is as great or greater than that of the sun. Other metal lines, including those of carbon, are weak compared to the O I line.

  17. Jupiter in blue, ultraviolet and near infrared

    NASA Technical Reports Server (NTRS)

    2000-01-01

    These three images of Jupiter, taken through the narrow angle camera of NASA's Cassini spacecraft from a distance of 77.6 million kilometers (48.2 million miles) on October 8, reveal more than is apparent to the naked eye through a telescope.

    The image on the left was taken through the blue filter. The one in the middle was taken in the ultraviolet. The one on the right was taken in the near infrared.

    The blue-light filter is within the part of the electromagnetic spectrum detectable by the human eye. The appearance of Jupiter in this image is, consequently, very familiar. The Great Red Spot (below and to the right of center) and the planet's well-known banded cloud lanes are obvious. The brighter bands of clouds are called zones and are probably composed of ammonia ice particles. The darker bands are called belts and are made dark by particles of unknown composition intermixed with the ammonia ice.

    Jupiter's appearance changes dramatically in the ultraviolet and near infrared images. These images are near negatives of each other and illustrate the way in which observations in different wavelength regions can reveal different physical regimes on the planet.

    All gases scatter sunlight efficiently at short wavelengths; this is why the sky appears blue on Earth. The effect is even more pronounced in the ultraviolet. The gases in Jupiter's atmosphere, above the clouds, are no different. They scatter strongly in the ultraviolet, making the deep banded cloud layers invisible in the middle image. Only the very high altitude haze appears dark against the bright background. The contrast is reversed in the near infrared, where methane gas, abundant on Jupiter but not on Earth, is strongly absorbing and therefore appears dark. Again the deep clouds are invisible, but now the high altitude haze appears relatively bright against the dark background. High altitude haze is seen over the poles and the equator.

    The Great Red Spot, prominent in all images, is

  18. Bright Basin on Tethys

    NASA Image and Video Library

    2015-07-27

    With the expanded range of colors visible to Cassini's cameras, differences in materials and their textures become apparent that are subtle or unseen in natural color views. Here, the giant impact basin Odysseus on Saturn's moon Tethys stands out brightly from the rest of the illuminated icy crescent. This distinct coloration may result from differences in either the composition or structure of the terrain exposed by the giant impact. Odysseus (280 miles, or 450 kilometers, across) is one of the largest impact craters on Saturn's icy moons, and may have significantly altered the geologic history of Tethys. Tethys' dark side (at right) is faintly illuminated by reflected light from Saturn. Images taken using ultraviolet, green and infrared spectral filters were combined to create this color view. North on Tethys (660 miles or 1,062 kilometers across) is up in this view. The view was acquired on May 9, 2015 at a distance of approximately 186,000 miles (300,000 kilometers) from Tethys. Image scale is 1.1 mile (1.8 kilometers) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA18329

  19. The bright-bright and bright-dark mode coupling-based planar metamaterial for plasmonic EIT-like effect

    NASA Astrophysics Data System (ADS)

    Yu, Wei; Meng, Hongyun; Chen, Zhangjie; Li, Xianping; Zhang, Xing; Wang, Faqiang; Wei, Zhongchao; Tan, Chunhua; Huang, Xuguang; Li, Shuti

    2018-05-01

    In this paper, we propose a novel planar metamaterial structure for the electromagnetically induced transparency (EIT)-like effect, which consists of a split-ring resonator (SRR) and a pair of metal strips. The simulated results indicate that a single transparency window can be realized in the symmetry situation, which originates from the bright-bright mode coupling. Further, a dual-band EIT-like effect can be achieved in the asymmetry situation, which is due to the bright-bright mode coupling and bright-dark mode coupling, respectively. Different EIT-like effect can be simultaneously achieved in the proposed structure with the different situations. It is of certain significance for the study of EIT-like effect.

  20. Extreme Ultraviolet Explorer. Long look at the next window

    NASA Technical Reports Server (NTRS)

    Maran, Stephen P.

    1991-01-01

    The Extreme Ultraviolet Explorer (EUVE) will map the entire sky to determine the existence, direction, brightness, and temperature of thousands of objects that are sources of so-called extreme ultraviolet (EUV) radiation. The EUV spectral region is located between the x-ray and ultraviolet regions of the electromagnetic spectrum. From the sky survey by EUVE, astronomers will determine the nature of sources of EUV light in our galaxy, and infer the distribution of interstellar gas for hundreds of light years around the solar system. It is from this gas and the accompanying dust in space that new stars and solar systems are born and to which evolving and dying stars return much of their material in an endless cosmic cycle of birth, death, and rebirth. Besides surveying the sky, astronomers will make detailed studies of selected objects with EUVE to determine their physical properties and chemical compositions. Also, they will learn about the conditions that prevail and the processes at work in stars, planets, and other sources of EUV radiation, maybe even quasars. The EUVE mission and instruments are described. The objects that EUVE will likely find are described.

  1. Ultraviolet absorption cross-sections of hot carbon dioxide

    NASA Astrophysics Data System (ADS)

    Oehlschlaeger, Matthew A.; Davidson, David F.; Jeffries, Jay B.; Hanson, Ronald K.

    2004-12-01

    The temperature-dependent ultraviolet absorption cross-section for CO 2 has been measured in shock-heated gases between 1500 and 4500 K at 216.5, 244, 266, and 306 nm. Continuous-wave lasers provide the spectral brightness to enable precise time-resolved measurements with the microsecond time-response needed to monitor thermal decomposition of CO 2 at temperatures above 3000 K. The photophysics of the highly temperature dependent cross-section is discussed. The new data allows the extension of CO 2 absorption-based temperature sensing methods to higher temperatures, such as those found in behind detonation waves.

  2. Sparkling extreme-ultraviolet bright dots observed with Hi-C

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

    Régnier, S.; Alexander, C. E.; Walsh, R. W.

    Observing the Sun at high time and spatial scales is a step toward understanding the finest and fundamental scales of heating events in the solar corona. The high-resolution coronal (Hi-C) instrument has provided the highest spatial and temporal resolution images of the solar corona in the EUV wavelength range to date. Hi-C observed an active region on 2012 July 11 that exhibits several interesting features in the EUV line at 193 Å. One of them is the existence of short, small brightenings 'sparkling' at the edge of the active region; we call these EUV bright dots (EBDs). Individual EBDs havemore » a characteristic duration of 25 s with a characteristic length of 680 km. These brightenings are not fully resolved by the SDO/AIA instrument at the same wavelength; however, they can be identified with respect to the Hi-C location of the EBDs. In addition, EBDs are seen in other chromospheric/coronal channels of SDO/AIA, which suggests a temperature between 0.5 and 1.5 MK. Based on their frequency in the Hi-C time series, we define four different categories of EBDs: single peak, double peak, long duration, and bursty. Based on a potential field extrapolation from an SDO/HMI magnetogram, the EBDs appear at the footpoints of large-scale, trans-equatorial coronal loops. The Hi-C observations provide the first evidence of small-scale EUV heating events at the base of these coronal loops, which have a free magnetic energy of the order of 10{sup 26} erg.« less

  3. Influence of interplanetary magnetic field and solar wind on auroral brightness in different regions

    NASA Astrophysics Data System (ADS)

    Yang, Y. F.; Lu, J. Y.; Wang, J.-S.; Peng, Z.; Zhou, L.

    2013-01-01

    Abstract<p label="1">By integrating and averaging the auroral <span class="hlt">brightness</span> from Polar <span class="hlt">Ultraviolet</span> Imager auroral images, which have the whole auroral ovals, and combining the observation data of interplanetary magnetic field (IMF) and solar wind from NASA Operating Missions as a Node on the Internet (OMNI), we investigate the influence of IMF and solar wind on auroral activities, and analyze the separate roles of the solar wind dynamic pressure, density, and velocity on aurora, respectively. We statistically analyze the relations between the interplanetary conditions and the auroral <span class="hlt">brightness</span> in dawnside, dayside, duskside, and nightside. It is found that the three components of the IMF have different effects on the auroral <span class="hlt">brightness</span> in the different regions. Different from the nightside auroral <span class="hlt">brightness</span>, the dawnside, dayside, and duskside auroral <span class="hlt">brightness</span> are affected by the IMF Bx, and By components more significantly. The IMF Bx and By components have different effects on these three regional auroral <span class="hlt">brightness</span> under the opposite polarities of the IMF Bz. As expected, the nightside aurora is mainly affected by the IMF Bz, and under southward IMF, the larger the |Bz|, the brighter the nightside aurora. The IMF Bx and By components have no visible effects. On the other hand, it is also found that the aurora is not intensified singly with the increase of the solar wind dynamic pressure: when only the dynamic pressure is high, but the solar wind velocity is not very fast, the aurora will not necessarily be intensified significantly. These results can be used to qualitatively predict the auroral activities in different regions for various interplanetary conditions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/21451622','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/21451622"><span>Plasmonic EIT-like switching in <span class="hlt">bright-dark-bright</span> plasmon resonators.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Chen, Junxue; Wang, Pei; Chen, Chuncong; Lu, Yonghua; Ming, Hai; Zhan, Qiwen</p> <p>2011-03-28</p> <p>In this paper we report the study of the electromagnetically induced transparency (EIT)-like transmission in the <span class="hlt">bright-dark-bright</span> plasmon resonators. It is demonstrated that the interferences between the dark plasmons excited by two <span class="hlt">bright</span> plasmon resonators can be controlled by the incident light polarization. The constructive interference strengthens the coupling between the <span class="hlt">bright</span> and dark resonators, leading to a more prominent EIT-like transparency window of the metamaterial. In contrary, destructive interference suppresses the coupling between the <span class="hlt">bright</span> and dark resonators, destroying the interference pathway that forms the EIT-like transmission. Based on this observation, the plasmonic EIT switching can be realized by changing the polarization of incident light. This phenomenon may find applications in optical switching and plasmon-based information processing.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19840056759&hterms=Electric+current&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DElectric%2Bcurrent','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19840056759&hterms=Electric+current&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DElectric%2Bcurrent"><span>Photospheric electric current and transition region <span class="hlt">brightness</span> within an active region</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Deloach, A. C.; Hagyard, M. J.; Rabin, D.; Moore, R. L.; Smith, B. J., Jr.; West, E. A.; Tandberg-Hanssen, E.</p> <p>1984-01-01</p> <p>Distributions of vertical electrical current density J(z) calculated from vector measurements of the photospheric magnetic field are compared with <span class="hlt">ultraviolet</span> spectroheliograms to investigate whether resistive heating is an important source of enhanced emission in the transition region. The photospheric magnetic fields in Active Region 2372 were measured on April 6 and 7, 1980 with the Marshall Space Flight Center vector magnetograph; <span class="hlt">ultraviolet</span> wavelength spectroheliograms (L-alpha and N V 1239 A) were obtained with the UV Spectrometer and Polarimeter experiment aboard the Solar Maximum Mission satellite. Spatial registration of the J(z) (5 arcsec resolution) and UV (3 arcsec resolution) maps indicates that the maximum current density is cospatial with a minor but persistent UV enhancement, but there is little detected current associated with other nearby <span class="hlt">bright</span> areas. It is concluded that, although resistive heating may be important in the transition region, the currents responsible for the heating are largely unresolved in the present measurements and have no simple correlation with the residual current measured on 5-arcsec scales.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017SoSyR..51..579R','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017SoSyR..51..579R"><span>Galactic Astronomy in the <span class="hlt">Ultraviolet</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Rastorguev, A. S.; Sachkov, M. E.; Zabolotskikh, M. V.</p> <p>2017-12-01</p> <p>We propose a number of prospective observational programs for the <span class="hlt">ultraviolet</span> space observatory WSO-UV, which seem to be of great importance to modern galactic astronomy. The programs include the search for binary Cepheids; the search and detailed photometric study and the analysis of radial distribution of UV-<span class="hlt">bright</span> stars in globular clusters ("blue stragglers", blue horizontal-branch stars, RR Lyrae variables, white dwarfs, and stars with UV excesses); the investigation of stellar content and kinematics of young open clusters and associations; the study of spectral energy distribution in hot stars, including calculation of the extinction curves in the UV, optical and NIR; and accurate definition of the relations between the UV-colors and effective temperature. The high angular resolution of the observatory allows accurate astrometric measurements of stellar proper motions and their kinematic analysis.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19780055507&hterms=xxx&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dxxx','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19780055507&hterms=xxx&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dxxx"><span><span class="hlt">Ultraviolet</span> photometry from the orbiting astronomical observatory. XXX - The Orion reflection nebulosity</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Witt, A. N.; Lillie, C. F.</p> <p>1978-01-01</p> <p>Surface-<span class="hlt">brightness</span> measurements are presented that cover the region of Orion in nine intermediate-width bandpasses ranging from 4250 to 1550 A. The existence of an extended <span class="hlt">ultraviolet</span> reflection nebulosity in this area is confirmed, and the characteristics of its spectrum and spatial distribution are derived. The observations are consistent with a model in which the dense molecular cloud complex in Orion is illuminated by the foreground Orion aggregate of early-type stars. The interpretation is complicated by the fact that foreground dust may contribute to the observed scattered light. The scattering particles in the cloud appear to exhibit a wavelength-dependent albedo similar to that found for interstellar grains in general, with a strong indication that the phase function changes to a less forward-scattering form in the <span class="hlt">ultraviolet</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4992059','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4992059"><span><span class="hlt">Bright</span> high-order harmonic generation with controllable polarization from a relativistic plasma mirror</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Chen, Zi-Yu; Pukhov, Alexander</p> <p>2016-01-01</p> <p>Ultrafast extreme <span class="hlt">ultraviolet</span> (XUV) sources with a controllable polarization state are powerful tools for investigating the structural and electronic as well as the magnetic properties of materials. However, such light sources are still limited to only a few free-electron laser facilities and, very recently, to high-order harmonic generation from noble gases. Here we propose and numerically demonstrate a laser–plasma scheme to generate <span class="hlt">bright</span> XUV pulses with fully controlled polarization. In this scheme, an elliptically polarized laser pulse is obliquely incident on a plasma surface, and the reflected radiation contains pulse trains and isolated circularly or highly elliptically polarized attosecond XUV pulses. The harmonic polarization state is fully controlled by the laser–plasma parameters. The mechanism can be explained within the relativistically oscillating mirror model. This scheme opens a practical and promising route to generate <span class="hlt">bright</span> attosecond XUV pulses with desirable ellipticities in a straightforward and efficient way for a number of applications. PMID:27531047</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2009ApJS..185...20S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2009ApJS..185...20S"><span>Ten More New Sightlines for the Study of Intergalactic Helium, and Hundreds of Far-<span class="hlt">Ultraviolet-Bright</span> Quasars, from the Sloan Digital Sky Survey, Galaxy Evolution Explorer, and Hubble Space Telescope</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Syphers, David; Anderson, Scott F.; Zheng, Wei; Haggard, Daryl; Meiksin, Avery; Schneider, Donald P.; York, Donald G.</p> <p>2009-11-01</p> <p>Absorption along quasar sightlines remains among the most sensitive direct measures of He II reionization in much of the intergalactic medium (IGM). Until recently, fewer than a half-dozen unobscured quasar sightlines suitable for the He II Gunn-Peterson test were known; although these handful demonstrated great promise, the small sample size limited confidence in cosmological inferences. We have recently added nine more such clean He II quasars, exploiting Sloan Digital Sky Survey (SDSS) quasar samples, broadband <span class="hlt">ultraviolet</span> (UV) imaging from Galaxy Evolution Explorer (GALEX), and high-yield UV spectroscopic confirmations from Hubble Space Telescope (HST). Here we markedly expand this approach by cross-correlating SDSS DR7 and GALEX GR4+5 to catalog 428 SDSS and 165 other quasars with z > 2.78 having likely (~70%) GALEX detections, suggesting they are <span class="hlt">bright</span> into the far-UV. Reconnaissance HST Cycle 16 Supplemental prism data for 29 of these new quasar-GALEX matches spectroscopically confirm 17 as indeed far-UV <span class="hlt">bright</span>. At least 10 of these confirmations have clean sightlines all the way down to He II Lyα, substantially expanding the number of known clean He II quasars, and reaffirming the order of magnitude enhanced efficiency of our selection technique. Combined confirmations from this and our past programs yield more than 20 He II quasars, quintupling the sample. These provide substantial progress toward a sample of He II quasar sightlines large enough, and spanning a sufficient redshift range, to enable statistical IGM studies that may avoid individual object peculiarity and sightline variance. Our expanded catalog of hundreds of high-likelihood far-UV-<span class="hlt">bright</span> QSOs additionally will be useful for understanding the extreme-UV properties of the quasars themselves. Based on observations with the NASA/ESA Hubble Space Telescope obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19720029859&hterms=twilight&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dtwilight','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19720029859&hterms=twilight&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dtwilight"><span>Vacuum <span class="hlt">ultraviolet</span> spectra of the late twilight airglow.</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Buckley, J. L.; Moos, H. W.</p> <p>1971-01-01</p> <p>Evaluation of sounding rocket spectra of the late twilight (solar-zenith angle of 120 deg) <span class="hlt">ultraviolet</span> airglow between 1260 and 1900 A. The only observed features are O I 1304 and 1356. When the instrument looked at an elevation of 17 deg above the western horizon, the <span class="hlt">brightnesses</span> were 70 and 33 rayleighs, respectively. The upper limits on the total intensity of the Lyman-Birge-Hopfield and Vegard-Kaplan systems of N2 were 26 plus or minus 26 and 55 plus or minus 55 rayleighs, respectively. An estimate shows that a large part of the O I emissions may be due to excitation by conjugate-point electrons.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1993LNP...416..157H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1993LNP...416..157H"><span>UIT <span class="hlt">ultraviolet</span> imaging of 30 Doradus</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hintzen, P.; Cheng, K.-P.; Michalitsianos, A.; Bohlin, R.; O'Connell, R.; Cornett, R.; Roberts, M.; Smith, A.; Smith, E.; Stecher, T.</p> <p></p> <p>During the Astro-1 mission, near- and far-UV images of the 30 Doradus region were obtained using the <span class="hlt">Ultraviolet</span> Imaging Telescope (UIT). These wide-field, 40 min in diameter, high spatial resolution, 2-3 sec, UIT UV images reveal a rich field of luminous UV-<span class="hlt">bright</span> stars, clusters, and associations. There are 181 stars brighter than m2558A = 16.5 and 197 stars brighter than m1615A = 16.4 within 3 min diameter of the 30 Doradus central cluster. We have derived UV fluxes emitted from the 30 Doradus central cluster and from its UV <span class="hlt">bright</span> core, R136. The region within 5 sec of R136 produces approximately 14% of the far-UV flux (lambda = 1892 A) and approximately 16% of the near-UV flux (lambda = 2558 A) emitted from the 3 min diameter central cluster. The derived UV luminosity of R136 at 1892 A is only 7.8 times that of the nearby O6-7 Iaf star, R139, and the m1892 - mv colors of R136 are similar to other O or Wolf-Rayet stars in the same region. These UIT data, combined with other published observations at longer wavelengths, indicate that there is no observational evidence for a supermassive star in R136.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19760051419&hterms=Early+dwarf+stars&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DEarly%2Bdwarf%2Bstars','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19760051419&hterms=Early+dwarf+stars&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DEarly%2Bdwarf%2Bstars"><span>Skylab <span class="hlt">ultraviolet</span> stellar spectra - A new white dwarf, HD 149499 B</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Parsons, S. B.; Wray, J. D.; Benedict, G. F.; Henize, K. G.; Laget, M.</p> <p>1976-01-01</p> <p>The letter reports the discovery of a cool star with excess <span class="hlt">brightness</span> in the vacuum <span class="hlt">ultraviolet</span> on an objective-prism photograph obtained during the second Skylab mission. This star, HD 149499, is of type K0 V and has a companion with an apparent magnitude of about 11.8; the relatively flat UV spectrum observed at the position of HD 149499 is characteristic of a 10th or 11th magnitude unreddened O- or early B-type star. It is shown that the excess VUV <span class="hlt">brightness</span> is due to the companion, HD 149499B, which probably lies in the region of the H-R diagram occupied by the hot white dwarfs. Inspection of white dwarf lists indicates that this star is the sixth or seventh brightest white dwarf known. A maximum orbital motion of 0.025 arcsec/yr is estimated along with a period of just under 500 yr.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018AAS...23212101B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018AAS...23212101B"><span>IRIS <span class="hlt">Ultraviolet</span> Spectral Properties of a Sample of X-Class Solar Flares</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Butler, Elizabeth; Kowalski, Adam; Cauzzi, Gianna; Allred, Joel C.; Daw, Adrian N.</p> <p>2018-06-01</p> <p>The white-light (near-<span class="hlt">ultraviolet</span> (NUV) and optical) continuum emission comprises the majority of the radiated energy in solar flares. However, there are nearly as many explanations for the origin of the white-light continuum radiation as there are white-light flares that have been studied in detail with spectra. Furthermore, there are rarely robust constraints on the time-resolved dynamics in the white-light emitting flare layers. We are conducting a statistical study of the properties of Fe II lines, Mg II lines, and NUV continuum intensity in <span class="hlt">bright</span> flare kernels observed by the Interface Region Imaging Spectrograph (IRIS), in order to provide comprehensive constraints for radiative-hydrodynamic flare models. Here we present a new technique for identifying <span class="hlt">bright</span> flare kernels and preliminary relationships among IRIS spectral properties for a sample of X-class solar flares.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2009A%26A...497..287D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2009A%26A...497..287D"><span>The plasma filling factor of coronal <span class="hlt">bright</span> points. II. Combined EIS and TRACE results</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Dere, K. P.</p> <p>2009-04-01</p> <p>Aims: In a previous paper, the volumetric plasma filling factor of coronal <span class="hlt">bright</span> points was determined from spectra obtained with the Extreme <span class="hlt">ultraviolet</span> Imaging Spectrometer (EIS). The analysis of these data showed that the median plasma filling factor was 0.015. One interpretation of this result was that the small filling factor was consistent with a single coronal loop with a width of 1-2´´, somewhat below the apparent width. In this paper, higher spatial resolution observations with the Transition Region and Corona Explorer (TRACE) are used to test this interpretation. Methods: Rastered spectra of regions of the quiet Sun were recorded by the EIS during operations with the Hinode satellite. Many of these regions were simultaneously observed with TRACE. Calibrated intensities of Fe xii lines were obtained and images of the quiet corona were constructed from the EIS measurements. Emission measures were determined from the EIS spectra and geometrical widths of coronal <span class="hlt">bright</span> points were obtained from the TRACE images. Electron densities were determined from density-sensitive line ratios measured with EIS. A comparison of the emission measure and <span class="hlt">bright</span> point widths with the electron densities yielded the plasma filling factor. Results: The median electron density of coronal <span class="hlt">bright</span> points is 3 × 109 cm-3 at a temperature of 1.6 × 106 K. The volumetric plasma filling factor of coronal <span class="hlt">bright</span> points was found to vary from 3 × 10-3 to 0.3 with a median value of 0.04. Conclusions: The current set of EIS and TRACE coronal <span class="hlt">bright</span>-point observations indicate the median value of their plasma filling factor is 0.04. This can be interpreted as evidence of a considerable subresolution structure in coronal <span class="hlt">bright</span> points or as the result of a single completely filled plasma loop with widths on the order of 0.2-1.5´´ that has not been spatially resolved in these measurements.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018ApJ...857..104G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018ApJ...857..104G"><span>Illuminating Low Surface <span class="hlt">Brightness</span> Galaxies with the Hyper Suprime-Cam Survey</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Greco, Johnny P.; Greene, Jenny E.; Strauss, Michael A.; Macarthur, Lauren A.; Flowers, Xzavier; Goulding, Andy D.; Huang, Song; Kim, Ji Hoon; Komiyama, Yutaka; Leauthaud, Alexie; Leisman, Lukas; Lupton, Robert H.; Sifón, Cristóbal; Wang, Shiang-Yu</p> <p>2018-04-01</p> <p>We present a catalog of extended low surface <span class="hlt">brightness</span> galaxies (LSBGs) identified in the Wide layer of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). Using the first ∼200 deg2 of the survey, we have uncovered 781 LSBGs, spanning red (g ‑ i ≥ 0.64) and blue (g ‑ i < 0.64) colors and a wide range of morphologies. Since we focus on extended galaxies (r eff = 2.″5–14″), our sample is likely dominated by low-redshift objects. We define LSBGs to have mean surface <span class="hlt">brightnesses</span> {\\bar{μ }}eff}(g)> 24.3 mag arcsec‑2, which allows nucleated galaxies into our sample. As a result, the central surface <span class="hlt">brightness</span> distribution spans a wide range of μ 0(g) = 18–27.4 mag arcsec‑2, with 50% and 95% of galaxies fainter than 24.3 and 22 mag arcsec‑2, respectively. Furthermore, the surface <span class="hlt">brightness</span> distribution is a strong function of color, with the red distribution being much broader and generally fainter than that of the blue LSBGs, and this trend shows a clear correlation with galaxy morphology. Red LSBGs typically have smooth light profiles that are well characterized by single-component Sérsic functions. In contrast, blue LSBGs tend to have irregular morphologies and show evidence for ongoing star formation. We cross-match our sample with existing optical, H I, and <span class="hlt">ultraviolet</span> catalogs to gain insight into the physical nature of the LSBGs. We find that our sample is diverse, ranging from dwarf spheroidals and ultradiffuse galaxies in nearby groups to gas-rich irregulars to giant LSB spirals, demonstrating the potential of the HSC-SSP to provide a truly unprecedented view of the LSBG population.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018ApJ...854...75S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018ApJ...854...75S"><span>Following the Cosmic Evolution of Pristine Gas. II. The Search for Pop III–<span class="hlt">bright</span> Galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sarmento, Richard; Scannapieco, Evan; Cohen, Seth</p> <p>2018-02-01</p> <p>Direct observational searches for Population III (Pop III) stars at high redshift are faced with the question of how to select the most promising targets for spectroscopic follow-up. To help answer this, we use a large-scale cosmological simulation, augmented with a new subgrid model that tracks the fraction of pristine gas, to follow the evolution of high-redshift galaxies and the Pop III stars they contain. We generate rest-frame <span class="hlt">ultraviolet</span> (UV) luminosity functions for our galaxies and find that they are consistent with current z≥slant 7 observations. Throughout the redshift range 7≤slant z≤slant 15, we identify “Pop III–bright” galaxies as those with at least 75% of their flux coming from Pop III stars. While less than 1% of galaxies brighter than {m}UV,{AB}}=31.4 mag are Pop III–<span class="hlt">bright</span> in the range 7≤slant z≤slant 8, roughly 17% of such galaxies are Pop III–<span class="hlt">bright</span> at z = 9, immediately before reionization occurs in our simulation. Moving to z = 10, {m}UV,{AB}}=31.4 mag corresponds to larger, more luminous galaxies, and the Pop III–<span class="hlt">bright</span> fraction falls off to 5%. Finally, at the highest redshifts, a large fraction (29% at z = 14 and 41% at z = 15) of all galaxies are Pop III–<span class="hlt">bright</span> regardless of magnitude. While {m}UV,{AB}}=31.4 mag galaxies are extremely rare during this epoch, we find that 13% of galaxies at z = 14 are Pop III–<span class="hlt">bright</span> with {m}UV,{AB}}≤slant 33 mag, a intrinsic magnitude within reach of the James Webb Space Telescope using lensing. Thus, we predict that the best redshift to search for luminous Pop III–<span class="hlt">bright</span> galaxies is just before reionization, while lensing surveys for fainter galaxies should push to the highest redshifts possible.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27103935','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27103935"><span>Circadian Phase-Shifting Effects of <span class="hlt">Bright</span> Light, Exercise, and <span class="hlt">Bright</span> Light + Exercise.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Youngstedt, Shawn D; Kline, Christopher E; Elliott, Jeffrey A; Zielinski, Mark R; Devlin, Tina M; Moore, Teresa A</p> <p>2016-02-26</p> <p>Limited research has compared the circadian phase-shifting effects of <span class="hlt">bright</span> light and exercise and additive effects of these stimuli. The aim of this study was to compare the phase-delaying effects of late night <span class="hlt">bright</span> light, late night exercise, and late evening <span class="hlt">bright</span> light followed by early morning exercise. In a within-subjects, counterbalanced design, 6 young adults completed each of three 2.5-day protocols. Participants followed a 3-h ultra-short sleep-wake cycle, involving wakefulness in dim light for 2h, followed by attempted sleep in darkness for 1 h, repeated throughout each protocol. On night 2 of each protocol, participants received either (1) <span class="hlt">bright</span> light alone (5,000 lux) from 2210-2340 h, (2) treadmill exercise alone from 2210-2340 h, or (3) <span class="hlt">bright</span> light (2210-2340 h) followed by exercise from 0410-0540 h. Urine was collected every 90 min. Shifts in the 6-sulphatoxymelatonin (aMT6s) cosine acrophase from baseline to post-treatment were compared between treatments. Analyses revealed a significant additive phase-delaying effect of <span class="hlt">bright</span> light + exercise (80.8 ± 11.6 [SD] min) compared with exercise alone (47.3 ± 21.6 min), and a similar phase delay following <span class="hlt">bright</span> light alone (56.6 ± 15.2 min) and exercise alone administered for the same duration and at the same time of night. Thus, the data suggest that late night <span class="hlt">bright</span> light followed by early morning exercise can have an additive circadian phase-shifting effect.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19730002669','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19730002669"><span>Development and testing of the <span class="hlt">ultraviolet</span> spectrometer for the Mariner Mars 1971 spacecraft</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Farrar, J. W.</p> <p>1972-01-01</p> <p>The Mariner Mars 1971 <span class="hlt">ultraviolet</span> spectrometer is an Ebert-Fastie type of the same basic design as the Mariner Mars 1969 instrument. Light enters the instrument and is split into component wavelengths by a scanning reflection diffraction grating. Two monochrometer exit slits allow the use of two independent photomultiplier tube sensors. Channel 1 has a spectral range of 1100 to 1692 A with a fixed gain, while Channel 2 has a spectral range of 1450 to 3528 A with an automatic step gain control, providing a dynamic range over the expected atmosphere and surface <span class="hlt">brightness</span> of Mars. The scientific objectives, basic operation, design, testing, and calibration for the Mariner Mars 1971 <span class="hlt">ultraviolet</span> spectrometer are described. The design discussion includes those modifications that were necessary to extend the lifetime of the instrument in order to accomplish the Mariner Mars 1971 mission objectives.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1234578-ultraviolet-surprise-efficient-soft-ray-high-harmonic-generation-multiply-ionized-plasmas','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1234578-ultraviolet-surprise-efficient-soft-ray-high-harmonic-generation-multiply-ionized-plasmas"><span>The <span class="hlt">Ultraviolet</span> Surprise. Efficient Soft X-Ray High Harmonic Generation in Multiply-Ionized Plasmas</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Popmintchev, Dimitar; Hernandez-Garcia, Carlos; Dollar, Franklin; ...</p> <p>2015-12-04</p> <p>High-harmonic generation is a universal response of matter to strong femtosecond laser fields, coherently upconverting light to much shorter wavelengths. Optimizing the conversion of laser light into soft x-rays typically demands a trade-off between two competing factors. Reduced quantum diffusion of the radiating electron wave function results in emission from each species which is highest when a short-wavelength <span class="hlt">ultraviolet</span> driving laser is used. But, phase matching—the constructive addition of x-ray waves from a large number of atoms—favors longer-wavelength mid-infrared lasers. We identified a regime of high-harmonic generation driven by 40-cycle <span class="hlt">ultraviolet</span> lasers in waveguides that can generate <span class="hlt">bright</span> beams inmore » the soft x-ray region of the spectrum, up to photon energies of 280 electron volts. Surprisingly, the high <span class="hlt">ultraviolet</span> refractive indices of both neutral atoms and ions enabled effective phase matching, even in a multiply ionized plasma. We observed harmonics with very narrow linewidths, while calculations show that the x-rays emerge as nearly time-bandwidth–limited pulse trains of ~100 attoseconds.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28488591','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28488591"><span>Red-emission phosphor's <span class="hlt">brightness</span> deterioration by x-ray and <span class="hlt">brightness</span> recovery phenomenon by heating.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Nakamura, Masaaki; Chida, Koichi; Inaba, Yohei; Kobayashi, Ryota; Zuguchi, Masayuki</p> <p>2017-06-26</p> <p>There are no feasible real-time and direct skin dosimeters for interventional radiology. One would be available if there were x-ray phosphors that had no <span class="hlt">brightness</span> change caused by x-ray irradiation, but the emission of the Y 2 O 3 :Eu, (Y, Gd, Eu)BO 3 , and YVO 4 :Eu phosphors investigated in our previous study was reduced by x-ray irradiation. We found that the <span class="hlt">brightness</span> of those phosphors recovered, and the purpose of this study is to investigate their recovery phenomena. It is expected that more kinds of phosphors could be used in x-ray dosimeters if the <span class="hlt">brightness</span> changes caused by x-rays are elucidated and prevented. Three kinds of phosphors-Y 2 O 3 :Eu, (Y, Gd, Eu)BO 3 , and YVO 4 :Eu-were irradiated by x-rays (2 Gy) to reduce their <span class="hlt">brightness</span>. After the irradiation, <span class="hlt">brightness</span> changes occurring at room temperature and at 80 °C were investigated. The irradiation reduced the <span class="hlt">brightness</span> of all the phosphors by 5%-10%, but the <span class="hlt">brightness</span> of each recovered immediately both at room temperature and at 80 °C. The recovery at 80 °C was faster than that at room temperature, and at both temperatures the recovered <span class="hlt">brightness</span> remained at 95%-98% of the <span class="hlt">brightness</span> before the x-ray irradiation. The <span class="hlt">brightness</span> recovery phenomena of Y 2 O 3 :Eu, (Y, Gd, Eu)BO 3 , and YVO 4 :Eu phosphors occurring after <span class="hlt">brightness</span> deterioration due to x-ray irradiation were found to be more significant at 80 °C than at room temperature. More kinds of phosphors could be used in x-ray scintillation dosimeters if the reasons for the <span class="hlt">brightness</span> changes caused by x-rays were elucidated.</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_2");'>2</a></li> <li><a href="#" onclick='return showDiv("page_3");'>3</a></li> <li class="active"><span>4</span></li> <li><a href="#" onclick='return showDiv("page_5");'>5</a></li> <li><a href="#" onclick='return showDiv("page_6");'>6</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_4 --> <div id="page_5" 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_3");'>3</a></li> <li><a href="#" onclick='return showDiv("page_4");'>4</a></li> <li class="active"><span>5</span></li> <li><a href="#" onclick='return showDiv("page_6");'>6</a></li> <li><a href="#" onclick='return showDiv("page_7");'>7</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="81"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4834751','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4834751"><span>Circadian Phase-Shifting Effects of <span class="hlt">Bright</span> Light, Exercise, and <span class="hlt">Bright</span> Light + Exercise</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Kline, Christopher E.; Elliott, Jeffrey A.; Zielinski, Mark R.; Devlin, Tina M.; Moore, Teresa A.</p> <p>2016-01-01</p> <p>Limited research has compared the circadian phase-shifting effects of <span class="hlt">bright</span> light and exercise and additive effects of these stimuli. The aim of this study was to compare the phase-delaying effects of late night <span class="hlt">bright</span> light, late night exercise, and late evening <span class="hlt">bright</span> light followed by early morning exercise. In a within-subjects, counterbalanced design, 6 young adults completed each of three 2.5-day protocols. Participants followed a 3-h ultra-short sleep-wake cycle, involving wakefulness in dim light for 2h, followed by attempted sleep in darkness for 1 h, repeated throughout each protocol. On night 2 of each protocol, participants received either (1) <span class="hlt">bright</span> light alone (5,000 lux) from 2210–2340 h, (2) treadmill exercise alone from 2210–2340 h, or (3) <span class="hlt">bright</span> light (2210–2340 h) followed by exercise from 0410–0540 h. Urine was collected every 90 min. Shifts in the 6-sulphatoxymelatonin (aMT6s) cosine acrophase from baseline to post-treatment were compared between treatments. Analyses revealed a significant additive phase-delaying effect of <span class="hlt">bright</span> light + exercise (80.8 ± 11.6 [SD] min) compared with exercise alone (47.3 ± 21.6 min), and a similar phase delay following <span class="hlt">bright</span> light alone (56.6 ± 15.2 min) and exercise alone administered for the same duration and at the same time of night. Thus, the data suggest that late night <span class="hlt">bright</span> light followed by early morning exercise can have an additive circadian phase-shifting effect. PMID:27103935</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19950057219&hterms=r136+system&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Dr136%2Bsystem','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19950057219&hterms=r136+system&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Dr136%2Bsystem"><span>UIT <span class="hlt">ultraviolet</span> imaging of 30 Doradus</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hintzen, P.; Cheng, K.-P.; Michalitsianos, A.; Bohlin, R.; O'Connell, R.; Cornett, R.; Roberts, M.; Smith, A.; Smith, E.; Stecher, T.</p> <p>1992-01-01</p> <p>During the Astro-1 mission, near- and far-UV images of the 30 Doradus region were obtained using the <span class="hlt">Ultraviolet</span> Imaging Telescope (UIT). These wide-field, 40 min in diameter, high spatial resolution, 2-3 sec, UIT UV images reveal a rich field of luminous UV-<span class="hlt">bright</span> stars, clusters, and associations. There are 181 stars brighter than m(sub 2558A) = 16.5 and 197 stars brighter than m(sub 1615A) = 16.4 within 3 min diameter of the 30 Doradus central cluster. We have derived UV fluxes emitted from the 30 Doradus central cluster and from its UV <span class="hlt">bright</span> core, R136. The region within 5 sec of R136 produces approximately 14% of the far-UV flux (lambda = 1892 A) and approximately 16% of the near-UV flux (lambda = 2558 A) emitted from the 3 min diameter central cluster. The derived UV luminosity of R136 at 1892 A is only 7.8 times that of the nearby O6-7 Iaf star, R139, and the m(sub 1892) - m(sub v) colors of R136 are similar to other O or Wolf-Rayet stars in the same region. These UIT data, combined with other published observations at longer wavelengths, indicate that there is no observational evidence for a supermassive star in R136.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2007AGUFM.A33E1653H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2007AGUFM.A33E1653H"><span>Development of Yellow Sand Image Products Using Infrared <span class="hlt">Brightness</span> Temperature Difference Method</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ha, J.; Kim, J.; Kwak, M.; Ha, K.</p> <p>2007-12-01</p> <p>A technique for detection of airborne yellow sand dust using meteorological satellite has been developed from various bands from <span class="hlt">ultraviolet</span> to infrared channels. Among them, Infrared (IR) channels have an advantage of detecting aerosols over high reflecting surface as well as during nighttime. There had been suggestion of using <span class="hlt">brightness</span> temperature difference (BTD) between 11 and 12¥ìm. We have found that the technique is highly depends on surface temperature, emissivity, and zenith angle, which results in changing the threshold of BTD. In order to overcome these problems, we have constructed the background <span class="hlt">brightness</span> temperature threshold of BTD and then aerosol index (AI) has been determined from subtracting the background threshold from BTD of our interested scene. Along with this, we utilized high temporal coverage of geostationary satellite, MTSAT, to improve the reliability of the determined AI signal. The products have been evaluated by comparing the forecasted wind field with the movement fiend of AI. The statistical score test illustrates that this newly developed algorithm produces a promising result for detecting mineral dust by reducing the errors with respect to the current BTD method.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/26785483','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/26785483"><span><span class="hlt">Ultraviolet</span> surprise: Efficient soft x-ray high-harmonic generation in multiply ionized plasmas.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Popmintchev, Dimitar; Hernández-García, Carlos; Dollar, Franklin; Mancuso, Christopher; Pérez-Hernández, Jose A; Chen, Ming-Chang; Hankla, Amelia; Gao, Xiaohui; Shim, Bonggu; Gaeta, Alexander L; Tarazkar, Maryam; Romanov, Dmitri A; Levis, Robert J; Gaffney, Jim A; Foord, Mark; Libby, Stephen B; Jaron-Becker, Agnieszka; Becker, Andreas; Plaja, Luis; Murnane, Margaret M; Kapteyn, Henry C; Popmintchev, Tenio</p> <p>2015-12-04</p> <p>High-harmonic generation is a universal response of matter to strong femtosecond laser fields, coherently upconverting light to much shorter wavelengths. Optimizing the conversion of laser light into soft x-rays typically demands a trade-off between two competing factors. Because of reduced quantum diffusion of the radiating electron wave function, the emission from each species is highest when a short-wavelength <span class="hlt">ultraviolet</span> driving laser is used. However, phase matching--the constructive addition of x-ray waves from a large number of atoms--favors longer-wavelength mid-infrared lasers. We identified a regime of high-harmonic generation driven by 40-cycle <span class="hlt">ultraviolet</span> lasers in waveguides that can generate <span class="hlt">bright</span> beams in the soft x-ray region of the spectrum, up to photon energies of 280 electron volts. Surprisingly, the high <span class="hlt">ultraviolet</span> refractive indices of both neutral atoms and ions enabled effective phase matching, even in a multiply ionized plasma. We observed harmonics with very narrow linewidths, while calculations show that the x-rays emerge as nearly time-bandwidth-limited pulse trains of ~100 attoseconds. Copyright © 2015, American Association for the Advancement of Science.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2008AGUFM.P23A1361H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2008AGUFM.P23A1361H"><span><span class="hlt">Ultraviolet</span> Spectroscopy of the Surfaces of the Inner Icy Saturnian Satellites</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hendrix, A. R.; Hansen, C. J.</p> <p>2008-12-01</p> <p>The Cassini mission has provided a unique opportunity to make high-resolution, multi-spectral measurements of Saturn's icy moons, to investigate their surface compositions, processes and evolution. Here we present results from the <span class="hlt">Ultraviolet</span> Imaing Spectrograph (UVIS). This instrument allows for the first measurements of the icy satellites in the extreme <span class="hlt">ultraviolet</span> (EUV) to far-<span class="hlt">ultraviolet</span> (FUV) wavelength range. The icy satellites of the Saturn system exhibit a remarkable amount of variability: Dark, battered Phoebe orbiting at a distant 200 RS, black-and-white Iapetus, the wispy streaks of Dione, cratered Rhea and Mimas, <span class="hlt">bright</span> Tethys and geologically active Enceladus. Phoebe, Iapetus and Hyperion all orbit largely outside Saturn's magnetosphere, while the inner icy satellites Mimas, Enceladus, Dione Tethys and Rhea all orbit within the magnetosphere. Furthermore, the inner icy satellites all orbit within the E-ring - so the extent of exogenic effects on these icy satellites is wide-ranging. We present an overview of UVIS results from Tethys, Dione, Mimas, Enceladus and Rhea, focusing on surface investigations. We expect that the UV signatures of these icy satellites are strongly influenced not only by their water ice composition, but by external effects and magnetospheric environments. We study the FUV reflectance spectra to learn about the surface composition, map out water ice grain size variations, investigate effects of coating by E-ring grains, examine disk-resolved and hemispheric compositional and <span class="hlt">brightness</span> variations, and investigate the presence of radiation products. This is new work: FUV spectra of surfaces have not been well-studied in the past. Spectra of the inner icy moons have been used to better develop spectral models, to further understand existing lab data of water ice and to help with understanding instrument performance. Analysis is challenged by a lack of laboratory data in this wavelength region, but intriguing results are being found</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19930054484&hterms=Karovska&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAuthor-Name%26N%3D0%26No%3D20%26Ntt%3DKarovska','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19930054484&hterms=Karovska&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAuthor-Name%26N%3D0%26No%3D20%26Ntt%3DKarovska"><span><span class="hlt">Ultraviolet</span> continuum variability and visual flickering in the peculiar object MWC 560</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Michalitsianos, A. G.; Perez, M.; Shore, S. N.; Maran, S. P.; Karovska, M.; Sonneborn, G.; Webb, J. R.; Barnes, Thomas G., III; Frueh, Marian L.; Oliversen, R. J.</p> <p>1993-01-01</p> <p>High-speed U-band photometry of the peculiar emission object MWC 560 obtained with the ground-based instrumentation, and V-band photometry obtained with the International <span class="hlt">Ultraviolet</span> Explorer-Fine Error Sensor indicates irregular <span class="hlt">brightness</span> variations are quasi-periodic. Multiple peaks of relative <span class="hlt">brightness</span> power indicate statistically significant quasi periods existing in a range of 3-35 minutes, that are superposed on slower hourly varying components. We present a preliminary model that explains the minute and hourly time-scale variations in MWC 560 in terms of a velocity-shear instability that arises because a white dwarf magnetosphere impinges on an accretion disk. We also find evidence for Fe II multiplet pseudocontinuum absorption opacity in far-UV spectra of CH Cygni which is also present in MWC 560. Both CH Cyg and MWC 560 may be in an evolutionary stage that is characterized by strong UV continuum opacity which changes significantly during outburst, occurring before they permanently enter the symbiotic nebular emission phase.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/19243743','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/19243743"><span>A selective deficit in the appreciation and recognition of <span class="hlt">brightness</span>: <span class="hlt">brightness</span> agnosia?</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Nijboer, Tanja C W; Nys, Gudrun M S; van der Smagt, Maarten J; de Haan, Edward H F</p> <p>2009-01-01</p> <p>We report a patient with extensive brain damage in the right hemisphere who demonstrated a severe impairment in the appreciation of <span class="hlt">brightness</span>. Acuity, contrast sensitivity as well as luminance discrimination were normal, suggesting her <span class="hlt">brightness</span> impairment is not a mere consequence of low-level sensory impairments. The patient was not able to indicate the darker or the lighter of two grey squares, even though she was able to see that they differed. In addition, she could not indicate whether the lights in a room were switched on or off, nor was she able to differentiate between normal greyscale images and inverted greyscale images. As the patient recognised objects, colours, and shapes correctly, the impairment is specific for <span class="hlt">brightness</span>. As low-level, sensory processing is normal, this specific deficit in the recognition and appreciation of <span class="hlt">brightness</span> appears to be of a higher, cognitive level, the level of semantic knowledge. This appears to be the first report of '<span class="hlt">brightness</span> agnosia'.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/26252685','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/26252685"><span>Generation of <span class="hlt">Bright</span>, Spatially Coherent Soft X-Ray High Harmonics in a Hollow Waveguide Using Two-Color Synthesized Laser Pulses.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Jin, Cheng; Stein, Gregory J; Hong, Kyung-Han; Lin, C D</p> <p>2015-07-24</p> <p>We investigate the efficient generation of low-divergence high-order harmonics driven by waveform-optimized laser pulses in a gas-filled hollow waveguide. The drive waveform is obtained by synthesizing two-color laser pulses, optimized such that highest harmonic yields are emitted from each atom. Optimization of the gas pressure and waveguide configuration has enabled us to produce <span class="hlt">bright</span> and spatially coherent harmonics extending from the extreme <span class="hlt">ultraviolet</span> to soft x rays. Our study on the interplay among waveguide mode, atomic dispersion, and plasma effect uncovers how dynamic phase matching is accomplished and how an optimized waveform is maintained when optimal waveguide parameters (radius and length) and gas pressure are identified. Our analysis should help laboratory development in the generation of high-flux <span class="hlt">bright</span> coherent soft x rays as tabletop light sources for applications.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016DPS....4811617S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016DPS....4811617S"><span>Probing 67P/Churyumov-Gerasimenko's Electron Environment Through <span class="hlt">Ultraviolet</span> Emission by Rosetta Alice Observations</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Schindhelm, Eric; Noonan, John; Keeney, Brian A.; Broiles, Thomas; Bieler, Andre; A'Hearn, Michael F.; Bertaux, Jean-Loup; Feaga, Lori M.; Feldman, Paul D.; Parker, Joel Wm.; Steffl, Andrew Joseph; Stern, S. Alan; Weaver, Harold A.</p> <p>2016-10-01</p> <p>The Alice Far-<span class="hlt">Ultraviolet</span> (FUV) Spectrograph onboard ESA's Rosetta spacecraft has observed the coma of comet 67P/Churyumov-Gerasimenko from far approach in summer 2014 until the end of mission in September 2016. We present an overall perspective of the <span class="hlt">bright</span> FUV emission lines (HI 1026 Å, OI 1302/1305/1306 Å multiplet, OI] 1356 Å, CO 1510 (1-0) Å, and CI 1657 Å) above the sunward hemisphere, detailing their spatial extent and <span class="hlt">brightness</span> as a function of time and the heliocentric distance of the comet. We compare our observed gas column densities derived using electron temperatures and densities from the Ion Electron Sensor (IES) with those derived using the Inner Coma Environment Simulator (ICES) models in periods when electron-impact excited emission dominates over solar fluorescence emission. The electron population is characterized with 2 three-dimensional kappa functions, one dense and warm, one rarefied and hot.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=PIA10374&hterms=hydra&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dhydra','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=PIA10374&hterms=hydra&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dhydra"><span><span class="hlt">Ultraviolet</span> Extensions</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>2008-01-01</p> <p><p/> [figure removed for brevity, see original site] Side-by-Side Comparison Click on image for larger view <p/> This <span class="hlt">ultraviolet</span> image from NASA's Galaxy Evolution Explorer shows the Southern Pinwheel galaxy, also know as Messier 83 or M83. It is located 15 million light-years away in the southern constellation Hydra. <p/> <span class="hlt">Ultraviolet</span> light traces young populations of stars; in this image, young stars can be seen way beyond the main spiral disk of M83 up to 140,000 light-years from its center. Could life exist around one of these far-flung stars? Scientists say it's unlikely because the outlying regions of a galaxy are lacking in the metals required for planets to form. <p/> The image was taken at scheduled intervals between March 15 and May 20, 2007. It is one of the longest-exposure, or deepest, images ever taken of a nearby galaxy in <span class="hlt">ultraviolet</span> light. Near-<span class="hlt">ultraviolet</span> light (or longer-wavelength <span class="hlt">ultraviolet</span> light) is colored yellow, and far-<span class="hlt">ultraviolet</span> light is blue. <p/> What Lies Beyond the Edge of a Galaxy The side-by-side comparison shows the Southern Pinwheel galaxy, or M83, as seen in <span class="hlt">ultraviolet</span> light (right) and at both <span class="hlt">ultraviolet</span> and radio wavelengths (left). While the radio data highlight the galaxy's long, octopus-like arms stretching far beyond its main spiral disk (red), the <span class="hlt">ultraviolet</span> data reveal clusters of baby stars (blue) within the extended arms. <p/> The <span class="hlt">ultraviolet</span> image was taken by NASA's Galaxy Evolution Explorer between March 15 and May 20, 2007, at scheduled intervals. Back in 2005, the telescope first photographed M83 over a shorter period of time. That picture was the first to reveal far-flung baby stars forming up to 63,000 light-years from the edge of the main spiral disk. This came as a surprise to astronomers because a galaxy's outer territory typically lacks high densities of star-forming materials. <p/> The newest picture of M83 from the Galaxy Evolution Explorer is shown at the right, and was taken over a longer period of</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/29543278','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/29543278"><span>High-<span class="hlt">brightness</span> and high-color purity red-emitting Ca3Lu(AlO)3(BO3)4:Eu3+ phosphors with internal quantum efficiency close to unity for near-<span class="hlt">ultraviolet</span>-based white-light-emitting diodes.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Huang, Xiaoyong; Wang, Shaoying; Li, Bin; Sun, Qi; Guo, Heng</p> <p>2018-03-15</p> <p>In this work, we reported on high-<span class="hlt">brightness</span> Eu 3+ -activated Ca 3 Lu(AlO) 3 (BO 3 ) 4 (CLAB) red-emitting phosphors. Under 397 nm excitation, the CLAB:Eu 3+ phosphors showed intense red emissions at around 621 nm with CIE coordinates of (0.657, 0.343). The optimal doping concentration of Eu 3+ ions was found to be 30 mol. %, and the CLAB:0.3Eu 3+ sample possessed high-color purity of 93% and ultra-high internal quantum efficiency as great as 98.5%. Importantly, the CLAB:0.3Eu 3+ also had good thermal stability. Finally, a white-light-emitting diode (WLED) lamp with good color-rendering index was fabricated by using a 365 nm <span class="hlt">ultraviolet</span> chip and the phosphor blends of CLAB:0.3Eu 3+ red-emitting phosphors, (Ba,Sr) 2 SiO 4 :Eu 2+ green-emitting phosphors, and BaMgAl 10 O 7 :Eu 2+ blue-emitting phosphors.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.dtic.mil/docs/citations/ADA560292','DTIC-ST'); return false;" href="http://www.dtic.mil/docs/citations/ADA560292"><span>Supernova 2009kf: An <span class="hlt">Ultraviolet</span> <span class="hlt">Bright</span> Type IIP Supernova Discovered With Pan-Starrs 1 and Galex</span></a></p> <p><a target="_blank" href="http://www.dtic.mil/">DTIC Science & Technology</a></p> <p></p> <p>2010-07-01</p> <p>The 7 deg2 camera and 1.8 m aperture could allow IIP SNe to be used as cosmological probes at z ∼ 0.2 and the brightest events to be found out to z...<span class="hlt">ultraviolet</span> (NUV). We discuss the implication of this rare SN for understanding the explosions and the use of Type IIP events for probing cosmology and...SFR at high redshifts. We adopt the cosmological parameters H0 = 70 km s−1 Mpc−1, ΩM = 0.3, ΩΛ = 0.7. 2. DISCOVERY AND OBSERVATIONAL DATA SN 2009kf</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4216005','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4216005"><span>Intermittent Episodes of <span class="hlt">Bright</span> Light Suppress Myopia in the Chicken More than Continuous <span class="hlt">Bright</span> Light</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Lan, Weizhong; Feldkaemper, Marita; Schaeffel, Frank</p> <p>2014-01-01</p> <p>Purpose <span class="hlt">Bright</span> light has been shown a powerful inhibitor of myopia development in animal models. We studied which temporal patterns of <span class="hlt">bright</span> light are the most potent in suppressing deprivation myopia in chickens. Methods Eight-day-old chickens wore diffusers over one eye to induce deprivation myopia. A reference group (n = 8) was kept under office-like illuminance (500 lux) at a 10∶14 light∶dark cycle. Episodes of <span class="hlt">bright</span> light (15 000 lux) were super-imposed on this background as follows. Paradigm I: exposure to constant <span class="hlt">bright</span> light for either 1 hour (n = 5), 2 hours (n = 5), 5 hours (n = 4) or 10 hours (n = 4). Paradigm II: exposure to repeated cycles of <span class="hlt">bright</span> light with 50% duty cycle and either 60 minutes (n = 7), 30 minutes (n = 8), 15 minutes (n = 6), 7 minutes (n = 7) or 1 minute (n = 7) periods, provided for 10 hours. Refraction and axial length were measured prior to and immediately after the 5-day experiment. Relative changes were analyzed by paired t-tests, and differences among groups were tested by one-way ANOVA. Results Compared with the reference group, exposure to continuous <span class="hlt">bright</span> light for 1 or 2 hours every day had no significant protective effect against deprivation myopia. Inhibition of myopia became significant after 5 hours of <span class="hlt">bright</span> light exposure but extending the duration to 10 hours did not offer an additional benefit. In comparison, repeated cycles of 1∶1 or 7∶7 minutes of <span class="hlt">bright</span> light enhanced the protective effect against myopia and could fully suppress its development. Conclusions The protective effect of <span class="hlt">bright</span> light depends on the exposure duration and, to the intermittent form, the frequency cycle. Compared to the saturation effect of continuous <span class="hlt">bright</span> light, low frequency cycles of <span class="hlt">bright</span> light (1∶1 min) provided the strongest inhibition effect. However, our quantitative results probably might not be directly translated into humans, but rather need further amendments in clinical</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25360635','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25360635"><span>Intermittent episodes of <span class="hlt">bright</span> light suppress myopia in the chicken more than continuous <span class="hlt">bright</span> light.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Lan, Weizhong; Feldkaemper, Marita; Schaeffel, Frank</p> <p>2014-01-01</p> <p><span class="hlt">Bright</span> light has been shown a powerful inhibitor of myopia development in animal models. We studied which temporal patterns of <span class="hlt">bright</span> light are the most potent in suppressing deprivation myopia in chickens. Eight-day-old chickens wore diffusers over one eye to induce deprivation myopia. A reference group (n = 8) was kept under office-like illuminance (500 lux) at a 10:14 light:dark cycle. Episodes of <span class="hlt">bright</span> light (15 000 lux) were super-imposed on this background as follows. Paradigm I: exposure to constant <span class="hlt">bright</span> light for either 1 hour (n = 5), 2 hours (n = 5), 5 hours (n = 4) or 10 hours (n = 4). Paradigm II: exposure to repeated cycles of <span class="hlt">bright</span> light with 50% duty cycle and either 60 minutes (n = 7), 30 minutes (n = 8), 15 minutes (n = 6), 7 minutes (n = 7) or 1 minute (n = 7) periods, provided for 10 hours. Refraction and axial length were measured prior to and immediately after the 5-day experiment. Relative changes were analyzed by paired t-tests, and differences among groups were tested by one-way ANOVA. Compared with the reference group, exposure to continuous <span class="hlt">bright</span> light for 1 or 2 hours every day had no significant protective effect against deprivation myopia. Inhibition of myopia became significant after 5 hours of <span class="hlt">bright</span> light exposure but extending the duration to 10 hours did not offer an additional benefit. In comparison, repeated cycles of 1:1 or 7:7 minutes of <span class="hlt">bright</span> light enhanced the protective effect against myopia and could fully suppress its development. The protective effect of <span class="hlt">bright</span> light depends on the exposure duration and, to the intermittent form, the frequency cycle. Compared to the saturation effect of continuous <span class="hlt">bright</span> light, low frequency cycles of <span class="hlt">bright</span> light (1:1 min) provided the strongest inhibition effect. However, our quantitative results probably might not be directly translated into humans, but rather need further amendments in clinical studies.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2008AJ....136.1810A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2008AJ....136.1810A"><span>Chandra's Darkest <span class="hlt">Bright</span> Star: not so Dark after All?</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ayres, Thomas R.</p> <p>2008-11-01</p> <p>The Chandra High Resolution camera (HRC) has obtained numerous short exposures of the <span class="hlt">ultraviolet</span> (UV)-<span class="hlt">bright</span> star Vega (α Lyrae; HD 172167: A0 V), to calibrate the response of the detector to out-of-band (non-X-ray) radiation. A new analysis uncovered a stronger "blue leak" in the imaging section (HRC-I) than reported in an earlier study of Vega based on a subset of the pointings. The higher count rate—a factor of nearly 2 above prelaunch estimates—raised the possibility that genuine coronal X-rays might lurk among the out-of-band events. Exploiting the broader point-spread function of the UV leak compared with soft X-rays identified an excess of counts centered on the target, technically at 3σ significance. A number of uncertainties, however, prevent a clear declaration of a Vegan corona. A more secure result would be within reach of a deep uninterrupted HRC-I pointing.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19900028899&hterms=Pleiades&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DPleiades','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19900028899&hterms=Pleiades&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DPleiades"><span>First <span class="hlt">ultraviolet</span> observations of the transition regions of X-ray <span class="hlt">bright</span> solar-type stars in the Pleiades</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Caillault, J.-P.; Vilhu, O.; Linsky, J. L.</p> <p>1990-01-01</p> <p>Results are reported from A UV study of the transition regions of two X-ray-<span class="hlt">bright</span> solar-type stars from the Pleiades, in an attempt to extend the main sequence age baseline for the transition-region activity-age relation over more than two orders of magnitude. However, no emission lines were detected from either star; the upper limits to the fluxes are consistent with previously determined saturation levels, but do not help to further constrain evolutionary models.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19890033162&hterms=bright+hour&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dbright%2Bhour','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19890033162&hterms=bright+hour&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dbright%2Bhour"><span>Coronal <span class="hlt">bright</span> points in microwaves</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Kundu, M. R.; Nitta, N.</p> <p>1988-01-01</p> <p>An excellent map of the quiet sun showing coronal <span class="hlt">bright</span> points at 20-cm wavelength was produced using the VLA on February 13, 1987. The locations of <span class="hlt">bright</span> points (BPs) were studied relative to features on the photospheric magnetogram and Ca K spectroheliogram. Most <span class="hlt">bright</span> points appearing in the full 5-hour synthesized map are associated with small bipolar structures on the photospheric magnetogram; and the brightest part of a BP tends to lie on the boundary of a supergranulation network. The <span class="hlt">bright</span> points exhibit rapid variations in intensity superposed on an apparently slow variation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA12525.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA12525.html"><span>Faint Ring, <span class="hlt">Bright</span> Arc</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2010-01-12</p> <p>In this image taken by NASA Cassini spacecraft, the <span class="hlt">bright</span> arc in Saturn faint G ring contains a little something special. Although it cant be seen here, the tiny moonlet Aegaeon orbits within the <span class="hlt">bright</span> arc.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2005AJ....129.2777H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2005AJ....129.2777H"><span>The Loopy <span class="hlt">Ultraviolet</span> Line Profiles of RU Lupi: Accretion, Outflows, and Fluorescence</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Herczeg, Gregory J.; Walter, Frederick M.; Linsky, Jeffrey L.; Gahm, Gösta F.; Ardila, David R.; Brown, Alexander; Johns-Krull, Christopher M.; Simon, Michal; Valenti, Jeff A.</p> <p>2005-06-01</p> <p>We present far-<span class="hlt">ultraviolet</span> (FUV) spectra of the classical T Tauri star RU Lup covering the 912-1710 Å spectral range, as observed by the Hubble Space Telescope STIS and the Far <span class="hlt">Ultraviolet</span> Spectroscopic Explorer satellite. We use these spectra, which are rich in emission and absorption lines, to probe both the accreting and outflowing gas. Absorption in the Lyα profile constrains the extinction to AV~0.07 mag, which we confirm with other diagnostics. We estimate a mass accretion rate of (5+/-2)×10-8 Msolar yr-1 using the optical-NUV accretion continuum. The accreting gas is also detected in <span class="hlt">bright</span>, broad lines of C IV, Si IV, and N V, which all show complex structures across the line profile. Many other emission lines, including those of H2 and Fe II, are pumped by Lyα. RU Lup's spectrum varies significantly in the FUV; our STIS observations occurred when RU Lup was brighter than several other observations in the FUV, possibly because of a high mass accretion rate.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016SPD....47.0203M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016SPD....47.0203M"><span>Differential Rotation via Tracking of Coronal <span class="hlt">Bright</span> Points.</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>McAteer, James; Boucheron, Laura E.; Osorno, Marcy</p> <p>2016-05-01</p> <p>The accurate computation of solar differential rotation is important both as a constraint for, and evidence towards, support of models of the solar dynamo. As such, the use of Xray and Extreme <span class="hlt">Ultraviolet</span> <span class="hlt">bright</span> points to elucidate differential rotation has been studied in recent years. In this work, we propose the automated detection and tracking of coronal <span class="hlt">bright</span> points (CBPs) in a large set of SDO data for re-evaluation of solar differential rotation and comparison to other results. The big data aspects, and high cadence, of SDO data mitigate a few issues common to detection and tracking of objects in image sequences and allow us to focus on the use of CBPs to determine differential rotation. The high cadence of the data allows to disambiguate individual CBPs between subsequent images by allowing for significant spatial overlap, i.e., by the fact that the CBPs will rotate a short distance relative to their size. The significant spatial overlap minimizes the effects of incorrectly detected CBPs by reducing the occurrence of outlier values of differential rotation. The big data aspects of the data allows to be more conservative in our detection of CBPs (i.e., to err on the side of missing CBPs rather than detecting extraneous CBPs) while still maintaining statistically larger populations over which to study characteristics. The ability to compute solar differential rotation through the automated detection and tracking of a large population of CBPs will allow for further analyses such as the N-S asymmetry of differential rotation, variation of differential rotation over the solar cycle, and a detailed study of the magnetic flux underlying the CBPs.</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_3");'>3</a></li> <li><a href="#" onclick='return showDiv("page_4");'>4</a></li> <li class="active"><span>5</span></li> <li><a href="#" onclick='return showDiv("page_6");'>6</a></li> <li><a href="#" onclick='return showDiv("page_7");'>7</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_5 --> <div id="page_6" 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_4");'>4</a></li> <li><a href="#" onclick='return showDiv("page_5");'>5</a></li> <li class="active"><span>6</span></li> <li><a href="#" onclick='return showDiv("page_7");'>7</a></li> <li><a href="#" onclick='return showDiv("page_8");'>8</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="101"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017MNRAS.466.1061P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017MNRAS.466.1061P"><span>The calibration of read-out-streak photometry in the XMM-Newton Optical Monitor and the construction of a <span class="hlt">bright</span>-source catalogue</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Page, M. J.; Chan, N.; Breeveld, A. A.; Talavera, A.; Yershov, V.; Kennedy, T.; Kuin, N. P. M.; Hancock, B.; Smith, P. J.; Carter, M.</p> <p>2017-04-01</p> <p>The dynamic range of the XMM-Newton Optical Monitor (XMM-OM) is limited at the <span class="hlt">bright</span> end by coincidence loss, the superposition of multiple photons in the individual frames recorded from its micro-channel-plate (MCP) intensified charge-coupled device (CCD) detector. One way to overcome this limitation is to use photons that arrive during the frame transfer of the CCD, forming vertical read-out streaks for <span class="hlt">bright</span> sources. We calibrate these read-out streaks for photometry of <span class="hlt">bright</span> sources observed with XMM-OM. The <span class="hlt">bright</span>-source limit for read-out-streak photometry is set by the recharge time of the MCPs. For XMM-OM, we find that the MCP recharge time is 5.5 × 10-4 s. We determine that the effective <span class="hlt">bright</span> limits for read-out-streak photometry with XMM-OM are approximately 1.5 mag brighter than the <span class="hlt">bright</span>-source limits for normal aperture photometry in full-frame images. This translates into <span class="hlt">bright</span>-source limits in Vega magnitudes of UVW2=7.1, UVM2=8.0, UVW1=9.4, U=10.5, B=11.5, V=10.2, and White=12.5 for data taken early in the mission. The limits brighten by up to 0.2 mag, depending on filter, over the course of the mission as the detector ages. The method is demonstrated by deriving UVW1 photometry for the symbiotic nova RR Telescopii, and the new photometry is used to constrain the e-folding time of its decaying <span class="hlt">ultraviolet</span> (UV) emission. Using the read-out-streak method, we obtain photometry for 50 per cent of the missing UV source measurements in version 2.1 of the XMM-Newton Serendipitous UV Source Survey catalogue.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19850024747','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19850024747"><span>Research in extreme <span class="hlt">ultraviolet</span> and far <span class="hlt">ultraviolet</span> astronomy</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Labov, S. E.</p> <p>1985-01-01</p> <p>Instruments designed to explore different aspects of far and extreme <span class="hlt">ultraviolet</span> cosmic radiation were studied. The far <span class="hlt">ultraviolet</span> imager (FUVI) was flown on the Aries sounding rocket. Its unique large format 75mm detector mapped out the far <span class="hlt">ultraviolet</span> background radiation with a resolution of only a few arc minutes. Analysis of this data indicates to what extent the FUVI background is extra galactic in origin. A power spectrum of the spatial fluctuations will have direct consequences for galactic evolution.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19790052445&hterms=MOOS&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3DMOOS','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19790052445&hterms=MOOS&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3DMOOS"><span>Extreme <span class="hlt">ultraviolet</span> observations from Voyager 1 encounter with Jupiter</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Broadfoot, A. L.; Belton, M. J. S.; Takacs, P. Z.; Sandel, B. R.; Shemansky, D. E.; Holberg, J. B.; Ajello, J. M.; Atreya, S. K.; Donahue, T. M.; Moos, H. W.</p> <p>1979-01-01</p> <p>Observations of the optical extreme <span class="hlt">ultraviolet</span> spectrum of the Jupiter planetary system during the Voyager 1 encounter have revealed previously undetected physical processes of significant proportions. <span class="hlt">Bright</span> emission lines of S(+2), S(+3), O(+2) indicating an electron temperature of 100,000 K have been identified in preliminary analyses of the Io plasma torus spectrum. Strong auroral atomic and molecular hydrogen emissions have been observed in the polar regions of Jupiter near magnetic field lines that map the torus into the atmosphere of Jupiter. The observed resonance scattering of solar hydrogen Lyman alpha by the atmosphere of Jupiter and the solar occultation experiment suggest a hot thermosphere (greater than or equal to 1000 K) with a large atomic hydrogen abundance. A stellar occultation by Ganymede indicates that its atmosphere is at most an exosphere.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2006ApJ...642L.115H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2006ApJ...642L.115H"><span>Intrinsic <span class="hlt">Brightness</span> Temperatures of AGN Jets</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Homan, D. C.; Kovalev, Y. Y.; Lister, M. L.; Ros, E.; Kellermann, K. I.; Cohen, M. H.; Vermeulen, R. C.; Zensus, J. A.; Kadler, M.</p> <p>2006-05-01</p> <p>We present a new method for studying the intrinsic <span class="hlt">brightness</span> temperatures of the parsec-scale jet cores of active galactic nuclei (AGNs). Our method uses observed superluminal motions and observed <span class="hlt">brightness</span> temperatures for a large sample of AGNs to constrain the characteristic intrinsic <span class="hlt">brightness</span> temperature of the sample as a whole. To study changes in intrinsic <span class="hlt">brightness</span> temperature, we assume that the Doppler factors of individual jets are constant in time, as justified by their relatively small changes in observed flux density. We find that in their median-low <span class="hlt">brightness</span> temperature state, the sources in our sample have a narrow range of intrinsic <span class="hlt">brightness</span> temperatures centered on a characteristic temperature, Tint~=3×1010 K, which is close to the value expected for equipartition, when the energy in the radiating particles equals the energy stored in the magnetic fields. However, in their maximum <span class="hlt">brightness</span> state, we find that sources in our sample have a characteristic intrinsic <span class="hlt">brightness</span> temperature greater than 2×1011 K, which is well in excess of the equipartition temperature. In this state, we estimate that the energy in radiating particles exceeds the energy in the magnetic field by a factor of ~105. We suggest that the excess of particle energy when sources are in their maximum <span class="hlt">brightness</span> state is due to injection or acceleration of particles at the base of the jet. Our results suggest that the common method of estimating jet Doppler factors by using a single measurement of observed <span class="hlt">brightness</span> temperature, the assumption of equipartition, or both may lead to large scatter or systematic errors in the derived values.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018SPIE10508E..06T','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018SPIE10508E..06T"><span>Red and near-infrared fluorophores inspired by chlorophylls: consideration of practical <span class="hlt">brightness</span> in multicolor flow cytometry and biomedical sciences</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Taniguchi, Masahiko; Hu, Gongfang; Liu, Rui; Du, Hai; Lindsey, Jonathan S.</p> <p>2018-02-01</p> <p>Demands in flow cytometry for increased multiplexing (for detection of multiple antigens) and <span class="hlt">brightness</span> (for detection of rare entities) require new fluorophores (i.e., "colors") with spectrally distinct fluorescence outside the relatively congested visible spectral region. Flow cytometry fluorophores typically must function in aqueous solution upon bioconjugation and ideally should exhibit a host of photophysical features: (i) strong absorption, (ii) sizable Stokes shift, (iii) modest if not strong fluorescence, and (iv) narrow fluorescence band. Tandem dyes have long been pursued to achieve a large effective Stokes shift, increased <span class="hlt">brightness</span>, and better control over the excitation and emission wavelengths. Here, the attractive photophysical features of chlorophylls and bacteriochlorophylls - Nature's chosen photoactive pigments for photosynthesis - are described with regards to use in flow cytometry. A chlorophyll (or bacteriochlorophyll) constitutes an intrinsic tandem dye given the red (or near-infrared) fluorescence upon excitation in the higher energy <span class="hlt">ultraviolet</span> (UV) or visible absorption bands (due to rapid internal conversion to the lowest energy state). Synthetic (bacterio)chlorins are available with strong absorption (near-UV molar absorption coefficient ɛ(λexc) 105 M-1cm-1), modest fluorescence quantum yield (Φf = 0.05-0.30), and narrow fluorescence band (10-25 nm) tunable from 600-900 nm depending on synthetic design. The "relative practical <span class="hlt">brightness</span>" is given by intrinsic <span class="hlt">brightness</span> [ɛ(λexc) x Φf] times ηf, the fraction of the fluorescence band that is captured by an emission filter in a multicolor experiment. The spectroscopic features of (bacterio)chlorins are evaluated quantitatively to illustrate practical <span class="hlt">brightness</span> for this novel class of fluorophores in a prospective 8-color panel.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017ApJ...847...37C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017ApJ...847...37C"><span>Do Low Surface <span class="hlt">Brightness</span> Galaxies Host Stellar Bars?</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Cervantes Sodi, Bernardo; Sánchez García, Osbaldo</p> <p>2017-09-01</p> <p>With the aim of assessing if low surface <span class="hlt">brightness</span> galaxies host stellar bars and by studying the dependence of the occurrence of bars as a function of surface <span class="hlt">brightness</span>, we use the Galaxy Zoo 2 data set to construct a large volume-limited sample of galaxies and then segregate these galaxies as having low or high surface <span class="hlt">brightness</span> in terms of their central surface <span class="hlt">brightness</span>. We find that the fraction of low surface <span class="hlt">brightness</span> galaxies hosting strong bars is systematically lower than that found for high surface <span class="hlt">brightness</span> galaxies. The dependence of the bar fraction on the central surface <span class="hlt">brightness</span> is mostly driven by a correlation of the surface <span class="hlt">brightness</span> with the spin and the gas richness of the galaxies, showing only a minor dependence on the surface <span class="hlt">brightness</span>. We also find that the length of the bars is strongly dependent on the surface <span class="hlt">brightness</span>, and although some of this dependence is attributed to the gas content, even at a fixed gas-to-stellar mass ratio, high surface <span class="hlt">brightness</span> galaxies host longer bars than their low surface <span class="hlt">brightness</span> counterparts, which we attribute to an anticorrelation of the surface <span class="hlt">brightness</span> with the spin.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22679825-do-low-surface-brightness-galaxies-host-stellar-bars','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22679825-do-low-surface-brightness-galaxies-host-stellar-bars"><span>Do Low Surface <span class="hlt">Brightness</span> Galaxies Host Stellar Bars?</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>Cervantes Sodi, Bernardo; Sánchez García, Osbaldo, E-mail: b.cervantes@irya.unam.mx, E-mail: o.sanchez@irya.unam.mx</p> <p></p> <p>With the aim of assessing if low surface <span class="hlt">brightness</span> galaxies host stellar bars and by studying the dependence of the occurrence of bars as a function of surface <span class="hlt">brightness</span>, we use the Galaxy Zoo 2 data set to construct a large volume-limited sample of galaxies and then segregate these galaxies as having low or high surface <span class="hlt">brightness</span> in terms of their central surface <span class="hlt">brightness</span>. We find that the fraction of low surface <span class="hlt">brightness</span> galaxies hosting strong bars is systematically lower than that found for high surface <span class="hlt">brightness</span> galaxies. The dependence of the bar fraction on the central surface <span class="hlt">brightness</span> ismore » mostly driven by a correlation of the surface <span class="hlt">brightness</span> with the spin and the gas richness of the galaxies, showing only a minor dependence on the surface <span class="hlt">brightness</span>. We also find that the length of the bars is strongly dependent on the surface <span class="hlt">brightness</span>, and although some of this dependence is attributed to the gas content, even at a fixed gas-to-stellar mass ratio, high surface <span class="hlt">brightness</span> galaxies host longer bars than their low surface <span class="hlt">brightness</span> counterparts, which we attribute to an anticorrelation of the surface <span class="hlt">brightness</span> with the spin.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2000hpdl.conf..225B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2000hpdl.conf..225B"><span>Properties and Frequency Conversion of High-<span class="hlt">Brightness</span> Diode-Laser Systems</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Boller, Klaus-Jochen; Beier, Bernard; Wallenstein, Richard</p> <p></p> <p>An overview of recent developments in the field of high-power, high-<span class="hlt">brightness</span> diode-lasers, and the optically nonlinear conversion of their output into other wavelength ranges, is given. We describe the generation of continuous-wave (CW) laser beams at power levels of several hundreds of milliwatts to several watts with near-perfect spatial and spectral properties using Master-Oscillator Power-Amplifier (MOPA) systems. With single- or double-stage systems, using amplifiers of tapered or rectangular geometry, up to 2.85 W high-<span class="hlt">brightness</span> radiation is generated at wavelengths around 810nm with AlGaAs diodes. Even higher powers, up to 5.2W of single-frequency and high spatial quality beams at 925nm, are obtained with InGaAs diodes. We describe the basic properties of the oscillators and amplifiers used. A strict proof-of-quality for the diode radiation is provided by direct and efficient nonlinear optical conversion of the diode MOPA output into other wavelength ranges. We review recent experiments with the highest power levels obtained so far by direct frequency doubling of diode radiation. In these experiments, 100mW single-frequency <span class="hlt">ultraviolet</span> light at 403nm was generated, as well as 1W of single-frequency blue radiation at 465nm. Nonlinear conversion of diode radiation into widely tunable infrared radiation has recently yielded record values. We review the efficient generation of widely tunable single-frequency radiation in the infrared with diode-pumped Optical Parametric Oscillators (OPOs). With this system, single-frequency output radiation with powers of more than 0.5W was generated, widely tunable around wavelengths of <!- MATH 2.1 mu mathrm{m} -> 2.1,m and <!- MATH 1.65 mu mathrm{m} -> 1.65,m and with excellent spectral and spatial quality. These developments are clear indicators of recent advances in the field of high-<span class="hlt">brightness</span> diode-MOPA systems, and may emphasize their future central importance for applications within a vast range of optical</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA21914.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA21914.html"><span>Map of Ceres' <span class="hlt">Bright</span> Spots</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2017-12-12</p> <p>This map from NASA's Dawn mission shows locations of <span class="hlt">bright</span> material on dwarf planet Ceres. There are more than 300 <span class="hlt">bright</span> areas, called "faculae," on Ceres. Scientists have divided them into four categories: <span class="hlt">bright</span> areas on the floors of crater (red), on the rims or walls of craters (green), in the ejecta blankets of craters (blue), and on the flanks of the mountain Ahuna Mons (yellow). https://photojournal.jpl.nasa.gov/catalog/PIA21914</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19850041298&hterms=usher&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dusher','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19850041298&hterms=usher&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dusher"><span>A medium-<span class="hlt">bright</span> quasar sample - New quasar surface densities in the magnitude range from 16.4 to 17.65 for B</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Mitchell, K. J.; Warnock, A., III; Usher, P. D.</p> <p>1984-01-01</p> <p>A new medium-<span class="hlt">bright</span> quasar sample (MBQS) is constructed from spectroscopic observations of 140 <span class="hlt">bright</span> objects selected for varying degrees of blue and <span class="hlt">ultraviolet</span> excess (B-UVX) in five Palomar 1.2 m Schmidt fields. The MBQS contains 32 quasars with B less than 17.65 mag. The new integral surface densities in the B range from 16.45 to 17.65 mag are approximately 40 percent (or more) higher than expected. The MBQS and its redshift distribution increase the area of the Hubble diagram covered by complete samples of quasars. The general spectroscopic results indicate that the three-color classification process used to catalog the spectroscopic candidates (1) has efficiently separated the intrinsically B-UVX stellar objects from the Population II subdwarfs and (2) has produced samples of B-UVX objects which are more complete than samples selected by (U - B) color alone.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA18300.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA18300.html"><span>Little <span class="hlt">Bright</span> Spot</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2015-01-12</p> <p>A <span class="hlt">bright</span> spot can be seen on the left side of Rhea in this image. The spot is the crater Inktomi, named for a Lakota spider spirit. Inktomi is believed to be the youngest feature on Rhea (949 miles or 1527 kilometers across). The relative youth of the feature is evident by its <span class="hlt">brightness</span>. Material that is newly excavated from below the moon's surface and tossed across the surface by a cratering event, appears <span class="hlt">bright</span>. But as the newly exposed surface is subjected to the harsh space environment, it darkens. This is one technique scientists use to date features on surfaces. This view looks toward the trailing hemisphere of Rhea. North on Rhea is up and rotated 21 degrees to the left. The image was taken in visible light with the Cassini spacecraft narrow-angle camera on July 29, 2013. The view was obtained at a distance of approximately 1.0 million miles (1.6 million kilometers) fro http://photojournal.jpl.nasa.gov/catalog/PIA18300</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19870037740&hterms=mass+wasting&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D80%26Ntt%3Dmass%2Bwasting','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19870037740&hterms=mass+wasting&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D80%26Ntt%3Dmass%2Bwasting"><span>Lunar and Venusian radar <span class="hlt">bright</span> rings</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Thompson, T. W.; Saunders, R. S.; Weissman, D. E.</p> <p>1986-01-01</p> <p>Twenty-one lunar craters have radar <span class="hlt">bright</span> ring appearances which are analogous to eleven complete ring features in the earth-based 12.5 cm observations of Venus. Radar ring diameters and widths for the lunar and Venusian features overlap for sizes from 45 to 100 km. Radar <span class="hlt">bright</span> areas for the lunar craters are associated with the slopes of the inner and outer rim walls, while level crater floors and level ejecta fields beyond the raised portion of the rim have average radar backscatter. It is proposed that the radar <span class="hlt">bright</span> areas of the Venusian rings are also associated with the slopes on the rims of craters. The lunar craters have evolved to radar <span class="hlt">bright</span> rings via mass wasting of crater rim walls and via post-impact flooding of crater floors. Aeolian deposits of fine-grained material on Venusian crater floors may produce radar scattering effects similar to lunar crater floor flooding. These Venusian aeolian deposits may preferentially cover blocky crater floors producing a radar <span class="hlt">bright</span> ring appearance. It is proposed that the Venusian features with complete <span class="hlt">bright</span> ring appearances and sizes less than 100 km are impact craters. They have the same sizes as lunar craters and could have evolved to radar <span class="hlt">bright</span> rings via analogous surface processes.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24353623','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24353623"><span>Psoralen-<span class="hlt">ultraviolet</span> A treatment with Psoralen-<span class="hlt">ultraviolet</span> B therapy in the treatment of psoriasis.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Ahmed Asim, Sadaf; Ahmed, Sitwat; Us-Sehar, Najam</p> <p>2013-05-01</p> <p>To compare the conventional psoralen-<span class="hlt">ultraviolet</span> A treatment with psoralen-<span class="hlt">ultraviolet</span> B therapy in the treatment of psoriasis. We studied 50 patients of plaque type psoriasis who were selected to receive either conventional psoralen-<span class="hlt">ultraviolet</span> A or psoralen-<span class="hlt">ultraviolet</span> B treatment. There was no significant difference between the two treatment groups in the number of patients whose skin cleared of psoriasis or the number of exposures required for clearance. Profile of side effects and disease status was also similar after three months of follow up. Psoralen-<span class="hlt">ultraviolet</span> B treatment is as effective as conventional psoralen-<span class="hlt">ultraviolet</span> A in the treatment of psoriasis. Further long term studies are needed to assess the safety of psoralen-<span class="hlt">ultraviolet</span> B.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014ApPhL.105f3303W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014ApPhL.105f3303W"><span>High performance organic integrated device with <span class="hlt">ultraviolet</span> photodetective and electroluminescent properties consisting of a charge-transfer-featured naphthalimide derivative</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wang, Hanyu; Zhou, Jie; Wang, Xu; Lu, Zhiyun; Yu, Junsheng</p> <p>2014-08-01</p> <p>A high performance organic integrated device (OID) with <span class="hlt">ultraviolet</span> photodetective and electroluminescent (EL) properties was fabricated by using a charge-transfer-featured naphthalimide derivative of 6-{3,5-bis-[9-(4-t-butylphenyl)-9H-carbazol-3-yl]-phenoxy}-2-(4-t-butylphenyl)-benzo[de]isoquinoline-1,3-dione (CzPhONI) as the active layer. The results showed that the OID had a high detectivity of 1.5 × 1011 Jones at -3 V under the UV-350 nm illumination with an intensity of 0.6 mW/cm2, and yielded an exciplex EL light emission with a maximum <span class="hlt">brightness</span> of 1437 cd/m2. Based on the energy band diagram, both the charge transfer feature of CzPhONI and matched energy level alignment were responsible for the dual <span class="hlt">ultraviolet</span> photodetective and EL functions of OID.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3809278','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3809278"><span>Psoralen-<span class="hlt">ultraviolet</span> A treatment with Psoralen-<span class="hlt">ultraviolet</span> B therapy in the treatment of psoriasis</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Ahmed Asim, Sadaf; Ahmed, Sitwat; us-Sehar, Najam</p> <p>2013-01-01</p> <p>Objective: To compare the conventional psoralen-<span class="hlt">ultraviolet</span> A treatment with psoralen-<span class="hlt">ultraviolet</span> B therapy in the treatment of psoriasis. Methodology: We studied 50 patients of plaque type psoriasis who were selected to receive either conventional psoralen-<span class="hlt">ultraviolet</span> A or psoralen-<span class="hlt">ultraviolet</span> B treatment. Results: There was no significant difference between the two treatment groups in the number of patients whose skin cleared of psoriasis or the number of exposures required for clearance. Profile of side effects and disease status was also similar after three months of follow up. Conclusion: Psoralen-<span class="hlt">ultraviolet</span> B treatment is as effective as conventional psoralen-<span class="hlt">ultraviolet</span> A in the treatment of psoriasis. Further long term studies are needed to assess the safety of psoralen-<span class="hlt">ultraviolet</span> B. PMID:24353623</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012DPS....4421507G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012DPS....4421507G"><span>Performance Results from In-Flight Commissioning of the Juno <span class="hlt">Ultraviolet</span> Spectrograph (Juno-UVS)</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Greathouse, Thomas K.; Gladstone, G. R.; Davis, M. W.; Slater, D. C.; Versteeg, M. H.; Persson, K. B.; Winters, G. S.; Persyn, S. C.; Eterno, J. S.</p> <p>2012-10-01</p> <p>We present a description of the Juno <span class="hlt">ultraviolet</span> spectrograph (Juno-UVS), results from the successful in-flight commissioning performed between December 5th and 13th 2011, and some predictions of future Jupiter observations. Juno-UVS is a modest power (9.0 W) <span class="hlt">ultraviolet</span> spectrograph based on the Alice instruments now in flight aboard the European Space Agency’s Rosetta spacecraft, NASA’s New Horizons spacecraft, and the LAMP instrument aboard NASA’s Lunar Reconnaissance Orbiter. However, unlike the other Alice spectrographs, Juno-UVS sits aboard a rotationally stabilized spacecraft. The planned 2 rpm rotation rate for the primary mission results in integration times per spatial resolution element per spin of only 17 ms. Thus, data was retrieved from many spins and then remapped and co-added to build up integration times on <span class="hlt">bright</span> stars to measure the effective area, spatial resolution, map out scan mirror pointing positions, etc. The Juno-UVS scan mirror allows for pointing of the slit approximately ±30° from the spacecraft spin plane. This ability gives Juno-UVS access to half the sky at any given spacecraft orientation. We will describe our process for solving for the pointing of the scan mirror relative to the Juno spacecraft and present our initial half sky survey of UV <span class="hlt">bright</span> stars complete with constellation overlays. The primary job of Juno-UVS will be to characterize Jupiter’s UV auroral emissions and relate them to in situ particle measurements. The ability to point the slit will facilitate these measurements, allowing Juno-UVS to observe the surface positions of magnetic field lines Juno is flying through giving a direct connection between the particle measurements on the spacecraft to the observed reaction of Jupiter’s atmosphere to those particles. Finally, we will describe planned observations to be made during Earth flyby in October 2013 that will complete the in-flight characterization.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/18653259','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/18653259"><span><span class="hlt">Bright</span>Stat.com: free statistics online.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Stricker, Daniel</p> <p>2008-10-01</p> <p>Powerful software for statistical analysis is expensive. Here I present <span class="hlt">Bright</span>Stat, a statistical software running on the Internet which is free of charge. <span class="hlt">Bright</span>Stat's goals, its main capabilities and functionalities are outlined. Three different sample runs, a Friedman test, a chi-square test, and a step-wise multiple regression are presented. The results obtained by <span class="hlt">Bright</span>Stat are compared with results computed by SPSS, one of the global leader in providing statistical software, and VassarStats, a collection of scripts for data analysis running on the Internet. Elementary statistics is an inherent part of academic education and <span class="hlt">Bright</span>Stat is an alternative to commercial products.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/21044607','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/21044607"><span>Characterization of <span class="hlt">brightness</span> and stoichiometry of <span class="hlt">bright</span> particles by flow-fluorescence fluctuation spectroscopy.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Johnson, Jolene; Chen, Yan; Mueller, Joachim D</p> <p>2010-11-03</p> <p>Characterization of <span class="hlt">bright</span> particles at low concentrations by fluorescence fluctuation spectroscopy (FFS) is challenging, because the event rate of particle detection is low and fluorescence background contributes significantly to the measured signal. It is straightforward to increase the event rate by flow, but the high background continues to be problematic for fluorescence correlation spectroscopy. Here, we characterize the use of photon-counting histogram analysis in the presence of flow. We demonstrate that a photon-counting histogram efficiently separates the particle signal from the background and faithfully determines the <span class="hlt">brightness</span> and concentration of particles independent of flow speed, as long as undersampling is avoided. <span class="hlt">Brightness</span> provides a measure of the number of fluorescently labeled proteins within a complex and has been used to determine stoichiometry of protein complexes in vivo and in vitro. We apply flow-FFS to determine the stoichiometry of the group specific antigen protein within viral-like particles of the human immunodeficiency virus type-1 from the <span class="hlt">brightness</span>. Our results demonstrate that flow-FFS is a sensitive method for the characterization of complex macromolecular particles at low concentrations. Copyright © 2010 Biophysical Society. Published by Elsevier Inc. All rights reserved.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2001JChPh.114.7424H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2001JChPh.114.7424H"><span>The infrared-<span class="hlt">ultraviolet</span> dispersed fluorescence spectrum of acetylene: New classes of <span class="hlt">bright</span> states</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hoshina, Kennosuke; Iwasaki, Atsushi; Yamanouchi, Kaoru; Jacobson, Matthew P.; Field, Robert W.</p> <p>2001-05-01</p> <p>Single rotational levels of ungerade vibrational levels, 2ν3'+ν6' and 3ν3'+ν6' (both with bu symmetry), in the à 1Au electronically excited state of acetylene were excited by an IR-UV double resonance scheme via the ν3″ fundamental level in the X˜ 1Σg+ state, and the rotationally resolved dispersed fluorescence (DF) spectra were recorded at 3.2-4.5 cm-1 resolution. The term values of the new ungerade levels were determined within an accuracy of 0.56 cm-1(1σ) through careful calibration achieved by frequency standard atomic Fe and Hg lines. A total of 111 new ungerade vibrational levels with Σu+, Σu-, and Δu symmetry below 10 000 cm-1 was identified in the high-resolution IR-UV-DF spectra, which provide access to new classes of X˜ 1Σg+ <span class="hlt">bright</span> states: (i) (0,v2″,0,v4″1,1-1)Σu+, (0,v2″,0,v4″1,11)Δu, and (0,v2″,0,v4″3,1-1)Δu, which are the Franck-Condon (FC) <span class="hlt">bright</span> levels from the nν3'+ν6' (n=2,3) levels in the à 1Au state; (ii) (0,v2″,0,v4″-1,11)Σu- levels which appear through the a-axis Corioris interaction between nν3'+ν6' and nν3'+ν4' (n=2,3) in the à 1Au state; and (iii) (0,v2″,1,v4″0,0)Σu+ and (0,v2″,1,v4″2,0)Δu levels which gain transition intensity from the Duschinsky effect associated with the bent-linear ÖX˜ transition. All observed ungerade term values and previously determined gerade and ungerade term values below 10 000 cm-1 were fitted by two effective model Hamiltonians, i.e., a pure-bend effective Hamiltonian and a stretch-bend effective Hamiltonian. The stretch-bend effective Hamiltonian is expressed in terms of 31 Dunham expansion parameters and 11 anharmonic resonance parameters associated with (i) five stretch-bend anharmonic resonances; (ii) one stretch-stretch and two bend-bend Darling-Dennison resonances; and (iii) one vibrational l resonance. The parameters in this Hamiltonian were determined from a least-squares fit of 287 vibrational term values (111 new ungerade levels, 128 levels from</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA12753.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA12753.html"><span><span class="hlt">Bright</span> Enceladus</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2011-02-14</p> <p>Saturn moon Enceladus reflects sunlight <span class="hlt">brightly</span> while the planet and its rings fill the background in this view from NASA Cassini spacecraft. Enceladus is one of the most reflective bodies in the solar system.</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_4");'>4</a></li> <li><a href="#" onclick='return showDiv("page_5");'>5</a></li> <li class="active"><span>6</span></li> <li><a href="#" onclick='return showDiv("page_7");'>7</a></li> <li><a href="#" onclick='return showDiv("page_8");'>8</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_6 --> <div id="page_7" 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_5");'>5</a></li> <li><a href="#" onclick='return showDiv("page_6");'>6</a></li> <li class="active"><span>7</span></li> <li><a href="#" onclick='return showDiv("page_8");'>8</a></li> <li><a href="#" onclick='return showDiv("page_9");'>9</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="121"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016DPS....4850103S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016DPS....4850103S"><span>Formation of a <span class="hlt">Bright</span> Polar Hood over the Summer North Pole of Saturn 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>Sayanagi, Kunio M.; Blalock, John J.; Ingersoll, Andrew P.; Dyudina, Ulyana A.; Ewald, Shawn P.</p> <p>2016-10-01</p> <p>We report that a <span class="hlt">bright</span> polar hood has formed over the north pole of Saturn, seen first in images captured by the Cassini ISS camera in 2016. When the north pole was observed during the previous period of Cassini spacecraft's high-inclination orbits in 2012-2013, the concentration of light-scattering aerosols within 2-degree latitude of the north pole appeared to be less than that of the surrounding region, and appeared as a dark hole in all ISS filters, in particular in the shorter wavelength filters BL1 (460 nm), and VIO (420 nm). The north pole's appearance in 2012 was in contrast to that of the south pole in 2007, when the south pole had a <span class="hlt">bright</span> polar hood in those short wavelengths; the south pole appeared dark in all other ISS filters in 2007. The difference between the south pole in 2007 and the north pole in 2012 was interpreted to be seasonal; in 2007, Saturn was approaching the equinox of 2009 and the south pole had been continuously illuminated since the previous equinox in 1995. In 2012, the north pole had been illuminated for only ~3 years after the long winter polar night. The <span class="hlt">bright</span> hood over the summer south pole in 2007 was hypothesized to consist of aerosols produced by <span class="hlt">ultraviolet</span> photodissociation of hydrocarbon molecules. Fletcher et al (2015) predicted that a similar <span class="hlt">bright</span> hood should form over the north pole as Saturn approaches the 2017 solstice. In 2016, the Cassini spacecraft raised its orbital inclination again in preparation for its Grande Finale phase of the mission, from where it has a good view of the north pole. New images captured in 2016 show that the north pole has developed a <span class="hlt">bright</span> polar hood. We present new images of the north polar region captured in 2016 that show the north pole, and other seasonally evolving high-latitude features including the northern hexagon. Our research has been supported by the Cassini Project, NASA grants OPR NNX11AM45G, CDAPS NNX15AD33G PATM NNX14AK07G, and NSF grant AAG 1212216.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2008cosp...37.3090S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2008cosp...37.3090S"><span>Calculation of gyrosynchrotron radiation <span class="hlt">brightness</span> temperature for outer <span class="hlt">bright</span> loop of ICME</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sun, Weiying; Wu, Ji; Wang, C. B.; Wang, S.</p> <p></p> <p>:Solar polar orbit radio telescope (SPORT) is proposed to detect the high density plasma clouds of outer <span class="hlt">bright</span> loop of ICMEs from solar orbit with large inclination. Of particular interest is following the propagation of the plasma clouds with remote sensor in radio wavelength band. Gyrosynchrotron emission is a main radio radiation mechanism of the plasma clouds and can provide information of interplanetary magnetic field. In this paper, we statistically analyze the electron density, electron temperature and magnetic field of background solar wind in time of quiet sun and ICMEs propagation. We also estimate the fluctuation range of the electron density, electron temperature and magnetic field of outer <span class="hlt">bright</span> loop of ICMEs. Moreover, we calculate and analyze the emission <span class="hlt">brightness</span> temperature and degree of polarization on the basis of the study of gyrosynchrotron emission, absorption and polarization characteristics as the optical depth is less than or equal to 1.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19920045069&hterms=911&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3D911','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19920045069&hterms=911&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3D911"><span>The spectrum of the tropical oxygen nightglow observed at 3 A resolution with the Hopkins <span class="hlt">Ultraviolet</span> Telescope</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.; Davidsen, A. F.; Blair, W. P.; Bowers, C. W.; Durrance, S. T.; Kriss, G. A.; Ferguson, H. C.; Kimble, R. A.; Long, K. S.</p> <p>1992-01-01</p> <p><span class="hlt">Ultraviolet</span> spectra of the tropical oxygen nightglow in the range of 830 to 1850 A (in first order) at 3 A resolution were obtained with the Hopkins <span class="hlt">Ultraviolet</span> Telescope in December 1990. The data are presented which were obtained on a setting celestial target as the zenith angle of the line-of-sight varied from 77 to 95 deg. The dominant features in the spectrum (other than geocoronal hydrogen) are O I 1304 and 1356 and the radiative recombination continuum near 911 A. The continuum is resolved and found to be consistent with an electron temperature in the range 1000-1250 K. The observed ratio of the <span class="hlt">brightness</span> of O I 1356 to the continuum suggests that O(+)-O(-) mutual neutralization contributes about 40 percent to the 1356 A emission. The dependence of the optically thin emissions on zenith angle is consistent with a simple ionospheric model. Weak O I 989 emission is also detected, but there is no evidence for any similarly produced atomic nitrogen emissions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/23798032','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/23798032"><span><span class="hlt">Brightness</span> and transparency in the early visual cortex.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Salmela, Viljami R; Vanni, Simo</p> <p>2013-06-24</p> <p>Several psychophysical studies have shown that transparency can have drastic effects on <span class="hlt">brightness</span> and lightness. However, the neural processes generating these effects have remained unresolved. Several lines of evidence suggest that the early visual cortex is important for <span class="hlt">brightness</span> perception. While single cell recordings suggest that surface <span class="hlt">brightness</span> is represented in the primary visual cortex, the results of functional magnetic resonance imaging (fMRI) studies have been discrepant. In addition, the location of the neural representation of transparency is not yet known. We investigated whether the fMRI responses in areas V1, V2, and V3 correlate with <span class="hlt">brightness</span> and transparency. To dissociate the blood oxygen level-dependent (BOLD) response to <span class="hlt">brightness</span> from the response to local border contrast and mean luminance, we used variants of White's <span class="hlt">brightness</span> illusion, both opaque and transparent, in which luminance increments and decrements cancel each other out. The stimuli consisted of a target surface and a surround. The surround luminance was always sinusoidally modulated at 0.5 Hz to induce <span class="hlt">brightness</span> modulation to the target. The target luminance was constant or modulated in counterphase to null <span class="hlt">brightness</span> modulation. The mean signal changes were calculated from the voxels in V1, V2, and V3 corresponding to the retinotopic location of the target surface. The BOLD responses were significantly stronger for modulating <span class="hlt">brightness</span> than for stimuli with constant <span class="hlt">brightness</span>. In addition, the responses were stronger for transparent than for opaque stimuli, but there was more individual variation. No interaction between <span class="hlt">brightness</span> and transparency was found. The results show that the early visual areas V1-V3 are sensitive to surface <span class="hlt">brightness</span> and transparency and suggest that <span class="hlt">brightness</span> and transparency are represented separately.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016SPIE.9730E..0CH','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016SPIE.9730E..0CH"><span>Teradiode's high <span class="hlt">brightness</span> semiconductor lasers</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Huang, Robin K.; Chann, Bien; Burgess, James; Lochman, Bryan; Zhou, Wang; Cruz, Mike; Cook, Rob; Dugmore, Dan; Shattuck, Jeff; Tayebati, Parviz</p> <p>2016-03-01</p> <p>TeraDiode is manufacturing multi-kW-class ultra-high <span class="hlt">brightness</span> fiber-coupled direct diode lasers for industrial applications. A fiber-coupled direct diode laser with a power level of 4,680 W from a 100 μm core diameter, <0.08 numerical aperture (NA) output fiber at a single center wavelength was demonstrated. Our TeraBlade industrial platform achieves world-record <span class="hlt">brightness</span> levels for direct diode lasers. The fiber-coupled output corresponds to a Beam Parameter Product (BPP) of 3.5 mm-mrad and is the lowest BPP multi-kW-class direct diode laser yet reported. This laser is suitable for industrial materials processing applications, including sheet metal cutting and welding. This 4-kW fiber-coupled direct diode laser has comparable <span class="hlt">brightness</span> to that of industrial fiber lasers and CO2 lasers, and is over 10x brighter than state-of-the-art direct diode lasers. We have also demonstrated novel high peak power lasers and high <span class="hlt">brightness</span> Mid-Infrared Lasers.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24323112','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24323112"><span><span class="hlt">Brightness</span> perception of unrelated self-luminous colors.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Withouck, Martijn; Smet, Kevin A G; Ryckaert, Wouter R; Pointer, Michael R; Deconinck, Geert; Koenderink, Jan; Hanselaer, Peter</p> <p>2013-06-01</p> <p>The perception of <span class="hlt">brightness</span> of unrelated self-luminous colored stimuli of the same luminance has been investigated. The Helmholtz-Kohlrausch (H-K) effect, i.e., an increase in <span class="hlt">brightness</span> perception due to an increase in saturation, is clearly observed. This <span class="hlt">brightness</span> perception is compared with the calculated <span class="hlt">brightness</span> according to six existing vision models, color appearance models, and models based on the concept of equivalent luminance. Although these models included the H-K effect and half of them were developed to work with unrelated colors, none of the models seemed to be able to fully predict the perceived <span class="hlt">brightness</span>. A tentative solution to increase the prediction accuracy of the color appearance model CAM97u, developed by Hunt, is presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA21398.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA21398.html"><span>Occator <span class="hlt">Bright</span> Spots in 3-D</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2017-03-09</p> <p>This 3-D image, or anaglyph, shows the center of Occator Crater, the brightest area on dwarf planet Ceres, using data from NASA's Dawn mission. The <span class="hlt">bright</span> central area, including a dome that is 0.25 miles (400 meters) high, is called Cerealia Facula. The secondary, scattered <span class="hlt">bright</span> areas are called Vinalia Faculae. A 2017 study suggests that the central <span class="hlt">bright</span> area is significantly younger than Occator Crater. Estimates put Cerealia Facula at 4 million years old, while Occator Crater is approximately 34 million years old. The reflective material that appears so <span class="hlt">bright</span> in this image is made of carbonate salts, according to Dawn researchers. The Vinalia Faculae seem to be composed of carbonates mixed with dark material. http://photojournal.jpl.nasa.gov/catalog/PIA21398</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018PhRvS..21c2802T','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018PhRvS..21c2802T"><span>Time-resolved <span class="hlt">brightness</span> measurements by streaking</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Torrance, Joshua S.; Speirs, Rory W.; McCulloch, Andrew J.; Scholten, Robert E.</p> <p>2018-03-01</p> <p><span class="hlt">Brightness</span> is a key figure of merit for charged particle beams, and time-resolved <span class="hlt">brightness</span> measurements can elucidate the processes involved in beam creation and manipulation. Here we report on a simple, robust, and widely applicable method for the measurement of beam <span class="hlt">brightness</span> with temporal resolution by streaking one-dimensional pepperpots, and demonstrate the technique to characterize electron bunches produced from a cold-atom electron source. We demonstrate <span class="hlt">brightness</span> measurements with 145 ps temporal resolution and a minimum resolvable emittance of 40 nm rad. This technique provides an efficient method of exploring source parameters and will prove useful for examining the efficacy of techniques to counter space-charge expansion, a critical hurdle to achieving single-shot imaging of atomic scale targets.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017PhDT........48F','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017PhDT........48F"><span><span class="hlt">Bright</span> Linearly and Circularly Polarized Extreme <span class="hlt">Ultraviolet</span> and Soft X-ray High Harmonics for Absorption Spectroscopy</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Fan, Tingting</p> <p></p> <p>High harmonic generation (HHG) is an extreme nonlinear optical process. When implemented in a phase-matched geometry, HHG coherent upconverts femtosecond laser light into coherent "X-ray laser" beams, while retaining excellent spatial and temporal coherence, as well as the polarization state of the driving laser. HHG has a tabletop footprint, with femtosecond to attosecond time resolution, combined with nanometer spatial resolution. As a consequence of these unique capabilities, HHG is now being widely adopted for use in molecular spectroscopy and imaging, materials science, as well as nanoimaging in general. In the first half of this thesis, I demonstrate high flux linearly polarized soft X-ray HHG, driven by a single-stage 10-mJ Ti:sapphire regenerative amplifier at a repetition rate of 1 kHz. I first down-converted the laser to 1.3 mum using an optical parametric amplifier, before up-converting it into the soft X-ray region using HHG in a high-pressure, phase-matched, hollow waveguide geometry. The resulting optimally phase-matched broadband spectrum extends to 200 eV, with a soft X-ray photon flux of > 106 photons/pulse/1% bandwidth at 1 kHz, corresponding to > 109 photons/s/1% bandwidth, or approximately a three orders-of-magnitude increase compared with past work. Using this broad bandwidth X-ray source, I demonstrated X-ray absorption spectroscopy of multiple elements and transitions in molecules in a single spectrum, with a spectral resolution of 0.25 eV, and with the ability to resolve the near edge fine structure. In the second half of this thesis, I discuss how to generate the first <span class="hlt">bright</span> circularly polarized (CP) soft X-ray HHG and also use them to implement the first tabletop X-ray magnetic circular dichroism (XMCD) measurements. Using counter-rotating CP lasers at 1.3 mum and 0.79 mum, I generated CPHHG with photon energies exceeding 160 eV. The harmonic spectra emerge as a sequence of closely spaced pairs of left and right CP peaks, with energies</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1986SPIE..601..140H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1986SPIE..601..140H"><span>Calculating Solar <span class="hlt">Ultraviolet</span> Irradiation Of The Human Cornea And Corresponding Required Sunglass Lens Transmittances</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hoover, Herbert L.; Marsaud, Serge G.</p> <p>1986-05-01</p> <p>Tinted ophthalmic lenses are used primarily for eye comfort in a <span class="hlt">brightly</span> lit environment. An ancillary benefit is the attenuation of <span class="hlt">ultraviolet</span> radiation. Some national product standards specify quantitative limits for <span class="hlt">ultraviolet</span> transmittances. Such limits ought to be founded on quantitative estimates of solar irradiances of ocular tissues, with actinic effectiveness taken into account. We use the equations of Green and coworkers for direct and diffuse solar irradiance at the earth's surface to calculate average sky and ground spectral radiances. We use the geometric factors derived by us for the coupling of radiation from these sources to the human cornea. Actinically weighted corneal spectral irradiances integrated over wavelength and time yield peak irradiances and accumulated exposure doses that are compared with recommended exposure limits. This provides the maximal effective <span class="hlt">ultraviolet</span> transmittances of tinted ophthalmic lenses such that these exposure limits will not be exceeded in the selected exposure environment. The influences on corneal irradiation of such exposure parameters as solar zenith angle, altitude of the exposure site, characteristics of atmospheric aerosols, and ground reflectances are illustrated. The relationships between the effective transmittance (which is a function of the environmental radiation and any actinicweighting function) and readily determined characteristics of the lens itself, viz., its mean transmittance, and a selected spectral transmittance, are derived for three lens transmittance curves. Limits of lens transmittance for the UV-B and UV-A wavelength regions are presented for several representative exposure sites in Europe and the U.S.A.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1304828-characterizing-mid-ultraviolet-optical-light-curves-nearby-type-iin-supernovae','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1304828-characterizing-mid-ultraviolet-optical-light-curves-nearby-type-iin-supernovae"><span>Characterizing mid-<span class="hlt">ultraviolet</span> to optical light curves of nearby type IIn supernovae</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>de la Rosa, Janie; Roming, Pete; Pritchard, Tyler; ...</p> <p>2016-03-21</p> <p>Here, we present early mid-<span class="hlt">ultraviolet</span> and optical observations of Type IIn supernovae (SNe IIn) observed from 2007 to 2013. Our results focus on the properties of UV light curves: peak absolute magnitudes, temporal decay, and color evolution. During early times, this sample demonstrates that UV light decays faster than optical, and each event transitions from a predominantly UV-<span class="hlt">bright</span> phase to an optically <span class="hlt">bright</span> phase. In order to understand early UV behavior, we generate and analyze the sample's blackbody luminosity, temperature, and radius as the SN ejecta expand and cool. Since most of our observations were detected post maximum luminosity, wemore » introduce a method for estimating the date of peak magnitude. When our observations are compared based on filter, we find that even though these SNe IIn vary in peak magnitudes, there are similarities in UV decay rates. We use a simple semi-analytical SN model in order to understand the effects of the explosion environment on our UV observations. Understanding the UV characteristics of nearby SNe IIn during an early phase can provide valuable information about the environment surrounding these explosions, leading us to evaluating the diversity of observational properties in this subclass.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018PhRvB..97o5403Y','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018PhRvB..97o5403Y"><span>Electromagnetically induced transparency control in terahertz metasurfaces based on <span class="hlt">bright-bright</span> mode coupling</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Yahiaoui, R.; Burrow, J. A.; Mekonen, S. M.; Sarangan, A.; Mathews, J.; Agha, I.; Searles, T. A.</p> <p>2018-04-01</p> <p>We demonstrate a classical analog of electromagnetically induced transparency (EIT) in a highly flexible planar terahertz metamaterial (MM) comprised of three-gap split-ring resonators. The keys to achieve EIT in this system are the frequency detuning and hybridization processes between two <span class="hlt">bright</span> modes coexisting in the same unit cell as opposed to <span class="hlt">bright</span>-dark modes. We present experimental verification of two <span class="hlt">bright</span> modes coupling for a terahertz EIT-MM in the context of numerical results and theoretical analysis based on a coupled Lorentz oscillator model. In addition, a hybrid variation of the EIT-MM is proposed and implemented numerically to dynamically tune the EIT window by incorporating photosensitive silicon pads in the split gap region of the resonators. As a result, this hybrid MM enables the active optical control of a transition from the on state (EIT mode) to the off state (dipole mode).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19850011592','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19850011592"><span>Research in extreme <span class="hlt">ultraviolet</span> and far <span class="hlt">ultraviolet</span> astronomy</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Bowyer, C. S.</p> <p>1985-01-01</p> <p>The Far <span class="hlt">Ultraviolet</span> imager (FUVI) was flown on the Aries class sounding rocket 24.015, producing outstanding results. The diffuse extreme <span class="hlt">ultraviolet</span> (EUV) background spectrometer which is under construction is described. It will be launched on the Black Brant sounding rocket flight number 27.086. Ongoing design studies of a high resolution spectrometer are discussed. This instrument incorporates a one meter normal incidence mirror and will be suitable for an advanced Spartan mission.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/7001490','DOE-PATENT-XML'); return false;" href="https://www.osti.gov/biblio/7001490"><span><span class="hlt">Ultraviolet</span> absorption hygrometer</span></a></p> <p><a target="_blank" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p>Gersh, M.E.; Bien, F.; Bernstein, L.S.</p> <p>1986-12-09</p> <p>An <span class="hlt">ultraviolet</span> absorption hygrometer is provided including a source of pulsed <span class="hlt">ultraviolet</span> radiation for providing radiation in a first wavelength region where water absorbs significantly and in a second proximate wavelength region where water absorbs weakly. <span class="hlt">Ultraviolet</span> radiation in the first and second regions which has been transmitted through a sample path of atmosphere is detected. The intensity of the radiation transmitted in each of the first and second regions is compared and from this comparison the amount of water in the sample path is determined. 5 figs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19970022610','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19970022610"><span>New Observations of Subarcsecond Photospheric <span class="hlt">Bright</span> Points</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Berger, T. E.; Schrijver, C. J.; Shine, R. A.; Tarbell, T. D.; Title, A. M.; Scharmer, G.</p> <p>1995-01-01</p> <p>We have used an interference filter centered at 4305 A within the bandhead of the CH radical (the 'G band') and real-time image selection at the Swedish Vacuum Solar Telescope on La Palma to produce very high contrast images of subarcsecond photospheric <span class="hlt">bright</span> points at all locations on the solar disk. During the 6 day period of 1993 September 15-20 we observed active region NOAA 7581 from its appearance on the East limb to a near-disk-center position on September 20. A total of 1804 <span class="hlt">bright</span> points were selected for analysis from the disk center image using feature extraction image processing techniques. The measured Full Width at Half Maximum (FWHM) distribution of the <span class="hlt">bright</span> points in the image is lognormal with a modal value of 220 km (0 sec .30) and an average value of 250 km (0 sec .35). The smallest measured <span class="hlt">bright</span> point diameter is 120 km (0 sec .17) and the largest is 600 km (O sec .69). Approximately 60% of the measured <span class="hlt">bright</span> points are circular (eccentricity approx. 1.0), the average eccentricity is 1.5, and the maximum eccentricity corresponding to filigree in the image is 6.5. The peak contrast of the measured <span class="hlt">bright</span> points is normally distributed. The contrast distribution variance is much greater than the measurement accuracy, indicating a large spread in intrinsic <span class="hlt">bright</span>-point contrast. When referenced to an averaged 'quiet-Sun' area in the image, the modal contrast is 29% and the maximum value is 75%; when referenced to an average intergranular lane <span class="hlt">brightness</span> in the image, the distribution has a modal value of 61% and a maximum of 119%. The bin-averaged contrast of G-band <span class="hlt">bright</span> points is constant across the entire measured size range. The measured area of the <span class="hlt">bright</span> points, corrected for pixelation and selection effects, covers about 1.8% of the total image area. Large pores and micropores occupy an additional 2% of the image area, implying a total area fraction of magnetic proxy features in the image of 3.8%. We discuss the implications of this</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19970023731','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19970023731"><span>New Observations of Subarcsecond Photospheric <span class="hlt">Bright</span> Points</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Berger, T. E.; Schrijver, C. J.; Shine, R. A.; Tarbell, T. D.; Title, A. M.; Scharmer, G.</p> <p>1995-01-01</p> <p>We have used an interference filter centered at 4305 A within the bandhead of the CH radical (the 'G band') and real-time image selection at the Swedish Vacuum Solar Telescope on La Palma to produce very high contrast images of subarcsecond photospheric <span class="hlt">bright</span> points at all locations on the solar disk. During the 6 day period of 15-20 Sept. 1993 we observed active region NOAA 7581 from its appearance on the East limb to a near-disk-center position on 20 Sept. A total of 1804 <span class="hlt">bright</span> points were selected for analysis from the disk center image using feature extraction image processing techniques. The measured FWHM distribution of the <span class="hlt">bright</span> points in the image is lognormal with a modal value of 220 km (0.30 sec) and an average value of 250 km (0.35 sec). The smallest measured <span class="hlt">bright</span> point diameter is 120 km (0.17 sec) and the largest is 600 km (O.69 sec). Approximately 60% of the measured <span class="hlt">bright</span> points are circular (eccentricity approx. 1.0), the average eccentricity is 1.5, and the maximum eccentricity corresponding to filigree in the image is 6.5. The peak contrast of the measured <span class="hlt">bright</span> points is normally distributed. The contrast distribution variance is much greater than the measurement accuracy, indicating a large spread in intrinsic <span class="hlt">bright</span>-point contrast. When referenced to an averaged 'quiet-Sun' area in the image, the modal contrast is 29% and the maximum value is 75%; when referenced to an average intergranular lane <span class="hlt">brightness</span> in the image, the distribution has a modal value of 61% and a maximum of 119%. The bin-averaged contrast of G-band <span class="hlt">bright</span> points is constant across the entire measured size range. The measured area of the <span class="hlt">bright</span> points, corrected for pixelation and selection effects, covers about 1.8% of the total image area. Large pores and micropores occupy an additional 2% of the image area, implying a total area fraction of magnetic proxy features in the image of 3.8%. We discuss the implications of this area fraction measurement in the context of</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017A%26A...606A..46G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017A%26A...606A..46G"><span>Magnetic topological analysis of coronal <span class="hlt">bright</span> points</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Galsgaard, K.; Madjarska, M. S.; Moreno-Insertis, F.; Huang, Z.; Wiegelmann, T.</p> <p>2017-10-01</p> <p>Context. We report on the first of a series of studies on coronal <span class="hlt">bright</span> points which investigate the physical mechanism that generates these phenomena. Aims: The aim of this paper is to understand the magnetic-field structure that hosts the <span class="hlt">bright</span> points. Methods: We use longitudinal magnetograms taken by the Solar Optical Telescope with the Narrowband Filter Imager. For a single case, magnetograms from the Helioseismic and Magnetic Imager were added to the analysis. The longitudinal magnetic field component is used to derive the potential magnetic fields of the large regions around the <span class="hlt">bright</span> points. A magneto-static field extrapolation method is tested to verify the accuracy of the potential field modelling. The three dimensional magnetic fields are investigated for the presence of magnetic null points and their influence on the local magnetic domain. Results: In nine out of ten cases the <span class="hlt">bright</span> point resides in areas where the coronal magnetic field contains an opposite polarity intrusion defining a magnetic null point above it. We find that X-ray <span class="hlt">bright</span> points reside, in these nine cases, in a limited part of the projected fan-dome area, either fully inside the dome or expanding over a limited area below which typically a dominant flux concentration resides. The tenth <span class="hlt">bright</span> point is located in a bipolar loop system without an overlying null point. Conclusions: All <span class="hlt">bright</span> points in coronal holes and two out of three <span class="hlt">bright</span> points in quiet Sun regions are seen to reside in regions containing a magnetic null point. An as yet unidentified process(es) generates the brigh points in specific regions of the fan-dome structure. The movies are available at http://www.aanda.org</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22365802-larger-planet-radii-inferred-from-stellar-flicker-brightness-variations-bright-planet-host-stars','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22365802-larger-planet-radii-inferred-from-stellar-flicker-brightness-variations-bright-planet-host-stars"><span>LARGER PLANET RADII INFERRED FROM STELLAR ''FLICKER'' <span class="hlt">BRIGHTNESS</span> VARIATIONS OF <span class="hlt">BRIGHT</span> PLANET-HOST STARS</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>Bastien, Fabienne A.; Stassun, Keivan G.; Pepper, Joshua</p> <p>2014-06-10</p> <p>Most extrasolar planets have been detected by their influence on their parent star, typically either gravitationally (the Doppler method) or by the small dip in <span class="hlt">brightness</span> as the planet blocks a portion of the star (the transit method). Therefore, the accuracy with which we know the masses and radii of extrasolar planets depends directly on how well we know those of the stars, the latter usually determined from the measured stellar surface gravity, log g. Recent work has demonstrated that the short-timescale <span class="hlt">brightness</span> variations ({sup f}licker{sup )} of stars can be used to measure log g to a high accuracymore » of ∼0.1-0.2 dex. Here, we use flicker measurements of 289 <span class="hlt">bright</span> (Kepmag < 13) candidate planet-hosting stars with T {sub eff} = 4500-6650 K to re-assess the stellar parameters and determine the resulting impact on derived planet properties. This re-assessment reveals that for the brightest planet-host stars, Malmquist bias contaminates the stellar sample with evolved stars: nearly 50% of the <span class="hlt">bright</span> planet-host stars are subgiants. As a result, the stellar radii, and hence the radii of the planets orbiting these stars, are on average 20%-30% larger than previous measurements had suggested.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19780021057','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19780021057"><span>Unusual satellite data: A black hole?. [International <span class="hlt">Ultraviolet</span> Explorer observations</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>1978-01-01</p> <p>Data obtained by the NASA-launched European Space Agency's International <span class="hlt">Ultraviolet</span> Explorer satellite suggests the possibility of a massive black hole at the center of some globular clusters (star groups) in our galaxy. Six of these clusters, three of them X-ray sources, were closely examined. Onboard short wavelength UV instrumentation penetrated the background denseness of the clusters 15,000 light years away where radiation, probably from a group of 10 to 20 <span class="hlt">bright</span> blue stars orbiting the core, was observed. The stars may well be orbiting a massive black hole the size of 1,000 solar systems. The existence of the black hole is uncertain. The dynamics of the stars must be studied first to determine how they rotate in relation to the center of the million-star cluster. This may better indicate what provides the necessary gravitational pull that holds them in orbit.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2009AAS...21330108M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2009AAS...21330108M"><span>Network based sky <span class="hlt">Brightness</span> Monitor</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>McKenna, Dan; Pulvermacher, R.; Davis, D. R.</p> <p>2009-01-01</p> <p>We have developed and are currently testing an autonomous 2 channel photometer designed to measure the night sky <span class="hlt">brightness</span> in the visual wavelengths over a multi-year campaign. The photometer uses a robust silicon sensor filtered with Hoya CM500 glass. The Sky <span class="hlt">brightness</span> is measured every minute at two elevation angles typically zenith and 20 degrees to monitor <span class="hlt">brightness</span> and transparency. The Sky <span class="hlt">Brightness</span> monitor consists of two units, the remote photometer and a network interface. Currently these devices use 2.4 Ghz transceivers with a free space range of 100 meters. The remote unit is battery powered with day time recharging using a solar panel. Data received by the network interface transmits data via standard POP Email protocol. A second version is under development for radio sensitive areas using an optical fiber for data transmission. We will present the current comparison with the National Park Service sky monitoring camera. We will also discuss the calibration methods used for standardization and temperature compensation. This system is expected to be deployed in the next year and be operated by the International Dark Sky Association SKYMONITOR project.</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_5");'>5</a></li> <li><a href="#" onclick='return showDiv("page_6");'>6</a></li> <li class="active"><span>7</span></li> <li><a href="#" onclick='return showDiv("page_8");'>8</a></li> <li><a href="#" onclick='return showDiv("page_9");'>9</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_7 --> <div id="page_8" 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_6");'>6</a></li> <li><a href="#" onclick='return showDiv("page_7");'>7</a></li> <li class="active"><span>8</span></li> <li><a href="#" onclick='return showDiv("page_9");'>9</a></li> <li><a href="#" onclick='return showDiv("page_10");'>10</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="141"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24076544','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24076544"><span><span class="hlt">Bright</span> light induces choroidal thickening in chickens.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Lan, Weizhong; Feldkaemper, Marita; Schaeffel, Frank</p> <p>2013-11-01</p> <p><span class="hlt">Bright</span> light is a potent inhibitor of myopia development in animal models. Because development of refractive errors has been linked to changes in choroidal thickness, we have studied in chickens whether <span class="hlt">bright</span> light may exert its effects on myopia also through changes in choroidal thickness. Three-day-old chickens were exposed to "<span class="hlt">bright</span> light" (15,000 lux; n = 14) from 10 AM to 4 PM but kept under "normal light" (500 lux) during the remaining time of the light phase for 5 days (total duration of light phase 8 AM to 6 PM). A control group (n = 14) was kept under normal light during the entire light phase. Choroidal thickness was measured in alert, hand-held animals with optical coherence tomography at 10 AM, 4 PM, and 8 PM every day. Complete data sets were available for 12 chicks in <span class="hlt">bright</span> light group and nine in normal light group. The striking inter-individual variability in choroidal thickness (coefficient of variance: 23%) made it necessary to normalize changes to the individual baseline thickness of the choroid. During the 6 hours of exposure to <span class="hlt">bright</span> light, choroidal thickness decreased by -5.2 ± 4.0% (mean ± SEM). By contrast, in the group kept under normal light, choroidal thickness increased by +15.4 ± 4.7% (difference between both groups p = 0.003). After an additional 4 hours, choroidal thickness increased also in the "<span class="hlt">bright</span> light group" by +17.8 ± 3.5%, while there was little further change (+0.6 ± 4.0%) in the "normal light group" (difference p = 0.004). Finally, the choroid was thicker in the "<span class="hlt">bright</span> light group" (+7.6 ± 26.0%) than in the "normal light group" (day 5: -18.6 ± 26.9%; difference p = 0.036). <span class="hlt">Bright</span> light stimulates choroidal thickening in chickens, although the response is smaller than with experimentally imposed myopic defocus, and it occurs with some time delay. It nevertheless suggests that choroidal thickening is also involved in myopia inhibition by <span class="hlt">bright</span> light.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1995AJ....110..573M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1995AJ....110..573M"><span>Galaxy Selection and the Surface <span class="hlt">Brightness</span> Distribution</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>McGaugh, Stacy S.; Bothun, Gregory D.; Schombert, James M.</p> <p>1995-08-01</p> <p>Optical surveys for galaxies are biased against the inclusion of low surface <span class="hlt">brightness</span> (LSB) galaxies. Disney [Nature, 263,573(1976)] suggested that the constancy of disk central surface <span class="hlt">brightness</span> noticed by Freeman [ApJ, 160,811(1970)] was not a physical result, but instead was an artifact of sample selection. Since LSB galaxies do exist, the pertinent and still controversial issue is if these newly discovered galaxies constitute a significant percentage of the general galaxy population. In this paper, we address this issue by determining the space density of galaxies as a function of disk central surface <span class="hlt">brightness</span>. Using the physically reasonable assumption (which is motivated by the data) that central surface <span class="hlt">brightness</span> is independent of disk scale length, we arrive at a distribution which is roughly flat (i.e., approximately equal numbers of galaxies at each surface <span class="hlt">brightness</span>) faintwards of the Freeman (1970) value. Brightwards of this, we find a sharp decline in the distribution which is analogous to the turn down in the luminosity function at L^*^. An intrinsically sharply peaked "Freeman law" distribution can be completely ruled out, and no Gaussian distribution can fit the data. Low surface <span class="hlt">brightness</span> galaxies (those with central surface <span class="hlt">brightness</span> fainter than 22 B mag arcsec^-2^) comprise >~ 1/2 the general galaxy population, so a representative sample of galaxies at z = 0 does not really exist at present since past surveys have been insensitive to this component of the general galaxy population.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19920061065&hterms=MOOS&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DMOOS','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19920061065&hterms=MOOS&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DMOOS"><span>Jovian <span class="hlt">ultraviolet</span> auroral activity, 1981-1991</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Livengood, T. A.; Moos, H. W.; Ballester, G. E.; Prange, R. M.</p> <p>1992-01-01</p> <p>IUE observations of H2 UV emissions for the 1981-1991 period are presently used to investigate the auroral <span class="hlt">brightness</span> distribution on the surface of Jupiter. The <span class="hlt">brightness</span>, which is diagnostic of energy input to the atmosphere as well as of magnetospheric processes, is determined by comparing model-predicted <span class="hlt">brightnesses</span> against empirical ones. The north and south aurorae appear to be correlated in <span class="hlt">brightness</span> and in variations of the longitude of peak <span class="hlt">brightness</span>. There are strong fluctuations in all the parameters of the <span class="hlt">brightness</span> distribution on much shorter time scales than those of solar maximum-minimum.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3152653','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3152653"><span>Spatiotemporal analysis of <span class="hlt">brightness</span> induction</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>McCourt, Mark E.</p> <p>2011-01-01</p> <p><span class="hlt">Brightness</span> induction refers to a class of visual illusions in which the perceived intensity of a region of space is influenced by the luminance of surrounding regions. These illusions are significant because they provide insight into the neural organization of the visual system. A novel quadrature-phase motion cancelation technique was developed to measure the magnitude of the grating induction <span class="hlt">brightness</span> illusion across a wide range of spatial frequencies, temporal frequencies and test field heights. Canceling contrast is greatest at low frequencies and declines with increasing frequency in both dimensions, and with increasing test field height. Canceling contrast scales as the product of inducing grating spatial frequency and test field height (the number of inducing grating cycles per test field height). When plotted using a spatial axis which indexes this product, the spatiotemporal induction surfaces for four test field heights can be described as four partially overlapping sections of a single larger surface. These properties of <span class="hlt">brightness</span> induction are explained in the context of multiscale spatial filtering. The present study is the first to measure the magnitude of grating induction as a function of temporal frequency. Taken in conjunction with several other studies (Blakeslee & McCourt, 2008; Robinson & de Sa, 2008; Magnussen & Glad, 1975) the results of this study illustrate that at least one form of <span class="hlt">brightness</span> induction is very much faster than that reported by DeValois et al. (1986) and Rossi and Paradiso (1996), and are inconsistent with the proposition that <span class="hlt">brightness</span> induction results from a slow “filling in” process. PMID:21763339</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2006PhDT.........6O','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2006PhDT.........6O"><span>Structural, electrical and optical characterization of high <span class="hlt">brightness</span> phosphor-free white light emitting diodes</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Omiya, Hiromasa</p> <p></p> <p>Much interest currently exists in GaN and related materials for applications such as light-emitting devices operating in the amber to <span class="hlt">ultraviolet</span> range. Solid-state lighting (SSL) using these materials is widely being investigated worldwide, especially due to their high-energy efficiency and its impact on environmental issues. A new approach for solid-state lighting uses phosphor-free white light emitting diodes (LEDs) that consist of blue, green, and red quantum wells (QW), all in a single device. This approach leads to improved color rendering, and directionality, compared to the conventional white LEDs that use yellow phosphor on blue or <span class="hlt">ultraviolet</span> emitters. Improving the <span class="hlt">brightness</span> of these phosphor-free white LEDs should enhance and accelerate the development of SSL technology. The main objective of the research reported in this dissertation is to provide a comprehensive understanding of the nature of the multiple quantum wells used in phosphor-free white LEDs. This dissertation starts with an introduction to lighting history, the fundamental concepts of nitride semiconductors, and the evolution of LED technology. Two important challenges in LED technology today are metal-semiconductor contacts and internal piezoelectric fields present in quantum well structures. Thus, the main portion of this dissertation consists of three parts dealing with metal-semiconductor interfaces, single quantum well structures, and multiple quantum well devices. Gold-nickel alloys are widely used as contacts to the p-region of LEDs. We have performed a detailed study for its evolution under standard annealing steps. The atomic arrangement of gold at its interface with GaN gives a clear explanation for the improved ohmic contact performance. We next focus on the nature of InGaN QWs. The dynamic response of the QWs was studied with electron holography and time-resolved cathodoluminescence. Establishing the correlation between energy band structure and the light emission spectra</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013RScI...84h3703N','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013RScI...84h3703N"><span>A <span class="hlt">brightness</span> exceeding simulated Langmuir limit</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Nakasuji, Mamoru</p> <p>2013-08-01</p> <p>When an excitation of the first lens determines a beam is parallel beam, a <span class="hlt">brightness</span> that is 100 times higher than Langmuir limit is measured experimentally, where Langmuir limits are estimated using a simulated axial cathode current density which is simulated based on a measured emission current. The measured <span class="hlt">brightness</span> is comparable to Langmuir limit, when the lens excitation is such that an image position is slightly shorter than a lens position. Previously measured values of <span class="hlt">brightness</span> for cathode apical radii of curvature 20, 60, 120, 240, and 480 μm were 8.7, 5.3, 3.3, 2.4, and 3.9 times higher than their corresponding Langmuir limits, respectively, in this experiment, the lens excitation was such that the lens and the image positions were 180 mm and 400 mm, respectively. From these measured <span class="hlt">brightness</span> for three different lens excitation conditions, it is concluded that the <span class="hlt">brightness</span> depends on the first lens excitation. For the electron gun operated in a space charge limited condition, some of the electrons emitted from the cathode are returned to the cathode without having crossed a virtual cathode. Therefore, method that assumes a Langmuir limit defining method using a Maxwellian distribution of electron velocities may need to be revised. For the condition in which the values of the exceeding the Langmuir limit are measured, the simulated trajectories of electrons that are emitted from the cathode do not cross the optical axis at the crossover, thus the law of sines may not be valid for high <span class="hlt">brightness</span> electron beam systems.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/11837952','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/11837952"><span><span class="hlt">Bright</span>-light mask treatment of delayed sleep phase syndrome.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Cole, Roger J; Smith, Julian S; Alcalá, Yvonne C; Elliott, Jeffrey A; Kripke, Daniel F</p> <p>2002-02-01</p> <p>We treated delayed sleep phase syndrome (DSPS) with an illuminated mask that provides light through closed eyelids during sleep. Volunteers received either <span class="hlt">bright</span> white light (2,700 lux, n = 28) or dim red light placebo (0.1 lux, n = 26) for 26 days at home. Mask lights were turned on (< 0.01 lux) 4 h before arising, ramped up for 1 h, and remained on at full <span class="hlt">brightness</span> until arising. Volunteers also attempted to systematically advance sleep time, avoid naps, and avoid evening <span class="hlt">bright</span> light. The light mask was well tolerated and produced little sleep disturbance. The acrophase of urinary 6-sulphatoxymelatonin (6-SMT) excretion advanced significantly from baseline in the <span class="hlt">bright</span> group (p < 0.0006) and not in the dim group, but final phases were not significantly earlier in the <span class="hlt">bright</span> group (ANCOVA ns). <span class="hlt">Bright</span> treatment did produce significantly earlier phases, however, among volunteers whose baseline 6-SMT acrophase was later than the median of 0602 h (<span class="hlt">bright</span> shift: 0732-0554 h, p < 0.0009; dim shift: 0746-0717 h, ns; ANCOVA p = 0.03). In this subgroup, sleep onset advanced significantly only with <span class="hlt">bright</span> but not dim treatment (sleep onset shift: <span class="hlt">bright</span> 0306-0145 h, p < 0.0002; dim 0229-0211 h, ns; ANCOVA p < .05). Despite equal expectations at baseline, participants rated <span class="hlt">bright</span> treatment as more effective than dim treatment (p < 0.04). We conclude that <span class="hlt">bright</span>-light mask treatment advances circadian phase and provides clinical benefit in DSPS individuals whose initial circadian delay is relatively severe.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25818045','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25818045"><span><span class="hlt">Brightness</span> masking is modulated by disparity structure.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Pelekanos, Vassilis; Ban, Hiroshi; Welchman, Andrew E</p> <p>2015-05-01</p> <p>The luminance contrast at the borders of a surface strongly influences surface's apparent <span class="hlt">brightness</span>, as demonstrated by a number of classic visual illusions. Such phenomena are compatible with a propagation mechanism believed to spread contrast information from borders to the interior. This process is disrupted by masking, where the perceived <span class="hlt">brightness</span> of a target is reduced by the brief presentation of a mask (Paradiso & Nakayama, 1991), but the exact visual stage that this happens remains unclear. In the present study, we examined whether <span class="hlt">brightness</span> masking occurs at a monocular-, or a binocular-level of the visual hierarchy. We used backward masking, whereby a briefly presented target stimulus is disrupted by a mask coming soon afterwards, to show that <span class="hlt">brightness</span> masking is affected by binocular stages of the visual processing. We manipulated the 3-D configurations (slant direction) of the target and mask and measured the differential disruption that masking causes on <span class="hlt">brightness</span> estimation. We found that the masking effect was weaker when stimuli had a different slant. We suggest that <span class="hlt">brightness</span> masking is partly mediated by mid-level neuronal mechanisms, at a stage where binocular disparity edge structure has been extracted. Copyright © 2015 The Authors. Published by Elsevier Ltd.. All rights reserved.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2010-title21-vol8/pdf/CFR-2010-title21-vol8-sec872-6350.pdf','CFR'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2010-title21-vol8/pdf/CFR-2010-title21-vol8-sec872-6350.pdf"><span>21 CFR 872.6350 - <span class="hlt">Ultraviolet</span> detector.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2010&page.go=Go">Code of Federal Regulations, 2010 CFR</a></p> <p></p> <p>2010-04-01</p> <p>... 21 Food and Drugs 8 2010-04-01 2010-04-01 false <span class="hlt">Ultraviolet</span> detector. 872.6350 Section 872.6350...) MEDICAL DEVICES DENTAL DEVICES Miscellaneous Devices § 872.6350 <span class="hlt">Ultraviolet</span> detector. (a) Identification. An <span class="hlt">ultraviolet</span> detector is a device intended to provide a source of <span class="hlt">ultraviolet</span> light which is used...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2014-title21-vol8/pdf/CFR-2014-title21-vol8-sec872-6350.pdf','CFR2014'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2014-title21-vol8/pdf/CFR-2014-title21-vol8-sec872-6350.pdf"><span>21 CFR 872.6350 - <span class="hlt">Ultraviolet</span> detector.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2014&page.go=Go">Code of Federal Regulations, 2014 CFR</a></p> <p></p> <p>2014-04-01</p> <p>... 21 Food and Drugs 8 2014-04-01 2014-04-01 false <span class="hlt">Ultraviolet</span> detector. 872.6350 Section 872.6350...) MEDICAL DEVICES DENTAL DEVICES Miscellaneous Devices § 872.6350 <span class="hlt">Ultraviolet</span> detector. (a) Identification. An <span class="hlt">ultraviolet</span> detector is a device intended to provide a source of <span class="hlt">ultraviolet</span> light which is used...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2011-title21-vol8/pdf/CFR-2011-title21-vol8-sec872-6350.pdf','CFR2011'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2011-title21-vol8/pdf/CFR-2011-title21-vol8-sec872-6350.pdf"><span>21 CFR 872.6350 - <span class="hlt">Ultraviolet</span> detector.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2011&page.go=Go">Code of Federal Regulations, 2011 CFR</a></p> <p></p> <p>2011-04-01</p> <p>... 21 Food and Drugs 8 2011-04-01 2011-04-01 false <span class="hlt">Ultraviolet</span> detector. 872.6350 Section 872.6350...) MEDICAL DEVICES DENTAL DEVICES Miscellaneous Devices § 872.6350 <span class="hlt">Ultraviolet</span> detector. (a) Identification. An <span class="hlt">ultraviolet</span> detector is a device intended to provide a source of <span class="hlt">ultraviolet</span> light which is used...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2012-title21-vol8/pdf/CFR-2012-title21-vol8-sec872-6350.pdf','CFR2012'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2012-title21-vol8/pdf/CFR-2012-title21-vol8-sec872-6350.pdf"><span>21 CFR 872.6350 - <span class="hlt">Ultraviolet</span> detector.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2012&page.go=Go">Code of Federal Regulations, 2012 CFR</a></p> <p></p> <p>2012-04-01</p> <p>... 21 Food and Drugs 8 2012-04-01 2012-04-01 false <span class="hlt">Ultraviolet</span> detector. 872.6350 Section 872.6350...) MEDICAL DEVICES DENTAL DEVICES Miscellaneous Devices § 872.6350 <span class="hlt">Ultraviolet</span> detector. (a) Identification. An <span class="hlt">ultraviolet</span> detector is a device intended to provide a source of <span class="hlt">ultraviolet</span> light which is used...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2013-title21-vol8/pdf/CFR-2013-title21-vol8-sec872-6350.pdf','CFR2013'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2013-title21-vol8/pdf/CFR-2013-title21-vol8-sec872-6350.pdf"><span>21 CFR 872.6350 - <span class="hlt">Ultraviolet</span> detector.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2013&page.go=Go">Code of Federal Regulations, 2013 CFR</a></p> <p></p> <p>2013-04-01</p> <p>... 21 Food and Drugs 8 2013-04-01 2013-04-01 false <span class="hlt">Ultraviolet</span> detector. 872.6350 Section 872.6350...) MEDICAL DEVICES DENTAL DEVICES Miscellaneous Devices § 872.6350 <span class="hlt">Ultraviolet</span> detector. (a) Identification. An <span class="hlt">ultraviolet</span> detector is a device intended to provide a source of <span class="hlt">ultraviolet</span> light which is used...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/20551588','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/20551588"><span>Effect of evening exposure to <span class="hlt">bright</span> or dim light after daytime <span class="hlt">bright</span> light on absorption of dietary carbohydrates the following morning.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Hirota, Naoko; Sone, Yoshiaki; Tokura, Hiromi</p> <p>2010-01-01</p> <p>We had previously reported on the effect of exposure to light on the human digestive system: daytime <span class="hlt">bright</span> light exposure has a positive effect, whereas, evening <span class="hlt">bright</span> light exposure has a negative effect on the efficiency of dietary carbohydrate absorption from the evening meal. These results prompted us to examine whether the light intensity to which subjects are exposed in the evening affects the efficiency of dietary carbohydrate absorption the following morning. In this study, subjects were exposed to either 50 lux (dim light conditions) or 2,000 lux (<span class="hlt">bright</span> light conditions) in the evening for 9 h (from 15:00 to 24:00) after staying under <span class="hlt">bright</span> light in the daytime (under 2,000 lux from 07:00 to 15:00). We measured unabsorbed dietary carbohydrates using the breath-hydrogen test the morning after exposure to either <span class="hlt">bright</span> light or dim light the previous evening. Results showed that there was no significant difference between the two conditions in the amount of breath hydrogen. This indicates that evening exposure to <span class="hlt">bright</span> or dim light after <span class="hlt">bright</span> light exposure in the daytime has no varying effect on digestion or absorption of dietary carbohydrates in the following morning's breakfast.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19990023305','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19990023305"><span>Microwave <span class="hlt">Brightness</span> Temperatures of Tilted Convective Systems</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hong, Ye; Haferman, Jeffrey L.; Olson, William S.; Kummerow, Christian D.</p> <p>1998-01-01</p> <p>Aircraft and ground-based radar data from the Tropical Ocean and Global Atmosphere Coupled-Ocean Atmosphere Response Experiment (TOGA COARE) show that convective systems are not always vertical. Instead, many are tilted from vertical. Satellite passive microwave radiometers observe the atmosphere at a viewing angle. For example, the Special Sensor Microwave/Imager (SSM/I) on Defense Meteorological Satellite Program (DMSP) satellites and the Tropical Rainfall Measurement Mission (TRMM) Microwave Imager (TMI) on the TRMM satellite have an incident angle of about 50deg. Thus, the <span class="hlt">brightness</span> temperature measured from one direction of tilt may be different than that viewed from the opposite direction due to the different optical depth. This paper presents the investigation of passive microwave <span class="hlt">brightness</span> temperatures of tilted convective systems. To account for the effect of tilt, a 3-D backward Monte Carlo radiative transfer model has been applied to a simple tilted cloud model and a dynamically evolving cloud model to derive the <span class="hlt">brightness</span> temperature. The radiative transfer results indicate that <span class="hlt">brightness</span> temperature varies when the viewing angle changes because of the different optical depth. The tilt increases the displacements between high 19 GHz <span class="hlt">brightness</span> temperature (Tb(sub 19)) due to liquid emission from lower level of cloud and the low 85 GHz <span class="hlt">brightness</span> temperature (Tb(sub 85)) due to ice scattering from upper level of cloud. As the resolution degrades, the difference of <span class="hlt">brightness</span> temperature due to the change of viewing angle decreases dramatically. The dislocation between Tb(sub 19) and Tb(sub 85), however, remains prominent.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018A%26A...613A..30M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018A%26A...613A..30M"><span>A near-infrared, optical, and <span class="hlt">ultraviolet</span> polarimetric and timing investigation of complex equatorial dusty structures</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Marin, F.; Rojas Lobos, P. A.; Hameury, J. M.; Goosmann, R. W.</p> <p>2018-05-01</p> <p>Context. From stars to active galactic nuclei, many astrophysical systems are surrounded by an equatorial distribution of dusty material that is, in a number of cases, spatially unresolved even with cutting edge facilities. Aims: In this paper, we investigate if and how one can determine the unresolved and heterogeneous morphology of dust distribution around a central <span class="hlt">bright</span> source using time-resolved polarimetric observations. Methods: We used polarized radiative transfer simulations to study a sample of circumnuclear dusty morphologies. We explored a grid of geometrically variable models that are uniform, fragmented, and density stratified in the near-infrared, optical, and <span class="hlt">ultraviolet</span> bands, and we present their distinctive time-dependent polarimetric signatures. Results: As expected, varying the structure of the obscuring equatorial disk has a deep impact on the inclination-dependent flux, polarization degree and angle, and time lags we observe. We find that stratified media are distinguishable by time-resolved polarimetric observations, and that the expected polarization is much higher in the infrared band than in the <span class="hlt">ultraviolet</span>. However, because of the physical scales imposed by dust sublimation, the average time lags of months to years between the total and polarized fluxes are important; these time lags lengthens the observational campaigns necessary to break more sophisticated, and therefore also more degenerated, models. In the <span class="hlt">ultraviolet</span> band, time lags are slightly shorter than in the infrared or optical bands, and, coupled to lower diluting starlight fluxes, time-resolved polarimetry in the UV appears more promising for future campaigns. Conclusions: Equatorial dusty disks differ in terms of inclination-dependent photometric, polarimetric, and timing observables, but only the coupling of these different markers can lead to inclination-independent constraints on the unresolved structures. Even though it is complex and time consuming, polarized</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=2659800','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=2659800"><span>The <span class="hlt">Brightness</span> of Colour</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Corney, David; Haynes, John-Dylan; Rees, Geraint; Lotto, R. Beau</p> <p>2009-01-01</p> <p>Background The perception of <span class="hlt">brightness</span> depends on spatial context: the same stimulus can appear light or dark depending on what surrounds it. A less well-known but equally important contextual phenomenon is that the colour of a stimulus can also alter its <span class="hlt">brightness</span>. Specifically, stimuli that are more saturated (i.e. purer in colour) appear brighter than stimuli that are less saturated at the same luminance. Similarly, stimuli that are red or blue appear brighter than equiluminant yellow and green stimuli. This non-linear relationship between stimulus intensity and <span class="hlt">brightness</span>, called the Helmholtz-Kohlrausch (HK) effect, was first described in the nineteenth century but has never been explained. Here, we take advantage of the relative simplicity of this ‘illusion’ to explain it and contextual effects more generally, by using a simple Bayesian ideal observer model of the human visual ecology. We also use fMRI brain scans to identify the neural correlates of <span class="hlt">brightness</span> without changing the spatial context of the stimulus, which has complicated the interpretation of related fMRI studies. Results Rather than modelling human vision directly, we use a Bayesian ideal observer to model human visual ecology. We show that the HK effect is a result of encoding the non-linear statistical relationship between retinal images and natural scenes that would have been experienced by the human visual system in the past. We further show that the complexity of this relationship is due to the response functions of the cone photoreceptors, which themselves are thought to represent an efficient solution to encoding the statistics of images. Finally, we show that the locus of the response to the relationship between images and scenes lies in the primary visual cortex (V1), if not earlier in the visual system, since the <span class="hlt">brightness</span> of colours (as opposed to their luminance) accords with activity in V1 as measured with fMRI. Conclusions The data suggest that perceptions of <span class="hlt">brightness</span></p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/29809046','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/29809046"><span>Exposure to <span class="hlt">bright</span> light biases effort-based decisions.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Bijleveld, Erik; Knufinke, Melanie</p> <p>2018-06-01</p> <p>Secreted in the evening and the night, melatonin suppresses activity of the mesolimbic dopamine pathway, a brain pathway involved in reward processing. However, exposure to <span class="hlt">bright</span> light diminishes-or even prevents-melatonin secretion. Thus, we hypothesized that reward processing, in the evening, is more pronounced in <span class="hlt">bright</span> light (vs. dim light). Healthy human participants carried out three tasks that tapped into various aspects of reward processing (effort expenditure for rewards task [EEfRT]; two-armed bandit task [2ABT]; balloon analogue risk task [BART). <span class="hlt">Brightness</span> was manipulated within-subjects (<span class="hlt">bright</span> vs. dim light), in separate evening sessions. During the EEfRT, participants used reward-value information more strongly when they were exposed to <span class="hlt">bright</span> light (vs. dim light). This finding supported our hypothesis. However, exposure to <span class="hlt">bright</span> light did not significantly affect task behavior on the 2ABT and the BART. While future research is necessary (e.g., to zoom in on working mechanisms), these findings have potential implications for the design of physical work environments. (PsycINFO Database Record (c) 2018 APA, all rights reserved).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19930028542&hterms=SCI&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3DSCI','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19930028542&hterms=SCI&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3DSCI"><span><span class="hlt">Ultraviolet</span> Imaging Telescope observations of the ScI galaxy NGC 628 (M74)</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Chen, Peter C.; Cornett, Robert H.; Roberts, Morton S.; Bohlin, Ralph C.; Neff, Susan G.; O'Connell, Robert W.; Parise, Ronald A.; Smith, Andrew M.; Stecher, Theodore P.</p> <p>1992-01-01</p> <p><span class="hlt">Ultraviolet</span> images of NGC 628 at 1520 and 2490 A show that the nucleus has an oblong appearance and that the arms and disk exhibit features not seen in blue or H-alpha images. Aperture photometry of the nucleus gives results that are compatible with observations in other bandpasses and with models. The spiral arms appear more symmetrical in the UV than in other colors; in particular, two gaps are seen on either side of the nucleus. Combined UV and radio data appear to support a large-scale collective phenomenon, perhaps a quasi-static spiral structure mechanism, as being the dominant mode of spiral formation in this galaxy. We report the detection of a low surface <span class="hlt">brightness</span> object at a distance of 7.6 arcmin southwest of the nucleus.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013SPIE.8859E..0TG','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013SPIE.8859E..0TG"><span>Performance results from in-flight commissioning of the Juno <span class="hlt">Ultraviolet</span> Spectrograph (Juno-UVS)</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Greathouse, T. K.; Gladstone, G. R.; Davis, M. W.; Slater, D. C.; Versteeg, M. H.; Persson, K. B.; Walther, B. C.; Winters, G. S.; Persyn, S. C.; Eterno, J. S.</p> <p>2013-09-01</p> <p>We present a description of the Juno <span class="hlt">ultraviolet</span> spectrograph (Juno-UVS) and results from its in-flight commissioning performed between December 5th and 13th 2011 and its first periodic maintenance between October 10th and 12th 2012. Juno-UVS is a modest power (9.0 W) <span class="hlt">ultraviolet</span> spectrograph based on the Alice instruments now in flight aboard the European Space Agency's Rosetta spacecraft, NASA's New Horizons spacecraft, and the LAMP instrument aboard NASA's Lunar Reconnaissance Orbiter. However, unlike the other Alice spectrographs, Juno-UVS sits aboard a spin stabilized spacecraft. The Juno-UVS scan mirror allows for pointing of the slit approximately +/-30° from the spacecraft spin plane. This ability gives Juno-UVS access to half the sky at any given spacecraft orientation. The planned 2 rpm spin rate for the primary mission results in integration times per 0.2° spatial resolution element per spin of only ~17 ms. Thus, for calibration purposes, data were retrieved from many spins and then remapped and co-added to build up exposure times on <span class="hlt">bright</span> stars to measure the effective area, spatial resolution, scan mirror pointing positions, etc. The primary job of Juno-UVS will be to characterize Jupiter's UV auroral emissions and relate them to in-situ particle measurements. The ability to point the slit will make operations more flexible, allowing Juno-UVS to observe the atmospheric footprints of magnetic field lines through which Juno flies, giving a direct connection between energetic particle measurements on the spacecraft and the far-<span class="hlt">ultraviolet</span> emissions produced by Jupiter's atmosphere in response to those particles.</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_6");'>6</a></li> <li><a href="#" onclick='return showDiv("page_7");'>7</a></li> <li class="active"><span>8</span></li> <li><a href="#" onclick='return showDiv("page_9");'>9</a></li> <li><a href="#" onclick='return showDiv("page_10");'>10</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_8 --> <div id="page_9" 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_7");'>7</a></li> <li><a href="#" onclick='return showDiv("page_8");'>8</a></li> <li class="active"><span>9</span></li> <li><a href="#" onclick='return showDiv("page_10");'>10</a></li> <li><a href="#" onclick='return showDiv("page_11");'>11</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="161"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19900042461&hterms=bright+hour&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dbright%2Bhour','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19900042461&hterms=bright+hour&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dbright%2Bhour"><span>Coronal <span class="hlt">bright</span> points at 6cm wavelength</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Fu, Qijun; Kundu, M. R.; Schmahl, E. J.</p> <p>1988-01-01</p> <p>Results are presented from observations of <span class="hlt">bright</span> points at a wavelength of 6-cm using the VLA with a spatial resolution of 1.2 arcsec. During two hours of observations, 44 sources were detected with <span class="hlt">brightness</span> temperatures between 2000 and 30,000 K. Of these sources, 27 are associated with weak dark He 10830 A features at distances less than 40 arcsecs. Consideration is given to variations in the source parameters and the relationship between ephemeral regions and <span class="hlt">bright</span> points.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20170002529','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20170002529"><span>Si III OV <span class="hlt">Bright</span> Line of Scattering Polarized Light That Has Been Observed in the CLASP and Its Center-to-Limb Variation</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Katsukawa, Yukio; Ishikawa, Ryoko; Kano, Ryohei; Kubo, Masahito; Noriyuki, Narukage; Kisei, Bando; Hara, Hirohisa; Yoshiho, Suematsu; Goto, Motouji; Ishikawa, Shinnosuke; <a style="text-decoration: none; " href="javascript:void(0); " onClick="displayelement('author_20170002529'); toggleEditAbsImage('author_20170002529_show'); toggleEditAbsImage('author_20170002529_hide'); "> <img style="display:inline; width:12px; height:12px; " src="images/arrow-up.gif" width="12" height="12" border="0" alt="hide" id="author_20170002529_show"> <img style="width:12px; height:12px; display:none; " src="images/arrow-down.gif" width="12" height="12" border="0" alt="hide" id="author_20170002529_hide"></p> <p>2017-01-01</p> <p>The CLASP (Chromospheric Lyman-Alpha Spectro- Polarimeter) rocket experiment, in addition to the <span class="hlt">ultraviolet</span> region of the Ly alpha emission line (121.57 nm), emission lines of Si III (120.65 nm) and OV (121.83 nm) is can be observed. These are optically thin line compared to a Ly alpha line, if Rarere captured its polarization, there is a possibility that dripping even a new physical diagnosis chromosphere-transition layer. In particular, OV <span class="hlt">bright</span> light is a release from the transition layer, further, three P one to one S(sub 0) is a forbidden line (cross-triplet transition between lines), it was not quite know whether to polarization.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19810059463&hterms=MOOS&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3DMOOS','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19810059463&hterms=MOOS&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3DMOOS"><span><span class="hlt">Ultraviolet</span> observations of the Io torus from the IUE observatory</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Moos, H. W.; Clarke, J. T.</p> <p>1981-01-01</p> <p>The short wavelength spectrograph on the International <span class="hlt">Ultraviolet</span> Explorer (IUE) has been used to obtain 11 A resolution spectra of the Io torus from 1175-1950 A. The four spectra, obtained in the springs of 1979 and 1980, show emissions (about 40R) of S II A1256A and S III A1199A. An unidentified feature is also present at 1729 A; a tentative identification as an intercombination line of S III is proposed. Weak features, probably due to O III A1664A and S IV A1406A, appear in some of the spectra. Abundances of the ions are determined from the <span class="hlt">brightnesses</span> of the observed features. Upper limits are also set for the abundances of a number of ionic and neutral species. An observation of Io itself does not show any additional or enhanced spectral features, permitting upper limits to be set on the injection rate for a number of species.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018ATel11688....1F','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018ATel11688....1F"><span>The ZTF <span class="hlt">Bright</span> Transient Survey</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Fremling, C.; Sharma, Y.; Kulkarni, S. R.; Miller, A. A.; Taggart, K.; Perley, D. A.; Gooba, A.</p> <p>2018-06-01</p> <p>As a supplement to the Zwicky Transient Facility (ZTF; ATel #11266) public alerts (ATel #11685) we plan to report (following ATel #11615) <span class="hlt">bright</span> probable supernovae identified in the raw alert stream from the ZTF Northern Sky Survey ("Celestial Cinematography"; see Bellm & Kulkarni, 2017, Nature Astronomy 1, 71) to the Transient Name Server (https://wis-tns.weizmann.ac.il) on a daily basis; the ZTF <span class="hlt">Bright</span> Transient Survey (BTS; see Kulkarni et al., 2018; arXiv:1710.04223).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19760035678&hterms=mcdonald&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dmcdonald','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19760035678&hterms=mcdonald&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dmcdonald"><span>The night sky <span class="hlt">brightness</span> at McDonald Observatory</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Kalinowski, J. K.; Roosen, R. G.; Brandt, J. C.</p> <p>1975-01-01</p> <p>Baseline observations of the night sky <span class="hlt">brightness</span> in B and V are presented for McDonald Observatory. In agreement with earlier work by Elvey and Rudnick (1937) and Elvey (1943), significant night-to-night and same-night variations in sky <span class="hlt">brightness</span> are found. Possible causes for these variations are discussed. The largest variation in sky <span class="hlt">brightness</span> found during a single night is approximately a factor of two, a value which corresponds to a factor-of-four variation in airglow <span class="hlt">brightness</span>. The data are used to comment on the accuracy of previously published surface photometry of M 81.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-GSFC_20171208_Archive_e002110.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-GSFC_20171208_Archive_e002110.html"><span><span class="hlt">Bright</span> Solar Flare</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2017-12-08</p> <p>A <span class="hlt">bright</span> solar flare is captured by the EIT 195Å instrument on 1998 May 2. A solar flare (a sudden, rapid, and intense variation in <span class="hlt">brightness</span>) occurs when magnetic energy that has built up in the solar atmosphere is suddenly released, launching material outward at millions of km per hour. The Sun’s magnetic fields tend to restrain each other and force the buildup of tremendous energy, like twisting rubber bands, so much that they eventually break. At some point, the magnetic lines of force merge and cancel in a process known as magnetic reconnection, causing plasma to forcefully escape from the Sun. Credit: NASA/GSFC/SOHO/ESA To learn more go to the SOHO website: sohowww.nascom.nasa.gov/home.html To learn more about NASA's Sun Earth Day go here: sunearthday.nasa.gov/2010/index.php</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017APS..DMP.Q1100K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017APS..DMP.Q1100K"><span>Dark-<span class="hlt">Bright</span> Soliton Dynamics Beyond the Mean-Field Approximation</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Katsimiga, Garyfallia; Koutentakis, Georgios; Mistakidis, Simeon; Kevrekidis, Panagiotis; Schmelcher, Peter; Theory Group of Fundamental Processes in Quantum Physics Team</p> <p>2017-04-01</p> <p>The dynamics of dark <span class="hlt">bright</span> solitons beyond the mean-field approximation is investigated. We first examine the case of a single dark-<span class="hlt">bright</span> soliton and its oscillations within a parabolic trap. Subsequently, we move to the setting of collisions, comparing the mean-field approximation to that involving multiple orbitals in both the dark and the <span class="hlt">bright</span> component. Fragmentation is present and significantly affects the dynamics, especially in the case of slower solitons and in that of lower atom numbers. It is shown that the presence of fragmentation allows for bipartite entanglement between the distinguishable species. Most importantly the interplay between fragmentation and entanglement leads to the decay of each of the initial mean-field dark-<span class="hlt">bright</span> solitons into fast and slow fragmented dark-<span class="hlt">bright</span> structures. A variety of excitations including dark-<span class="hlt">bright</span> solitons in multiple (concurrently populated) orbitals is observed. Dark-antidark states and domain-wall-<span class="hlt">bright</span> soliton complexes can also be observed to arise spontaneously in the beyond mean-field dynamics. Deutsche Forschungsgemeinschaft (DFG) in the framework of the SFB 925 ``Light induced dynamics and control of correlated quantum systems''.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016EGUGA..18.3729J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016EGUGA..18.3729J"><span>Relationship between extreme <span class="hlt">ultraviolet</span> microflares and small-scale magnetic fields in the quiet Sun</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jiang, Fayu; Zhang, Jun; Yang, Shuhong</p> <p>2016-04-01</p> <p>Microflares are small dynamic signatures observed in X-ray and extreme-<span class="hlt">ultraviolet</span> channels. Because of their impulsive emission enhancements and wide distribution, they are thought to be closely related to coronal heating. By using the high resolution 171 Å images from the Atmospheric Imaging Assembly and the lines-of-sight magnetograms obtained by the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory, we trace 10794 microflares in a quiet region near the disk center with a field of view of 960''× 1068'' during 24 hr. The microflares have an occurrence rate of 4.4 × 103 hr-1 extrapolated over the whole Sun. Their average <span class="hlt">brightness</span>, size, and lifetime are 1.7 I0 (of the quiet Sun), 9.6 Mm2, and 3.6 min, respectively. There exists a mutual positive correlation between the microflares' <span class="hlt">brightness</span>, area and lifetime. In general, the microflares distribute uniformly across the solar disk, but form network patterns locally, which are similar to and matched with the magnetic network structures. Typical cases show that the microflares prefer to occur in magnetic cancellation regions of network boundaries. We roughly calculate the upper limit of energy flux supplied by the microflares and find that the result is still a factor of ˜15 below the coronal heating requirement.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=1088641','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=1088641"><span>Egg colour matching in an African cuckoo, as revealed by <span class="hlt">ultraviolet</span>-visible reflectance spectrophotometry.</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Cherry, M I; Bennett, A T</p> <p>2001-01-01</p> <p>Despite major differences between human and avian colour vision, previous studies of cuckoo egg mimicry have used human colour vision (or standards based thereon) to assess colour matching. Using <span class="hlt">ultraviolet</span>-visible reflectance spectrophotometry (300-700 nm), we measured museum collections of eggs of the red-chested cuckoo and its hosts. The first three principal components explained more than 99% of the variance in spectra, and measures of cuckoo host egg similarity derived from these transformations were compared with measures of cuckoo host egg similarity estimated by human observers unaware of the hypotheses we were testing. Monte Carlo methods were used to simulate laying of cuckoo eggs at random in nests. Results showed that host and cuckoo eggs were very highly matched for an <span class="hlt">ultraviolet</span> versus greenness component, which was not detected by humans. Furthermore, whereas cuckoo and host were dissimilar in achromatic <span class="hlt">brightness</span>, humans did not detect this difference. Our study thus reveals aspects of cuckoo-host egg colour matching which have hitherto not been described. These results suggest subtleties and complexities in the evolution of host-cuckoo egg mimicry that were not previously suspected. Our results also have the potential to explain the longstanding paradox that some host species accept cuckoo eggs that are non-mimetic to the human eye. PMID:11297172</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018PhRvA..97d3623K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018PhRvA..97d3623K"><span>Dark-<span class="hlt">bright</span> soliton pairs: Bifurcations and collisions</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Katsimiga, G. C.; Kevrekidis, P. G.; Prinari, B.; Biondini, G.; Schmelcher, P.</p> <p>2018-04-01</p> <p>The statics, stability, and dynamical properties of dark-<span class="hlt">bright</span> soliton pairs are investigated here, motivated by applications in a homogeneous two-component repulsively interacting Bose-Einstein condensate. One of the intraspecies interaction coefficients is used as the relevant parameter controlling the deviation from the integrable Manakov limit. Two different families of stationary states are identified consisting of dark-<span class="hlt">bright</span> solitons that are either antisymmetric (out-of-phase) or asymmetric (mass imbalanced) with respect to their <span class="hlt">bright</span> soliton. Both of the above dark-<span class="hlt">bright</span> configurations coexist at the integrable limit of equal intra and interspecies repulsions and are degenerate in that limit. However, they are found to bifurcate from it in a transcritical bifurcation. This bifurcation interchanges the stability properties of the bound dark-<span class="hlt">bright</span> pairs rendering the antisymmetric states unstable and the asymmetric ones stable past the associated critical point (and vice versa before it). Finally, on the dynamical side, it is found that large kinetic energies and thus rapid soliton collisions are essentially unaffected by the intraspecies variation, while cases involving near equilibrium states or breathing dynamics are significantly modified under such a variation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20060048198','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20060048198"><span>Solar CIV Vacuum-<span class="hlt">Ultraviolet</span> Fabry-Perot Interferometers</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Gary, G. Allen; West, Edward A.; Rees, David; McKay, Jack A.; Zukic, Maumer; Herman, Peter</p> <p>2006-01-01</p> <p>Aims: A tunable, high spectral resolution, high effective finesse, vacuum <span class="hlt">ultraviolet</span> (VUV) Fabry-Perot interferometer (PPI) is designed for obtaining narrow-passband images, magnetograms, and Dopplergrams of the transition region emission line of CIV (155 nm). Methods: The integral part of the CIV narrow passband filter package (with a 2-10 pm FWHM) consists of a multiple etalon system composed of a tunable interferometer that provides high-spectral resolution and a static low-spectral resolution interferometer that allows a large effective free spectral range. The prefilter for the interferometers is provided by a set of four mirrors with dielectric high-reflective coatings. A tunable interferometer, a VUV piezoelectric-control etalon, has undergone testing using the surrogate F2 eximer laser line at 157 nm for the CIV line. We present the results of the tests with a description of the overall concept for a complete narrow-band CIV spectral filter. The static interferometer of the filter is envisioned as being hudt using a set of fixed MgF2 plates. The four-mirror prefilter is designed to have dielectric multilayer n-stacks employing the design concept used in the <span class="hlt">Ultraviolet</span> Imager of NASA's Polar Spacecraft. A dual etalon system allows the effective free spectral range to be commensurate with the prefilter profile. With an additional etalon, a triple etalon system would allow a spectrographic resolution of 2 pm. The basic strategy has been to combine the expertise of spaceflight etalon manufacturing with VUV coating technology to build a VUV FPI which combines the best attributes of imagers and spectrographs into a single compact instrument. Results. Spectro-polarimetry observations of the transition region CIV emission can be performed to increase the understanding of the magnetic forces, mass motion, evolution, and energy release within the solar atmosphere at the base of the corona where most of the magnetic field is approximately force-free. The 2D imaging</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013RAA....13.1255Y','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013RAA....13.1255Y"><span>Moon night sky <span class="hlt">brightness</span> simulation for the Xinglong station</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Yao, Song; Zhang, Hao-Tong; Yuan, Hai-Long; Zhao, Yong-Heng; Dong, Yi-Qiao; Bai, Zhong-Rui; Deng, Li-Cai; Lei, Ya-Juan</p> <p>2013-10-01</p> <p>Using a sky <span class="hlt">brightness</span> monitor at the Xinglong station of National Astronomical Observatories, Chinese Academy of Sciences, we collected data from 22 dark clear nights and 90 moon nights. We first measured the sky <span class="hlt">brightness</span> variation with time for dark nights and found a clear correlation between sky <span class="hlt">brightness</span> and human activity. Then with a modified sky <span class="hlt">brightness</span> model of moon nights and data from these nights, we derived the typical value for several important parameters in the model. With these results, we calculated the sky <span class="hlt">brightness</span> distribution under a given moon condition for the Xinglong station. Furthermore, we simulated the sky <span class="hlt">brightness</span> distribution of a moon night for a telescope with a 5° field of view (such as LAMOST). These simulations will be helpful for determining the limiting magnitude and exposure time, as well as planning the survey for LAMOST during moon nights.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014JEI....23b3011W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014JEI....23b3011W"><span>Color constancy using <span class="hlt">bright</span>-neutral pixels</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wang, Yanfang; Luo, Yupin</p> <p>2014-03-01</p> <p>An effective illuminant-estimation approach for color constancy is proposed. <span class="hlt">Bright</span> and near-neutral pixels are selected to jointly represent the illuminant color and utilized for illuminant estimation. To assess the representing capability of pixels, <span class="hlt">bright</span>-neutral strength (BNS) is proposed by combining pixel chroma and <span class="hlt">brightness</span>. Accordingly, a certain percentage of pixels with the largest BNS is selected to be the representative set. For every input image, a proper percentage value is determined via an iterative strategy by seeking the optimal color-corrected image. To compare various color-corrected images of an input image, image color-cast degree (ICCD) is devised using means and standard deviations of RGB channels. Experimental evaluation on standard real-world datasets validates the effectiveness of the proposed approach.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20040112701&hterms=pacemaker&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dpacemaker','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20040112701&hterms=pacemaker&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dpacemaker"><span>Dynamic resetting of the human circadian pacemaker by intermittent <span class="hlt">bright</span> light</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Rimmer, D. W.; Boivin, D. B.; Shanahan, T. L.; Kronauer, R. E.; Duffy, J. F.; Czeisler, C. A.</p> <p>2000-01-01</p> <p>In humans, experimental studies of circadian resetting typically have been limited to lengthy episodes of exposure to continuous <span class="hlt">bright</span> light. To evaluate the time course of the human endogenous circadian pacemaker's resetting response to brief episodes of intermittent <span class="hlt">bright</span> light, we studied 16 subjects assigned to one of two intermittent lighting conditions in which the subjects were presented with intermittent episodes of <span class="hlt">bright</span>-light exposure at 25- or 90-min intervals. The effective duration of <span class="hlt">bright</span>-light exposure was 31% or 63% compared with a continuous 5-h <span class="hlt">bright</span>-light stimulus. Exposure to intermittent <span class="hlt">bright</span> light elicited almost as great a resetting response compared with 5 h of continuous <span class="hlt">bright</span> light. We conclude that exposure to intermittent <span class="hlt">bright</span> light produces robust phase shifts of the endogenous circadian pacemaker. Furthermore, these results demonstrate that humans, like other species, exhibit an enhanced sensitivity to the initial minutes of <span class="hlt">bright</span>-light exposure.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/19547213','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/19547213"><span>Dark-<span class="hlt">bright</span> soliton pairs in nonlocal nonlinear media.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Lin, Yuan Yao; Lee, Ray-Kuang</p> <p>2007-07-09</p> <p>We study the formation of dark-<span class="hlt">bright</span> vector soliton pairs in nonlocal Kerr-type nonlinear medium. We show, by analytical analysis and direct numerical calculation, that in addition to stabilize of vector soliton pairs nonlocal nonlinearity also helps to reduce the threshold power for forming a guided <span class="hlt">bright</span> soliton. With help of the nonlocality, it is expected that the observation of dark-<span class="hlt">bright</span> vector soliton pairs in experiments becomes more workable.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013SPIE.9044E..0YH','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013SPIE.9044E..0YH"><span>Detection of latent fingerprints by <span class="hlt">ultraviolet</span> spectral imaging</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Huang, Wei; Xu, Xiaojing; Wang, Guiqiang</p> <p>2013-12-01</p> <p>Spectral imaging technology research is becoming more popular in the field of forensic science. <span class="hlt">Ultraviolet</span> spectral imaging technology is an especial part of the full spectrum of imaging technology. This paper finished the experiment contents of the <span class="hlt">ultraviolet</span> spectrum imaging method and image acquisition system based on <span class="hlt">ultraviolet</span> spectral imaging technology. <span class="hlt">Ultraviolet</span> spectral imaging experiments explores a wide variety of <span class="hlt">ultraviolet</span> reflectance spectra of the object material curve and its <span class="hlt">ultraviolet</span> spectrum of imaging modalities, can not only gives a reference for choosing <span class="hlt">ultraviolet</span> wavelength to show the object surface potential traces of substances, but also gives important data for the <span class="hlt">ultraviolet</span> spectrum of imaging technology development.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19740005323','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19740005323"><span>Transmitting and reflecting diffuser. [for <span class="hlt">ultraviolet</span> light</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Keafer, L. S., Jr.; Burcher, E. E.; Kopia, L. P. (Inventor)</p> <p>1973-01-01</p> <p>A near-Lambertian diffuser is described which transmits and reflects <span class="hlt">ultraviolet</span> light. An <span class="hlt">ultraviolet</span> grade fused silica substrate is coated with vaporized fuse silica. The coating thickness is controlled, one thickness causing <span class="hlt">ultraviolet</span> light to diffuse and another thickness causing <span class="hlt">ultraviolet</span> light to reflect a near Lambertian pattern.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19930007840','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19930007840"><span>International <span class="hlt">Ultraviolet</span> Explorer (IUE)</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Boehm, Karl-Heinz</p> <p>1992-01-01</p> <p>The observation, data reduction, and interpretation of <span class="hlt">ultraviolet</span> spectra (obtained with the International <span class="hlt">Ultraviolet</span> Explorer) of Herbig-Haro objects, stellar jets, and (in a few cases) reflection nebulae in star-forming regions is discussed. Intermediate results have been reported in the required semi-annual reports. The observations for this research were obtained in 23 (US1) IUE shifts. The spectra were taken in the low resolution mode with the large aperture. The following topics were investigated: (1) detection of UV spectra of high excitation Herbig-Haro (HH) objects, identification of emission lines, and a preliminary study of the energy distribution of the <span class="hlt">ultraviolet</span> continuum; (2) details of the continuum energy distribution of these spectra and their possible interpretation; (3) the properties of the reddening (extinction) of HH objects; (4) the possible time variation of strong emission lines in high excitation HH objects; (5) the <span class="hlt">ultraviolet</span> emission of low excitation HH objects, especially in the fluorescent lines of the H2 molecule; (6) the <span class="hlt">ultraviolet</span> emission in the peculiar object HH24; (7) the spatial emission distribution of different lines and different parts of the continuum in different HH objects; and (8) some properties of reflection nebula, in the environment of Herbig-Haro objects. Each topic is discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014SPIE.9286E..0NL','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014SPIE.9286E..0NL"><span>Design of high-<span class="hlt">brightness</span> TEM00-mode solar-pumped laser for renewable material processing</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Liang, D.; Almeida, J.</p> <p>2014-08-01</p> <p>The conversion of sunlight into laser light by direct solar pumping is of ever-increasing importance because broadband, temporally constant, sunlight is converted into laser light, which can be a source of narrowband, collimated, rapidly pulsed, radiation with the possibility of obtaining extremely high <span class="hlt">brightness</span> and intensity. Nonlinear processes, such as harmonic generation, might be used to obtain broad wavelength coverage, including the <span class="hlt">ultraviolet</span> wavelengths, where the solar flux is very weak. The direct excitation of large lasers by sunlight offers the prospect of a drastic reduction in the cost of coherent optical radiation for high average power materials processing. This renewable laser has a large potential for many applications such as high-temperature materials processing, renewable magnesium-hydrogen energy cycle and so on. We propose here a scalable TEM00 mode solar laser pumping scheme, which is composed of four firststage 1.13 m diameter Fresnel lenses with its respective folding mirrors mounted on a two-axis automatic solar tracker. Concentrated solar power at the four focal spots of these Fresnel lenses are focused individually along a common 3.5 mm diameter, 70 mm length Nd:YAG rod via four pairs of second-stage fused-silica spherical lenses and third-stage 2D-CPCs (Compound Parabolic Concentrator), sitting just above the laser rod which is also double-pass pumped by four V-shaped pumping cavities. Distilled water cools both the rod and the concentrators. 15.4 W TEM00 solar laser power is numerically calculated, corresponding to 6.7 times enhancement in laser beam <span class="hlt">brightness</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018ATel11615....1F','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018ATel11615....1F"><span><span class="hlt">Bright</span> ZTF transients</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Fremling, C.; Kulkarni, S. R.; Taggart, K.; Perley, D.</p> <p>2018-05-01</p> <p>As a part of ongoing commissioning of the Zwicky Transient Facility (ZTF; ATel #11266) Alert Infrastructure, here we report <span class="hlt">bright</span> probable supernovae identified in the raw alert stream resulting from the public ZTF Northern Sky Survey ("Celestial Cinematagrophy"; see Bellm & Kulkarni, Nature Astronomy 1, 71, 2017).</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_7");'>7</a></li> <li><a href="#" onclick='return showDiv("page_8");'>8</a></li> <li class="active"><span>9</span></li> <li><a href="#" onclick='return showDiv("page_10");'>10</a></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_9 --> <div id="page_10" 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_8");'>8</a></li> <li><a href="#" onclick='return showDiv("page_9");'>9</a></li> <li class="active"><span>10</span></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li><a href="#" onclick='return showDiv("page_12");'>12</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="181"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017JInst..12P1006G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017JInst..12P1006G"><span>Absolute sensitivity calibration of an extreme <span class="hlt">ultraviolet</span> spectrometer for tokamak measurements</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Guirlet, R.; Schwob, J. L.; Meyer, O.; Vartanian, S.</p> <p>2017-01-01</p> <p>An extreme <span class="hlt">ultraviolet</span> spectrometer installed on the Tore Supra tokamak has been calibrated in absolute units of <span class="hlt">brightness</span> in the range 10-340 Å. This has been performed by means of a combination of techniques. The range 10-113 Å was absolutely calibrated by using an ultrasoft-X ray source emitting six spectral lines in this range. The calibration transfer to the range 113-182 Å was performed using the spectral line intensity branching ratio method. The range 182-340 Å was calibrated thanks to radiative-collisional modelling of spectral line intensity ratios. The maximum sensitivity of the spectrometer was found to lie around 100 Å. Around this wavelength, the sensitivity is fairly flat in a 80 Å wide interval. The spatial variations of sensitivity along the detector assembly were also measured. The observed trend is related to the quantum efficiency decrease as the angle of the incoming photon trajectories becomes more grazing.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19930028539&hterms=r136a1&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dr136a1','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19930028539&hterms=r136a1&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dr136a1"><span>Astro-1 <span class="hlt">ultraviolet</span> imaging of the 30 Doradus and SN 1987A fields with the <span class="hlt">Ultraviolet</span> Imaging Telescope</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Cheng, Kwang-Ping; Michalitsianos, Andrew G.; Hintzen, Paul; Bohlin, Ralph C.; O'Connell, Robert W.; Cornett, Robert H.; Roberts, Morton S.; Smith, Andrew M.; Smith, Eric P.; Stecher, Theodore P.</p> <p>1992-01-01</p> <p>A preliminary analysis of <span class="hlt">Ultraviolet</span> Imaging Telescope (UIT) images in the 30 Doradus region is reported. Photometry was obtained for the 30 Doradus cluster and its UV-<span class="hlt">bright</span> core, R136, in various UIT bandpasses. It is found that about 14 percent of the total FUV light and about 16 percent of the total near-UV light of the 3-arcmin diameter 30 Doradus cluster originates from the region within 5 arcsec of R136. The UV magnitudes and colors of R136 and other known O and Wolf-Rayet WN stars in the same field were measured. The UIT data, combined with published observations at longer wavelengths, indicate that R136a1, the brightest component of R136, is not a supermassive stars. A qualitative comparison between the UIT images, Einstein X-ray data, IRAS HiRes images, and ground-based CCD images in forbidden O III 5007 A, H-alpha, B, R, U, and Stromgren u is performed. The extended diffuse UV feature detected in the UIT images is correlated with the IR structure seen in the IRAS 60-micron HiRes image, which suggests the existence of large amounts of widely distributed dust in this region.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1992ApJ...395L..29C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1992ApJ...395L..29C"><span>Astro-1 <span class="hlt">ultraviolet</span> imaging of the 30 Doradus and SN 1987A fields with the <span class="hlt">Ultraviolet</span> Imaging Telescope</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Cheng, Kwang-Ping; Michalitsianos, Andrew G.; Hintzen, Paul; Bohlin, Ralph C.; O'Connell, Robert W.; Cornett, Robert H.; Roberts, Morton S.; Smith, Andrew M.; Smith, Eric P.; Stecher, Theodore P.</p> <p>1992-08-01</p> <p>A preliminary analysis of <span class="hlt">Ultraviolet</span> Imaging Telescope (UIT) images in the 30 Doradus region is reported. Photometry was obtained for the 30 Doradus cluster and its UV-<span class="hlt">bright</span> core, R136, in various UIT bandpasses. It is found that about 14 percent of the total FUV light and about 16 percent of the total near-UV light of the 3-arcmin diameter 30 Doradus cluster originates from the region within 5 arcsec of R136. The UV magnitudes and colors of R136 and other known O and Wolf-Rayet WN stars in the same field were measured. The UIT data, combined with published observations at longer wavelengths, indicate that R136a1, the brightest component of R136, is not a supermassive stars. A qualitative comparison between the UIT images, Einstein X-ray data, IRAS HiRes images, and ground-based CCD images in forbidden O III 5007 A, H-alpha, B, R, U, and Stromgren u is performed. The extended diffuse UV feature detected in the UIT images is correlated with the IR structure seen in the IRAS 60-micron HiRes image, which suggests the existence of large amounts of widely distributed dust in this region.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://eric.ed.gov/?q=phi&pg=4&id=EJ838375','ERIC'); return false;" href="https://eric.ed.gov/?q=phi&pg=4&id=EJ838375"><span>Does Stevens's Power Law for <span class="hlt">Brightness</span> Extend to Perceptual <span class="hlt">Brightness</span> Averaging?</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>Bauer, Ben</p> <p>2009-01-01</p> <p>Stevens's power law ([Psi][infinity][Phi][beta]) captures the relationship between physical ([Phi]) and perceived ([Psi]) magnitude for many stimulus continua (e.g., luminance and <span class="hlt">brightness</span>, weight and heaviness, area and size). The exponent ([beta]) indicates whether perceptual magnitude grows more slowly than physical magnitude ([beta] less…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017NatAs...1..612S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017NatAs...1..612S"><span>The nature of solar <span class="hlt">brightness</span> variations</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Shapiro, A. I.; Solanki, S. K.; Krivova, N. A.; Cameron, R. H.; Yeo, K. L.; Schmutz, W. K.</p> <p>2017-09-01</p> <p>Determining the sources of solar <span class="hlt">brightness</span> variations1,2, often referred to as solar noise3, is important because solar noise limits the detection of solar oscillations3, is one of the drivers of the Earth's climate system4,5 and is a prototype of stellar variability6,7—an important limiting factor for the detection of extrasolar planets. Here, we model the magnetic contribution to solar <span class="hlt">brightness</span> variability using high-cadence8,9 observations from the Solar Dynamics Observatory (SDO) and the Spectral And Total Irradiance REconstruction (SATIRE)10,11 model. The <span class="hlt">brightness</span> variations caused by the constantly evolving cellular granulation pattern on the solar surface were computed with the Max Planck Institute for Solar System Research (MPS)/University of Chicago Radiative Magnetohydrodynamics (MURaM)12 code. We found that the surface magnetic field and granulation can together precisely explain solar noise (that is, solar variability excluding oscillations) on timescales from minutes to decades, accounting for all timescales that have so far been resolved or covered by irradiance measurements. We demonstrate that no other sources of variability are required to explain the data. Recent measurements of Sun-like stars by the COnvection ROtation and planetary Transits (CoRoT)13 and Kepler14 missions uncovered <span class="hlt">brightness</span> variations similar to that of the Sun, but with a much wider variety of patterns15. Our finding that solar <span class="hlt">brightness</span> variations can be replicated in detail with just two well-known sources will greatly simplify future modelling of existing CoRoT and Kepler as well as anticipated Transiting Exoplanet Survey Satellite16 and PLAnetary Transits and Oscillations of stars (PLATO)17 data.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016A%26A...589A..46S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016A%26A...589A..46S"><span>Are solar <span class="hlt">brightness</span> variations faculae- or spot-dominated?</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Shapiro, A. I.; Solanki, S. K.; Krivova, N. A.; Yeo, K. L.; Schmutz, W. K.</p> <p>2016-05-01</p> <p>Context. Regular spaceborne measurements have revealed that solar <span class="hlt">brightness</span> varies on multiple timescales, variations on timescales greater than a day being attributed to a surface magnetic field. Independently, ground-based and spaceborne measurements suggest that Sun-like stars show a similar, but significantly broader pattern of photometric variability. Aims: To understand whether the broader pattern of stellar variations is consistent with the solar paradigm, we assess relative contributions of faculae and spots to solar magnetically-driven <span class="hlt">brightness</span> variability. We investigate how the solar <span class="hlt">brightness</span> variability and its facular and spot contributions depend on the wavelength, timescale of variability, and position of the observer relative to the ecliptic plane. Methods: We performed calculations with the SATIRE model, which returns solar <span class="hlt">brightness</span> with daily cadence from solar disc area coverages of various magnetic features. We took coverages as seen by an Earth-based observer from full-disc SoHO/MDI and SDO/HMI data and projected them to mimic out-of-ecliptic viewing by an appropriate transformation. Results: Moving the observer away from the ecliptic plane increases the amplitude of 11-year variability as it would be seen in Strömgren (b + y)/2 photometry, but decreases the amplitude of the rotational <span class="hlt">brightness</span> variations as it would appear in Kepler and CoRoT passbands. The spot and facular contributions to the 11-year solar variability in the Strömgren (b + y)/2 photometry almost fully compensate each other so that the Sun appears anomalously quiet with respect to its stellar cohort. Such a compensation does not occur on the rotational timescale. Conclusions: The rotational solar <span class="hlt">brightness</span> variability as it would appear in the Kepler and CoRoT passbands from the ecliptic plane is spot-dominated, but the relative contribution of faculae increases for out-of-ecliptic viewing so that the apparent <span class="hlt">brightness</span> variations are faculae-dominated for</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20090017530&hterms=good+poster&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dgood%2Bposter','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20090017530&hterms=good+poster&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dgood%2Bposter"><span>Future Directions in <span class="hlt">Ultraviolet</span> Spectroscopy</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Sonneborn, George (Editor); Moos, Warren; VanSteenberg, Michael</p> <p>2009-01-01</p> <p>The 'Future Directions in <span class="hlt">Ultraviolet</span> Spectroscopy' conference was inspired by the accomplishments of the Far <span class="hlt">Ultraviolet</span> Spectroscopic Explorer (FUSE) Mission. The FUSE mission was launched in June 1999 and spent over eight years exploring the far-<span class="hlt">ultraviolet</span> universe, gathering over 64 million seconds of high-resolution spectral data on nearly 3000 astronomical targets. The goal of this conference was not only to celebrate the accomplishments of FUSE, but to look toward the future and understand the major scientific drivers for the <span class="hlt">ultraviolet</span> capabilities of the next generation fo space observatories. Invited speakers presented discussions based on measurements made by FUSE and other <span class="hlt">ultraviolet</span> instruments, assessed their connection with measurements made with other techniques and, where appropriate, discussed the implications of low-z measurements for high-z phenomena. In addition to the oral presentations, many participants presented poster papers. The breadth of these presentation made it clear that much good science is still in progress with FUSE data and that these result will continue to have relevance in many scientific areas.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA06483.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA06483.html"><span><span class="hlt">Ultraviolet</span> Enceladus</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2004-09-23</p> <p>Looking beyond Saturn's south pole, this was the Cassini spacecraft's view of the distant, icy moon Enceladus on July 28, 2004. The planet itself shows few obvious features at these <span class="hlt">ultraviolet</span> wavelengths, due to scattering of light by molecules of the gases high in the atmosphere. Enceladus is 499 kilometers (310 miles) wide. The image was taken with the Cassini spacecraft narrow angle camera at a distance of 7.4 million kilometers (4.6 million miles) from Saturn through a filter sensitive to <span class="hlt">ultraviolet</span> wavelengths of light. The image scale is 44 kilometers (27 miles) per pixel of Saturn. http://photojournal.jpl.nasa.gov/catalog/PIA06483</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/863021','DOE-PATENT-XML'); return false;" href="https://www.osti.gov/servlets/purl/863021"><span><span class="hlt">Ultraviolet</span> radiation induced discharge laser</span></a></p> <p><a target="_blank" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p>Gilson, Verle A.; Schriever, Richard L.; Shearer, James W.</p> <p>1978-01-01</p> <p>An <span class="hlt">ultraviolet</span> radiation source associated with a suitable cathode-anode electrode structure, disposed in a gas-filled cavity of a high pressure pulsed laser, such as a transverse electric atmosphere (TEA) laser, to achieve free electron production in the gas by photoelectric interaction between <span class="hlt">ultraviolet</span> radiation and the cathode prior to the gas-exciting cathode-to-anode electrical discharge, thereby providing volume ionization of the gas. The <span class="hlt">ultraviolet</span> radiation is produced by a light source or by a spark discharge.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA13301.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA13301.html"><span><span class="hlt">Bright</span> Lights, Green City</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2010-07-28</p> <p>Two extremely <span class="hlt">bright</span> stars illuminate a greenish mist in this image from the new GLIMPSE360 survey from NASA Spitzer Space Telescope. The fog is comprised of hydrogen and carbon compounds called polycyclic aromatic hydrocarbons.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015PASJ...67...40J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015PASJ...67...40J"><span>Relationship between extreme <span class="hlt">ultraviolet</span> microflares and small-scale magnetic fields in the quiet Sun</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jiang, Fayu; Zhang, Jun; Yang, Shuhong</p> <p>2015-06-01</p> <p>Microflares are small dynamic signatures observed in X-ray and extreme-<span class="hlt">ultraviolet</span> channels. Because of their impulsive emission enhancements and wide distribution, they are thought to be closely related to coronal heating. By using the high-resolution 171 Å images from the Atmospheric Imaging Assembly and the lines-of-sight magnetograms obtained by the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory, we trace 10794 microflares in a quiet region near the disk center with a field of view of 960″ × 1068″ during 24 hr. The microflares have an occurrence rate of 4.4 × 103 hr-1 extrapolated over the whole Sun. Their average <span class="hlt">brightness</span>, size, and lifetime are 1.7I0 (of the quiet Sun), 9.6 Mm2, and 3.6 min, respectively. There exists a mutual positive correlation between the microflares' <span class="hlt">brightness</span>, area, and lifetime. In general, the microflares distribute uniformly across the solar disk, but form network patterns locally, which are similar to and matched with the magnetic network structures. Typical cases show that the microflares prefer to occur in magnetic cancellation regions of network boundaries. We roughly calculate the upper limit of energy flux supplied by the microflares and find that the result is still a factor of ˜ 15 below the coronal heating requirement.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018AJ....155..104R','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018AJ....155..104R"><span>The Magellan Evolution of Galaxies Spectroscopic and <span class="hlt">Ultraviolet</span> Reference Atlas (MegaSaura). I. The Sample and the Spectra</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Rigby, J. R.; Bayliss, M. B.; Sharon, K.; Gladders, M. D.; Chisholm, J.; Dahle, H.; Johnson, T.; Paterno-Mahler, R.; Wuyts, E.; Kelson, D. D.</p> <p>2018-03-01</p> <p>We introduce Project MEGaSaURA: the Magellan Evolution of Galaxies Spectroscopic and <span class="hlt">Ultraviolet</span> Reference Atlas. MEGaSaURA comprises medium-resolution, rest-frame <span class="hlt">ultraviolet</span> spectroscopy of N = 15 <span class="hlt">bright</span> gravitationally lensed galaxies at redshifts of 1.68 < z < 3.6, obtained with the MagE spectrograph on the Magellan telescopes. The spectra cover the observed-frame wavelength range 3200 < λ o < 8280 Å the average spectral resolving power is R = 3300. The median spectrum has a signal-to-noise ratio (S/N) = 21 per resolution element at 5000 Å. As such, the MEGaSaURA spectra have superior S/N and wavelength coverage compared to what COS/HST provides for starburst galaxies in the local universe. This paper describes the sample, the observations, and the data reduction. We compare the measured redshifts for the stars, the ionized gas as traced by nebular lines, and the neutral gas as traced by absorption lines; we find the expected bulk outflow of the neutral gas, and no systemic offset between the redshifts measured from nebular lines and the redshifts measured from the stellar continuum. We provide the MEGaSaURA spectra to the astronomical community through a data release.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22370436-investigation-moving-structures-coronal-bright-point','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22370436-investigation-moving-structures-coronal-bright-point"><span>Investigation of the moving structures in a coronal <span class="hlt">bright</span> point</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>Ning, Zongjun; Guo, Yang, E-mail: ningzongjun@pmo.ac.cn</p> <p>2014-10-10</p> <p>We have explored the moving structures in a coronal <span class="hlt">bright</span> point (CBP) observed by the Solar Dynamic Observatory Atmospheric Imaging Assembly (AIA) on 2011 March 5. This CBP event has a lifetime of ∼20 minutes and is <span class="hlt">bright</span> with a curved shape along a magnetic loop connecting a pair of negative and positive fields. AIA imaging observations show that a lot of <span class="hlt">bright</span> structures are moving intermittently along the loop legs toward the two footpoints from the CBP <span class="hlt">brightness</span> core. Such moving <span class="hlt">bright</span> structures are clearly seen at AIA 304 Å. In order to analyze their features, the CBP ismore » cut along the motion direction with a curved slit which is wide enough to cover the bulk of the CBP. After integrating the flux along the slit width, we get the spacetime slices at nine AIA wavelengths. The oblique streaks starting from the edge of the CBP <span class="hlt">brightness</span> core are identified as moving <span class="hlt">bright</span> structures, especially on the derivative images of the <span class="hlt">brightness</span> spacetime slices. They seem to originate from the same position near the loop top. We find that these oblique streaks are bi-directional, simultaneous, symmetrical, and periodic. The average speed is about 380 km s{sup –1}, and the period is typically between 80 and 100 s. Nonlinear force-free field extrapolation shows the possibility that magnetic reconnection takes place during the CBP, and our findings indicate that these moving <span class="hlt">bright</span> structures could be the observational outflows after magnetic reconnection in the CBP.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24787595','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24787595"><span>Zernike analysis of all-sky night <span class="hlt">brightness</span> maps.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Bará, Salvador; Nievas, Miguel; Sánchez de Miguel, Alejandro; Zamorano, Jaime</p> <p>2014-04-20</p> <p>All-sky night <span class="hlt">brightness</span> maps (calibrated images of the night sky with hemispherical field-of-view (FOV) taken at standard photometric bands) provide useful data to assess the light pollution levels at any ground site. We show that these maps can be efficiently described and analyzed using Zernike circle polynomials. The relevant image information can be compressed into a low-dimensional coefficients vector, giving an analytical expression for the sky <span class="hlt">brightness</span> and alleviating the effects of noise. Moreover, the Zernike expansions allow us to quantify in a straightforward way the average and zenithal sky <span class="hlt">brightness</span> and its variation across the FOV, providing a convenient framework to study the time course of these magnitudes. We apply this framework to analyze the results of a one-year campaign of night sky <span class="hlt">brightness</span> measurements made at the UCM observatory in Madrid.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2003ChPhy..12.1124L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2003ChPhy..12.1124L"><span>Self-deflection of a <span class="hlt">bright</span> soliton in a separate <span class="hlt">bright</span>-dark spatial soliton pair based on a higher-order space charge field</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Liu, Jin-Song; Hao, Zhong-Hua</p> <p>2003-10-01</p> <p>The self-deflection of a <span class="hlt">bright</span> solitary beam can be controlled by a dark solitary beam via a parametric coupling effect between the <span class="hlt">bright</span> and dark solitary beams in a separate <span class="hlt">bright</span>-dark spatial soliton pair supported by an unbiased series photorefractive crystal circuit. The spatial shift of the <span class="hlt">bright</span> solitary beam centre as a function of the input intensity of the dark solitary beam (hat rho) is investigated by taking into account the higher-order space charge field in the dynamics of the <span class="hlt">bright</span> solitary beam via both numerical and perturbation methods under steady-state conditions. The deflection amount (Deltas0), defined as the value of the spatial shift at the output surface of the crystal, is a monotonic and nonlinear function of hat rho. When hat rho is weak or strong enough, Deltas0 is, in fact, unchanged with hat rho, whereas Deltas0 increases or decreases monotonically with hat rho in a middle range of hat rho. The corresponding variation range (deltas) depends strongly on the value of the input intensity of the <span class="hlt">bright</span> solitary beam (r). There are some peak and valley values in the curve of deltas versus r under some conditions. When hat rho increases, the <span class="hlt">bright</span> solitary beam can scan toward both the direction same as and opposite to the crystal's c-axis. Whether the direction is the same as or opposite to the c-axis depends on the parameter values and configuration of the crystal circuit, as well as the value of r. Some potential applications are discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017RAA....17...37R','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017RAA....17...37R"><span>Spatial Model of Sky <span class="hlt">Brightness</span> Magnitude in Langkawi Island, Malaysia</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Redzuan Tahar, Mohammad; Kamarudin, Farahana; Umar, Roslan; Khairul Amri Kamarudin, Mohd; Sabri, Nor Hazmin; Ahmad, Karzaman; Rahim, Sobri Abdul; Sharul Aikal Baharim, Mohd</p> <p>2017-03-01</p> <p>Sky <span class="hlt">brightness</span> is an essential topic in the field of astronomy, especially for optical astronomical observations that need very clear and dark sky conditions. This study presents the spatial model of sky <span class="hlt">brightness</span> magnitude in Langkawi Island, Malaysia. Two types of Sky Quality Meter (SQM) manufactured by Unihedron are used to measure the sky <span class="hlt">brightness</span> on a moonless night (or when the Moon is below the horizon), when the sky is cloudless and the locations are at least 100 m from the nearest light source. The selected locations are marked by their GPS coordinates. The sky <span class="hlt">brightness</span> data obtained in this study were interpolated and analyzed using a Geographic Information System (GIS), thus producing a spatial model of sky <span class="hlt">brightness</span> that clearly shows the dark and <span class="hlt">bright</span> sky areas in Langkawi Island. Surprisingly, our results show the existence of a few dark sites nearby areas of high human activity. The sky <span class="hlt">brightness</span> of 21.45 mag arcsec{}-2 in the Johnson-Cousins V-band, as the average of sky <span class="hlt">brightness</span> equivalent to 2.8 × {10}-4{cd} {{{m}}}-2 over the entire island, is an indication that the island is, overall, still relatively dark. However, the amount of development taking place might reduce the number in the near future as the island is famous as a holiday destination.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA15454.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA15454.html"><span>Apparent <span class="hlt">Brightness</span> and Topography Images of Vibidia Crater</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2012-03-09</p> <p>The left-hand image from NASA Dawn spacecraft shows the apparent <span class="hlt">brightness</span> of asteroid Vesta surface. The right-hand image is based on this apparent <span class="hlt">brightness</span> image, with a color-coded height representation of the topography overlain onto it.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/16661893','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/16661893"><span>Inhibition of seagrass photosynthesis by <span class="hlt">ultraviolet</span>-B radiation.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Trocine, R P; Rice, J D; Wells, G N</p> <p>1981-07-01</p> <p>Effects of <span class="hlt">ultraviolet</span>-B radiation on the photosynthesis of seagrasses (Halophila engelmanni Aschers, Halodule wrightii Aschers, and Syringodium filiforme Kütz) were examined. The intrinsic tolerance of each seagrass to <span class="hlt">ultraviolet</span>-B, the presence and effectiveness of photorepair mechanisms to <span class="hlt">ultraviolet</span>-B-induced photosynthetic inhibition, and the role of epiphytic growth as a shield from <span class="hlt">ultraviolet</span>-B were investigated.Halodule was found to possess the greatest photosynthetic tolerance for <span class="hlt">ultraviolet</span>-B. Photosynthesis in Syringodium was slightly more sensitive to <span class="hlt">ultraviolet</span>-B while Halophila showed relatively little photosynthetic tolerance. Evidence for a photorepair mechanism was found only in Halodule. This mechanism effectively attenuated photosynthetic inhibition induced by <span class="hlt">ultraviolet</span>-B dose rates and dosages in excess of natural conditions. Syringodium appeared to rely primarily on a thick epidermal cell layer to reduce photosynthetic damage. Halophila seemed to have no morphological or photorepair capabilities to deal with <span class="hlt">ultraviolet</span>-B. This species appeared to rely on epiphytic and detrital shielding and the shade provided by other seagrasses to reduce <span class="hlt">ultraviolet</span>-B irradiation to tolerable levels. The presence of epiphytes on leaf surfaces was found to reduce the extent of photosynthetic inhibition from <span class="hlt">ultraviolet</span>-B exposure in all species.Observations obtained in this study seem to suggest the possibility of anthocyanin and/or other flavonoid synthesis as an adaptation to long term <span class="hlt">ultraviolet</span>-B irradiation by these species. In addition, Halophila appears to obtain an increased photosynthetic tolerance to <span class="hlt">ultraviolet</span>-B as an indirect benefit of chloroplast clumping to avoid photo-oxidation by intense levels of photosynthetically active radiation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/6120647-inhibition-seagrass-photosynthesis-ultraviolet-radiation','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/6120647-inhibition-seagrass-photosynthesis-ultraviolet-radiation"><span>Inhibition of seagrass photosynthesis by <span class="hlt">ultraviolet</span>-B radiation</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>Trocine, R.P.; Rice, J.D.; Wells, G.N.</p> <p>1981-07-01</p> <p>Effects of <span class="hlt">ultraviolet</span>-B radiation on the photosynthesis of seagrasses (Halophila engelmanni Aschers, Halodule wrightii Aschers, and Syringodium filiforme (Kuetz) were examined. The intrinsic tolerance of each seagrass to <span class="hlt">ultraviolet</span>-B, the presence and effectiveness of photorepair mechanisms to <span class="hlt">ultraviolet</span>-B-induced photosynthetic inhibition, and the role of epiphytic growth as a shield from <span class="hlt">ultraviolet</span>-B were investigated. Halodule was found to possess the greatest photosynthetic tolerance for <span class="hlt">ultraviolet</span>-B. Photosynthesis in Syringodium was slightly more sensitive to <span class="hlt">ultraviolet</span>-B while Halophila showed relatively little photosynthetic tolerance. Evidence for a photorepair mechanism was found only in Halodule. Syringodium appeared to rely primarily on a thick epidermal cellmore » layer to reduce photosynthetic damage. Halophila seemed to have no morphological or photorepair capabilities to deal with <span class="hlt">ultraviolet</span>-B. This species appeared to rely on epiphytic and detrital shielding and the shade provided by other seagrasses to reduce <span class="hlt">ultraviolet</span>-B irradiation to tolerable levels. The presence of epiphytes on leaf surfaces was found to reduce the extent of photosynthetic inhibition from <span class="hlt">ultraviolet</span>-B exposure in all species. Halophila appears to obtain an increased photosynthetic tolerance to <span class="hlt">ultraviolet</span>-B as an indirect benefit of chloroplast clumping to avoid photo-oxidation by intense levels of photosynthetically active radiation.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19840065159&hterms=active+site&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D80%26Ntt%3Dactive%2Bsite','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19840065159&hterms=active+site&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D80%26Ntt%3Dactive%2Bsite"><span>Frequent <span class="hlt">ultraviolet</span> brightenings observed in a solar active region with solar maximum mission</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Porter, J. G.; Toomre, J.; Gebbie, K. B.</p> <p>1984-01-01</p> <p>Observations of the temporal behavior of <span class="hlt">ultraviolet</span> emission from <span class="hlt">bright</span> points within an active region of the sun are reported. Frequent and rapid brightenings in Si IV and O IV line emission are seen. The observations suggest that intermittent heating events of modest amplitude are occurring at many sites within an active region. By selecting the brightest site at any given time within an active region and then sampling its behavior in detail within a 120 s interval, it is found that about two-thirds of the samples show variations of the Si IV line intensity. The brightenings typically last about 40-60 s; intensity increases of about 20-100 percent are frequently observed. The results suggest that heating due to magnetic field reconnection within an active region is proceeding almost stochastically. Events involving only a modest release of energy occur the most frequently.</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_8");'>8</a></li> <li><a href="#" onclick='return showDiv("page_9");'>9</a></li> <li class="active"><span>10</span></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li><a href="#" onclick='return showDiv("page_12");'>12</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_10 --> <div id="page_11" 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_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> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="201"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017MNRAS.469..267D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017MNRAS.469..267D"><span>Far-<span class="hlt">ultraviolet</span> observation of the globular cluster NGC 6397</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Dieball, A.; Rasekh, A.; Knigge, C.; Shara, M.; Zurek, D.</p> <p>2017-07-01</p> <p>We present an observational far-<span class="hlt">ultraviolet</span> (FUV) and near-<span class="hlt">ultraviolet</span> (NUV) study of the core region of the globular cluster (GC) NGC 6397. The observations were obtained with the Space Telescope Imaging Spectrograph (STIS, FUV) and the Wide Field Camera 3 (NUV) on board the Hubble Space Telescope. Here, we focus on the UV-<span class="hlt">bright</span> stellar populations such as blue stragglers (BSs), white dwarfs (WDs) and cataclysmic variables (CVs). We present the first FUV - NUV colour-magnitude diagram (CMD) for this cluster. To support our classification of the stellar populations, we compare our FUV - NUV CMD with optical data from the ACS Survey of Galactic Globular Clusters. The FUV - NUV CMD indicates 16 sources located in the WD area, and 10 BSs within the 25 × 25 arcsec2 of the STIS FUV data. 18 Chandra X-ray sources are located within the FUV field of view. 13 of those have an NUV counterpart, of which 9 sources also have an FUV counterpart. Out of those, five sources are previously suggested CVs, and indeed, all five are located in the WD/CV region in our FUV - NUV CMD. Another CV has only an FUV but no NUV counterpart. We also detect an NUV (but no FUV) counterpart to the millisecond pulsar (MSP) located in the core of this cluster. The NUV light curves of the CVs and MSP show flickering behaviour typical of CVs. We found that the BSs and CVs are the most centrally concentrated populations. This might be an effect of mass segregation or it might indicate the preferred birth place of BSs and CVs via dynamical interactions in the dense core region of GCs. Horizontal branch stars are the least centrally concentrated population and absent in the innermost area of the core.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19930000460&hterms=corona+discharge&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dcorona%2Bdischarge','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19930000460&hterms=corona+discharge&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dcorona%2Bdischarge"><span>Corona And <span class="hlt">Ultraviolet</span> Equipment For Testing Materials</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Laue, Eric G.</p> <p>1993-01-01</p> <p>Two assemblies of laboratory equipment developed for use in testing abilities of polymers, paints, and other materials to withstand <span class="hlt">ultraviolet</span> radiation and charged particles. One is vacuum <span class="hlt">ultraviolet</span> source built around commercial deuterium lamp. Other exposes specimen in partial vacuum to both <span class="hlt">ultraviolet</span> radiation and brush corona discharge. Either or both assemblies used separately or together to simulate approximately combination of solar radiation and charged particles encountered by materials aboard spacecraft in orbit around Earth. Also used to provide rigorous environmental tests of materials exposed to artificial <span class="hlt">ultraviolet</span> radiation and charged particles in industrial and scientific settings or to natural <span class="hlt">ultraviolet</span> radiation and charged particles aboard aircraft at high altitudes.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2000cucg.confE..25A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2000cucg.confE..25A"><span>The Coma Cluster Luminosity Function from <span class="hlt">Ultraviolet</span> to Near-Infrared</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Andreon, S.; Cuillandre, J.-C.; Pello, R.</p> <p></p> <p>The Coma cluster luminosity function (LF) from <span class="hlt">ultraviolet</span> (2000 AA ) to the near-infrared (H band) is summarized. In the UV the LF is very steep, much steeper than in the optical. The steep Coma UV LF implies that faint and <span class="hlt">bright</span> galaxies give similar contributions to the total UV flux and to the total metal production rate. The ComaUV LF is dominated in number and luminosity by blue galaxies, which are often faint in the optical. Therefore the Coma UV LF is dominated by star forming galaxies, not by massive and large galaxies. The optical Coma LF is relatively steep (alpha=-1.4) over the 11 magnitudes sampled, but its slope and shape depend on considered filter and magnitude. We found a clear steeping of the FL going from B to R bands, indicative of the presence of a large number of red dwarfs, as faint as three <span class="hlt">bright</span> globular clusters. Furthermore, using Hubble Space Telescope images, we discover that blends of globular clusters, not resolved in individual components due to seeing, look like dwarf galaxies when observed from the ground and are numerous and <span class="hlt">bright</span>. The existence of these fake extended sources increases the steepness of the LF at faint magnitudes, if not deal on. This concern affects previous deep probing of the luminosity function, but not the present work. The near-infrared LF wa s computed on a near-infrared selected sample of galaxies which photometry is complete down to the typical dwarf (M* +5) luminosity. The Coma LF can be described by a Schechter function with intermediate slope (alpha sim-1.3), plus a dip at MH~-22 mag. The shape of the Coma LF in H band is quite similar to th e one found in the B band. The similarity of the LF in the optical and H bands implies that in the central region of Coma there is no new population of galaxies which is too faint to be observed in the optical band (because dust enshrouded, for instance), down to the magnitudes of dwarfs. The exponential cut of the LF at the <span class="hlt">bright</span> end is in good agreement with</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19830010947','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19830010947"><span>Polymerizable <span class="hlt">ultraviolet</span> stabilizers for outdoor use</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Vogl, O.</p> <p>1982-01-01</p> <p>Polymeric materials that are stable enough to use outdoors without changes in excess of 20 years are investigated. <span class="hlt">Ultraviolet</span> stabilizers or plastic materials were synthesized, polymerizable <span class="hlt">ultraviolet</span> stabilizers, particularly of the 2(2-hydroxyphenyl)2H-benzotriazole family were prepared their polymerization, copolymerization and grafting onto other polymers were demonstrated, and <span class="hlt">ultraviolet</span> stabilizing systems were devised. These materials were evaluated from the photophysical point of view.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017NatAs...1..823H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017NatAs...1..823H"><span>Stunningly <span class="hlt">bright</span> optical emission</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Heinke, Craig O.</p> <p>2017-12-01</p> <p>The detection of <span class="hlt">bright</span>, rapid optical pulsations from pulsar PSR J1023+0038 have provided a surprise for researchers working on neutron stars. This discovery poses more questions than it answers and will spur on future work and instrumentation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012PlST...14..353Y','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012PlST...14..353Y"><span>Mutagenesis of Trichoderma Viride by <span class="hlt">Ultraviolet</span> and Plasma</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Yao, Risheng; Li, Manman; Deng, Shengsong; Hu, Huajia; Wang, Huai; Li, Fenghe</p> <p>2012-04-01</p> <p>Considering the importance of a microbial strain capable of increased cellulase production, a mutant strain UP4 of Trichoderma viride was developed by <span class="hlt">ultraviolet</span> (UV) and plasma mutation. The mutant produced a 21.0 IU/mL FPase which was 98.1% higher than that of the parent strain Trichoderma viride ZY-1. In addition, the effect of <span class="hlt">ultraviolet</span> and plasma mutagenesis was not merely simple superimposition of single <span class="hlt">ultraviolet</span> mutation and single plasma mutation. Meanwhile, there appeared a capsule around some of the spores after the <span class="hlt">ultraviolet</span> and plasma treatment, namely, the spore surface of the strain became fuzzy after <span class="hlt">ultraviolet</span> or <span class="hlt">ultraviolet</span> and plasma mutagenesis.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28612080','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28612080"><span>Color and emotion: effects of hue, saturation, and <span class="hlt">brightness</span>.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Wilms, Lisa; Oberfeld, Daniel</p> <p>2017-06-13</p> <p>Previous studies on emotional effects of color often failed to control all the three perceptual dimensions of color: hue, saturation, and <span class="hlt">brightness</span>. Here, we presented a three-dimensional space of chromatic colors by independently varying hue (blue, green, red), saturation (low, medium, high), and <span class="hlt">brightness</span> (dark, medium, <span class="hlt">bright</span>) in a factorial design. The 27 chromatic colors, plus 3 <span class="hlt">brightness</span>-matched achromatic colors, were presented via an LED display. Participants (N = 62) viewed each color for 30 s and then rated their current emotional state (valence and arousal). Skin conductance and heart rate were measured continuously. The emotion ratings showed that saturated and <span class="hlt">bright</span> colors were associated with higher arousal. The hue also had a significant effect on arousal, which increased from blue and green to red. The ratings of valence were the highest for saturated and <span class="hlt">bright</span> colors, and also depended on the hue. Several interaction effects of the three color dimensions were observed for both arousal and valence. For instance, the valence ratings were higher for blue than for the remaining hues, but only for highly saturated colors. Saturated and <span class="hlt">bright</span> colors caused significantly stronger skin conductance responses. Achromatic colors resulted in a short-term deceleration in the heart rate, while chromatic colors caused an acceleration. The results confirm that color stimuli have effects on the emotional state of the observer. These effects are not only determined by the hue of a color, as is often assumed, but by all the three color dimensions as well as their interactions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27835724','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27835724"><span>A Systematic Review of <span class="hlt">Bright</span> Light Therapy for Eating Disorders.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Beauchamp, Marshall T; Lundgren, Jennifer D</p> <p>2016-10-27</p> <p><span class="hlt">Bright</span> light therapy is a noninvasive biological intervention for disorders with nonnormative circadian features. Eating disorders, particularly those with binge-eating and night-eating features, have documented nonnormative circadian eating and mood patterns, suggesting that <span class="hlt">bright</span> light therapy may be an efficacious stand-alone or adjunctive intervention. The purpose of this systematic literature review, using PRISMA (Preferred Reporting Items for Systematic Reviews and Meta-Analyses) guidelines, was (1) to evaluate the state of the empirical treatment outcome literature on <span class="hlt">bright</span> light therapy for eating disorders and (2) to explore the timing of eating behavior, mood, and sleep-related symptom change so as to understand potential mechanisms of <span class="hlt">bright</span> light therapy action in the context of eating disorder treatment. A comprehensive literature search using PsycInfo and PubMed/MEDLINE was conducted in April 2016 with no date restrictions to identify studies published using <span class="hlt">bright</span> light therapy as a treatment for eating disorders. Keywords included combinations of terms describing disordered eating (eating disorder, anorexia nervosa, bulimia nervosa, binge eating, binge, eating behavior, eating, and night eating) and the use of <span class="hlt">bright</span> light therapy (<span class="hlt">bright</span> light therapy, light therapy, phototherapy). After excluding duplicates, 34 articles were reviewed for inclusion. 14 published studies of <span class="hlt">bright</span> light therapy for eating disorders met inclusion criteria (included participants with an eating disorder/disordered-eating behaviors; presented as a case study, case series, open-label clinical trial, or randomized/nonrandomized controlled trial; written in English; and published and available by the time of manuscript review). Results suggest that <span class="hlt">bright</span> light therapy is potentially effective at improving both disordered-eating behavior and mood acutely, although the timing of symptom response and the duration of treatment effects remain unknown. Future research should</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/17990214','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/17990214"><span><span class="hlt">Bright</span> light and thermoregulatory responses to exercise.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Atkinson, G; Barr, D; Chester, N; Drust, B; Gregson, W; Reilly, T; Waterhouse, J</p> <p>2008-03-01</p> <p>The thermoregulatory responses to morning exercise after exposure to different schedules of <span class="hlt">bright</span> light were examined. At 07:00 h, six males ran on two occasions in an environmental chamber (temperature = 31.4 +/- 1.0 degrees C, humidity = 66 +/- 6 %) for 40 min at 60 % of maximal oxygen uptake. Participants were exposed to <span class="hlt">bright</span> light (10,000 lux) either between 22:00 - 23:00 h (BT (low)) or 06:00 - 07:00 h (BT (high)). Otherwise, participants remained in dim light (< 50 lux). It was hypothesized that BT (low) attenuates core temperature during morning exercise via the phase-delaying properties of evening <span class="hlt">bright</span> light and by avoiding <span class="hlt">bright</span> light in the morning. Evening <span class="hlt">bright</span> light in BT (low) suppressed (p = 0.037) the increase in melatonin compared to dim light (1.1 +/- 11.4 vs. 15.2 +/- 19.7 pg x ml (-1)) and delayed (p = 0.034) the core temperature minimum by 1.46 +/- 1.24 h. Core temperature was 0.20 +/- 0.17 degrees C lower in BT (low) compared to BT (high) during the hour before exercise (p = 0.036), with evidence (p = 0.075) that this difference was maintained during exercise. Conversely, mean skin temperature was 1.0 +/- 1.7 degrees C higher during the first 10 min of exercise in BT (low) than in BT (high) (p = 0.030). There was evidence that the increase in perceived exertion was attenuated in BT (low) (p = 0.056). A chronobiologically-based light schedule can lower core temperature before and during morning exercise in hot conditions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=PIA00348&hterms=asphalt&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dasphalt','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=PIA00348&hterms=asphalt&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dasphalt"><span>Iapetus <span class="hlt">Bright</span> and Dark Terrains</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>1990-01-01</p> <p>Saturn's outermost large moon, Iapetus, has a <span class="hlt">bright</span>, heavily cratered icy terrain and a dark terrain, as shown in this Voyager 2 image taken on August 22, 1981. Amazingly, the dark material covers precisely the side of Iapetus that leads in the direction of orbital motion around Saturn (except for the poles), whereas the <span class="hlt">bright</span> material occurs on the trailing hemisphere and at the poles. The <span class="hlt">bright</span> terrain is made of dirty ice, and the dark terrain is surfaced by carbonaceous molecules, according to measurements made with Earth-based telescopes. Iapetus' dark hemisphere has been likened to tar or asphalt and is so dark that no details within this terrain were visible to Voyager 2. The <span class="hlt">bright</span> icy hemisphere, likened to dirty snow, shows many large impact craters. The closest approach by Voyager 2 to Iapetus was a relatively distant 600,000 miles, so that our best images, such as this, have a resolution of about 12 miles. The dark material is made of organic substances, probably including poisonous cyano compounds such as frozen hydrogen cyanide polymers. Though we know a little about the dark terrain's chemical nature, we do not understand its origin. Two theories have been developed, but neither is fully satisfactory--(1) the dark material may be organic dust knocked off the small neighboring satellite Phoebe and 'painted' onto the leading side of Iapetus as the dust spirals toward Saturn and Iapetus hurtles through the tenuous dust cloud, or (2) the dark material may be made of icy-cold carbonaceous 'cryovolcanic' lavas that were erupted from Iapetus' interior and then blackened by solar radiation, charged particles, and cosmic rays. A determination of the actual cause, as well as discovery of any other geologic features smaller than 12 miles across, awaits the Cassini Saturn orbiter to arrive in 2004.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2009SPIE.7495E..48H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2009SPIE.7495E..48H"><span>Automatic <span class="hlt">brightness</span> control of laser spot vision inspection system</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Han, Yang; Zhang, Zhaoxia; Chen, Xiaodong; Yu, Daoyin</p> <p>2009-10-01</p> <p>The laser spot detection system aims to locate the center of the laser spot after long-distance transmission. The accuracy of positioning laser spot center depends very much on the system's ability to control <span class="hlt">brightness</span>. In this paper, an automatic <span class="hlt">brightness</span> control system with high-performance is designed using the device of FPGA. The <span class="hlt">brightness</span> is controlled by combination of auto aperture (video driver) and adaptive exposure algorithm, and clear images with proper exposure are obtained under different conditions of illumination. Automatic <span class="hlt">brightness</span> control system creates favorable conditions for positioning of the laser spot center later, and experiment results illuminate the measurement accuracy of the system has been effectively guaranteed. The average error of the spot center is within 0.5mm.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20120002989','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20120002989"><span>Visible Color and Photometry of <span class="hlt">Bright</span> Materials on Vesta</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Schroder, S. E.; Li, J. Y.; Mittlefehldt, D. W.; Pieters, C. M.; De Sanctis, M. C.; Hiesinger, H.; Blewett, D. T.; Russell, C. T.; Raymond, C. A.; Keller, H. U.</p> <p>2012-01-01</p> <p>The Dawn Framing Camera (FC) collected images of the surface of Vesta at a pixel scale of 70 m in the High Altitude Mapping Orbit (HAMO) phase through its clear and seven color filters spanning from 430 nm to 980 nm. The surface of Vesta displays a large diversity in its <span class="hlt">brightness</span> and colors, evidently related to the diverse geology [1] and mineralogy [2]. Here we report a detailed investigation of the visible colors and photometric properties of the apparently <span class="hlt">bright</span> materials on Vesta in order to study their origin. The global distribution and the spectroscopy of <span class="hlt">bright</span> materials are discussed in companion papers [3, 4], and the synthesis results about the origin of Vestan <span class="hlt">bright</span> materials are reported in [5].</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017AGUFM.P23D2780A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017AGUFM.P23D2780A"><span>Emirates Mars <span class="hlt">Ultraviolet</span> Spectrometer's (EMUS) Prediction of Oxygen OI 135.6 nm and CO 4PG Emissions in the Martian Atmosphere</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Almatroushi, H. R.; Lootah, F. H.; Deighan, J.; Fillingim, M. O.; Jain, S.; Bougher, S. W.; England, S.; Schneider, N. M.</p> <p>2017-12-01</p> <p>This research focuses on developing empirical and theoretical models for OI 135.6 nm and CO 4PG band system FUV dayglow emissions in the Martian thermosphere as predicted to be seen from the Emirates Mars <span class="hlt">Ultraviolet</span> Spectrometer (EMUS), one of the three scientific instruments aboard the Emirates Mars Mission (EMM) to be launched in 2020. These models will aid in simulating accurate disk radiances which will be utilized as an input to an EMUS instrument simulator. The developed zonally averaged empirical models are based on FUV data from the IUVS instrument onboard the MAVEN mission, while the theoretical models are based on a basic Chapman profile. The models calculate the <span class="hlt">brightness</span> (B) of those emissions taking into consideration observation geometry parameters such as emission angle (EA), solar zenith angle (SZA) and planet distance from the sun (Ds). Specifically, the empirical models takes a general form of Bn=A*cos(SZA)n/cos(EA)m , where Bn is the normalized <span class="hlt">brightness</span> value of an emission feature, and A, n, and m are positive constant values. The model form shows that the <span class="hlt">brightness</span> has a positive correlation with EA and a negative correlation with SZA. A comparison of both models are explained in this research while examining full Mars and half Mars disk images generated using geometry code specially developed for the EMUS instrument. Sensitivity analyses have also been conducted for the theoretical modeling to observe the contributions of electron impact on atomic oxygen and CO2 to the <span class="hlt">brightness</span> of OI 135.6nm, in addition to the effect of electron temperature on the CO2± dissociative recombination contribution to the CO 4PG band system.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017NIMPA.865...95K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017NIMPA.865...95K"><span>Ultrashort high-<span class="hlt">brightness</span> pulses from storage rings</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Khan, Shaukat</p> <p>2017-09-01</p> <p>The <span class="hlt">brightness</span> of short-wavelength radiation from accelerator-based sources can be increased by coherent emission in which the radiation intensity scales with the number of contributing electrons squared. This requires a microbunched longitudinal electron distribution, which is the case in free-electron lasers. The <span class="hlt">brightness</span> of light sources based on electron storage rings was steadily improved, but could profit further from coherent emission. The modulation of the electron energy by a continuous-wave laser field may provide steady-state microbunching in the infrared regime. For shorter wavelengths, the energy modulation can be converted into a temporary density modulation by a dispersive chicane. One particular goal is coherent emission from a very short "slice" within an electron bunch in order to produce ultrashort radiation pulses with high <span class="hlt">brightness</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA12605.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA12605.html"><span><span class="hlt">Bright</span> Spokes, Dark Shadow</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2010-04-06</p> <p><span class="hlt">Bright</span> spokes and the shadow of a moon grace Saturn B ring in this NASA Cassini spacecraft image. Spokes are radial markings scientists continue to study, and they can be seen here stretching from the far left to upper right of the image.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20150002873','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20150002873"><span>Extremely Low Passive Microwave <span class="hlt">Brightness</span> Temperatures Due to Thunderstorms</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Cecil, Daniel J.</p> <p>2015-01-01</p> <p>Extreme events by their nature fall outside the bounds of routine experience. With imperfect or ambiguous measuring systems, it is appropriate to question whether an unusual measurement represents an extreme event or is the result of instrument errors or other sources of noise. About three weeks after the Tropical Rainfall Measuring Mission (TRMM) satellite began collecting data in Dec 1997, a thunderstorm was observed over northern Argentina with 85 GHz <span class="hlt">brightness</span> temperatures below 50 K and 37 GHz <span class="hlt">brightness</span> temperatures below 70 K (Zipser et al. 2006). These values are well below what had previously been observed from satellite sensors with lower resolution. The 37 GHz <span class="hlt">brightness</span> temperatures are also well below those measured by TRMM for any other storm in the subsequent 16 years. Without corroborating evidence, it would be natural to suspect a problem with the instrument, or perhaps an irregularity with the platform during the first weeks of the satellite mission. Automated quality control flags or other procedures in retrieval algorithms could treat these measurements as errors, because they fall outside the expected bounds. But the TRMM satellite also carries a radar and a lightning sensor, both confirming the presence of an intense thunderstorm. The radar recorded 40+ dBZ reflectivity up to about 19 km altitude. More than 200 lightning flashes per minute were recorded. That same storm's 19 GHz <span class="hlt">brightness</span> temperatures below 150 K would normally be interpreted as the result of a low-emissivity water surface (e.g., a lake, or flood waters) if not for the simultaneous measurements of such intense convection. This paper will examine records from TRMM and related satellite sensors including SSMI, AMSR-E, and the new GMI to find the strongest signatures resulting from thunderstorms, and distinguishing those from sources of noise. The lowest <span class="hlt">brightness</span> temperatures resulting from thunderstorms as seen by TRMM have been in Argentina in November and December. For</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20130013639','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20130013639"><span>The <span class="hlt">Ultraviolet</span> Radiation Environment around M Dwarf Exoplanet Host Stars</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>France, Kevin; Froning, Cynthia S.; Linsky, Jeffrey L.; Roberge, Aki; Stocke, John T.; Tian, Feng; Bushinsky, Rachel; Desert, Jean-Michel; Mauas, Pablo; Mauas, Pablo; <a style="text-decoration: none; " href="javascript:void(0); " onClick="displayelement('author_20130013639'); toggleEditAbsImage('author_20130013639_show'); toggleEditAbsImage('author_20130013639_hide'); "> <img style="display:inline; width:12px; height:12px; " src="images/arrow-up.gif" width="12" height="12" border="0" alt="hide" id="author_20130013639_show"> <img style="width:12px; height:12px; display:none; " src="images/arrow-down.gif" width="12" height="12" border="0" alt="hide" id="author_20130013639_hide"></p> <p>2013-01-01</p> <p>The spectral and temporal behavior of exoplanet host stars is a critical input to models of the chemistry and evolution of planetary atmospheres. <span class="hlt">Ultraviolet</span> photons influence the atmospheric temperature profiles and production of potential biomarkers on Earth-like planets around these stars. At present, little observational or theoretical basis exists for understanding the <span class="hlt">ultraviolet</span> spectra of M dwarfs, despite their critical importance to predicting and interpreting the spectra of potentially habitable planets as they are obtained in the coming decades. Using observations from the Hubble Space Telescope, we present a study of the UV radiation fields around nearby M dwarf planet hosts that covers both far-UV (FUV) and near-UV (NUV) wavelengths. The combined FUV+NUV spectra are publicly available in machine-readable format. We find that all six exoplanet host stars in our sample (GJ 581, GJ 876, GJ 436, GJ 832, GJ 667C, and GJ 1214) exhibit some level of chromospheric and transition region UV emission. No "UV-quiet" M dwarfs are observed. The <span class="hlt">bright</span> stellar Lyman-alpha emission lines are reconstructed, and we find that the Lyman-alpha line fluxes comprise approximately 37%-75% of the total 1150-3100 A flux from most M dwarfs; approximately greater than 10(exp3) times the solar value. We develop an empirical scaling relation between Lyman-alpha and Mg II emission, to be used when interstellar H I attenuation precludes the direct observation of Lyman-alpha. The intrinsic unreddened flux ratio is F(Lyman-alpha)/F(Mg II) = 10(exp3). The F(FUV)/F(NUV) flux ratio, a driver for abiotic production of the suggested biomarkers O2 and O3, is shown to be approximately 0.5-3 for all M dwarfs in our sample, greather than 10(exp3) times the solar ratio. For the four stars with moderate signal-to-noise Cosmic Origins Spectrograph time-resolved spectra, we find UV emission line variability with amplitudes of 50%.500% on 10(exp2)-10(exp3) s timescales. This effect should be taken</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20120013214','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20120013214"><span>Synthesizing SMOS Zero-Baselines with Aquarius <span class="hlt">Brightness</span> Temperature Simulator</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Colliander, A.; Dinnat, E.; Le Vine, D.; Kainulainen, J.</p> <p>2012-01-01</p> <p>SMOS [1] and Aquarius [2] are ESA and NASA missions, respectively, to make L-band measurements from the Low Earth Orbit. SMOS makes passive measurements whereas Aquarius measures both passive and active. SMOS was launched in November 2009 and Aquarius in June 2011.The scientific objectives of the missions are overlapping: both missions aim at mapping the global Sea Surface Salinity (SSS). Additionally, SMOS mission produces soil moisture product (however, Aquarius data will eventually be used for retrieving soil moisture too). The consistency of the <span class="hlt">brightness</span> temperature observations made by the two instruments is essential for long-term studies of SSS and soil moisture. For resolving the consistency, the calibration of the instruments is the key. The basis of the SMOS <span class="hlt">brightness</span> temperature level is the measurements performed with the so-called zero-baselines [3]; SMOS employs an interferometric measurement technique which forms a <span class="hlt">brightness</span> temperature image from several baselines constructed by combination of multiple receivers in an array; zero-length baseline defines the overall <span class="hlt">brightness</span> temperature level. The basis of the Aquarius <span class="hlt">brightness</span> temperature level is resolved from the <span class="hlt">brightness</span> temperature simulator combined with ancillary data such as antenna patterns and environmental models [4]. Consistency between the SMOS zero-baseline measurements and the simulator output would provide a robust basis for establishing the overall comparability of the missions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/26863420','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/26863420"><span>Music for a Brighter World: <span class="hlt">Brightness</span> Judgment Bias by Musical Emotion.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Bhattacharya, Joydeep; Lindsen, Job P</p> <p>2016-01-01</p> <p>A prevalent conceptual metaphor is the association of the concepts of good and evil with <span class="hlt">brightness</span> and darkness, respectively. Music cognition, like metaphor, is possibly embodied, yet no study has addressed the question whether musical emotion can modulate <span class="hlt">brightness</span> judgment in a metaphor consistent fashion. In three separate experiments, participants judged the <span class="hlt">brightness</span> of a grey square that was presented after a short excerpt of emotional music. The results of Experiment 1 showed that short musical excerpts are effective emotional primes that cross-modally influence <span class="hlt">brightness</span> judgment of visual stimuli. Grey squares were consistently judged as brighter after listening to music with a positive valence, as compared to music with a negative valence. The results of Experiment 2 revealed that the bias in <span class="hlt">brightness</span> judgment does not require an active evaluation of the emotional content of the music. By applying a different experimental procedure in Experiment 3, we showed that this <span class="hlt">brightness</span> judgment bias is indeed a robust effect. Altogether, our findings demonstrate a powerful role of musical emotion in biasing <span class="hlt">brightness</span> judgment and that this bias is aligned with the metaphor viewpoint.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018AcSpA.197..103T','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018AcSpA.197..103T"><span>Far-<span class="hlt">ultraviolet</span> spectral changes of titanium dioxide with gold nanoparticles by <span class="hlt">ultraviolet</span> and visible light</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Tanabe, Ichiro; Kurawaki, Yuji</p> <p>2018-05-01</p> <p>Attenuated total reflectance spectra including the far-<span class="hlt">ultraviolet</span> (FUV, ≤ 200 nm) region of titanium dioxide (TiO2) with and without gold (Au) nanoparticles were measured. A newly developed external light-irradiation system enabled to observe spectral changes of TiO2 with Au nanoparticles upon light irradiations. Absorption in the FUV region decreased and increased by the irradiation with <span class="hlt">ultraviolet</span> and visible light, respectively. These spectral changes may reflect photo-induced electron transfer from TiO2 to Au nanoparticles under <span class="hlt">ultraviolet</span> light and from Au nanoparticles to TiO2 under visible light, 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_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=3283774','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3283774"><span>Excitation Spectra and <span class="hlt">Brightness</span> Optimization of Two-Photon Excited Probes</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Mütze, Jörg; Iyer, Vijay; Macklin, John J.; Colonell, Jennifer; Karsh, Bill; Petrášek, Zdeněk; Schwille, Petra; Looger, Loren L.; Lavis, Luke D.; Harris, Timothy D.</p> <p>2012-01-01</p> <p>Two-photon probe excitation data are commonly presented as absorption cross section or molecular <span class="hlt">brightness</span> (the detected fluorescence rate per molecule). We report two-photon molecular <span class="hlt">brightness</span> spectra for a diverse set of organic and genetically encoded probes with an automated spectroscopic system based on fluorescence correlation spectroscopy. The two-photon action cross section can be extracted from molecular <span class="hlt">brightness</span> measurements at low excitation intensities, while peak molecular <span class="hlt">brightness</span> (the maximum molecular <span class="hlt">brightness</span> with increasing excitation intensity) is measured at higher intensities at which probe photophysical effects become significant. The spectral shape of these two parameters was similar across all dye families tested. Peak molecular <span class="hlt">brightness</span> spectra, which can be obtained rapidly and with reduced experimental complexity, can thus serve as a first-order approximation to cross-section spectra in determining optimal wavelengths for two-photon excitation, while providing additional information pertaining to probe photostability. The data shown should assist in probe choice and experimental design for multiphoton microscopy studies. Further, we show that, by the addition of a passive pulse splitter, nonlinear bleaching can be reduced—resulting in an enhancement of the fluorescence signal in fluorescence correlation spectroscopy by a factor of two. This increase in fluorescence signal, together with the observed resemblance of action cross section and peak <span class="hlt">brightness</span> spectra, suggests higher-order photobleaching pathways for two-photon excitation. PMID:22385865</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/11892755','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/11892755"><span>[<span class="hlt">Ultraviolet</span> radiation and long term space flight].</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Wu, H B; Su, S N; Ba, F S</p> <p>2000-08-01</p> <p>With the prolongation of space flight, influences of various aerospace environmental factors on the astronauts become more and more severe, while <span class="hlt">ultraviolet</span> radiation is lacking. Some studies indicated that low doses of <span class="hlt">ultraviolet</span> rays are useful and essential for human body. In space flight, <span class="hlt">ultraviolet</span> rays can improve the hygienic condition in the space cabin, enhance astronaut's working ability and resistance to unfavorable factors, prevent mineral metabolic disorders, cure purulent skin diseases and deallergize the allergens. So in long-term space flight, moderate amount of <span class="hlt">ultraviolet</span> rays in the space cabin would be beneficial.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017PASP..129c5003P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017PASP..129c5003P"><span>Night Sky <span class="hlt">Brightness</span> at San Pedro Martir Observatory</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Plauchu-Frayn, I.; Richer, M. G.; Colorado, E.; Herrera, J.; Córdova, A.; Ceseña, U.; Ávila, F.</p> <p>2017-03-01</p> <p>We present optical UBVRI zenith night sky <span class="hlt">brightness</span> measurements collected on 18 nights during 2013 to 2016 and SQM measurements obtained daily over 20 months during 2014 to 2016 at the Observatorio Astronómico Nacional on the Sierra San Pedro Mártir (OAN-SPM) in México. The UBVRI data is based upon CCD images obtained with the 0.84 m and 2.12 m telescopes, while the SQM data is obtained with a high-sensitivity, low-cost photometer. The typical moonless night sky <span class="hlt">brightness</span> at zenith averaged over the whole period is U = 22.68, B = 23.10, V = 21.84, R = 21.04, I = 19.36, and SQM = 21.88 {mag} {{arcsec}}-2, once corrected for zodiacal light. We find no seasonal variation of the night sky <span class="hlt">brightness</span> measured with the SQM. The typical night sky <span class="hlt">brightness</span> values found at OAN-SPM are similar to those reported for other astronomical dark sites at a similar phase of the solar cycle. We find a trend of decreasing night sky <span class="hlt">brightness</span> with decreasing solar activity during period of the observations. This trend implies that the sky has become darker by Δ U = 0.7, Δ B = 0.5, Δ V = 0.3, Δ R=0.5 mag arcsec-2 since early 2014 due to the present solar cycle.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19860055326&hterms=spectrophotometry&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3Dspectrophotometry','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19860055326&hterms=spectrophotometry&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3Dspectrophotometry"><span><span class="hlt">Ultraviolet</span> spectrophotometry of three LINERs</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Goodrich, R. W.; Keel, W. C.</p> <p>1986-01-01</p> <p>Three galaxies known to be LINERs were observed spectroscopically in the <span class="hlt">ultraviolet</span> in an attempt to detect the presumed nonthermal continuum source thought to be the source of photoionization in the nuclei. NGC 4501 was found to be too faint for study with the IUE spectrographs, while NGC 5005 had an extended <span class="hlt">ultraviolet</span> light profile. Comparison with the optical light profile of NGC 5005 indicates that the <span class="hlt">ultraviolet</span> source is distributed spatially in the same manner as the optical starlight, probably indicating that the <span class="hlt">ultraviolet</span> excess is due to a component of hot stars in the nucleus. These stars contribute detectable absorption features longward of 2500 A; together with optical data, the IUE spectra suggest a burst of star formation about 1 billion yr ago, with a lower rate continuing to produce a few OB stars. In NGC 4579, a point source contributing most of the <span class="hlt">ultraviolet</span> excess is found that is much different than the optical light distribution. Furthermore, the <span class="hlt">ultraviolet</span> to X-ray spectral index in NGC 4579 is 1.4, compatible with the UV to X-ray indices found for samples of Seyfert galaxies. This provides compelling evidence for the detection of the photoionizing continuum in NGC 4579 and draws the research fields of normal galaxies and active galactic nuclei closer together. The emission-line spectrum of NGC 4579 is compared with calculations from a photoionization code, CLOUDY, and several shock models. The photoionization code is found to give superior results, adding to the increasing weight of evidence that the LINER phenomenon is essentially a scaled-down version of the Seyfert phenomenon.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1990ApJ...363..422K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1990ApJ...363..422K"><span>Vacuum <span class="hlt">ultraviolet</span> imagery of the Virgo Cluster region. II - Total far-<span class="hlt">ultraviolet</span> flux of galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kodaira, K.; Watanabe, T.; Onaka, T.; Tanaka, W.</p> <p>1990-11-01</p> <p>The total flux in the far-<span class="hlt">ultraviolet</span> region around 150 nm was measured for more than 40 galaxies in the central region of the Virgo Cluster, using two imaging telescopes on board a sounding rocket. The observed far-<span class="hlt">ultraviolet</span> flux shows positive correlations with the H I 21 cm flux and the far-infrared flux for spiral galaxies, and with the X-ray flux and the radio continuum flux for elliptical galaxies. The former correlations of spiral galaxies are interpreted in terms of star formation activity, which indicates substantial depletion in the Virgo galaxies in accordance with the H I stripping. The latter correlations of elliptical galaxies indicate possible far-<span class="hlt">ultraviolet</span> sources of young population, in addition to evolved hot stars. Far-<span class="hlt">ultraviolet</span> fluxes from two dwarf elliptical galaxies were obtained tentatively, indicating star formation activity in elliptical galaxies. A high-resolution UV imagery by HST would be effective to distinguish the young population and the old population in elliptical galaxies.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3311899','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3311899"><span>Simultaneous <span class="hlt">brightness</span> contrast of foraging Papilio butterflies</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Kinoshita, Michiyo; Takahashi, Yuki; Arikawa, Kentaro</p> <p>2012-01-01</p> <p>This study focuses on the sense of <span class="hlt">brightness</span> in the foraging Japanese yellow swallowtail butterfly, Papilio xuthus. We presented two red discs of different intensity on a grey background to butterflies, and trained them to select one of the discs. They were successfully trained to select either a high intensity or a low intensity disc. The trained butterflies were tested on their ability to perceive <span class="hlt">brightness</span> in two different protocols: (i) two orange discs of different intensity presented on the same intensity grey background and (ii) two orange discs of the same intensity separately presented on a grey background that was either higher or lower in intensity than the training background. The butterflies trained to high intensity red selected the orange disc of high intensity in protocol 1, and the disc on the background of low intensity grey in protocol 2. We obtained similar results in another set of experiments with purple discs instead of orange discs. The choices of the butterflies trained to low intensity red were opposite to those just described. Taken together, we conclude that Papilio has the ability to learn <span class="hlt">brightness</span> and darkness of targets independent of colour, and that they have the so-called simultaneous <span class="hlt">brightness</span> contrast. PMID:22179808</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27043058','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27043058"><span><span class="hlt">Ultraviolet</span> safety assessments of insect light traps.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Sliney, David H; Gilbert, David W; Lyon, Terry</p> <p>2016-01-01</p> <p>Near-<span class="hlt">ultraviolet</span> (UV-A: 315-400 nm), "black-light," electric lamps were invented in 1935 and <span class="hlt">ultraviolet</span> insect light traps (ILTs) were introduced for use in agriculture around that time. Today ILTs are used indoors in several industries and in food-service as well as in outdoor settings. With recent interest in photobiological lamp safety, safety standards are being developed to test for potentially hazardous <span class="hlt">ultraviolet</span> emissions. A variety of UV "Black-light" ILTs were measured at a range of distances to assess potential exposures. Realistic time-weighted human exposures are shown to be well below current guidelines for human exposure to <span class="hlt">ultraviolet</span> radiation. These UV-A exposures would be far less than the typical UV-A exposure in the outdoor environment. Proposals are made for realistic <span class="hlt">ultraviolet</span> safety standards for ILT products.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22133973-far-ultraviolet-observations-spica-nebula-interaction-zone','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22133973-far-ultraviolet-observations-spica-nebula-interaction-zone"><span>FAR-<span class="hlt">ULTRAVIOLET</span> OBSERVATIONS OF THE SPICA NEBULA AND THE INTERACTION ZONE</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>Choi, Yeon-Ju; Min, Kyoung-Wook; Lim, Tae-Ho</p> <p>2013-09-01</p> <p>We report the analysis results of far-<span class="hlt">ultraviolet</span> (FUV) observations, made for a broad region around {alpha} Vir (Spica) including the interaction zone of Loop I and the Local Bubble. The whole region was optically thin and a general correlation was seen between the FUV continuum intensity and the dust extinction, except in the neighborhood of the <span class="hlt">bright</span> central star, indicating the dust scattering nature of the FUV continuum. We performed Monte Carlo radiative transfer simulations to obtain the optical parameters related to the dust scattering as well as to the geometrical structure of the region. The albedo and asymmetry factormore » were found to be 0.38 {+-} 0.06 and 0.46 {+-} 0.06, respectively, in good agreement with the Milky Way dust grain models. The distance to and the thickness of the interaction zone were estimated to be 70{sup +4}{sub -8} pc and 40{sup +8}{sub -10} pc, respectively. The diffuse FUV continuum in the northern region above Spica was mostly the result of scattering of the starlight from Spica, while that in the southern region was mainly due to the background stars. The C IV {lambda}{lambda}1548, 1551 emission was found throughout the whole region, in contrast to the Si II* {lambda}1532 emission which was <span class="hlt">bright</span> only within the H II region. This indicates that the C IV line arises mostly at the shell boundaries of the bubbles, with a larger portion likely from the Loop I than from the Local Bubble side, whereas the Si II* line is from the photoionized Spica Nebula.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA10374.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA10374.html"><span><span class="hlt">Ultraviolet</span> Extensions</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2008-04-16</p> <p>This <span class="hlt">ultraviolet</span> image from NASA Galaxy Evolution Explorer shows the Southern Pinwheel galaxy, also know as Messier 83 or M83. It is located 15 million light-years away in the southern constellation Hydra.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19890031691&hterms=bright+hour&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dbright%2Bhour','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19890031691&hterms=bright+hour&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dbright%2Bhour"><span>A study of coronal <span class="hlt">bright</span> points at 20 cm wavelength</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Nitta, N.; Kundu, M. R.</p> <p>1988-01-01</p> <p>The paper presents the results of a study of coronal <span class="hlt">bright</span> points observed at 20 cm with the VLA on a day when the sun was exceptionally quiet. Microwave maps of <span class="hlt">bright</span> points were obtained using data for the entire observing period of 5 hours, as well as for shorter periods of a few minutes. Most <span class="hlt">bright</span> points, especially those appearing in the full-period maps, appear to be associated with small bipolar structures on the photospheric magnetogram. Overlays of <span class="hlt">bright</span> point (BP) maps on the Ca(+) K picture, show that the brightest part of BP tends to lie on the boundary of a supergranulation network.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19990116038&hterms=EIT&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DEIT','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19990116038&hterms=EIT&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DEIT"><span>Micro Coronal <span class="hlt">Bright</span> Points Observed in the Quiet Magnetic Network by SOHO/EIT</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Falconer, D. A.; Moore, R. L.; Porter, J. G.</p> <p>1997-01-01</p> <p>When one looks at SOHO/EIT Fe XII images of quiet regions, one can see the conventional coronal <span class="hlt">bright</span> points (> 10 arcsec in diameter), but one will also notice many smaller faint enhancements in <span class="hlt">brightness</span> (Figure 1). Do these micro coronal <span class="hlt">bright</span> points belong to the same family as the conventional <span class="hlt">bright</span> points? To investigate this question we compared SOHO/EIT Fe XII images with Kitt Peak magnetograms to determine whether the micro <span class="hlt">bright</span> points are in the magnetic network and mark magnetic bipoles within the network. To identify the coronal <span class="hlt">bright</span> points, we applied a picture frame filter to the Fe XII images; this brings out the Fe XII network and <span class="hlt">bright</span> points (Figure 2) and allows us to study the <span class="hlt">bright</span> points down to the resolution limit of the SOHO/EIT instrument. This picture frame filter is a square smoothing function (hlargelyalf a network cell wide) with a central square (quarter of a network cell wide) removed so that a <span class="hlt">bright</span> point's intensity does not effect its own background. This smoothing function is applied to the full disk image. Then we divide the original image by the smoothed image to obtain our filtered image. A <span class="hlt">bright</span> point is defined as any contiguous set of pixels (including diagonally) which have enhancements of 30% or more above the background; a micro <span class="hlt">bright</span> point is any <span class="hlt">bright</span> point 16 pixels or smaller in size. We then analyzed the <span class="hlt">bright</span> points that were fully within quiet regions (0.6 x 0.6 solar radius) centered on disk center on six different days.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5228668','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5228668"><span>Life-threatening motor vehicle crashes in <span class="hlt">bright</span> sunlight</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Redelmeier, Donald A.; Raza, Sheharyar</p> <p>2017-01-01</p> <p>Abstract <span class="hlt">Bright</span> sunlight may create visual illusions that lead to driver error, including fallible distance judgment from aerial perspective. We tested whether the risk of a life-threatening motor vehicle crash was increased when driving in <span class="hlt">bright</span> sunlight. This longitudinal, case-only, paired-comparison analysis evaluated patients hospitalized because of a motor vehicle crash between January 1, 1995 and December 31, 2014. The relative risk of a crash associated with <span class="hlt">bright</span> sunlight was estimated by evaluating the prevailing weather at the time and place of the crash compared with the weather at the same hour and location on control days a week earlier and a week later. The majority of patients (n = 6962) were injured during daylight hours and <span class="hlt">bright</span> sunlight was the most common weather condition at the time and place of the crash. The risk of a life-threatening crash was 16% higher during <span class="hlt">bright</span> sunlight than normal weather (95% confidence interval: 9–24, P < 0.001). The increased risk was accentuated in the early afternoon, disappeared at night, extended to patients with different characteristics, involved crashes with diverse features, not apparent with cloudy weather, and contributed to about 5000 additional patient-days in hospital. The increased risk extended to patients with high crash severity as indicated by ambulance involvement, surgical procedures, length of hospital stay, intensive care unit admission, and patient mortality. The increased risk was not easily attributed to differences in alcohol consumption, driving distances, or anomalies of adverse weather. <span class="hlt">Bright</span> sunlight is associated with an increased risk of a life-threatening motor vehicle crash. An awareness of this risk might inform driver education, trauma staffing, and safety warnings to prevent a life-threatening motor vehicle crash. Level of evidence: Epidemiologic Study, level III. PMID:28072708</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28072708','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28072708"><span>Life-threatening motor vehicle crashes in <span class="hlt">bright</span> sunlight.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Redelmeier, Donald A; Raza, Sheharyar</p> <p>2017-01-01</p> <p><span class="hlt">Bright</span> sunlight may create visual illusions that lead to driver error, including fallible distance judgment from aerial perspective. We tested whether the risk of a life-threatening motor vehicle crash was increased when driving in <span class="hlt">bright</span> sunlight.This longitudinal, case-only, paired-comparison analysis evaluated patients hospitalized because of a motor vehicle crash between January 1, 1995 and December 31, 2014. The relative risk of a crash associated with <span class="hlt">bright</span> sunlight was estimated by evaluating the prevailing weather at the time and place of the crash compared with the weather at the same hour and location on control days a week earlier and a week later.The majority of patients (n = 6962) were injured during daylight hours and <span class="hlt">bright</span> sunlight was the most common weather condition at the time and place of the crash. The risk of a life-threatening crash was 16% higher during <span class="hlt">bright</span> sunlight than normal weather (95% confidence interval: 9-24, P < 0.001). The increased risk was accentuated in the early afternoon, disappeared at night, extended to patients with different characteristics, involved crashes with diverse features, not apparent with cloudy weather, and contributed to about 5000 additional patient-days in hospital. The increased risk extended to patients with high crash severity as indicated by ambulance involvement, surgical procedures, length of hospital stay, intensive care unit admission, and patient mortality. The increased risk was not easily attributed to differences in alcohol consumption, driving distances, or anomalies of adverse weather.<span class="hlt">Bright</span> sunlight is associated with an increased risk of a life-threatening motor vehicle crash. An awareness of this risk might inform driver education, trauma staffing, and safety warnings to prevent a life-threatening motor vehicle crash. Epidemiologic Study, level III.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4749205','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4749205"><span>Music for a Brighter World: <span class="hlt">Brightness</span> Judgment Bias by Musical Emotion</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>A prevalent conceptual metaphor is the association of the concepts of good and evil with <span class="hlt">brightness</span> and darkness, respectively. Music cognition, like metaphor, is possibly embodied, yet no study has addressed the question whether musical emotion can modulate <span class="hlt">brightness</span> judgment in a metaphor consistent fashion. In three separate experiments, participants judged the <span class="hlt">brightness</span> of a grey square that was presented after a short excerpt of emotional music. The results of Experiment 1 showed that short musical excerpts are effective emotional primes that cross-modally influence <span class="hlt">brightness</span> judgment of visual stimuli. Grey squares were consistently judged as brighter after listening to music with a positive valence, as compared to music with a negative valence. The results of Experiment 2 revealed that the bias in <span class="hlt">brightness</span> judgment does not require an active evaluation of the emotional content of the music. By applying a different experimental procedure in Experiment 3, we showed that this <span class="hlt">brightness</span> judgment bias is indeed a robust effect. Altogether, our findings demonstrate a powerful role of musical emotion in biasing <span class="hlt">brightness</span> judgment and that this bias is aligned with the metaphor viewpoint. PMID:26863420</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1994iue..prop.4856W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1994iue..prop.4856W"><span>Augmentation of the IUE <span class="hlt">Ultraviolet</span> Spectral Atlas</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wu, Chi-Chao</p> <p></p> <p>IUE is the only and last satellite which will support a survey program to record the <span class="hlt">ultraviolet</span> spectrum of a large number of <span class="hlt">bright</span> normal stars. It is important to have a library of high quality low dispersion spectra of sufficient number of stars that provide good coverage in spectral type and luminosity class. Such a library is invaluable for stellar population synthesis of galaxies, studying the nature of distant galaxies, establishing a UV spectral classification system, providing comparison stars for interstellar extinction studies and for peculiar objects or binary systems, studying the effects of temperature, gravity and metallicity on stellar UV spectra, and as a teaching aid. We propose to continue observations of normal stars in order to provide (1) a stellar library as complete as practical, which will be able to support astronomical research by the scientific community long into the future, and (2) a sufficient sample of stars to guard against variability and peculiarity, and to allow a finite range of temperature, gravity, and metallicity in a given spectral type-luminosity class combination. Our primary goal is to collect the data and make them available to the community immediately (without claiming the 6-month proprietary right). The data will be published in the IUE Newsletter as soon as practical, and the data will be prepared for distribution by the IUE Observatory and the NSSDC.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1991iue..prop.4056W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1991iue..prop.4056W"><span>Augmentation of the IUE <span class="hlt">Ultraviolet</span> Spectral Atlas</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wu, Chi-Chao</p> <p></p> <p>Most likely IUE is the only and last satellite which will support a survey program to record the <span class="hlt">ultraviolet</span> spectrum of a large number of <span class="hlt">bright</span> normal stars. It is important to have a library of high quality Low dispersion spectra of sufficient number of stars that provide good coverage in spectral type and luminosity class. Such a library is invaluable for stellar population synthesis of galaxies, studying the nature of distant galaxies, establishing a UV spectral classification system, providing comparison stars for interstellar extinction studies and for peculiar objects or binary systems, studying the effects of temperature, gravity and metallicity on stellar UV spectra, and as a teaching aid. We propose to continue observations of normal stars in order to provide (1) a more complete coverage of the spectral type and luminosity class, and (2) more than one star per spectral typeluminosity class combination to guard against variability and peculiarity, and to allow a finite range of temperature, gravity, and metallicity in a given combination. Our primary goal is to collect the data and make them available to the community immediately (without claiming the 6-month proprietary right). The data will be published in the IUE Newsletter as soon as practical, and the data will be prepared for distribution by the IUE Observatory and the NSSDC.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018eMetN...3...51K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018eMetN...3...51K"><span>Two <span class="hlt">bright</span> fireballs over Great Britain</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Koukal, Jakub; Káčerek, Richard</p> <p>2018-02-01</p> <p>On November 24, 2017 shortly before midnight and on November 25, 2017 shortly before sunrise, two very <span class="hlt">bright</span> fireballs lit up the sky over the United Kingdom. The UKMON (United Kingdom Meteor Observation Network) cameras and onboard cameras in the automobiles recorded their flight. The fireballs paths in the Earth's atmosphere were calculated, as well as the orbits of bodies in the Solar System. The flight of both bodies, the absolute magnitude of which approached the <span class="hlt">brightness</span> of the full Moon, was also observed by numerous random observers from the public in Great Britain, Ireland and France.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=425892','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=425892"><span>Inhibition of Seagrass Photosynthesis by <span class="hlt">Ultraviolet</span>-B Radiation 1</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Trocine, Robert P.; Rice, John D.; Wells, Gary N.</p> <p>1981-01-01</p> <p>Effects of <span class="hlt">ultraviolet</span>-B radiation on the photosynthesis of seagrasses (Halophila engelmanni Aschers, Halodule wrightii Aschers, and Syringodium filiforme Kütz) were examined. The intrinsic tolerance of each seagrass to <span class="hlt">ultraviolet</span>-B, the presence and effectiveness of photorepair mechanisms to <span class="hlt">ultraviolet</span>-B-induced photosynthetic inhibition, and the role of epiphytic growth as a shield from <span class="hlt">ultraviolet</span>-B were investigated. Halodule was found to possess the greatest photosynthetic tolerance for <span class="hlt">ultraviolet</span>-B. Photosynthesis in Syringodium was slightly more sensitive to <span class="hlt">ultraviolet</span>-B while Halophila showed relatively little photosynthetic tolerance. Evidence for a photorepair mechanism was found only in Halodule. This mechanism effectively attenuated photosynthetic inhibition induced by <span class="hlt">ultraviolet</span>-B dose rates and dosages in excess of natural conditions. Syringodium appeared to rely primarily on a thick epidermal cell layer to reduce photosynthetic damage. Halophila seemed to have no morphological or photorepair capabilities to deal with <span class="hlt">ultraviolet</span>-B. This species appeared to rely on epiphytic and detrital shielding and the shade provided by other seagrasses to reduce <span class="hlt">ultraviolet</span>-B irradiation to tolerable levels. The presence of epiphytes on leaf surfaces was found to reduce the extent of photosynthetic inhibition from <span class="hlt">ultraviolet</span>-B exposure in all species. Observations obtained in this study seem to suggest the possibility of anthocyanin and/or other flavonoid synthesis as an adaptation to long term <span class="hlt">ultraviolet</span>-B irradiation by these species. In addition, Halophila appears to obtain an increased photosynthetic tolerance to <span class="hlt">ultraviolet</span>-B as an indirect benefit of chloroplast clumping to avoid photo-oxidation by intense levels of photosynthetically active radiation. Images PMID:16661893</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/29133130','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/29133130"><span>Far-<span class="hlt">ultraviolet</span> spectral changes of titanium dioxide with gold nanoparticles by <span class="hlt">ultraviolet</span> and visible light.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Tanabe, Ichiro; Kurawaki, Yuji</p> <p>2018-05-15</p> <p>Attenuated total reflectance spectra including the far-<span class="hlt">ultraviolet</span> (FUV, ≤200nm) region of titanium dioxide (TiO 2 ) with and without gold (Au) nanoparticles were measured. A newly developed external light-irradiation system enabled to observe spectral changes of TiO 2 with Au nanoparticles upon light irradiations. Absorption in the FUV region decreased and increased by the irradiation with <span class="hlt">ultraviolet</span> and visible light, respectively. These spectral changes may reflect photo-induced electron transfer from TiO 2 to Au nanoparticles under <span class="hlt">ultraviolet</span> light and from Au nanoparticles to TiO 2 under visible light, respectively. Copyright © 2017 Elsevier B.V. All rights reserved.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016JPhCS.771a2033H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016JPhCS.771a2033H"><span>Sky <span class="hlt">brightness</span> and twilight measurements at Jogyakarta city, Indonesia</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Herdiwijaya, Dhani</p> <p>2016-11-01</p> <p>The sky <span class="hlt">brightness</span> measurements were performed using a portable photometer. A pocket-sized and low-cost photometer has 20 degree area measurement, and spectral ranges between 320-720 nm with output directly in magnitudes per arc second square (mass) unit. The sky <span class="hlt">brightness</span> with 3 seconds temporal resolutions was recorded at Jogyakarta city (110° 25’ E; 70° 52’ S; elevation 100 m) within 136 days in years from 2014 to 2016. The darkest night could reach 22.61 mpass only in several seconds, with mean value 18.8±0.7 mpass and temperature variation 23.1±1.2 C. The difference of mean sky <span class="hlt">brightness</span> between before and after midnight was about -0.76 mpass or 2.0 times brighter. Moreover, the sky <span class="hlt">brightness</span> and temperature fluctuations were more stable in after midnight than in before midnight. It is suggested that city light pollution affects those variations, and subsequently duration of twilight. By comparing twilight <span class="hlt">brightness</span> for several places, we also suggest a 17° solar dip or about 66 minutes before sunrise for new time of Fajr prayer.</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/2017ApJS..229...12K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017ApJS..229...12K"><span><span class="hlt">Brightness</span> of Solar Magnetic Elements As a Function of Magnetic Flux at High Spatial Resolution</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kahil, F.; Riethmüller, T. L.; Solanki, S. K.</p> <p>2017-03-01</p> <p>We investigate the relationship between the photospheric magnetic field of small-scale magnetic elements in the quiet-Sun (QS) at disk center and the <span class="hlt">brightness</span> at 214, 300, 313, 388, 397, and 525.02 nm. To this end, we analyzed spectropolarimetric and imaging time series acquired simultaneously by the Imaging Magnetograph eXperiment magnetograph and the SuFI filter imager on board the balloon-borne observatory {{S}}{{UNRISE}} during its first science flight in 2009, with high spatial and temporal resolution. We find a clear dependence of the contrast in the near <span class="hlt">ultraviolet</span> and the visible on the line-of-sight component of the magnetic field, B LOS, which is best described by a logarithmic model. This function effectively represents the relationship between the Ca II H-line emission and B LOS and works better than the power-law fit adopted by previous studies. This, along with the high contrast reached at these wavelengths, will help with determining the contribution of small-scale elements in the QS to the irradiance changes for wavelengths below 388 nm. At all wavelengths, including the continuum at 525.40 nm, the intensity contrast does not decrease with increasing B LOS. This result also strongly supports the fact that {{S}}{{UNRISE}} has resolved small strong magnetic field elements in the internetwork, resulting in constant contrasts for large magnetic fields in our continuum contrast at 525.40 nm versus the B LOS scatterplot, unlike the turnover obtained in previous observational studies. This turnover is due to the intermixing of the <span class="hlt">bright</span> magnetic features with the dark intergranular lanes surrounding them.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4867860','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4867860"><span><span class="hlt">Ultraviolet</span> safety assessments of insect light traps</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Sliney, David H.; Gilbert, David W.; Lyon, Terry</p> <p>2016-01-01</p> <p>ABSTRACT Near-<span class="hlt">ultraviolet</span> (UV-A: 315–400 nm), “black-light,” electric lamps were invented in 1935 and <span class="hlt">ultraviolet</span> insect light traps (ILTs) were introduced for use in agriculture around that time. Today ILTs are used indoors in several industries and in food-service as well as in outdoor settings. With recent interest in photobiological lamp safety, safety standards are being developed to test for potentially hazardous <span class="hlt">ultraviolet</span> emissions. A variety of UV “Black-light” ILTs were measured at a range of distances to assess potential exposures. Realistic time-weighted human exposures are shown to be well below current guidelines for human exposure to <span class="hlt">ultraviolet</span> radiation. These UV-A exposures would be far less than the typical UV-A exposure in the outdoor environment. Proposals are made for realistic <span class="hlt">ultraviolet</span> safety standards for ILT products. PMID:27043058</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28582774','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28582774"><span>A giant planet undergoing extreme-<span class="hlt">ultraviolet</span> irradiation by its hot massive-star host.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Gaudi, B Scott; Stassun, Keivan G; Collins, Karen A; Beatty, Thomas G; Zhou, George; Latham, David W; Bieryla, Allyson; Eastman, Jason D; Siverd, Robert J; Crepp, Justin R; Gonzales, Erica J; Stevens, Daniel J; Buchhave, Lars A; Pepper, Joshua; Johnson, Marshall C; Colon, Knicole D; Jensen, Eric L N; Rodriguez, Joseph E; Bozza, Valerio; Novati, Sebastiano Calchi; D'Ago, Giuseppe; Dumont, Mary T; Ellis, Tyler; Gaillard, Clement; Jang-Condell, Hannah; Kasper, David H; Fukui, Akihiko; Gregorio, Joao; Ito, Ayaka; Kielkopf, John F; Manner, Mark; Matt, Kyle; Narita, Norio; Oberst, Thomas E; Reed, Phillip A; Scarpetta, Gaetano; Stephens, Denice C; Yeigh, Rex R; Zambelli, Roberto; Fulton, B J; Howard, Andrew W; James, David J; Penny, Matthew; Bayliss, Daniel; Curtis, Ivan A; DePoy, D L; Esquerdo, Gilbert A; Gould, Andrew; Joner, Michael D; Kuhn, Rudolf B; Labadie-Bartz, Jonathan; Lund, Michael B; Marshall, Jennifer L; McLeod, Kim K; Pogge, Richard W; Relles, Howard; Stockdale, Christopher; Tan, T G; Trueblood, Mark; Trueblood, Patricia</p> <p>2017-06-22</p> <p>The amount of <span class="hlt">ultraviolet</span> irradiation and ablation experienced by a planet depends strongly on the temperature of its host star. Of the thousands of extrasolar planets now known, only six have been found that transit hot, A-type stars (with temperatures of 7,300-10,000 kelvin), and no planets are known to transit the even hotter B-type stars. For example, WASP-33 is an A-type star with a temperature of about 7,430 kelvin, which hosts the hottest known transiting planet, WASP-33b (ref. 1); the planet is itself as hot as a red dwarf star of type M (ref. 2). WASP-33b displays a large heat differential between its dayside and nightside, and is highly inflated-traits that have been linked to high insolation. However, even at the temperature of its dayside, its atmosphere probably resembles the molecule-dominated atmospheres of other planets and, given the level of <span class="hlt">ultraviolet</span> irradiation it experiences, its atmosphere is unlikely to be substantially ablated over the lifetime of its star. Here we report observations of the <span class="hlt">bright</span> star HD 195689 (also known as KELT-9), which reveal a close-in (orbital period of about 1.48 days) transiting giant planet, KELT-9b. At approximately 10,170 kelvin, the host star is at the dividing line between stars of type A and B, and we measure the dayside temperature of KELT-9b to be about 4,600 kelvin. This is as hot as stars of stellar type K4 (ref. 5). The molecules in K stars are entirely dissociated, and so the primary sources of opacity in the dayside atmosphere of KELT-9b are probably atomic metals. Furthermore, KELT-9b receives 700 times more extreme-<span class="hlt">ultraviolet</span> radiation (that is, with wavelengths shorter than 91.2 nanometres) than WASP-33b, leading to a predicted range of mass-loss rates that could leave the planet largely stripped of its envelope during the main-sequence lifetime of the host star.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/6773294','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/6773294"><span>Aqueous humour and <span class="hlt">ultraviolet</span> radiation.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Ringvold, A</p> <p>1980-01-01</p> <p>Studies on the <span class="hlt">ultraviolet</span> ray absorption in the aqueous humour of rabbit, cat, monkey, guinea pig, and rat showed marked species differences. In the rabbit aqueous the ascorbic acid, the proteins, and some amino acids (tyrosine, phenylalanine, cystine, and tryptophane) are together responsible for the total absorption, and a very great part of it refers to the ascorbic acid content. Accordingly, species with significant amounts of ascorbic acid in the aqueous (monkey, rabbit, guinea pig) have a greater absorption capacity towards <span class="hlt">ultraviolet</span> radiation than species (cat, rat) lacking this substance. This effect of the ascorbic acid may contribute in protecting the lens against the most biotoxic <span class="hlt">ultraviolet</span> rays. It seems that the ascorbic acid concentration is highest in the aqueous of typical day animals and lowest in species being active in the dark, indicating a correlation between the aqueous' ascorbic acid level and the quantity of incident light on the eye. The possible significance of changed aqueous <span class="hlt">ultraviolet</span> ray absorption in the pathogenesis of human cataract development is discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017SPIE10212E..0SQ','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017SPIE10212E..0SQ"><span>The <span class="hlt">ultraviolet</span> detection component based on Te-Cs image intensifier</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Qian, Yunsheng; Zhou, Xiaoyu; Wu, Yujing; Wang, Yan; Xu, Hua</p> <p>2017-05-01</p> <p><span class="hlt">Ultraviolet</span> detection technology has been widely focused and adopted in the fields of <span class="hlt">ultraviolet</span> warning and corona detection for its significant value and practical meaning. The component structure of <span class="hlt">ultraviolet</span> ICMOS, imaging driving and the photon counting algorithm are studied in this paper. Firstly, the one-inch and wide dynamic range CMOS chip with the coupling optical fiber panel is coupled to the <span class="hlt">ultraviolet</span> image intensifier. The photocathode material in <span class="hlt">ultraviolet</span> image intensifier is Te-Cs, which contributes to the solar blind characteristic, and the dual micro-channel plates (MCP) structure ensures the sufficient gain to achieve the single photon counting. Then, in consideration of the <span class="hlt">ultraviolet</span> detection demand, the drive circuit of the CMOS chip is designed and the corresponding program based on Verilog language is written. According to the characteristics of <span class="hlt">ultraviolet</span> imaging, the histogram equalization method is applied to enhance the <span class="hlt">ultraviolet</span> image and the connected components labeling way is utilized for the <span class="hlt">ultraviolet</span> single photon counting. Moreover, one visible light video channel is reserved in the <span class="hlt">ultraviolet</span> ICOMS camera, which can be used for the fusion of <span class="hlt">ultraviolet</span> and visible images. Based upon the module, the <span class="hlt">ultraviolet</span> optical lens and the deep cut-off solar blind filter are adopted to construct the <span class="hlt">ultraviolet</span> detector. At last, the detection experiment of the single photon signal is carried out, and the test results are given and analyzed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20110015533','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20110015533"><span><span class="hlt">Ultraviolet</span> Spectroscopy of Asteroid(4) Vesta</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Li, Jian-Yang; Bodewits, Dennis; Feaga, Lori M.; Landsman, Wayne; A'Hearn, Michael F.; Mutchler, Max J.; Russell, Christopher T.; McFadden, Lucy A.; Raymond, Carol A.</p> <p>2011-01-01</p> <p>We report a comprehensive review of the UV-visible spectrum and rotational lightcurve of Vesta combining new observations by Hubble Space Telescope and Swift with archival International <span class="hlt">Ultraviolet</span> Explorer observations. The geometric albedos of Vesta from 220 nm to 953 nm arc derived by carefully comparing these observations from various instruments at different times and observing geometries. Vesta has a rotationally averaged geometric albedo of 0.09 at 250 nm, 0.14 at 300 nm, 0.26 at 373 nm, 0.38 at 673 nm, and 0.30 at 950 nm. The linear spectral slope in the <span class="hlt">ultraviolet</span> displays a sharp minimum ncar sub-Earth longitude of 20deg, and maximum in the eastern hemisphere. This is completely consistent with the distribution of the spectral slope in the visible wavelength. The uncertainty of the measurement in the <span class="hlt">ultraviolet</span> is approx.20%, and in the visible wavelengths better than 10%. The amplitude of Vesta's rotational lightcurves is approx.10% throughout the range of wavelengths we observed, but is smaller at 950 nm (approx.6%) ncar the 1-micron mafic band center. Contrary to earlier reports, we found no evidence for any difference between the phasing of the <span class="hlt">ultraviolet</span> and visible/ncar-infrared lightcurves with respect to sub-Earth longitude. Vesta's average spectrum between 220 and 950 nm can well be described by measured reflectance spectra of fine particle howardite-like materials of basaltic achondrite meteorites. Combining this with the in-phase behavior of the <span class="hlt">ultraviolet</span>, visible. and ncar-infrared lightcurves, and the spectral slopes with respect to the rotational phase, we conclude that there is no global <span class="hlt">ultraviolet</span>/visible reversal on Vesta. Consequently, this implies lack of global space weathering on Vesta. Keyword,: Asteroid Vesta; Spectrophotometry; Spectroscopy; <span class="hlt">Ultraviolet</span> observations; Hubble Space Telescope observations</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012ApJ...760..108B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012ApJ...760..108B"><span>The Brightest of Reionizing Galaxies Survey: Constraints on the <span class="hlt">Bright</span> End of the z ~ 8 Luminosity Function</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Bradley, L. D.; Trenti, M.; Oesch, P. A.; Stiavelli, M.; Treu, T.; Bouwens, R. J.; Shull, J. M.; Holwerda, B. W.; Pirzkal, N.</p> <p>2012-12-01</p> <p>We report the discovery of 33 Lyman-break galaxy candidates at z ~ 8 detected in Hubble Space Telescope Wide Field Camera 3 (WFC3) imaging as part of the Brightest of Reionizing Galaxies (BoRG) pure-parallel survey. The ongoing BoRG survey currently has the largest area (274 arcmin2) with Y 098 (or Y 105), J 125, and H 160 band coverage needed to search for z ~ 8 galaxies, about three times the current CANDELS area, and slightly larger than what will be the final CANDELS wide component with Y 105 data (required to select z ~ 8 sources). Our sample of 33 relatively <span class="hlt">bright</span> Y 098-dropout galaxies have J 125-band magnitudes between 25.5 and 27.4 mag. This is the largest sample of <span class="hlt">bright</span> (J 125 <~ 27.4) z ~ 8 galaxy candidates presented to date. Combining our data set with the Hubble Ultra-Deep Field data set, we constrain the rest-frame <span class="hlt">ultraviolet</span> galaxy luminosity function at z ~ 8 over the widest dynamic range currently available. The combined data sets are well fitted by a Schechter function, i.e., \\phi (L) = \\phi _{*} (L/L_{*})^{\\alpha }\\ e^{-(L/L_{*})}, without evidence for an excess of sources at the <span class="hlt">bright</span> end. At 68% confidence, for h = 0.7 we derive phi* = (4.3+3.5 -2.1) × 10-4 Mpc-3, M * = -20.26+0.29 -0.34, and a very steep faint-end slope α = -1.98+0.23 -0.22. While the best-fit parameters still have a strong degeneracy, especially between phi* and M *, our improved coverage at the <span class="hlt">bright</span> end has reduced the uncertainty of the faint-end power-law slope at z ~ 8 compared to the best previous determination at ±0.4. With a future expansion of the BoRG survey, combined with planned ultradeep WFC3/IR observations, it will be possible to further reduce this uncertainty and clearly demonstrate the steepening of the faint-end slope compared to measurements at lower redshift, thereby confirming the key role played by small galaxies in the reionization of the universe. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19770034005&hterms=MOOS&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D80%26Ntt%3DMOOS','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19770034005&hterms=MOOS&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D80%26Ntt%3DMOOS"><span>The far <span class="hlt">ultraviolet</span> /1200-1900 A/ spectrum of Jupiter obtained with a rocket-borne multichannel spectrometer</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Giles, J. W.; Moos, H. W.; Mckinney, W. R.</p> <p>1976-01-01</p> <p>Far-<span class="hlt">ultraviolet</span> spectra of Jupiter with a significant improvement in sensitivity and spectral resolution have been obtained from a sounding rocket by using a 10-channel spectrometer behind a pointing telescope. The major results obtained from these spectra are: (1) measurement of the Jovian H I 1216-A <span class="hlt">brightness</span> (a comparison with other measurements indicates that the Ly-alpha emission is likely to be variable); (2) measurement of the wavelength-dependent albedo for Rayleigh-scattered solar radiation from about 1550 to 1875 A with approximately 25-A resolution, making it possible to set revised upper limits on the abundances of some of the minor constituents in the upper Jovian atmosphere; and (3) a demonstration that weak emissions between approximately 1250 and 1500 A and near 1600 A are probably the Lyman bands of H2 excited by low-energy electrons.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2006AAS...20915406C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2006AAS...20915406C"><span>A New Sky <span class="hlt">Brightness</span> Monitor</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Crawford, David L.; McKenna, D.</p> <p>2006-12-01</p> <p>A good estimate of sky <span class="hlt">brightness</span> and its variations throughout the night, the months, and even the years is an essential bit of knowledge both for good observing and especially as a tool in efforts to minimize sky <span class="hlt">brightness</span> through local action. Hence a stable and accurate monitor can be a valuable and necessary tool. We have developed such a monitor, with the financial help of Vatican Observatory and Walker Management. The device is now undergoing its Beta test in preparation for production. It is simple, accurate, well calibrated, and automatic, sending its data directly to IDA over the internet via E-mail . Approximately 50 such monitors will be ready soon for deployment worldwide including most major observatories. Those interested in having one should enquire of IDA about details.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24329024','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24329024"><span>Normal dimensions of the posterior pituitary <span class="hlt">bright</span> spot on magnetic resonance imaging.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Côté, Martin; Salzman, Karen L; Sorour, Mohammad; Couldwell, William T</p> <p>2014-02-01</p> <p>The normal pituitary <span class="hlt">bright</span> spot seen on unenhanced T1-weighted MRI is thought to result from the T1-shortening effect of the vasopressin stored in the posterior pituitary. Individual variations in its size may be difficult to differentiate from pathological conditions resulting in either absence of the pituitary <span class="hlt">bright</span> spot or in T1-hyperintense lesions of the sella. The objective of this paper was to define a range of normal dimensions of the pituitary <span class="hlt">bright</span> spot and to illustrate some of the most commonly encountered pathologies that result in absence or enlargement of the pituitary <span class="hlt">bright</span> spot. The authors selected normal pituitary MRI studies from 106 patients with no pituitary abnormality. The size of each pituitary <span class="hlt">bright</span> spot was measured in the longest axis and in the dimension perpendicular to this axis to describe the typical dimensions. The authors also present cases of patients with pituitary abnormalities to highlight the differences and potential overlap between normal and pathological pituitary imaging. All of the studies evaluated were found to have pituitary <span class="hlt">bright</span> spots, and the mean dimensions were 4.8 mm in the long axis and 2.4 mm in the short axis. The dimension of the pituitary <span class="hlt">bright</span> spot in the long axis decreased with patient age. The distribution of dimensions of the pituitary <span class="hlt">bright</span> spot was normal, indicating that 99.7% of patients should have a pituitary <span class="hlt">bright</span> spot measuring between 1.2 and 8.5 mm in its long axis and between 0.4 and 4.4 mm in its short axis, an interval corresponding to 3 standard deviations below and above the mean. In cases where the dimension of the pituitary <span class="hlt">bright</span> spot is outside this range, pathological conditions should be considered. The pituitary <span class="hlt">bright</span> spot should always be demonstrated on T1-weighted MRI, and its dimensions should be within the identified normal range in most patients. Outside of this range, pathological conditions affecting the pituitary <span class="hlt">bright</span> spot should be considered.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017RSPTA.37560202P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017RSPTA.37560202P"><span>Insights into the deactivation of 5-bromouracil after <span class="hlt">ultraviolet</span> excitation</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Peccati, Francesca; Mai, Sebastian; González, Leticia</p> <p>2017-03-01</p> <p>5-Bromouracil is a nucleobase analogue that can replace thymine in DNA strands and acts as a strong radiosensitizer, with potential applications in molecular biology and cancer therapy. Here, the deactivation of 5-bromouracil after <span class="hlt">ultraviolet</span> irradiation is investigated in the singlet and triplet manifold by accurate quantum chemistry calculations and non-adiabatic dynamics simulations. It is found that, after irradiation to the <span class="hlt">bright</span> ππ* state, three main relaxation pathways are, in principle, possible: relaxation back to the ground state, intersystem crossing (ISC) and C-Br photodissociation. Based on accurate MS-CASPT2 optimizations, we propose that ground-state relaxation should be the predominant deactivation pathway in the gas phase. We then employ different electronic structure methods to assess their suitability to carry out excited-state dynamics simulations. MRCIS (multi-reference configuration interaction including single excitations) was used in surface hopping simulations to compute the ultrafast ISC dynamics, which mostly involves the 1nOπ* and 3ππ* states. This article is part of the themed issue 'Theoretical and computational studies of non-equilibrium and non-statistical dynamics in the gas phase, in the condensed phase and at interfaces'.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5360901','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5360901"><span>Insights into the deactivation of 5-bromouracil after <span class="hlt">ultraviolet</span> excitation</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>2017-01-01</p> <p>5-Bromouracil is a nucleobase analogue that can replace thymine in DNA strands and acts as a strong radiosensitizer, with potential applications in molecular biology and cancer therapy. Here, the deactivation of 5-bromouracil after <span class="hlt">ultraviolet</span> irradiation is investigated in the singlet and triplet manifold by accurate quantum chemistry calculations and non-adiabatic dynamics simulations. It is found that, after irradiation to the <span class="hlt">bright</span> ππ* state, three main relaxation pathways are, in principle, possible: relaxation back to the ground state, intersystem crossing (ISC) and C–Br photodissociation. Based on accurate MS-CASPT2 optimizations, we propose that ground-state relaxation should be the predominant deactivation pathway in the gas phase. We then employ different electronic structure methods to assess their suitability to carry out excited-state dynamics simulations. MRCIS (multi-reference configuration interaction including single excitations) was used in surface hopping simulations to compute the ultrafast ISC dynamics, which mostly involves the 1nOπ* and 3ππ* states. This article is part of the themed issue ‘Theoretical and computational studies of non-equilibrium and non-statistical dynamics in the gas phase, in the condensed phase and at interfaces’. PMID:28320905</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22590800-nonthermal-combined-ultraviolet-vacuum-ultraviolet-curing-process-organosilicate-dielectrics','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22590800-nonthermal-combined-ultraviolet-vacuum-ultraviolet-curing-process-organosilicate-dielectrics"><span>Nonthermal combined <span class="hlt">ultraviolet</span> and vacuum-<span class="hlt">ultraviolet</span> curing process for organosilicate dielectrics</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>Zheng, H.; Guo, X.; Pei, D.</p> <p>2016-06-13</p> <p>Porous SiCOH films are of great interest in semiconductor fabrication due to their low-dielectric constant properties. Post-deposition treatments using <span class="hlt">ultraviolet</span> (UV) light on organosilicate thin films are required to decompose labile pore generators (porogens) and to ensure optimum network formation to improve the electrical and mechanical properties of low-k dielectrics. The goal of this work is to choose the best vacuum-<span class="hlt">ultraviolet</span> photon energy in conjunction with vacuum <span class="hlt">ultraviolet</span> (VUV) photons without the need for heating the dielectric to identify those wavelengths that will have the most beneficial effect on improving the dielectric properties and minimizing damage. VUV irradiation between 8.3more » and 8.9 eV was found to increase the hardness and elastic modulus of low-k dielectrics at room temperature. Combined with UV exposures of 6.2 eV, it was found that this “UV/VUV curing” process is improved compared with current UV curing. We show that UV/VUV curing can overcome drawbacks of UV curing and improve the properties of dielectrics more efficiently without the need for high-temperature heating of the dielectric.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/21196966','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/21196966"><span><span class="hlt">Brightness</span> field distributions of microlens arrays using micro molding.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Cheng, Hsin-Chung; Huang, Chiung-Fang; Lin, Yi; Shen, Yung-Kang</p> <p>2010-12-20</p> <p>This study describes the <span class="hlt">brightness</span> field distributions of microlens arrays fabricated by micro injection molding (μIM) and micro injection-compression molding (μICM). The process for fabricating microlens arrays used room-temperature imprint lithography, photoresist reflow, electroforming, μIM, μICM, and optical properties measurement. Analytical results indicate that the <span class="hlt">brightness</span> field distribution of the molded microlens arrays generated by μICM is better than those made using μIM. Our results further demonstrate that mold temperature is the most important processing parameter for <span class="hlt">brightness</span> field distribution of molded microlens arrays made by μIM or μICM.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://eric.ed.gov/?q=cross+AND+cultural+AND+social+AND+skills&pg=7&id=EJ777087','ERIC'); return false;" href="https://eric.ed.gov/?q=cross+AND+cultural+AND+social+AND+skills&pg=7&id=EJ777087"><span>Star<span class="hlt">Bright</span> Learning Exchange</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>Kalinowski, Michael</p> <p>2007-01-01</p> <p>This article features Star<span class="hlt">Bright</span> Learning Exchange, a program that provides a cross-cultural exchange between Australian and South African early childhood educators. The program was originated when its president, Carol Allen, and her colleague, Karen Williams, decided that they could no longer sit by and watch the unfolding social catastrophe that…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/1342752','SCIGOV-STC'); return false;" href="https://www.osti.gov/servlets/purl/1342752"><span>High <span class="hlt">Brightness</span> OLED Lighting</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>Spindler, Jeffrey; Kondakova, Marina; Boroson, Michael</p> <p>2016-05-25</p> <p>In this work we describe the technology developments behind our current and future generations of high <span class="hlt">brightness</span> OLED lighting panels. We have developed white and amber OLEDs with excellent performance based on the stacking approach. Current products achieve 40-60 lm/W, while future developments focus on achieving 80 lm/W or higher.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/29698847','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/29698847"><span>The universal and automatic association between <span class="hlt">brightness</span> and positivity.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Specker, Eva; Leder, Helmut; Rosenberg, Raphael; Hegelmaier, Lisa Mira; Brinkmann, Hanna; Mikuni, Jan; Kawabata, Hideaki</p> <p>2018-05-01</p> <p>The present study investigates the hypothesis that <span class="hlt">brightness</span> of colors is associated with positivity, postulating that this is an automatic and universal effect. The Implicit Association Test (IAT; Greenwald, McGhee, & Schwartz, 1998) was used in all studies. Study 1 used color patches varying on <span class="hlt">brightness</span>, Study 2 used achromatic stimuli to eliminate the potential confounding effects of hue and saturation. Study 3 replicated Study 2 in a different cultural context (Japan vs. Austria), both studies also included a measure of explicit association. All studies confirmed the hypothesis that <span class="hlt">brightness</span> is associated with positivity, at a significance level of p < .001 and Cohen's D varying from 0.90 to 3.99. Study 1-3 provided support for the notion that this is an automatic effect. Additionally, Study 2 and Study 3 showed that people also have an explicit association of <span class="hlt">brightness</span> with positivity. However, as expected, our results also show that the implicit association was stronger than the explicit association. Study 3 shows clear support for the universality of our effects. In sum, our results support the idea that <span class="hlt">brightness</span> is associated with positivity and that these associations are automatic and universal. Copyright © 2018 Elsevier B.V. All rights reserved.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018SPIE10621E..27P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018SPIE10621E..27P"><span>Evaluation and testing of image quality of the Space Solar Extreme <span class="hlt">Ultraviolet</span> Telescope</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Peng, Jilong; Yi, Zhong; Zhou, Shuhong; Yu, Qian; Hou, Yinlong; Wang, Shanshan</p> <p>2018-01-01</p> <p>For the space solar extreme <span class="hlt">ultraviolet</span> telescope, the star point test can not be performed in the x-ray band (19.5nm band) as there is not light source of <span class="hlt">bright</span> enough. In this paper, the point spread function of the optical system is calculated to evaluate the imaging performance of the telescope system. Combined with the actual processing surface error, such as small grinding head processing and magnetorheological processing, the optical design software Zemax and data analysis software Matlab are used to directly calculate the system point spread function of the space solar extreme <span class="hlt">ultraviolet</span> telescope. Matlab codes are programmed to generate the required surface error grid data. These surface error data is loaded to the specified surface of the telescope system by using the communication technique of DDE (Dynamic Data Exchange), which is used to connect Zemax and Matlab. As the different processing methods will lead to surface error with different size, distribution and spatial frequency, the impact of imaging is also different. Therefore, the characteristics of the surface error of different machining methods are studied. Combining with its position in the optical system and simulation its influence on the image quality, it is of great significance to reasonably choose the processing technology. Additionally, we have also analyzed the relationship between the surface error and the image quality evaluation. In order to ensure the final processing of the mirror to meet the requirements of the image quality, we should choose one or several methods to evaluate the surface error according to the different spatial frequency characteristics of the surface error.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19960001904','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19960001904"><span><span class="hlt">Ultraviolet</span> observations of the Saturnian north aurora and polar haze distribution with the HST-FOC</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Gerard, J. C.; Dols, V.; Grodent, D.; Waite, J. H.; Gladstone, G. R.; Prange, R.</p> <p>1995-01-01</p> <p>Near simultaneous observations of the Saturnian H2 north <span class="hlt">ultraviolet</span> aurora and the polar haze were made at 153 nm and 210 nm respectively with the Faint Object Camera on board the Hubble Space Telescope. The auroral observations cover a complete rotation of the planet and, when co-added, reveal the presence of an auroral emission near 80 deg N with a peak <span class="hlt">brightness</span> of about 150 kR of total H2 emission. The maximum optical depth of the polar haze layer is found to be located approximately 5 deg equatorward of the auroral emission zone. The haze particles are presumably formed by hydrocarbon aerosols initiated by H2+ auroral production. In this case, the observed haze optical depth requires an efficiency of aerosol formation of about 6 percent, indicating that auroral production of hydrocarbon aerosols is a viable source of high-latitude haze.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018NJPh...20c3009H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018NJPh...20c3009H"><span>Quantum noise in <span class="hlt">bright</span> soliton matterwave interferometry</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Haine, Simon A.</p> <p>2018-03-01</p> <p>There has been considerable recent interest in matterwave interferometry with <span class="hlt">bright</span> solitons in quantum gases with attractive interactions, for applications such as rotation sensing. We model the quantum dynamics of these systems and find that the attractive interactions required for the presence of <span class="hlt">bright</span> solitons causes quantum phase-diffusion, which severely impairs the sensitivity. We propose a scheme that partially restores the sensitivity, but find that in the case of rotation sensing, it is still better to work in a regime with minimal interactions if possible.</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('http://adsabs.harvard.edu/abs/2018AnPhy.390..180W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018AnPhy.390..180W"><span>Dynamics of <span class="hlt">bright-bright</span> solitons in Bose-Einstein condensate with Raman-induced one-dimensional spin-orbit coupling</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wen, Lin; Zhang, Xiao-Fei; Hu, Ai-Yuan; Zhou, Jing; Yu, Peng; Xia, Lei; Sun, Qing; Ji, An-Chun</p> <p>2018-03-01</p> <p>We investigate the dynamics of <span class="hlt">bright-bright</span> solitons in one-dimensional two-component Bose-Einstein condensates with Raman-induced spin-orbit coupling, via the variational approximation and the numerical simulation of Gross-Pitaevskii equations. For the uniform system without trapping potential, we obtain two population balanced stationary solitons. By performing the linear stability analysis, we find a Goldstone eigenmode and an oscillation eigenmode around these stationary solitons. Moreover, we derive a general dynamical solution to describe the center-of-mass motion and spin evolution of the solitons under the action of spin-orbit coupling. The effects of a harmonic trap have also been discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://pubs.er.usgs.gov/publication/70159370','USGSPUBS'); return false;" href="https://pubs.er.usgs.gov/publication/70159370"><span>The impact of bottom <span class="hlt">brightness</span> on spectral reflectance of suspended sediments</span></a></p> <p><a target="_blank" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p>Tolk, Brian L.; Han, L.; Rundquist, D. C.</p> <p>2000-01-01</p> <p>Two experiments were conducted outdoors to investigate how bottom <span class="hlt">brightness</span> impacts the spectral response of a water column under varied suspended sediment concentrations. A white aluminum panel placed at the bottom of the tank was used as the <span class="hlt">bright</span> bottom, and a flat-black tank liner served as the dark bottom. Sixteen levels of suspended sediment from 25 to 400 mg litre -1 were used in each experiment. Spectral data were collected using a Spectron SE-590 spectroradiometer. The major findings include the following: the <span class="hlt">bright</span> bottom had the greatest impact at visible wavelengths; when suspended sediment concentrations exceeded 100 mg litre -1, the <span class="hlt">bright</span> bottom response was found to be negligible; and, substrate <span class="hlt">brightness</span> has minimal impact between 740 and 900 nm, suggesting that these wavelengths are best for measuring suspended sediment concentrations by means of remote sensing.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018ApPhL.112o3106Z','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018ApPhL.112o3106Z"><span>Near unity <span class="hlt">ultraviolet</span> absorption in graphene without patterning</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Zhu, Jinfeng; Yan, Shuang; Feng, Naixing; Ye, Longfang; Ou, Jun-Yu; Liu, Qing Huo</p> <p>2018-04-01</p> <p>Enhancing the light-matter interaction of graphene is an important issue for related photonic devices and applications. In view of its potential <span class="hlt">ultraviolet</span> applications, we aim to achieve extremely high <span class="hlt">ultraviolet</span> absorption in graphene without any nanostructure or microstructure patterning. By manipulating the polarization and angle of incident light, the <span class="hlt">ultraviolet</span> power can be sufficiently coupled to the optical dissipation of graphene based on single-channel coherent perfect absorption in an optimized multilayered thin film structure. The <span class="hlt">ultraviolet</span> absorbance ratios of single and four atomic graphene layers are enhanced up to 71.4% and 92.2%, respectively. Our research provides a simple and efficient scheme to trap <span class="hlt">ultraviolet</span> light for developing promising photonic and optoelectronic devices based on graphene and potentially other 2D materials.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25620199','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25620199"><span>Phase advancing human circadian rhythms with morning <span class="hlt">bright</span> light, afternoon melatonin, and gradually shifted sleep: can we reduce morning <span class="hlt">bright</span>-light duration?</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Crowley, Stephanie J; Eastman, Charmane I</p> <p>2015-02-01</p> <p>Efficient treatments to phase-advance human circadian rhythms are needed to attenuate circadian misalignment and the associated negative health outcomes that accompany early-morning shift work, early school start times, jet lag, and delayed sleep phase disorder. This study compared three morning <span class="hlt">bright</span>-light exposure patterns from a single light box (to mimic home treatment) in combination with afternoon melatonin. Fifty adults (27 males) aged 25.9 ± 5.1 years participated. Sleep/dark was advanced 1 h/day for three treatment days. Participants took 0.5 mg of melatonin 5 h before the baseline bedtime on treatment day 1, and an hour earlier each treatment day. They were exposed to one of three <span class="hlt">bright</span>-light (~5000 lux) patterns upon waking each morning: four 30-min exposures separated by 30 min of room light (2-h group), four 15-min exposures separated by 45 min of room light (1-h group), and one 30-min exposure (0.5-h group). Dim-light melatonin onsets (DLMOs) before and after treatment determined the phase advance. Compared to the 2-h group (phase shift = 2.4 ± 0.8 h), smaller phase-advance shifts were seen in the 1-h (1.7 ± 0.7 h) and 0.5-h (1.8 ± 0.8 h) groups. The 2-h pattern produced the largest phase advance; however, the single 30-min <span class="hlt">bright</span>-light exposure was as effective as 1 h of <span class="hlt">bright</span> light spread over 3.25 h, and it produced 75% of the phase shift observed with 2 h of <span class="hlt">bright</span> light. A 30-min morning <span class="hlt">bright</span>-light exposure with afternoon melatonin is an efficient treatment to phase-advance human circadian rhythms. Copyright © 2014 Elsevier B.V. All rights reserved.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4344919','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4344919"><span>Phase advancing human circadian rhythms with morning <span class="hlt">bright</span> light, afternoon melatonin, and gradually shifted sleep: can we reduce morning <span class="hlt">bright</span> light duration?</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Crowley, Stephanie J.; Eastman, Charmane I.</p> <p>2015-01-01</p> <p>OBJECTIVE Efficient treatments to phase advance human circadian rhythms are needed to attenuate circadian misalignment and the associated negative health outcomes that accompany early morning shift work, early school start times, jet lag, and delayed sleep phase disorder. This study compared three morning <span class="hlt">bright</span> light exposure patterns from a single light box (to mimic home treatment) in combination with afternoon melatonin. METHODS Fifty adults (27 males) aged 25.9±5.1 years participated. Sleep/dark was advanced 1 hour/day for 3 treatment days. Participants took 0.5 mg melatonin 5 hours before baseline bedtime on treatment day 1, and an hour earlier each treatment day. They were exposed to one of three <span class="hlt">bright</span> light (~5000 lux) patterns upon waking each morning: four 30-minute exposures separated by 30 minutes of room light (2 h group); four 15-minute exposures separated by 45 minutes of room light (1 h group), and one 30-minute exposure (0.5 h group). Dim light melatonin onsets (DLMOs) before and after treatment determined the phase advance. RESULTS Compared to the 2 h group (phase shift=2.4±0.8 h), smaller phase advance shifts were seen in the 1 h (1.7±0.7 h) and 0.5 h (1.8±0.8 h) groups. The 2-hour pattern produced the largest phase advance; however, the single 30-minute <span class="hlt">bright</span> light exposure was as effective as 1 hour of <span class="hlt">bright</span> light spread over 3.25 h, and produced 75% of the phase shift observed with 2 hours of <span class="hlt">bright</span> light. CONCLUSIONS A 30-minute morning <span class="hlt">bright</span> light exposure with afternoon melatonin is an efficient treatment to phase advance human circadian rhythms. PMID:25620199</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010A%26A...519A..58T','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010A%26A...519A..58T"><span>Horizontal supergranule-scale motions inferred from TRACE <span class="hlt">ultraviolet</span> observations of the chromosphere</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Tian, H.; Potts, H. E.; Marsch, E.; Attie, R.; He, J.-S.</p> <p>2010-09-01</p> <p>Aims: We study horizontal supergranule-scale motions revealed by TRACE observation of the chromospheric emission, and investigate the coupling between the chromosphere and the underlying photosphere. Methods: A highly efficient feature-tracking technique called balltracking has been applied for the first time to the image sequences obtained by TRACE (transition region and coronal explorer) in the passband of white light and the three <span class="hlt">ultraviolet</span> passbands centered at 1700 Å, 1600 Å, and 1550 Å. The resulting velocity fields have been spatially smoothed and temporally averaged in order to reveal horizontal supergranule-scale motions that may exist at the emission heights of these passbands. Results: We find indeed a high correlation between the horizontal velocities derived in the white-light and <span class="hlt">ultraviolet</span> passbands. The horizontal velocities derived from the chromospheric and photospheric emission are comparable in magnitude. Conclusions: The horizontal motions derived in the UV passbands might indicate the existence of a supergranule-scale magneto-convection in the chromosphere, which may shed new light on the study of mass and energy supply to the corona and solar wind at the height of the chromosphere. However, it is also possible that the apparent motions reflect the chromospheric <span class="hlt">brightness</span> evolution as produced by acoustic shocks which might be modulated by the photospheric granular motions in their excitation process, or advected partly by the supergranule-scale flow towards the network while propagating upward from the photosphere. To reach a firm conclusion, it is necessary to investigate the role of granular motions in the excitation of shocks through numerical modeling, and future high-cadence chromospheric magnetograms must be scrutinized.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/19459701','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/19459701"><span>Ferri<span class="hlt">BRIGHT</span>: a rationally designed fluorescent probe for redox active metals.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Kennedy, Daniel P; Kormos, Chad M; Burdette, Shawn C</p> <p>2009-06-24</p> <p>The novel catechol-BODIPY dyad, 8-(3,4-dihydroxyphenyl)-2,6-bis(ethoxycarbonyl)-1,3,5,7-tetramethyl-4,4-difluoro-4-bora-3a,4a-diaza-s-indacene (Ferri<span class="hlt">BRIGHT</span>) was rationally designed with the aid of computational methods. Ferri<span class="hlt">BRIGHT</span> could be prepared by standard one-pot synthesis of BODIPY fluorophores from 3,4-bis(benzyloxy)benzaldehyde (1) and 3,5-dimethyl-4-(ethoxycarbonyl)pyrrole (3); however, isolating the dipyrrin intermediate 8-[3,4-bis(benzyloxy)phenyl]-2,6-bis(ethoxycarbonyl)-1,3,5,7-tetramethyl-4,4-diaza-s-indacene (7) prior to reaction with excess BF(3).OEt(2) led to marked improvements in the isolated overall yield of the desired compound. In addition to these improvements in fluorophore synthesis, microwave-assisted palladium-catalyzed hydrogenolysis of benzyl ethers was used to reduce reaction times and catalyst loading in preparation of the desired compound. When Ferri<span class="hlt">BRIGHT</span> is exposed to excess FeCl(3), CuCl(2), [Co(NH(3))(5)Cl]Cl(2), 2,3-dichloro-5,6-dicyanobenzoquinone, or ceric ammonium nitrate in methanol, a significant enhancement of fluorescence is observed. Ferri<span class="hlt">BRIGHT</span>-Q, the product resulting from the oxidation of the pendant catechol to the corresponding quinone, was found to be the emissive species. Ferri<span class="hlt">BRIGHT</span>-Q was synthesized independently, isolated, and fully characterized to allow for direct comparison with the spectroscopic data acquired in solution. Biologically relevant reactive oxygen species, such as H(2)O(2), (*)OH, (1)O(2), O(2)(*-), and bleach (NaOCl), failed to cause any changes in the emission intensity of Ferri<span class="hlt">BRIGHT</span>. In accordance with the quantum mechanical calculations, the quantum yield of fluorescence for Ferri<span class="hlt">BRIGHT</span> (Phi(fl) approximately 0) and Ferri<span class="hlt">BRIGHT</span>-Q (Phi(fl) = 0.026, lambda(ex)/lambda(em) = 490 nm/510 nm) suggests that photoinduced electron transfer between the catechol and the BODIPY dye is attenuated upon oxidation, which results in fluorescence enhancement. Binding studies of Ferri<span class="hlt">BRIGHT</span> with Ga(NO(3</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=10476&hterms=EIT&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3DEIT','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=10476&hterms=EIT&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3DEIT"><span>STEREO's Extreme <span class="hlt">UltraViolet</span> Imager (EUVI)</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>2007-01-01</p> <p>At a pixel resolution of 2048x2048, the STEREO EUVI instrument provides views of the Sun in <span class="hlt">ultraviolet</span> light that rivals the full-disk views of SOHO/EIT. This image is through the 171 Angstrom (<span class="hlt">ultraviolet</span>) filter which is characteristic of iron ions (missing eight and nine electrons) at 1 million degrees. There is a short data gap in the latter half of the movie that creates a freeze and then jump in the data view. This is a movie of the Sun in 171 Angstrom <span class="hlt">ultraviolet</span> light. The time frame is late January, 2007</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2010-title21-vol8/pdf/CFR-2010-title21-vol8-sec880-6710.pdf','CFR'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2010-title21-vol8/pdf/CFR-2010-title21-vol8-sec880-6710.pdf"><span>21 CFR 880.6710 - Medical <span class="hlt">ultraviolet</span> water purifier.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2010&page.go=Go">Code of Federal Regulations, 2010 CFR</a></p> <p></p> <p>2010-04-01</p> <p>... 21 Food and Drugs 8 2010-04-01 2010-04-01 false Medical <span class="hlt">ultraviolet</span> water purifier. 880.6710... Miscellaneous Devices § 880.6710 Medical <span class="hlt">ultraviolet</span> water purifier. (a) Identification. A medical <span class="hlt">ultraviolet</span> water purifier is a device intended for medical purposes that is used to destroy bacteria in water by...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2011-title21-vol8/pdf/CFR-2011-title21-vol8-sec880-6710.pdf','CFR2011'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2011-title21-vol8/pdf/CFR-2011-title21-vol8-sec880-6710.pdf"><span>21 CFR 880.6710 - Medical <span class="hlt">ultraviolet</span> water purifier.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2011&page.go=Go">Code of Federal Regulations, 2011 CFR</a></p> <p></p> <p>2011-04-01</p> <p>... 21 Food and Drugs 8 2011-04-01 2011-04-01 false Medical <span class="hlt">ultraviolet</span> water purifier. 880.6710... Miscellaneous Devices § 880.6710 Medical <span class="hlt">ultraviolet</span> water purifier. (a) Identification. A medical <span class="hlt">ultraviolet</span> water purifier is a device intended for medical purposes that is used to destroy bacteria in water by...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2013-title21-vol8/pdf/CFR-2013-title21-vol8-sec880-6710.pdf','CFR2013'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2013-title21-vol8/pdf/CFR-2013-title21-vol8-sec880-6710.pdf"><span>21 CFR 880.6710 - Medical <span class="hlt">ultraviolet</span> water purifier.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2013&page.go=Go">Code of Federal Regulations, 2013 CFR</a></p> <p></p> <p>2013-04-01</p> <p>... 21 Food and Drugs 8 2013-04-01 2013-04-01 false Medical <span class="hlt">ultraviolet</span> water purifier. 880.6710... Miscellaneous Devices § 880.6710 Medical <span class="hlt">ultraviolet</span> water purifier. (a) Identification. A medical <span class="hlt">ultraviolet</span> water purifier is a device intended for medical purposes that is used to destroy bacteria in water by...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2012-title21-vol8/pdf/CFR-2012-title21-vol8-sec880-6710.pdf','CFR2012'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2012-title21-vol8/pdf/CFR-2012-title21-vol8-sec880-6710.pdf"><span>21 CFR 880.6710 - Medical <span class="hlt">ultraviolet</span> water purifier.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2012&page.go=Go">Code of Federal Regulations, 2012 CFR</a></p> <p></p> <p>2012-04-01</p> <p>... 21 Food and Drugs 8 2012-04-01 2012-04-01 false Medical <span class="hlt">ultraviolet</span> water purifier. 880.6710... Miscellaneous Devices § 880.6710 Medical <span class="hlt">ultraviolet</span> water purifier. (a) Identification. A medical <span class="hlt">ultraviolet</span> water purifier is a device intended for medical purposes that is used to destroy bacteria in water by...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.dtic.mil/docs/citations/ADA622290','DTIC-ST'); return false;" href="http://www.dtic.mil/docs/citations/ADA622290"><span><span class="hlt">Ultraviolet</span> Communication for Medical Applications</span></a></p> <p><a target="_blank" href="http://www.dtic.mil/">DTIC Science & Technology</a></p> <p></p> <p>2015-06-01</p> <p>DEI procured several UVC phosphors and tested them with vacuum UV (VUV) excitation. Available emission peaks include: 226 nm, 230 nm, 234 nm, 242...SUPPLEMENTARY NOTES Report contains color. 14. ABSTRACT Under this Phase II SBIR effort, Directed Energy Inc.’s (DEI) proprietary <span class="hlt">ultraviolet</span> ( UV ...15. SUBJECT TERMS Non-line-of-sight (NLOS), networking, optical communication, plasma-shells, short range, <span class="hlt">ultraviolet</span> ( UV ) light 16. SECURITY</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25317374','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25317374"><span>Use of <span class="hlt">bright</span> light therapy among psychiatrists in massachusetts: an e-mail survey.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Oldham, Mark A; Ciraulo, Domenic A</p> <p>2014-01-01</p> <p>Evidence on the use of <span class="hlt">bright</span> light therapy for conditions beyond seasonal affective disorder continues to accrue; however, data on the prevalent use of <span class="hlt">bright</span> light therapy in the community or in hospitals remain limited, particularly in the United States. We conducted a 5-minute e-mail survey of practicing psychiatrists in Massachusetts using the membership roster through the Massachusetts Psychiatric Society to evaluate prevalent use of <span class="hlt">bright</span> light therapy as well as to solicit attitudes toward the treatment. Three e-mails were sent out over a 2-week period, and responses were obtained from March 2-24, 2013. An iPad raffle was used to incentivize survey completion. Of the 1,366 delivered e-mails, 197 responses were obtained. Of respondents, 72% indicated that they used <span class="hlt">bright</span> light therapy in their practice, and, among these, all but 1 used <span class="hlt">bright</span> light therapy for seasonal affective disorder. Only 55% of responding psychiatrists who use <span class="hlt">bright</span> light therapy consider it to treat nonseasonal depression, and 11% of respondents who recommend <span class="hlt">bright</span> light therapy would consider its use in inpatient settings. Lack of insurance coverage for light-delivery devices was identified as the largest barrier to using <span class="hlt">bright</span> light therapy, being cited by 55% of respondents. Survey results suggest that limitations in practitioner knowledge of <span class="hlt">bright</span> light therapy and the absence of <span class="hlt">bright</span> light therapy in treatment algorithms are the 2 leading modifiable factors to encourage broader implementation. The principal limitation of our survey was the low response rate. As such, we consider these data preliminary. Response bias very likely led to an overestimation in prevalent use of <span class="hlt">bright</span> light therapy; however, this bias notwithstanding, it appears that <span class="hlt">bright</span> light therapy is used significantly less often for nonseasonal depression than for seasonal affective disorder. Further, its use in inpatient settings is significantly less than in outpatient settings. We expect that efforts</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA12785.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA12785.html"><span>F Ring <span class="hlt">Bright</span> Core Clumps</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2010-07-20</p> <p><span class="hlt">Bright</span> clumps of ring material and a fan-like structure appear near the core of Saturn tenuous F ring in this mosaic of images from NASA Cassini spacecraft. Such features suggest the existence of additional objects in the F ring.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.ars.usda.gov/research/publications/publication/?seqNo115=270365','TEKTRAN'); return false;" href="http://www.ars.usda.gov/research/publications/publication/?seqNo115=270365"><span><span class="hlt">Ultraviolet</span> light-an FDA approved technology</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><span class="hlt">Ultraviolet</span> Light (254 nm) is a U.S. Food and Drug Administration approved nonthermal intervention technology that can be used for decontamination of food and food contact surfaces. <span class="hlt">Ultraviolet</span> light is a green technology that leaves no chemical residues. Results from our laboratory indicate that ex...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2013-title21-vol8/pdf/CFR-2013-title21-vol8-sec880-6500.pdf','CFR2013'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2013-title21-vol8/pdf/CFR-2013-title21-vol8-sec880-6500.pdf"><span>21 CFR 880.6500 - Medical <span class="hlt">ultraviolet</span> air purifier.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2013&page.go=Go">Code of Federal Regulations, 2013 CFR</a></p> <p></p> <p>2013-04-01</p> <p>... 21 Food and Drugs 8 2013-04-01 2013-04-01 false Medical <span class="hlt">ultraviolet</span> air purifier. 880.6500 Section... Miscellaneous Devices § 880.6500 Medical <span class="hlt">ultraviolet</span> air purifier. (a) Identification. A medical <span class="hlt">ultraviolet</span> air purifier is a device intended for medical purposes that is used to destroy bacteria in the air by exposure...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2011-title21-vol8/pdf/CFR-2011-title21-vol8-sec880-6500.pdf','CFR2011'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2011-title21-vol8/pdf/CFR-2011-title21-vol8-sec880-6500.pdf"><span>21 CFR 880.6500 - Medical <span class="hlt">ultraviolet</span> air purifier.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2011&page.go=Go">Code of Federal Regulations, 2011 CFR</a></p> <p></p> <p>2011-04-01</p> <p>... 21 Food and Drugs 8 2011-04-01 2011-04-01 false Medical <span class="hlt">ultraviolet</span> air purifier. 880.6500 Section... Miscellaneous Devices § 880.6500 Medical <span class="hlt">ultraviolet</span> air purifier. (a) Identification. A medical <span class="hlt">ultraviolet</span> air purifier is a device intended for medical purposes that is used to destroy bacteria in the air by exposure...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2010-title21-vol8/pdf/CFR-2010-title21-vol8-sec880-6500.pdf','CFR'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2010-title21-vol8/pdf/CFR-2010-title21-vol8-sec880-6500.pdf"><span>21 CFR 880.6500 - Medical <span class="hlt">ultraviolet</span> air purifier.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2010&page.go=Go">Code of Federal Regulations, 2010 CFR</a></p> <p></p> <p>2010-04-01</p> <p>... 21 Food and Drugs 8 2010-04-01 2010-04-01 false Medical <span class="hlt">ultraviolet</span> air purifier. 880.6500 Section... Miscellaneous Devices § 880.6500 Medical <span class="hlt">ultraviolet</span> air purifier. (a) Identification. A medical <span class="hlt">ultraviolet</span> air purifier is a device intended for medical purposes that is used to destroy bacteria in the air by exposure...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19820055202&hterms=malina&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3Dmalina','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19820055202&hterms=malina&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3Dmalina"><span>The Extreme <span class="hlt">Ultraviolet</span> Explorer</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Malina, R. F.; Bowyer, S.; Lampton, M.; Finley, D.; Paresce, F.; Penegor, G.; Heetderks, H.</p> <p>1982-01-01</p> <p>The Extreme <span class="hlt">Ultraviolet</span> Explorer Mission is described. The purpose of this mission is to search the celestial sphere for astronomical sources of extreme <span class="hlt">ultraviolet</span> (EUV) radiation (100 to 1000 A). The search will be accomplished with the use of three EUV telescopes, each sensitive to different bands within the EUV band. A fourth telescope will perform a higher sensitivity search of a limited sample of the sky in a single EUV band. In six months, the entire sky will be scanned at a sensitivity level comparable to existing surveys in other more traditional astronomical bandpasses.</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('https://ntrs.nasa.gov/search.jsp?R=20040121126&hterms=landcover&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dlandcover','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20040121126&hterms=landcover&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dlandcover"><span>Landcover Based Optimal Deconvolution of PALS L-band Microwave <span class="hlt">Brightness</span> Temperature</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Limaye, Ashutosh S.; Crosson, William L.; Laymon, Charles A.; Njoku, Eni G.</p> <p>2004-01-01</p> <p>An optimal de-convolution (ODC) technique has been developed to estimate microwave <span class="hlt">brightness</span> temperatures of agricultural fields using microwave radiometer observations. The technique is applied to airborne measurements taken by the Passive and Active L and S band (PALS) sensor in Iowa during Soil Moisture Experiments in 2002 (SMEX02). Agricultural fields in the study area were predominantly soybeans and corn. The <span class="hlt">brightness</span> temperatures of corn and soybeans were observed to be significantly different because of large differences in vegetation biomass. PALS observations have significant over-sampling; observations were made about 100 m apart and the sensor footprint extends to about 400 m. Conventionally, observations of this type are averaged to produce smooth spatial data fields of <span class="hlt">brightness</span> temperatures. However, the conventional approach is in contrast to reality in which the <span class="hlt">brightness</span> temperatures are in fact strongly dependent on landcover, which is characterized by sharp boundaries. In this study, we mathematically de-convolve the observations into <span class="hlt">brightness</span> temperature at the field scale (500-800m) using the sensor antenna response function. The result is more accurate spatial representation of field-scale <span class="hlt">brightness</span> temperatures, which may in turn lead to more accurate soil moisture retrieval.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/21096019','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/21096019"><span>A spectral k-means approach to <span class="hlt">bright</span>-field cell image segmentation.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Bradbury, Laura; Wan, Justin W L</p> <p>2010-01-01</p> <p>Automatic segmentation of <span class="hlt">bright</span>-field cell images is important to cell biologists, but difficult to complete due to the complex nature of the cells in <span class="hlt">bright</span>-field images (poor contrast, broken halo, missing boundaries). Standard approaches such as level set segmentation and active contours work well for fluorescent images where cells appear as round shape, but become less effective when optical artifacts such as halo exist in <span class="hlt">bright</span>-field images. In this paper, we present a robust segmentation method which combines the spectral and k-means clustering techniques to locate cells in <span class="hlt">bright</span>-field images. This approach models an image as a matrix graph and segment different regions of the image by computing the appropriate eigenvectors of the matrix graph and using the k-means algorithm. We illustrate the effectiveness of the method by segmentation results of C2C12 (muscle) cells in <span class="hlt">bright</span>-field images.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20040171815&hterms=nolan&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dnolan','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20040171815&hterms=nolan&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dnolan"><span><span class="hlt">Ultraviolet</span> Changes of the Central Source and the Very Nearby Ejecta</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Gull, Theodore R.; Nielsen, Krister; Vierira, Gladys; Hillier, John; Walborn, Nolan; Davidson, Kris</p> <p>2004-01-01</p> <p>We utilized the high spatial and high spectral resolution of the HST/STIS MAMA echelle modes in the <span class="hlt">ultraviolet</span> (0.025 inch spatial resolution and 30,000 to 120,000 spectral resolving power) to view changes in and around Eta Carinae before and after the X-Ray drop which occurred on June 29, 2003 (M. Corcoran, IAUC 8160). Major changes in the spectra of the Central Source and nearby nebulosities occurred between June 22 and July 5. Visibility of the Central Source dropped, especially between 1175 and 1350 Angstroms, but not uniformly throughout the <span class="hlt">ultraviolet</span>. This fading is likely due to multiple line absorptions both in the source and in the intervening ejecta. Nebular emission of Si III] and Fe III, located 0.09 sec. to the west, disappeared. By July 29, a <span class="hlt">bright</span> feature extending up to 0.071 sec. east of the Central Source became prominent in broad emission lines near 2500 Angstroms, but was not noticeable longward of 2900 Angstroms. ACS/HRC imagery and STIS CCD spectra taken concurrently are being examined for larger scale changes. Numerous narrow velocity components between -146 and -585 kilometers per second were identified in spectra before the minimum. New components appeared primarily in Fe II absorption lines with velocities between -170 and -380 kilometers per second. While the lines of the -513 kilometers per second component did not change, most lines of the -146 kilometers per second component changed considerably. Lines originating from high energy levels diminished or disappeared, while lines originating from lower energy levels strengthened. Strong absorption lines of Ti II, not present before the X-Ray drop, appeared within seven days, but disappeared by July 29. Further analysis of these unprecedented data will provide significant new information about the structure of Eta Carinae and its periodic variations.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2011epsc.conf.1247R','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2011epsc.conf.1247R"><span>LROC WAC <span class="hlt">Ultraviolet</span> Reflectance 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>Robinson, M. S.; Denevi, B. W.; Sato, H.; Hapke, B. W.; Hawke, B. R.</p> <p>2011-10-01</p> <p>Earth-based color filter photography, first acquired in the 1960s, showed color differences related to morphologic boundaries on the Moon [1]. These color units were interpreted to indicate compositional differences, thought to be the result of variations in titanium content [1]. Later it was shown that iron abundance (FeO) also plays a dominant role in controlling color in lunar soils [2]. Equally important is the maturity of a lunar soil in terms of its reflectance properties (albedo and color) [3]. Maturity is a measure of the state of alteration of surface materials due to sputtering and high velocity micrometeorite impacts over time [3]. The Clementine (CL) spacecraft provided the first global and digital visible through infrared observations of the Moon [4]. This pioneering dataset allowed significant advances in our understanding of compositional (FeO and TiO2) and maturation differences across the Moon [5,6]. Later, the Lunar Prospector (LP) gamma ray and neutron experiments provided the first global, <span class="hlt">albeit</span> low resolution, elemental maps [7]. Newly acquired Moon Mineralogic Mapper hyperspectral measurements are now providing the means to better characterize mineralogic variations on a global scale [8]. Our knowledge of <span class="hlt">ultraviolet</span> color differences between geologic units is limited to low resolution (km scale) nearside telescopic observations, and high resolution Hubble Space Telescope images of three small areas [9], and laboratory analyses of lunar materials [10,11]. These previous studies detailed color differences in the UV (100 to 400 nm) related to composition and physical state. HST UV (250 nm) and visible (502 nm) color differences were found to correlate with TiO2, and were relatively insensitive to maturity effects seen in visible ratios (CL) [9]. These two results led to the conclusion that improvements in TiO2 estimation accuracy over existing methods may be possible through a simple UV/visible ratio [9]. The Lunar Reconnaissance Orbiter Camera</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017JPhCS.884a2052U','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017JPhCS.884a2052U"><span>Tolerance limit value of <span class="hlt">brightness</span> and contrast adjustment on digitized radiographs</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Utami, S. N.; Kiswanjaya, B.; Syahraini, S. I.; Ustriyana, P.</p> <p>2017-08-01</p> <p>The aim of this study was to measure the tolerance limit value of <span class="hlt">brightness</span> and contrast adjustment on digitized radiograph with apical periodontitis and early apical abscess. <span class="hlt">Brightness</span> and contrast adjustment on 60 periapical radiograph with apical periodontitis and early apical abscess made by 2 observers. Reliabilities tested by Cohen’s Kappa Coefficient and significance tested by wilcoxon test. Tolerance limit value of <span class="hlt">brightness</span> and contrast adjustment for apical periodontitis is -5 and +5, early apical abscess is -10 and +10, and both is -5 and +5. <span class="hlt">Brightness</span> and contrast adjustment which not appropriate can alter the evaluation and differential diagnosis of periapical lesion.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015AGUFM.P13E..02R','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015AGUFM.P13E..02R"><span>The <span class="hlt">Ultraviolet</span> Spectrograph on the Europa Mission (Europa-UVS)</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Retherford, K. D.; Gladstone, R.; Greathouse, T. K.; Steffl, A.; Davis, M. W.; Feldman, P. D.; McGrath, M. A.; Roth, L.; Saur, J.; Spencer, J. R.; Stern, S. A.; Pope, S.; Freeman, M. A.; Persyn, S. C.; Araujo, M. F.; Cortinas, S. C.; Monreal, R. M.; Persson, K. B.; Trantham, B. J.; Versteeg, M. H.; Walther, B. C.</p> <p>2015-12-01</p> <p>NASA's Europa multi-flyby mission is designed to provide a diversity of measurements suited to enrich our understanding of the potential habitability of this intriguing ocean world. The Europa mission's <span class="hlt">Ultraviolet</span> Spectrograph, Europa-UVS, is the sixth in a series of successful <span class="hlt">ultraviolet</span> imaging spectrographs (Rosetta-Alice, New Horizons Pluto-Alice, LRO-LAMP) and, like JUICE-UVS (now under Phase B development), is largely based on the most recent of these to fly, Juno-UVS. Europa-UVS observes photons in the 55-210 nm wavelength range, at moderate spectral and spatial resolution along a 7.5° slit. Three distinct apertures send light to the off-axis telescope mirror feeding the long-slit spectrograph: i) a main entrance airglow port is used for most observations (e.g., airglow, aurora, surface mapping, and stellar occultations); ii) a high-spatial-resolution port consists of a small hole in an additional aperture door, and is used for detailed observations of <span class="hlt">bright</span> targets; and iii) a separate solar port allows for solar occultations, viewing at a 60° offset from the nominal payload boresight. Photon event time-tagging (pixel list mode) and programmable spectral imaging (histogram mode) allow for observational flexibility and optimal science data management. As on Juno-UVS, the effects of penetrating electron radiation on electronic parts and data quality are mitigated through contiguous shielding, filtering of pulse height amplitudes, management of high-voltage settings, and careful use of radiation-hard parts. The science goals of Europa-UVS are to: 1) Determine the composition & chemistry, source & sinks, and structure & variability of Europa's atmosphere, from equator to pole; 2) Search for and characterize active plumes in terms of global distribution, structure, composition, and variability; 3) Explore the surface composition & microphysics and their relation to endogenic & exogenic processes; and 4) Investigate how energy and mass flow in the Europa</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2011A%26A...531A..42L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2011A%26A...531A..42L"><span>Deceleration and dispersion of large-scale coronal <span class="hlt">bright</span> fronts</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Long, D. M.; Gallagher, P. T.; McAteer, R. T. J.; Bloomfield, D. S.</p> <p>2011-07-01</p> <p>Context. One of the most dramatic manifestations of solar activity are large-scale coronal <span class="hlt">bright</span> fronts (CBFs) observed in extreme <span class="hlt">ultraviolet</span> (EUV) images of the solar atmosphere. To date, the energetics and kinematics of CBFs remain poorly understood, due to the low image cadence and sensitivity of previous EUV imagers and the limited methods used to extract the features. Aims: In this paper, the trajectory and morphology of CBFs was determined in order to investigate the varying properties of a sample of CBFs, including their kinematics and pulse shape, dispersion, and dissipation. Methods: We have developed a semi-automatic intensity profiling technique to extract the morphology and accurate positions of CBFs in 2.5-10 min cadence images from STEREO/EUVI. The technique was applied to sequences of 171 Å and 195 Å images from STEREO/EUVI in order to measure the wave properties of four separate CBF events. Results: Following launch at velocities of ~240-450 km s-1 each of the four events studied showed significant negative acceleration ranging from ~-290 to -60 m s-2. The CBF spatial and temporal widths were found to increase from ~50 Mm to ~200 Mm and ~100 s to ~1500 s respectively, suggesting that they are dispersive in nature. The variation in position-angle averaged pulse-integrated intensity with propagation shows no clear trend across the four events studied. These results are most consistent with CBFs being dispersive magnetoacoustic waves. Figures 3-8, 10, 11, 13-15, 17, 18 and the movie are available in electronic form at http://www.aanda.org</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2010-title21-vol8/pdf/CFR-2010-title21-vol8-sec878-4635.pdf','CFR'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2010-title21-vol8/pdf/CFR-2010-title21-vol8-sec878-4635.pdf"><span>21 CFR 878.4635 - <span class="hlt">Ultraviolet</span> lamp for tanning.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2010&page.go=Go">Code of Federal Regulations, 2010 CFR</a></p> <p></p> <p>2010-04-01</p> <p>... 21 Food and Drugs 8 2010-04-01 2010-04-01 false <span class="hlt">Ultraviolet</span> lamp for tanning. 878.4635 Section 878... tanning. (a) Identification. An <span class="hlt">ultraviolet</span> lamp for tanning is a device that is a lamp (including a fixture) intended to provide <span class="hlt">ultraviolet</span> radiation to tan the skin. See § 1040.20 of this chapter. (b...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018ApJ...857...39M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018ApJ...857...39M"><span>Possible <span class="hlt">Bright</span> Starspots on TRAPPIST-1</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Morris, Brett M.; Agol, Eric; Davenport, James R. A.; Hawley, Suzanne L.</p> <p>2018-04-01</p> <p>The M8V star TRAPPIST-1 hosts seven roughly Earth-sized planets and is a promising target for exoplanet characterization. Kepler/K2 Campaign 12 observations of TRAPPIST-1 in the optical show an apparent rotational modulation with a 3.3-day period, though that rotational signal is not readily detected in the Spitzer light curve at 4.5 μm. If the rotational modulation is due to starspots, persistent dark spots can be excluded from the lack of photometric variability in the Spitzer light curve. We construct a photometric model for rotational modulation due to photospheric <span class="hlt">bright</span> spots on TRAPPIST-1 that is consistent with both the Kepler and Spitzer light curves. The maximum-likelihood model with three spots has typical spot sizes of R spot/R ⋆ ≈ 0.004 at temperature T spot ≳ 5300 ± 200 K. We also find that large flares are observed more often when the brightest spot is facing the observer, suggesting a correlation between the position of the <span class="hlt">bright</span> spots and flare events. In addition, these flares may occur preferentially when the spots are increasing in <span class="hlt">brightness</span>, which suggests that the 3.3-day periodicity may not be a rotational signal, but rather a characteristic timescale of active regions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010AAS...21547708D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010AAS...21547708D"><span>SKYMONITOR: A Global Network for Sky <span class="hlt">Brightness</span> Measurements</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Davis, Donald R.; Mckenna, D.; Pulvermacher, R.; Everett, M.</p> <p>2010-01-01</p> <p>We are implementing a global network to measure sky <span class="hlt">brightness</span> at dark-sky critical sites with the goal of creating a multi-decade database. The heart of this project is the Night Sky <span class="hlt">Brightness</span> Monitor (NSBM), an autonomous 2 channel photometer which measures night sky <span class="hlt">brightness</span> in the visual wavelengths (Mckenna et al, AAS 2009). Sky <span class="hlt">brightness</span> is measured every minute at two elevation angles typically zenith and 20 degrees to monitor <span class="hlt">brightness</span> and transparency. The NSBM consists of two parts, a remote unit and a base station with an internet connection. Currently these devices use 2.4 Ghz transceivers with a range of 100 meters. The remote unit is battery powered with daytime recharging using a solar panel. Data received by the base unit is transmitted via email protocol to IDA offices in Tucson where it will be collected, archived and made available to the user community via a web interface. Two other versions of the NSBM are under development: one for radio sensitive areas using an optical fiber link and the second that reads data directly to a laptop for sites without internet access. NSBM units are currently undergoing field testing at two observatories. With support from the National Science Foundation, we will construct and install a total of 10 units at astronomical observatories. With additional funding, we will locate additional units at other sites such as National Parks, dark-sky preserves and other sites where dark sky preservation is crucial. We will present the current comparison with the National Park Service sky monitoring camera. We anticipate that the SKYMONITOR network will be functioning by the end of 2010.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20050169997','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20050169997"><span><span class="hlt">Ultraviolet</span> Views of Enceladus, Tethys, and Dione</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hansen, C. J.; Hendrix, A. R.</p> <p>2005-01-01</p> <p>The Cassini <span class="hlt">Ultraviolet</span> Imaging Spectrograph (UVIS) has collected <span class="hlt">ultraviolet</span> observations of many of Saturn's icy moons since Cassini's insertion into orbit around Saturn. We will report on results from Enceladus, Tethys and Dione, orbiting in the Saturn system at distances of 3.95, 4.88 and 6.26 Saturn radii, respectively. Icy satellite science objectives of the UVIS include investigations of surface age and evolution, surface composition and chemistry, and tenuous exospheres. We address these objectives by producing albedo maps, and reflection and emission spectra, and observing stellar occultations. UVIS has four channels: EUV: Extreme <span class="hlt">Ultraviolet</span> (55 nm to 110 nm), FUV: Far <span class="hlt">Ultraviolet</span> (110 to 190 nm), HSP: High Speed Photometer, and HDAC: Hydrogen-Deuterium Absorption Cell. The EUV and FUV spectrographs image onto a 2-dimensional detector, with 64 spatial rows by 1024 spectral columns. To-date we have focused primarily on the far <span class="hlt">ultraviolet</span> data acquired with the low resolution slit width (4.8 angstrom spectral resolution). Additional information is included in the original extended abstract.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/29215851','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/29215851"><span>[Monitoring of <span class="hlt">brightness</span> temperature fluctuation of water in SHF range].</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Ivanov, Yu D; Kozlov, A F; Galiullin, R A; Tatu, V Yu; Vesnin, S G; Ziborov, V S; Ivanova, N D; Pleshakova, T O</p> <p>2017-01-01</p> <p>The purpose of the research consisted in detection of fluctuation of <span class="hlt">brightness</span> temperature (TSHF) of water in the area of the temperature Т = 42°С (that is critical for human) during its evaporation by SHF radiometry. Methods: Monitoring of the changes in <span class="hlt">brightness</span> temperature of water in superhigh frequency (SHF) range (3.8-4.2 GHz) near the phase transition temperature of water Т = 42°С during its evaporation in the cone dielectric cell. The <span class="hlt">brightness</span> temperature measurements were carried out using radiometer. Results: Fluctuation with maximum of <span class="hlt">brightness</span> temperature was detected in 3.8-4.2 GHz frequency range near at the temperature of water Т = 42°С. It was characteristic for these TSHF fluctuations that <span class="hlt">brightness</span> temperature rise time in this range of frequencies in ~4°С temperature range with 0.05-15°С/min gradient and a sharp decrease during 10 s connected with measuring vapor conditions. Then nonintensive fluctuation series was observed. At that, the environment temperature remained constant. Conclusion: The significant increasing in <span class="hlt">brightness</span> temperature of water during its evaporation in SHF range near the temperature of Т ~42°С were detected. It was shown that for water, ТSHF pull with the amplitude DТSHF ~4°C are observed. At the same time, thermodynamic temperature virtually does not change. The observed effects can be used in the development of the systems for diadnostics of pathologies in human and analytical system.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20010037596','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20010037596"><span>The Influence of Microphysical Cloud Parameterization on Microwave <span class="hlt">Brightness</span> Temperatures</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Skofronick-Jackson, Gail M.; Gasiewski, Albin J.; Wang, James R.; Zukor, Dorothy J. (Technical Monitor)</p> <p>2000-01-01</p> <p>The microphysical parameterization of clouds and rain-cells plays a central role in atmospheric forward radiative transfer models used in calculating passive microwave <span class="hlt">brightness</span> temperatures. The absorption and scattering properties of a hydrometeor-laden atmosphere are governed by particle phase, size distribution, aggregate density., shape, and dielectric constant. This study identifies the sensitivity of <span class="hlt">brightness</span> temperatures with respect to the microphysical cloud parameterization. Cloud parameterizations for wideband (6-410 GHz observations of baseline <span class="hlt">brightness</span> temperatures were studied for four evolutionary stages of an oceanic convective storm using a five-phase hydrometeor model in a planar-stratified scattering-based radiative transfer model. Five other microphysical cloud parameterizations were compared to the baseline calculations to evaluate <span class="hlt">brightness</span> temperature sensitivity to gross changes in the hydrometeor size distributions and the ice-air-water ratios in the frozen or partly frozen phase. The comparison shows that, enlarging the rain drop size or adding water to the partly Frozen hydrometeor mix warms <span class="hlt">brightness</span> temperatures by up to .55 K at 6 GHz. The cooling signature caused by ice scattering intensifies with increasing ice concentrations and at higher frequencies. An additional comparison to measured Convection and Moisture LA Experiment (CAMEX 3) <span class="hlt">brightness</span> temperatures shows that in general all but, two parameterizations produce calculated T(sub B)'s that fall within the observed clear-air minima and maxima. The exceptions are for parameterizations that, enhance the scattering characteristics of frozen hydrometeors.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20150001320','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20150001320"><span>The Evolution of the Galaxy Rest-Frame <span class="hlt">Ultraviolet</span> Luminosity Function Over the First Two Billion Years</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Finkelstein, Steven L.; Ryan, Russell E., Jr.; Papovich, Casey; Dickinson, Mark; Song, Mimi; Somerville, Rachel; Ferguson, Henry C.; Salmon, Brett; Giavalisco, Mauro; Koekomoer, Anton M.; <a style="text-decoration: none; " href="javascript:void(0); " onClick="displayelement('author_20150001320'); toggleEditAbsImage('author_20150001320_show'); toggleEditAbsImage('author_20150001320_hide'); "> <img style="display:inline; width:12px; height:12px; " src="images/arrow-up.gif" width="12" height="12" border="0" alt="hide" id="author_20150001320_show"> <img style="width:12px; height:12px; display:none; " src="images/arrow-down.gif" width="12" height="12" border="0" alt="hide" id="author_20150001320_hide"></p> <p>2014-01-01</p> <p>We present a robust measurement and analysis of the rest-frame <span class="hlt">ultraviolet</span> (UV) luminosity function at z = 4 to 8. We use deep Hubble Space Telescope imaging over the CANDELS/GOODS fields, the Hubble Ultra Deep Field and the Hubble Frontier Field deep parallel observations near the Abell 2744 and MACS J0416.1- 2403 clusters. The combination of these surveys provides an effective volume of 0.6-1.2 ×10(exp 6) Mpc(exp 3) over this epoch, allowing us to perform a robust search for <span class="hlt">bright</span> (M(sub UV) less than -21) and faint (M(sub UV) = -18) galaxies. We select galaxies using a well-tested photometric redshift technique with careful screening of contaminants, finding a sample of 7446 galaxies at 3.5 less than z less than 8.5, with more than 1000 galaxies at z of approximately 6 - 8. We measure both a stepwise luminosity function for galaxies in our redshift samples, as well as a Schechter function, using a Markov Chain Monte Carlo analysis to measure robust uncertainties. At the faint end our UV luminosity functions agree with previous studies, yet we find a higher abundance of UV-<span class="hlt">bright</span> galaxies at z of greater than or equal to 6. Our bestfit value of the characteristic magnitude M* is consistent with -21 at z of greater than or equal to 5, different than that inferred based on previous trends at lower redshift. At z = 8, a single power-law provides an equally good fit to the UV luminosity function, while at z = 6 and 7, an exponential cutoff at the <span class="hlt">bright</span>-end is moderately preferred. We compare our luminosity functions to semi-analytical models, and find that the lack of evolution in M* is consistent with models where the impact of dust attenuation on the <span class="hlt">bright</span>-end of the luminosity function decreases at higher redshift, though a decreasing impact of feedback may also be possible. We measure the evolution of the cosmic star-formation rate (SFR) density by integrating our observed luminosity functions to M(sub UV) = -17, correcting for dust attenuation, and find that</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27871912','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27871912"><span>The modulation of delta responses in the interaction of <span class="hlt">brightness</span> and emotion.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Kurt, Pınar; Eroğlu, Kübra; Bayram Kuzgun, Tubanur; Güntekin, Bahar</p> <p>2017-02-01</p> <p>The modulation of delta oscillations (0.5-3.5Hz) by emotional stimuli is reported. Physical attributes such as color, <span class="hlt">brightness</span> and spatial frequency of emotional visual stimuli have crucial effect on the perception of complex scene. <span class="hlt">Brightness</span> is intimately related with emotional valence. Here we explored the effect of <span class="hlt">brightness</span> on delta oscillatory responses upon presentation of pleasant, unpleasant and neutral pictures. We found that <span class="hlt">bright</span> unpleasant pictures elicited lower amplitude of delta response than original unpleasant pictures. The electrophysiological finding of the study was in accordance with behavioral data. These results denoted the importance of delta responses on the examination of the association between perceptual and conceptual processes while in the question of <span class="hlt">brightness</span> and emotion. Copyright © 2016 Elsevier B.V. All rights reserved.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=PIA05263&hterms=Ripple&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DRipple','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=PIA05263&hterms=Ripple&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DRipple"><span>Large <span class="hlt">Bright</span> Ripples</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>2004-01-01</p> <p>3 February 2004 Wind is the chief agent of change on Mars today. Wind blows dust and it can move coarser sediment such as sand and silt. This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows <span class="hlt">bright</span> ripples or small dunes on the floors of troughs northeast of Isidis Planitia near 31.1oN, 244.6oW. The picture covers an area 3 km (1.9 mi) wide; sunlight illuminates the scene from the lower left.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/23926241','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/23926241"><span>Single <span class="hlt">bright</span> light exposure decreases sweet taste threshold in healthy volunteers.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Srivastava, Shrikant; Donaldson, Lucy F; Rai, Dheeraj; Melichar, Jan K; Potokar, John</p> <p>2013-10-01</p> <p><span class="hlt">Bright</span> light exposure can alter circulating serotonin levels, and alteration of available serotonin by acute selective serotonin reuptake inhibition significantly lowers sweet but not salt taste recognition thresholds. We tested the hypothesis that <span class="hlt">bright</span> light exposure would increase sweet but not salt taste sensitivity in healthy adults. Fourteen healthy volunteers were exposed to <span class="hlt">bright</span> (10,000 lux) and dim (<20 lux) light for 30 min each, in counterbalanced order. Measures of taste perception (salt and sweet) and mood were determined at baseline, and before and after each light exposure period. Recognition thresholds for sucrose were significantly lower after <span class="hlt">bright</span> but not dim light exposure. Thresholds for salt were unaffected by either condition. There were no significant changes in taste acuity, intensity or pleasantness for both the taste modalities and on visual analogue scales (VASs) for mood, anxiety, sleepiness and alertness, under either light condition. Brief <span class="hlt">bright</span> light exposure reduces sweet but not salt taste recognition thresholds in healthy humans.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://eric.ed.gov/?q=solar+AND+panels&id=EJ976110','ERIC'); return false;" href="https://eric.ed.gov/?q=solar+AND+panels&id=EJ976110"><span>A <span class="hlt">Bright</span> Shining Lesson</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>Hurowitz, Amanda</p> <p>2010-01-01</p> <p>Sometimes students come up with crazy ideas. When this author first started teaching at Thomas Jefferson High School for Science and Technology in Virginia five years ago, she had a sophomore share such an idea with her. He wanted to put solar panels on the school's roof as a way to reduce the school's carbon footprint and set a <span class="hlt">bright</span> clean…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017JPhCS.901a2013H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017JPhCS.901a2013H"><span>Auroral <span class="hlt">bright</span> spot in Jupiter’s active region in corresponding to solar wind dynamic</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Haewsantati, K.; Wannawichian, S.; Clarke, J. T.; Nichols, J. D.</p> <p>2017-09-01</p> <p>Jupiter’s polar emission has <span class="hlt">brightness</span> whose behavior appears to be unstable. This work focuses on the <span class="hlt">bright</span> spot in active region which is a section of Jupiter’s polar emission. Images of the aurora were taken by Advanced Camera for Surveys (ACS) onboard the Hubble Space Telescope (HST). Previously, two <span class="hlt">bright</span> spots, which were found on 13 th May 2007, were suggested to be fixed on locations described by system III longitude. The <span class="hlt">bright</span> spot’s origin in equatorial plane was proposed to be at distance 80-90 Jovian radii and probably associated with the solar wind properties. This study analyzes additional data on May 2007 to study long-term variation of <span class="hlt">brightness</span> and locations of <span class="hlt">bright</span> spots. The newly modified magnetosphere-ionosphere mapping based on VIP4 and VIPAL model is used to locate the origin of <span class="hlt">bright</span> spot in magnetosphere. Furthermore, the Michigan Solar Wind Model or mSWiM is also used to study the variation of solar wind dynamic pressure during the time of <span class="hlt">bright</span> spot’s observation. We found that the <span class="hlt">bright</span> spots appear in similar locations which correspond to similar origins in magnetosphere. In addition, the solar wind dynamic pressure should probably affect the <span class="hlt">bright</span> spot’s variation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013AGUFM.P42A..06R','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013AGUFM.P42A..06R"><span>Unexpected Far-<span class="hlt">Ultraviolet</span> Photometric Characteristics On Mimas</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Royer, E. M.; Hendrix, A. R.</p> <p>2013-12-01</p> <p>While infrared and visible are the most common wavelength domains used to investigate planetary surfaces, <span class="hlt">ultraviolet</span> (UV) data are significant and useful. Here, we present the first far-UV phase curves of Mimas, thus displaying another piece of the Saturnian System puzzle. Our preliminary results shows that, one more time, Mimas surface properties are far from what we was expected. Namely, we observe a leading hemisphere brighter than the trailing hemisphere at some far-UV wavelengths. We used the far-UV channel of the Cassini/UVIS instrument, ranging from 118 to 190 nm. Disk-integrated phase curves for the leading hemisphere and the trailing hemisphere, at 180nm, have been produced. Data points span from 0.5 to 163.5 degrees in phase angle. Mimas displays a leading hemisphere brighter than its trailing hemisphere, when theory and previous Voyager observations at longer wavelengths attest of a brighter trailing hemisphere due to the impact of the E-ring grains on this face of the satellite. Surprisingly, UVIS data show a very <span class="hlt">bright</span> opposition effect on Mimas leading hemisphere, greater than what is observed on Tethys or Dione leading hemisphere at the same wavelength of 180 nm. Preliminary results of photometric properties modeling seem to indicate an important contribution of the coherent-backscattering process in the opposition surge. Exogenic processes such as bombardment by energetic electrons and/or E-ring grains are discussed to explain this unexpected surface property of Mimas.</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('https://www.ncbi.nlm.nih.gov/pubmed/647424','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/647424"><span>Entrainment of oviposition in the fowl using <span class="hlt">bright</span> and dim light cycles.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Morris, T R; Bhatti, B M</p> <p>1978-05-01</p> <p>1. Nine short trial, involving 96 different treatments, were used to investigate the critical intensities and duration of <span class="hlt">bright</span> and dim periods of lighting needed to entrain oviposition in cycles ranging from 21 to 30 h. 2. Entrainment was shown to depend upon the contrast between <span class="hlt">bright</span> and dim lighting, and to be independent of the absolute light intensity. 3. A <span class="hlt">bright</span>: dim ratio of 13:1 fully entrained oviposition in cycles of 25 h and 27 h. For 23-h and 28-h cycles a 30:1 ratio was required. Twenty-one-hour cycles required a ratio of 300:1 and with 30-h cycles a ratio of 1000:1 was needed to achieve full entrainment of oviposition. 4. In 24-h cycles, 1 h of <span class="hlt">bright</span> lighting at 02.00 h was sufficient to override other environmental signals and cause eggs to be laid in the late evening, but a minimum <span class="hlt">bright</span> period of 6 h was needed to cause full phase setting with 21-h cycles. 5. Circadian periodicity can easily be imposed on hens by providing a short exposure to <span class="hlt">bright</span> light with a background of continuous dim light; but the signal must be increased (by providing a greater contrast between <span class="hlt">bright</span> and dim lights and/or a longer period of <span class="hlt">bright</span> lighting) to entrain oviposition when the cycle deviates markedly from the natural period of 24 h.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28097379','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28097379"><span>T1 <span class="hlt">bright</span> appendix sign to exclude acute appendicitis in pregnant women.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Shin, Ilah; An, Chansik; Lim, Joon Seok; Kim, Myeong-Jin; Chung, Yong Eun</p> <p>2017-08-01</p> <p>To evaluate the diagnostic value of the T1 <span class="hlt">bright</span> appendix sign for the diagnosis of acute appendicitis in pregnant women. This retrospective study included 125 pregnant women with suspected appendicitis who underwent magnetic resonance (MR) imaging. The T1 <span class="hlt">bright</span> appendix sign was defined as a high intensity signal filling more than half length of the appendix on T1-weighted imaging. Sensitivity, specificity, positive predictive value (PPV) and negative predictive value (NPV) of the T1 <span class="hlt">bright</span> appendix sign for normal appendix identification were calculated in all patients and in those with borderline-sized appendices (6-7 mm). The T1 <span class="hlt">bright</span> appendix sign was seen in 51% of patients with normal appendices, but only in 4.5% of patients with acute appendicitis. The overall sensitivity, specificity, PPV, and NPV of the T1 <span class="hlt">bright</span> appendix sign for normal appendix diagnosis were 44.9%, 95.5%, 97.6%, and 30.0%, respectively. All four patients with borderline sized appendix with appendicitis showed negative T1 <span class="hlt">bright</span> appendix sign. The T1 <span class="hlt">bright</span> appendix sign is a specific finding for the diagnosis of a normal appendix in pregnant women with suspected acute appendicitis. • Magnetic resonance imaging is increasingly used in emergency settings. • Acute appendicitis is the most common cause of acute abdomen. • Magnetic resonance imaging is widely used in pregnant population. • T1 <span class="hlt">bright</span> appendix sign can be a specific sign representing normal appendix.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018ApJ...856...99P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018ApJ...856...99P"><span>The <span class="hlt">Bright</span> γ-ray Flare of 3C 279 in 2015 June: AGILE Detection and Multifrequency Follow-up Observations</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Pittori, C.; Lucarelli, F.; Verrecchia, F.; Raiteri, C. M.; Villata, M.; Vittorini, V.; Tavani, M.; Puccetti, S.; Perri, M.; Donnarumma, I.; Vercellone, S.; Acosta-Pulido, J. A.; Bachev, R.; Benítez, E.; Borman, G. A.; Carnerero, M. I.; Carosati, D.; Chen, W. P.; Ehgamberdiev, Sh. A.; Goded, A.; Grishina, T. S.; Hiriart, D.; Hsiao, H. Y.; Jorstad, S. G.; Kimeridze, G. N.; Kopatskaya, E. N.; Kurtanidze, O. M.; Kurtanidze, S. O.; Larionov, V. M.; Larionova, L. V.; Marscher, A. P.; Mirzaqulov, D. O.; Morozova, D. A.; Nilsson, K.; Samal, M. R.; Sigua, L. A.; Spassov, B.; Strigachev, A.; Takalo, L. O.; Antonelli, L. A.; Bulgarelli, A.; Cattaneo, P.; Colafrancesco, S.; Giommi, P.; Longo, F.; Morselli, A.; Paoletti, F.</p> <p>2018-04-01</p> <p>We report the AGILE detection and the results of the multifrequency follow-up observations of a <span class="hlt">bright</span> γ-ray flare of the blazar 3C 279 in 2015 June. We use AGILE and Fermi gamma-ray data, together with Swift X-ray andoptical-<span class="hlt">ultraviolet</span> data, and ground-based GASP-WEBT optical observations, including polarization information, to study the source variability and the overall spectral energy distribution during the γ-ray flare. The γ-ray flaring data, compared with as yet unpublished simultaneous optical data that will allow constraints on the big blue bump disk luminosity, show very high Compton dominance values of ∼100, with the ratio of γ-ray to optical emission rising by a factor of three in a few hours. The multiwavelength behavior of the source during the flare challenges one-zone leptonic theoretical models. The new observations during the 2015 June flare are also compared with already published data and nonsimultaneous historical 3C 279 archival data.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19830032747&hterms=bybee&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dbybee','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19830032747&hterms=bybee&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dbybee"><span>Photon-counting array detectors for space and ground-based studies at <span class="hlt">ultraviolet</span> and vacuum <span class="hlt">ultraviolet</span> /VUV/ wavelengths</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Timothy, J. G.; Bybee, R. L.</p> <p>1981-01-01</p> <p>The Multi-Anode Microchannel Arrays (MAMAs) are a family of photoelectric photon-counting array detectors, with formats as large as (256 x 1024)-pixels that can be operated in a windowless configuration at vacuum <span class="hlt">ultraviolet</span> (VUV) and soft X-ray wavelengths or in a sealed configuration at <span class="hlt">ultraviolet</span> and visible wavelengths. This paper describes the construction and modes of operation of (1 x 1024)-pixel and (24 x 1024)-pixel MAMA detector systems that are being built and qualified for use in sounding-rocket spectrometers for solar and stellar observations at wavelengths below 1300 A. The performance characteristics of the MAMA detectors at <span class="hlt">ultraviolet</span> and VUV wavelengths are also described.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018SciNa.105...18I','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018SciNa.105...18I"><span>Fifty shades of white: how white feather <span class="hlt">brightness</span> differs among species</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Igic, Branislav; D'Alba, Liliana; Shawkey, Matthew D.</p> <p>2018-04-01</p> <p>White colouration is a common and important component of animal visual signalling and camouflage, but how and why it varies across species is poorly understood. White is produced by wavelength-independent and diffuse scattering of light by the internal structures of materials, where the degree of <span class="hlt">brightness</span> is related to the amount of light scattered. Here, we investigated the morphological basis of <span class="hlt">brightness</span> differences among unpigmented pennaceous regions of white body feathers across 61 bird species. Using phylogenetically controlled comparisons of reflectance and morphometric measurements, we show that brighter white feathers had larger and internally more complex barbs than duller white feathers. Higher <span class="hlt">brightness</span> was also associated with more closely packed barbs and barbules, thicker and longer barbules, and rounder and less hollow barbs. Larger species tended to have brighter white feathers than smaller species because they had thicker and more complex barbs, but aquatic species were not significantly brighter than terrestrial species. As similar light scattering principals affect the <span class="hlt">brightness</span> of chromatic signals, not just white colours, these findings help broaden our general understanding of the mechanisms that affect plumage <span class="hlt">brightness</span>. Future studies should examine how feather layering on a bird's body contributes to differences between <span class="hlt">brightness</span> of white plumage patches within and across species.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://cfpub.epa.gov/si/si_public_record_report.cfm?dirEntryId=60139&keyword=uv+AND+visible&actType=&TIMSType=+&TIMSSubTypeID=&DEID=&epaNumber=&ntisID=&archiveStatus=Both&ombCat=Any&dateBeginCreated=&dateEndCreated=&dateBeginPublishedPresented=&dateEndPublishedPresented=&dateBeginUpdated=&dateEndUpdated=&dateBeginCompleted=&dateEndCompleted=&personID=&role=Any&journalID=&publisherID=&sortBy=revisionDate&count=50','EPA-EIMS'); return false;" href="https://cfpub.epa.gov/si/si_public_record_report.cfm?dirEntryId=60139&keyword=uv+AND+visible&actType=&TIMSType=+&TIMSSubTypeID=&DEID=&epaNumber=&ntisID=&archiveStatus=Both&ombCat=Any&dateBeginCreated=&dateEndCreated=&dateBeginPublishedPresented=&dateEndPublishedPresented=&dateBeginUpdated=&dateEndUpdated=&dateBeginCompleted=&dateEndCompleted=&personID=&role=Any&journalID=&publisherID=&sortBy=revisionDate&count=50"><span><span class="hlt">ULTRAVIOLET</span> PROTECTIVE COMPOUNDS AS A RESPONSE TO <span class="hlt">ULTRAVIOLET</span> RADIATION EXPOSURE</span></a></p> <p><a target="_blank" href="http://oaspub.epa.gov/eims/query.page">EPA Science Inventory</a></p> <p></p> <p></p> <p>Life on Earth has evolved adaptations to many environmental stresses over the epochs. One consistent stress has been exposure to <span class="hlt">ultraviolet</span> radiation. In response to UVR organisms have adapted myriad responses; behavioral, morphological and physiological. Behaviorally, some orga...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1994AAS...185.8607B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1994AAS...185.8607B"><span>On the Relation Between Facular <span class="hlt">Bright</span> Points and the Magnetic Field</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Berger, Thomas; Shine, Richard; Tarbell, Theodore; Title, Alan; Scharmer, Goran</p> <p>1994-12-01</p> <p>Multi-spectral images of magnetic structures in the solar photosphere are presented. The images were obtained in the summers of 1993 and 1994 at the Swedish Solar Telescope on La Palma using the tunable birefringent Solar Optical Universal Polarimeter (SOUP filter), a 10 Angstroms wide interference filter tuned to 4304 Angstroms in the band head of the CH radical (the Fraunhofer G-band), and a 3 Angstroms wide interference filter centered on the Ca II--K absorption line. Three large format CCD cameras with shuttered exposures on the order of 10 msec and frame rates of up to 7 frames per second were used to create time series of both quiet and active region evolution. The full field--of--view is 60times 80 arcseconds (44times 58 Mm). With the best seeing, structures as small as 0.22 arcseconds (160 km) in diameter are clearly resolved. Post--processing of the images results in rigid coalignment of the image sets to an accuracy comparable to the spatial resolution. Facular <span class="hlt">bright</span> points with mean diameters of 0.35 arcseconds (250 km) and elongated filaments with lengths on the order of arcseconds (10(3) km) are imaged with contrast values of up to 60 % by the G--band filter. Overlay of these images on contemporal Fe I 6302 Angstroms magnetograms and Ca II K images reveals that the <span class="hlt">bright</span> points occur, without exception, on sites of magnetic flux through the photosphere. However, instances of concentrated and diffuse magnetic flux and Ca II K emission without associated <span class="hlt">bright</span> points are common, leading to the conclusion that the presence of magnetic flux is a necessary but not sufficient condition for the occurence of resolvable facular <span class="hlt">bright</span> points. Comparison of the G--band and continuum images shows a complex relation between structures in the two bandwidths: <span class="hlt">bright</span> points exceeding 350 km in extent correspond to distinct <span class="hlt">bright</span> structures in the continuum; smaller <span class="hlt">bright</span> points show no clear relation to continuum structures. Size and contrast statistical cross</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/874475','DOE-PATENT-XML'); return false;" href="https://www.osti.gov/servlets/purl/874475"><span>Condenser for ring-field deep <span class="hlt">ultraviolet</span> and extreme <span class="hlt">ultraviolet</span> lithography</span></a></p> <p><a target="_blank" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p>Chapman, Henry N.; Nugent, Keith A.</p> <p>2002-01-01</p> <p>A condenser for use with a ring-field deep <span class="hlt">ultraviolet</span> or extreme <span class="hlt">ultraviolet</span> lithography system. A condenser includes a ripple-plate mirror which is illuminated by a collimated or converging beam at grazing incidence. The ripple plate comprises a flat or curved plate mirror into which is formed a series of channels along an axis of the mirror to produce a series of concave surfaces in an undulating pattern. Light incident along the channels of the mirror is reflected onto a series of cones. The distribution of slopes on the ripple plate leads to a distribution of angles of reflection of the incident beam. This distribution has the form of an arc, with the extremes of the arc given by the greatest slope in the ripple plate. An imaging mirror focuses this distribution to a ring-field arc at the mask plane.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/873545','DOE-PATENT-XML'); return false;" href="https://www.osti.gov/servlets/purl/873545"><span>Condenser for ring-field deep-<span class="hlt">ultraviolet</span> and extreme-<span class="hlt">ultraviolet</span> lithography</span></a></p> <p><a target="_blank" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p>Chapman, Henry N.; Nugent, Keith A.</p> <p>2001-01-01</p> <p>A condenser for use with a ring-field deep <span class="hlt">ultraviolet</span> or extreme <span class="hlt">ultraviolet</span> lithography system. A condenser includes a ripple-plate mirror which is illuminated by a collimated beam at grazing incidence. The ripple plate comprises a plate mirror into which is formed a series of channels along an axis of the mirror to produce a series of concave surfaces in an undulating pattern. Light incident along the channels of the mirror is reflected onto a series of cones. The distribution of slopes on the ripple plate leads to a distribution of angles of reflection of the incident beam. This distribution has the form of an arc, with the extremes of the arc given by the greatest slope in the ripple plate. An imaging mirror focuses this distribution to a ring-field arc at the mask plane.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017AGUFMSH43A2806I','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017AGUFMSH43A2806I"><span>ALMA Discovery of Solar Umbral <span class="hlt">Brightness</span> Enhancement at λ = 3 mm</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Iwai, K.; Loukitcheva, M.; Shimojo, M.; Solanki, S. K.; White, S. M.</p> <p>2017-12-01</p> <p>We report the discovery of a <span class="hlt">brightness</span> enhancement in the center of a large sunspot umbra at a wavelength of 3 mm using the Atacama Large Millimeter/sub-millimeter Array (ALMA). Sunspots are among the most prominent features on the solar surface, but many of their aspects are surprisingly poorly understood. We analyzed a λ = 3 mm (100 GHz) mosaic image obtained by ALMA that includes a large sunspot within the active region AR12470, on 2015 December 16. The 3 mm map has a 300''×300'' field of view and 4.9''×2.2'' spatial resolution, which is the highest spatial resolution map of an entire sunspot in this frequency range. We find a gradient of 3 mm <span class="hlt">brightness</span> from a high value in the outer penumbra to a low value in the inner penumbra/outer umbra. Within the inner umbra, there is a marked increase in 3 mm <span class="hlt">brightness</span> temperature, which we call an umbral <span class="hlt">brightness</span> enhancement. This enhanced emission corresponds to a temperature excess of 800 K relative to the surrounding inner penumbral region and coincides with excess <span class="hlt">brightness</span> in the 1330 and 1400 Å slit-jaw images of the Interface Region Imaging Spectrograph (IRIS), adjacent to a partial lightbridge. This λ = 3 mm <span class="hlt">brightness</span> enhancement may be an intrinsic feature of the sunspot umbra at chromospheric heights, such as a manifestation of umbral flashes, or it could be related to a coronal plume, since the <span class="hlt">brightness</span> enhancement was coincident with the footpoint of a coronal loop observed at 171 Å.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=MSFC-9126011&hterms=photo+image&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dphoto%2Bimage','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=MSFC-9126011&hterms=photo+image&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dphoto%2Bimage"><span>Astro-1 Image Taken by <span class="hlt">Ultraviolet</span> Imaging Telescope</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>1990-01-01</p> <p>This image shows a part of the Cygnus loop supernova remnant, taken by the <span class="hlt">Ultraviolet</span> Imaging Telescope (UIT) on the Astro Observatory during the Astro-1 mission (STS-35) on December 5, 1990. Pictured is a portion of the huge Cygnus loop, an array of interstellar gas clouds that have been blasted by a 900,000 mile per hour shock wave from a prehistoric stellar explosion, which occurred about 20,000 years ago, known as supernova. With <span class="hlt">ultraviolet</span> and x-rays, astronomers can see emissions from extremely hot gases, intense magnetic fields, and other high-energy phenomena that more faintly appear in visible and infrared light or in radio waves that are crucial to deepening the understanding of the universe. The Astro Observatory was designed to explore the universe by observing and measuring the <span class="hlt">ultraviolet</span> radiation from celestial objects. Three instruments make up the Astro Observatory: The Hopkins <span class="hlt">Ultraviolet</span> Telescope (HUT), the <span class="hlt">Ultraviolet</span> Imaging Telescope (UIT), and the Wisconsin <span class="hlt">Ultraviolet</span> Photo-Polarimetry Experiment (WUPPE). The Marshall Space Flight Center had managment responsibilities for the Astro-1 mission. The Astro-1 Observatory was launched aboard the Space Shuttle Orbiter Columbia (STS-35) on December 2, 1990.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://eric.ed.gov/?q=image+AND+processing&pg=3&id=EJ938874','ERIC'); return false;" href="https://eric.ed.gov/?q=image+AND+processing&pg=3&id=EJ938874"><span>Pen Ink as an <span class="hlt">Ultraviolet</span> Dosimeter</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>Downs, Nathan; Turner, Joanna; Parisi, Alfio; Spence, Jenny</p> <p>2008-01-01</p> <p>A technique for using highlighter ink as an <span class="hlt">ultraviolet</span> dosimeter has been developed for use by secondary school students. The technique requires the students to measure the percentage of colour fading in ink drawn onto strips of paper that have been exposed to sunlight, which can be calibrated to measurements of the <span class="hlt">ultraviolet</span> irradiance using…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/866798','DOE-PATENT-XML'); return false;" href="https://www.osti.gov/servlets/purl/866798"><span><span class="hlt">Ultraviolet</span> laser beam monitor using radiation responsive crystals</span></a></p> <p><a target="_blank" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p>McCann, Michael P.; Chen, Chung H.</p> <p>1988-01-01</p> <p>An apparatus and method for monitoring an <span class="hlt">ultraviolet</span> laser beam includes disposing in the path of an <span class="hlt">ultraviolet</span> laser beam a substantially transparent crystal that will produce a color pattern in response to <span class="hlt">ultraviolet</span> radiation. The crystal is exposed to the <span class="hlt">ultraviolet</span> laser beam and a color pattern is produced within the crystal corresponding to the laser beam intensity distribution therein. The crystal is then exposed to visible light, and the color pattern is observed by means of the visible light to determine the characteristics of the laser beam that passed through crystal. In this manner, a perpendicular cross sectional intensity profile and a longitudinal intensity profile of the <span class="hlt">ultraviolet</span> laser beam may be determined. The observation of the color pattern may be made with forward or back scattered light and may be made with the naked eye or with optical systems such as microscopes and television cameras.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5663359','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5663359"><span>CD56<span class="hlt">bright</span> NK cells exhibit potent antitumor responses following IL-15 priming</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Wagner, Julia A.; Berrien-Elliott, Melissa M.; Schneider, Stephanie E.; Leong, Jeffrey W.; Sullivan, Ryan P.; Jewell, Brea A.; Becker-Hapak, Michelle; Abdel-Latif, Sara; Ireland, Aaron R.; Jaishankar, Devika; King, Justin A.; Vij, Ravi; Clement, Dennis; Goodridge, Jodie; Malmberg, Karl-Johan; Wong, Hing C.; Fehniger, Todd A.</p> <p>2017-01-01</p> <p>NK cells, lymphocytes of the innate immune system, are important for defense against infectious pathogens and cancer. Classically, the CD56dim NK cell subset is thought to mediate antitumor responses, whereas the CD56<span class="hlt">bright</span> subset is involved in immunomodulation. Here, we challenge this paradigm by demonstrating that brief priming with IL-15 markedly enhanced the antitumor response of CD56<span class="hlt">bright</span> NK cells. Priming improved multiple CD56<span class="hlt">bright</span> cell functions: degranulation, cytotoxicity, and cytokine production. Primed CD56<span class="hlt">bright</span> cells from leukemia patients demonstrated enhanced responses to autologous blasts in vitro, and primed CD56<span class="hlt">bright</span> cells controlled leukemia cells in vivo in a murine xenograft model. Primed CD56<span class="hlt">bright</span> cells from multiple myeloma (MM) patients displayed superior responses to autologous myeloma targets, and furthermore, CD56<span class="hlt">bright</span> NK cells from MM patients primed with the IL-15 receptor agonist ALT-803 in vivo displayed enhanced ex vivo functional responses to MM targets. Effector mechanisms contributing to IL-15–based priming included improved cytotoxic protein expression, target cell conjugation, and LFA-1–, CD2-, and NKG2D-dependent activation of NK cells. Finally, IL-15 robustly stimulated the PI3K/Akt/mTOR and MEK/ERK pathways in CD56<span class="hlt">bright</span> compared with CD56dim NK cells, and blockade of these pathways attenuated antitumor responses. These findings identify CD56<span class="hlt">bright</span> NK cells as potent antitumor effectors that warrant further investigation as a cancer immunotherapy. PMID:28972539</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1985SPIE..525..181A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1985SPIE..525..181A"><span>Scatter Measurements Made With <span class="hlt">Ultraviolet</span> Light</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Anthon, Erik W.</p> <p>1985-09-01</p> <p>The quality of optical surfaces is generally evaluated by how much light (normally visible light) is scattered by the surface. Most optical glasses and many coating materials are completely opaque to <span class="hlt">ultraviolet</span> light (253.7 nm). <span class="hlt">Ultraviolet</span> light tends to scatter much more than visible light. Scatter measurements made with <span class="hlt">ultraviolet</span> light are therefore very sensitive and the scatter from second surfaces and from the interior (bulk) of the optical material is eliminated by the opacity. A novel scattermeter that operates with <span class="hlt">ultraviolet</span> light has been developed. The construction and operation of this scattermeter will be described. Cleaning soon becomes the limiting factor when measuring the surfaces with very low level of scatter. Sensitivity to repeated cleaning has been investigated. Different surfaces are compared and uniformity of surfaces is measured by mapping a surface area with an x-y stage. Polished glass surfaces generally have much higher scatter than natural glass surfaces (fire polished, drawn or floated surfaces). Very low scatter levels have been found on thin drawn glass.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22663156-orbit-calibrations-ultraviolet-imaging-telescope','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22663156-orbit-calibrations-ultraviolet-imaging-telescope"><span>In-orbit Calibrations of the <span class="hlt">Ultraviolet</span> Imaging Telescope</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>Tandon, S. N.; Subramaniam, Annapurni; Sankarasubramanian, K.</p> <p></p> <p>The <span class="hlt">Ultra-Violet</span> Imaging Telescope (UVIT) is one of the payloads in ASTROSAT, the first Indian Space Observatory. The UVIT instrument has two 375 mm telescopes: one for the far-<span class="hlt">ultraviolet</span> (FUV) channel (1300–1800 Å), and the other for the near-<span class="hlt">ultraviolet</span> (NUV) channel (2000–3000 Å) and the visible (VIS) channel (3200–5500 Å). UVIT is primarily designed for simultaneous imaging in the two <span class="hlt">ultraviolet</span> channels with spatial resolution better than 1.″8, along with provisions for slit-less spectroscopy in the NUV and FUV channels. The results of in-orbit calibrations of UVIT are presented in this paper.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19760013996','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19760013996"><span>Far <span class="hlt">ultraviolet</span> excitation processes in comets</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.; Opal, C. B.; Meier, R. R.; Nicolas, K. R.</p> <p>1976-01-01</p> <p>Recent observations of atomic oxygen and carbon in the far <span class="hlt">ultraviolet</span> spectrum of comet Kohoutek have demonstrated the existence of these atomic species in the cometary coma. However, in order to identify the source of their origin, it is necessary to relate the observed <span class="hlt">ultraviolet</span> flux to the atomic production rate. Analyses of observed OI wavelength 1304 and CI wavelength 1657 A multiplets have been carried out using high resolution solar spectra. Also examined is the possibility of observing <span class="hlt">ultraviolet</span> fluorescence from molecules such as CO and H2, as well as resonance scattering either from atomic ions for which there are strong corresponding solar lines (CII) or from atoms for which there is an accidental wavelength coincidence (SI).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/6893247','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/6893247"><span>[Effect of long-wave <span class="hlt">ultraviolet</span> light (UV-A) and medium-wave <span class="hlt">ultraviolet</span> rays (UV-B) on human skin. Critical comparison].</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Raab, W</p> <p>1980-04-15</p> <p>When discussing the effects of <span class="hlt">ultraviolet</span> radiation on human skin, one should carefully distinguish between the long wave <span class="hlt">ultraviolet</span> light (UV-A) and the short wave radiations (UV-B and UV-C). <span class="hlt">Ultraviolet</span> A induces immediate pigmentation but, if high energies are applied, a permanent pigmentation is elicited. This type of <span class="hlt">ultraviolet</span> A-induced pigmentation has been called "spontaneous" pigmentation as no erythematous reaction is necessary to induce or accelerate melanine formation. <span class="hlt">Ultraviolet</span> B provokes erythema and consecutive pigmentation. Upon chronic exposure, <span class="hlt">ultraviolet</span> B causes the wellknown actinic damage of the skin and even provokes carcinoma. With exposures to the sunlight (global radiation), one should be most careful. The public must be informed extensively about the dangers of excessive sunbaths. The use of artificial "suns" with spectra between 260 and 400 nm is limited as it may cause the same type of damage as the global radiation. An exact schedule for use of artificial lamps is strongly recommended. After one cycle of exposures, an interruption is necessary until the next cycle of irradiations may start. Upon continual use for tanning of the skin, artificial lamps may provoke irreversible damage of the skin. Radiation sources with emission spectra of wavelengths between 315 and 400 nm exclusively are well suited for the induction of skin pigmentation (cosmetic use). Potent radiation such as UVASUN systems provoke a "pleasant" permanent pigmentation after exposures for less than one hour. The use of <span class="hlt">ultraviolet</span> A (UV-A) does not carry any risk for the human skin.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA19706.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA19706.html"><span>Dark and <span class="hlt">Bright</span> Terrains of Pluto</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2015-07-10</p> <p>These circular maps shows the distribution of Pluto's dark and <span class="hlt">bright</span> terrains as revealed by NASA's New Horizons mission prior to July 4, 2015. Each map is an azimuthal equidistant projection centered on the north pole, with latitude and longitude indicated. Both a gray-scale and color version are shown. The gray-scale version is based on 7 days of panchromatic imaging from the Long Range Reconnaissance Imager (LORRI), whereas the color version uses the gray-scale base and incorporates lower-resolution color information from the Multi-spectral Visible Imaging Camera (MVIC), part of the Ralph instrument. The color version is also shown in a simple cylindrical projection in PIA19700. In these maps, the polar <span class="hlt">bright</span> terrain is surrounded by a somewhat darker polar fringe, one whose latitudinal position varies strongly with longitude. Especially striking are the much darker regions along the equator. A broad dark swath ("the whale") stretches along the equator from approximately 20 to 160 degrees of longitude. Several dark patches appear in a regular sequence centered near 345 degrees of longitude. A spectacular <span class="hlt">bright</span> region occupies Pluto's mid-latitudes near 180 degrees of longitude, and stretches southward over the equator. New Horizons' closest approach to Pluto will occur near this longitude, which will permit high-resolution visible imaging and compositional mapping of these various regions. http://photojournal.jpl.nasa.gov/catalog/PIA19706</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24305423','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24305423"><span>Ultrastructure study of hair damage after <span class="hlt">ultraviolet</span> irradiation.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Zuel-Fakkar, Nehal Mohamed; El Khateeb, Ekramy Ahmed; Cousha, Hala Sobhi; Hamed, Dina Mohamed</p> <p>2013-12-01</p> <p>Natural <span class="hlt">ultraviolet</span> exposure induces hair damage, which is difficult to avoid. Most of the research work is focused on the effect of <span class="hlt">ultraviolet</span> on the epidermis, dermis as well as the immune system, whereas the long-term effect of <span class="hlt">ultraviolet</span> on hair has not been investigated. we performed our experiment to find out the changes induced in hair follicle and shaft in those patients exposed to high doses of <span class="hlt">ultraviolet</span> (A and B) during treatment of other skin conditions. Light and transmission electron microscopy examination of scalp hair follicles and shafts of 10 patients with vitiligo under psoralen plus <span class="hlt">ultraviolet</span> A (group 1) and 10 patients with vitiligo under narrow band <span class="hlt">ultraviolet</span> B (group 2) was carried out and compared with those of 10 healthy volunteers (group 3). Physical changes in the appearance of hair were more in groups 1 and 2 than control. Reduced hair follicle thickness and perifollicular infiltrate and hyaline disorganized perifollicular collagen were observed more in group 1 than in group 2 with the absence of these changes in group 3. Transmission electron microscopy showed nonspecific cell injury in hair follicles in group 1 more than the other 2 groups, while the damaging effect on hair was more in the second group than the others. Due to the damaging effect of <span class="hlt">ultraviolet</span> on hair, patients under treatment with this modality should be cautious to protect their hair during treatment. © 2013 Wiley Periodicals, Inc.</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/2011ApJ...728..107A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2011ApJ...728..107A"><span>A New z = 0 Metagalactic <span class="hlt">Ultraviolet</span> Background Limit</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Adams, Joshua J.; Uson, Juan M.; Hill, Gary J.; MacQueen, Phillip J.</p> <p>2011-02-01</p> <p>We present new integral-field spectroscopy in the outskirts of two nearby, edge-on, late-type galaxies to search for the Hα emission that is expected from the exposure of their hydrogen gas to the metagalactic <span class="hlt">ultraviolet</span> background (UVB). Despite the sensitivity of the VIRUS-P spectrograph on the McDonald 2.7 m telescope to low surface <span class="hlt">brightness</span> emission and the large field of view, we do not detect Hα to 5σ upper limits of 6.4 × 10-19 erg s-1 cm-2 arcsec-2 in UGC 7321 and of 25 × 10-19 erg s-1 cm-2 arcsec-2 in UGC 1281 in each of the hundreds of independent spatial elements (fibers). We fit gas distribution models from overlapping 21 cm data of H I, extrapolate one scale length beyond the H I data, and estimate predicted Hα surface <span class="hlt">brightness</span> maps. We analyze three types of limits from the data with stacks formed from increasingly large spatial regions and compare to the model predictions: (1) single fibers, (2) convolution of the fiber grid with a Gaussian, circular kernel (10'' full width at half-maximum), and (3) the co-added spectra from a few hundred fibers over the brightest model regions. None of these methods produce a significant detection (>5σ) with the most stringent constraints on the H I photoionization rate of Γ(z = 0) < 1.7 × 10-14 s-1 in UGC 7321 and Γ(z = 0) < 14 × 10-14 s-1 in UGC 1281. The UGC 7321 limit is below previous measurement limits and also below current theoretical models. Restricting the analysis to the fibers bound by the H I data leads to a comparable limit; the limit is Γ(z = 0) < 2.3 × 10-14 s-1 in UGC 7321. We discuss how a low Lyman limit escape fraction in z ~ 0 redshift star-forming galaxies might explain this lower than predicted UVB strength and the prospects of deeper data to make a direct detection. This paper includes data taken at the McDonald Observatory of the University of Texas at Austin.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22340013-ultraviolet-attenuation-law-backlit-spiral-galaxies','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22340013-ultraviolet-attenuation-law-backlit-spiral-galaxies"><span>The <span class="hlt">ultraviolet</span> attenuation law in backlit spiral galaxies</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>Keel, William C.; Manning, Anna M.; Holwerda, Benne W.</p> <p></p> <p>The effective extinction law (attenuation behavior) in galaxies in the emitted <span class="hlt">ultraviolet</span> (UV) regime is well known only for actively star-forming objects and combines effects of the grain properties, fine structure in the dust distribution, and relative distributions of stars and dust. We use Galaxy Evolution Explorer, XMM Optical Monitor, and Hubble Space Telescope (HST) data to explore the UV attenuation in the outer parts of spiral disks which are backlit by other UV-<span class="hlt">bright</span> galaxies, starting with the candidate list of pairs provided by Galaxy Zoo participants. New optical images help to constrain the geometry and structure of the targetmore » galaxies. Our analysis incorporates galaxy symmetry, using non-overlapping regions of each galaxy to derive error estimates on the attenuation measurements. The entire sample has an attenuation law across the optical and UV that is close to the Calzetti et al. form; the UV slope for the overall sample is substantially shallower than found by Wild et al., which is a reasonable match to the more distant galaxies in our sample but not to the weighted combination including NGC 2207. The nearby, <span class="hlt">bright</span> spiral NGC 2207 alone gives an accuracy almost equal to the rest of our sample, and its outer arms have a very low level of foreground starlight. Thus, this widespread, fairly 'gray' law can be produced from the distribution of dust alone, without a necessary contribution from differential escape of stars from dense clouds. Our results indicate that the extrapolation needed to compare attenuation between backlit galaxies at moderate redshifts from HST data, and local systems from Sloan Digital Sky Survey and similar data, is mild enough to allow the use of galaxy overlaps to trace the cosmic history of dust in galaxies. For NGC 2207, HST data in the near-UV F336W band show that the covering factor of clouds with small optical attenuation becomes a dominant factor farther into the UV, which opens the possibility that</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015SPIE.9521E..0SL','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015SPIE.9521E..0SL"><span>Design of fire detection equipment based on <span class="hlt">ultraviolet</span> detection technology</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Liu, Zhenji; Liu, Jin; Chu, Sheng; Ping, Chao; Yuan, Xiaobing</p> <p>2015-03-01</p> <p>Utilized the feature of wide bandgap semiconductor of MgZnO, researched and developed a kind of Mid-<span class="hlt">Ultraviolet</span>-Band(MUV) <span class="hlt">ultraviolet</span> detector which has passed the simulation experiment in the sun circumstance. Based on the <span class="hlt">ultraviolet</span> detector, it gives out a design scheme of gun-shot detection device, which is composed of twelve <span class="hlt">ultraviolet</span> detectors, signal amplifier, processor, annunciator , azimuth indicator and the bracket. Through Analysing the feature of solar blind, <span class="hlt">ultraviolet</span> responsivity, fire feature of gunshots and detection distance, the feasibility of this design scheme is proved.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=PIA10140&hterms=bright+hour&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dbright%2Bhour','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=PIA10140&hterms=bright+hour&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dbright%2Bhour"><span>Active Processes: <span class="hlt">Bright</span> Streaks and Dark Fans</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>2007-01-01</p> <p><p/> [figure removed for brevity, see original site] [figure removed for brevity, see original site] Figure 1Figure 2 <p/> In a region of the south pole known informally as 'Ithaca' numerous fans of dark frost form every spring. HiRISE collected a time lapse series of these images, starting at L<sub>s</sub> = 185 and culminating at L<sub>s</sub> = 294. 'L<sub>s</sub>' is the way we measure time on Mars: at L<sub>s</sub> = 180 the sun passes the equator on its way south; at L<sub>s</sub> = 270 it reaches its maximum subsolar latitude and summer begins. <p/> In the earliest image (figure 1) fans are dark, but small narrow <span class="hlt">bright</span> streaks can be detected. In the next image (figure 2), acquired at L<sub>s</sub> = 187, just 106 hours later, dramatic differences are apparent. The dark fans are larger and the <span class="hlt">bright</span> fans are more pronounced and easily detectable. The third image in the sequence shows no <span class="hlt">bright</span> fans at all. <p/> We believe that the <span class="hlt">bright</span> streaks are fine frost condensed from the gas exiting the vent. The conditions must be just right for the <span class="hlt">bright</span> frost to condense. <p/> Observation Geometry Image PSP_002622_0945 was taken by the High Resolution Imaging Science Experiment (HiRISE) camera onboard the Mars Reconnaissance Orbiter spacecraft on 16-Feb-2007. The complete image is centered at -85.2 degrees latitude, 181.5 degrees East longitude. The range to the target site was 246.9 km (154.3 miles). At this distance the image scale is 49.4 cm/pixel (with 2 x 2 binning) so objects 148 cm across are resolved. The image shown here has been map-projected to 50 cm/pixel . The image was taken at a local Mars time of 05:46 PM and the scene is illuminated from the west with a solar incidence angle of 88 degrees, thus the sun was about 2 degrees above the horizon. At a solar longitude of 185.1 degrees, the season on Mars is Northern Autumn.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22365607-hubble-space-telescope-near-ultraviolet-spectroscopy-bright-cemp-star-bd+44493','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22365607-hubble-space-telescope-near-ultraviolet-spectroscopy-bright-cemp-star-bd+44493"><span>Hubble space telescope near-<span class="hlt">ultraviolet</span> spectroscopy of the <span class="hlt">bright</span> cemp-no star BD+44°493</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>Placco, Vinicius M.; Beers, Timothy C.; Smith, Verne V.</p> <p>2014-07-20</p> <p>We present an elemental-abundance analysis, in the near-<span class="hlt">ultraviolet</span> (NUV) spectral range, for the extremely metal-poor star BD+44°493 a ninth magnitude subgiant with [Fe/H] =–3.8 and enhanced carbon, based on data acquired with the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. This star is the brightest example of a class of objects that, unlike the great majority of carbon-enhanced metal-poor (CEMP) stars, does not exhibit over-abundances of heavy neutron-capture elements (CEMP-no). In this paper, we validate the abundance determinations for a number of species that were previously studied in the optical region, and obtain strong upper limits for berylliummore » and boron, as well as for neutron-capture elements from zirconium to platinum, many of which are not accessible from ground-based spectra. The boron upper limit we obtain for BD+44°493, log ε (B) <–0.70, the first such measurement for a CEMP star, is the lowest yet found for very and extremely metal-poor stars. In addition, we obtain even lower upper limits on the abundances of beryllium, log ε (Be) <–2.3, and lead, log ε (Pb) <–0.23 ([Pb/Fe] <+1.90), than those reported by previous analyses in the optical range. Taken together with the previously measured low abundance of lithium, the very low upper limits on Be and B suggest that BD+44°493 was formed at a very early time, and that it could well be a bona-fide second-generation star. Finally, the Pb upper limit strengthens the argument for non-s-process production of the heavy-element abundance patterns in CEMP-no stars.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27333609','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27333609"><span>Automated Adaptive <span class="hlt">Brightness</span> in Wireless Capsule Endoscopy Using Image Segmentation and Sigmoid Function.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Shrestha, Ravi; Mohammed, Shahed K; Hasan, Md Mehedi; Zhang, Xuechao; Wahid, Khan A</p> <p>2016-08-01</p> <p>Wireless capsule endoscopy (WCE) plays an important role in the diagnosis of gastrointestinal (GI) diseases by capturing images of human small intestine. Accurate diagnosis of endoscopic images depends heavily on the quality of captured images. Along with image and frame rate, <span class="hlt">brightness</span> of the image is an important parameter that influences the image quality which leads to the design of an efficient illumination system. Such design involves the choice and placement of proper light source and its ability to illuminate GI surface with proper <span class="hlt">brightness</span>. Light emitting diodes (LEDs) are normally used as sources where modulated pulses are used to control LED's <span class="hlt">brightness</span>. In practice, instances like under- and over-illumination are very common in WCE, where the former provides dark images and the later provides <span class="hlt">bright</span> images with high power consumption. In this paper, we propose a low-power and efficient illumination system that is based on an automated <span class="hlt">brightness</span> algorithm. The scheme is adaptive in nature, i.e., the <span class="hlt">brightness</span> level is controlled automatically in real-time while the images are being captured. The captured images are segmented into four equal regions and the <span class="hlt">brightness</span> level of each region is calculated. Then an adaptive sigmoid function is used to find the optimized <span class="hlt">brightness</span> level and accordingly a new value of duty cycle of the modulated pulse is generated to capture future images. The algorithm is fully implemented in a capsule prototype and tested with endoscopic images. Commercial capsules like Pillcam and Mirocam were also used in the experiment. The results show that the proposed algorithm works well in controlling the <span class="hlt">brightness</span> level accordingly to the environmental condition, and as a result, good quality images are captured with an average of 40% <span class="hlt">brightness</span> level that saves power consumption of the capsule.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018JQSRT.205..278H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018JQSRT.205..278H"><span>Measuring night sky <span class="hlt">brightness</span>: methods and challenges</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hänel, Andreas; Posch, Thomas; Ribas, Salvador J.; Aubé, Martin; Duriscoe, Dan; Jechow, Andreas; Kollath, Zoltán; Lolkema, Dorien E.; Moore, Chadwick; Schmidt, Norbert; Spoelstra, Henk; Wuchterl, Günther; Kyba, Christopher C. M.</p> <p>2018-01-01</p> <p>Measuring the <span class="hlt">brightness</span> of the night sky has become an increasingly important topic in recent years, as artificial lights and their scattering by the Earth's atmosphere continue spreading around the globe. Several instruments and techniques have been developed for this task. We give an overview of these, and discuss their strengths and limitations. The different quantities that can and should be derived when measuring the night sky <span class="hlt">brightness</span> are discussed, as well as the procedures that have been and still need to be defined in this context. We conclude that in many situations, calibrated consumer digital cameras with fisheye lenses provide the best relation between ease-of-use and wealth of obtainable information on the night sky. While they do not obtain full spectral information, they are able to sample the complete sky in a period of minutes, with colour information in three bands. This is important, as given the current global changes in lamp spectra, changes in sky radiance observed only with single band devices may lead to incorrect conclusions regarding long term changes in sky <span class="hlt">brightness</span>. The acquisition of all-sky information is desirable, as zenith-only information does not provide an adequate characterization of a site. Nevertheless, zenith-only single-band one-channel devices such as the "Sky Quality Meter" continue to be a viable option for long-term studies of night sky <span class="hlt">brightness</span> and for studies conducted from a moving platform. Accurate interpretation of such data requires some understanding of the colour composition of the sky light. We recommend supplementing long-term time series derived with such devices with periodic all-sky sampling by a calibrated camera system and calibrated luxmeters or luminance meters.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA17471.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA17471.html"><span>Dark Lakes on a <span class="hlt">Bright</span> Landscape</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2013-10-23</p> <p>Ultracold hydrocarbon lakes and seas dark shapes near the north pole of Saturn moon Titan can be seen embedded in some kind of <span class="hlt">bright</span> surface material in this infrared mosaic from NASA Cassini mission.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22654467-alma-discovery-solar-umbral-brightness-enhancement-mm','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22654467-alma-discovery-solar-umbral-brightness-enhancement-mm"><span>ALMA Discovery of Solar Umbral <span class="hlt">Brightness</span> Enhancement at λ = 3 mm</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>Iwai, Kazumasa; Loukitcheva, Maria; Shimojo, Masumi</p> <p></p> <p>We report the discovery of a <span class="hlt">brightness</span> enhancement in the center of a large sunspot umbra at a wavelength of 3 mm using the Atacama Large Millimeter/sub-millimeter Array (ALMA). Sunspots are among the most prominent features on the solar surface, but many of their aspects are surprisingly poorly understood. We analyzed a λ = 3 mm (100 GHz) mosaic image obtained by ALMA that includes a large sunspot within the active region AR12470, on 2015 December 16. The 3 mm map has a 300″ × 300″ field of view and 4.″9 × 2.″2 spatial resolution, which is the highest spatialmore » resolution map of an entire sunspot in this frequency range. We find a gradient of 3 mm <span class="hlt">brightness</span> from a high value in the outer penumbra to a low value in the inner penumbra/outer umbra. Within the inner umbra, there is a marked increase in 3 mm <span class="hlt">brightness</span> temperature, which we call an umbral <span class="hlt">brightness</span> enhancement. This enhanced emission corresponds to a temperature excess of 800 K relative to the surrounding inner penumbral region and coincides with excess <span class="hlt">brightness</span> in the 1330 and 1400 Å slit-jaw images of the Interface Region Imaging Spectrograph ( IRIS ), adjacent to a partial lightbridge. This λ = 3 mm <span class="hlt">brightness</span> enhancement may be an intrinsic feature of the sunspot umbra at chromospheric heights, such as a manifestation of umbral flashes, or it could be related to a coronal plume, since the <span class="hlt">brightness</span> enhancement was coincident with the footpoint of a coronal loop observed at 171 Å.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018SPIE10514E..0FK','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018SPIE10514E..0FK"><span>Diode lasers optimized in <span class="hlt">brightness</span> for fiber laser pumping</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kelemen, M.; Gilly, J.; Friedmann, P.; Hilzensauer, S.; Ogrodowski, L.; Kissel, H.; Biesenbach, J.</p> <p>2018-02-01</p> <p>In diode laser applications for fiber laser pumping and fiber-coupled direct diode laser systems high <span class="hlt">brightness</span> becomes essential in the last years. Fiber coupled modules benefit from continuous improvements of high-power diode lasers on chip level regarding output power, efficiency and beam characteristics resulting in record highbrightness values and increased pump power. To gain high <span class="hlt">brightness</span> not only output power must be increased, but also near field widths and far field angles have to be below a certain value for higher power levels because <span class="hlt">brightness</span> is proportional to output power divided by beam quality. While fast axis far fields typically show a current independent behaviour, for broadarea lasers far-fields in the slow axis suffer from a strong current and temperature dependence, limiting the <span class="hlt">brightness</span> and therefore their use in fibre coupled modules. These limitations can be overcome by carefully optimizing chip temperature, thermal lensing and lateral mode structure by epitaxial and lateral resonator designs and processing. We present our latest results for InGaAs/AlGaAs broad-area single emitters with resonator lengths of 4mm emitting at 976nm and illustrate the improvements in beam quality over the last years. By optimizing the diode laser design a record value of the <span class="hlt">brightness</span> for broad-area lasers with 4mm resonator length of 126 MW/cm2sr has been demonstrated with a maximum wall-plug efficiency of more than 70%. From these design also pump modules based on 9 mini-bars consisting of 5 emitters each have been realized with 360W pump power.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017SPIE10378E..0NH','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017SPIE10378E..0NH"><span>Progress in extremely high <span class="hlt">brightness</span> LED-based light sources</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hoelen, Christoph; Antonis, Piet; de Boer, Dick; Koole, Rolf; Kadijk, Simon; Li, Yun; Vanbroekhoven, Vincent; Van De Voorde, Patrick</p> <p>2017-09-01</p> <p>Although the maximum <span class="hlt">brightness</span> of LEDs has been increasing continuously during the past decade, their luminance is still far from what is required for multiple applications that still rely on the high <span class="hlt">brightness</span> of discharge lamps. In particular for high <span class="hlt">brightness</span> applications with limited étendue, e.g. front projection, only very modest luminance values in the beam can be achieved with LEDs compared to systems based on discharge lamps or lasers. With dedicated architectures, phosphor-converted green LEDs for projection may achieve luminance values up to 200-300 Mnit. In this paper we report on the progress made in the development of light engines based on an elongated luminescent concentrator pumped by blue LEDs. This concept has recently been introduced to the market as ColorSpark High Lumen Density LED technology. These sources outperform the maximum <span class="hlt">brightness</span> of LEDs by multiple factors. In LED front projection, green LEDs are the main limiting factor. With our green modules, we now have achieved peak luminance values of 2 Gnit, enabling LED-based projection systems with over 4000 ANSI lm. Extension of this concept to yellow and red light sources is presented. The light source efficiency has been increased considerably, reaching 45-60 lm/W for green under practical application conditions. The module architecture, beam shaping, and performance characteristics are reviewed, as well as system aspects. The performance increase, spectral range extensions, beam-shaping flexibility, and cost reductions realized with the new module architecture enable a breakthrough in LED-based projection systems and in a wide variety of other high <span class="hlt">brightness</span> applications.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/26016658','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/26016658"><span>Afternoon nap and <span class="hlt">bright</span> light exposure improve cognitive flexibility post lunch.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Slama, Hichem; Deliens, Gaétane; Schmitz, Rémy; Peigneux, Philippe; Leproult, Rachel</p> <p>2015-01-01</p> <p>Beneficial effects of napping or <span class="hlt">bright</span> light exposure on cognitive performance have been reported in participants exposed to sleep loss. Nonetheless, few studies investigated the effect of these potential countermeasures against the temporary drop in performance observed in mid-afternoon, and even less so on cognitive flexibility, a crucial component of executive functions. This study investigated the impact of either an afternoon nap or <span class="hlt">bright</span> light exposure on post-prandial alterations in task switching performance in well-rested participants. Twenty-five healthy adults participated in two randomized experimental conditions, either wake versus nap (n=15), or <span class="hlt">bright</span> light versus placebo (n=10). Participants were tested on a switching task three times (morning, post-lunch and late afternoon sessions). The interventions occurred prior to the post-lunch session. In the nap/wake condition, participants either stayed awake watching a 30-minute documentary or had the opportunity to take a nap for 30 minutes. In the <span class="hlt">bright</span> light/placebo condition, participants watched a documentary under either <span class="hlt">bright</span> blue light or dim orange light (placebo) for 30 minutes. The switch cost estimates cognitive flexibility and measures task-switching efficiency. Increased switch cost scores indicate higher difficulties to switch between tasks. In both control conditions (wake or placebo), accuracy switch-cost score increased post lunch. Both interventions (nap or <span class="hlt">bright</span> light) elicited a decrease in accuracy switch-cost score post lunch, which was associated with diminished fatigue and decreased variability in vigilance. Additionally, there was a trend for a post-lunch benefit of <span class="hlt">bright</span> light with a decreased latency switch-cost score. In the nap group, improvements in accuracy switch-cost score were associated with more NREM sleep stage N1. Thus, exposure to <span class="hlt">bright</span> light during the post-lunch dip, a countermeasure easily applicable in daily life, results in similar beneficial effects as</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4446306','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4446306"><span>Afternoon Nap and <span class="hlt">Bright</span> Light Exposure Improve Cognitive Flexibility Post Lunch</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Schmitz, Rémy; Peigneux, Philippe; Leproult, Rachel</p> <p>2015-01-01</p> <p>Beneficial effects of napping or <span class="hlt">bright</span> light exposure on cognitive performance have been reported in participants exposed to sleep loss. Nonetheless, few studies investigated the effect of these potential countermeasures against the temporary drop in performance observed in mid-afternoon, and even less so on cognitive flexibility, a crucial component of executive functions. This study investigated the impact of either an afternoon nap or <span class="hlt">bright</span> light exposure on post-prandial alterations in task switching performance in well-rested participants. Twenty-five healthy adults participated in two randomized experimental conditions, either wake versus nap (n=15), or <span class="hlt">bright</span> light versus placebo (n=10). Participants were tested on a switching task three times (morning, post-lunch and late afternoon sessions). The interventions occurred prior to the post-lunch session. In the nap/wake condition, participants either stayed awake watching a 30-minute documentary or had the opportunity to take a nap for 30 minutes. In the <span class="hlt">bright</span> light/placebo condition, participants watched a documentary under either <span class="hlt">bright</span> blue light or dim orange light (placebo) for 30 minutes. The switch cost estimates cognitive flexibility and measures task-switching efficiency. Increased switch cost scores indicate higher difficulties to switch between tasks. In both control conditions (wake or placebo), accuracy switch-cost score increased post lunch. Both interventions (nap or <span class="hlt">bright</span> light) elicited a decrease in accuracy switch-cost score post lunch, which was associated with diminished fatigue and decreased variability in vigilance. Additionally, there was a trend for a post-lunch benefit of <span class="hlt">bright</span> light with a decreased latency switch-cost score. In the nap group, improvements in accuracy switch-cost score were associated with more NREM sleep stage N1. Thus, exposure to <span class="hlt">bright</span> light during the post-lunch dip, a countermeasure easily applicable in daily life, results in similar beneficial effects as</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22522118-time-dead-time-timing-analysis-bright-black-hole-binaries-nustar','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22522118-time-dead-time-timing-analysis-bright-black-hole-binaries-nustar"><span>NO TIME FOR DEAD TIME: TIMING ANALYSIS OF <span class="hlt">BRIGHT</span> BLACK HOLE BINARIES WITH NuSTAR</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>Bachetti, Matteo; Barret, Didier; Harrison, Fiona A.</p> <p></p> <p>Timing of high-count-rate sources with the NuSTAR Small Explorer Mission requires specialized analysis techniques. NuSTAR was primarily designed for spectroscopic observations of sources with relatively low count rates rather than for timing analysis of <span class="hlt">bright</span> objects. The instrumental dead time per event is relatively long (∼2.5 msec) and varies event-to-event by a few percent. The most obvious effect is a distortion of the white noise level in the power density spectrum (PDS) that cannot be easily modeled with standard techniques due to the variable nature of the dead time. In this paper, we show that it is possible to exploitmore » the presence of two completely independent focal planes and use the cospectrum, the real part of the cross PDS, to obtain a good proxy of the white-noise-subtracted PDS. Thereafter, one can use a Monte Carlo approach to estimate the remaining effects of dead time, namely, a frequency-dependent modulation of the variance and a frequency-independent drop of the sensitivity to variability. In this way, most of the standard timing analysis can be performed, <span class="hlt">albeit</span> with a sacrifice in signal-to-noise ratio relative to what would be achieved using more standard techniques. We apply this technique to NuSTAR observations of the black hole binaries GX 339–4, Cyg X-1, and GRS 1915+105.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19760013983','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19760013983"><span>Comet <span class="hlt">brightness</span> parameters: Definition, determination, and correlations</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Meisel, D. D.; Morris, C. S.</p> <p>1976-01-01</p> <p>The power-law definition of comet <span class="hlt">brightness</span> is reviewed and possible systematic influences are discussed that can affect the derivation of m sub o and n values from visual magnitude estimates. A rationale for the Bobrovnikoff aperture correction method is given and it is demonstrated that the Beyer extrafocal method leads to large systematic effects which if uncorrected by an instrumental relationship result in values significantly higher than those derived according to the Bobrovnikoff guidelines. A series of visual <span class="hlt">brightness</span> parameter sets are presented which have been reduced to the same photometric system. Recommendations are given to insure that future observations are reduced to the same system.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://eric.ed.gov/?q=laser+AND+spot&id=EJ515345','ERIC'); return false;" href="https://eric.ed.gov/?q=laser+AND+spot&id=EJ515345"><span>Just How <span class="hlt">Bright</span> Is a Laser?</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>Van Baak, David A.</p> <p>1995-01-01</p> <p>Attempts to quantify the subjective sensation of <span class="hlt">brightness</span> of the spot projected by a helium-neon laser and compares this with conventional sources of light. Provides an exercise in using the blackbody radiation formulas. (JRH)</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24258716','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24258716"><span><span class="hlt">Ultraviolet</span> vision in birds: the importance of transparent eye media.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Lind, Olle; Mitkus, Mindaugas; Olsson, Peter; Kelber, Almut</p> <p>2014-01-07</p> <p><span class="hlt">Ultraviolet</span> (UV)-sensitive visual pigments are widespread in the animal kingdom but many animals, for example primates, block UV light from reaching their retina by pigmented lenses. Birds have UV-sensitive (UVS) visual pigments with sensitivity maxima around 360-373 nm (UVS) or 402-426 nm (violet-sensitive, VS). We describe how these pigments are matched by the ocular media transmittance in 38 bird species. Birds with UVS pigments have ocular media that transmit more UV light (wavelength of 50% transmittance, λ(T0.5), 323 nm) than birds with VS pigments (λ(T0.5), 358 nm). Yet, visual models predict that colour discrimination in <span class="hlt">bright</span> light is mostly dependent on the visual pigment (UVS or VS) and little on the ocular media. We hypothesize that the precise spectral tuning of the ocular media is mostly relevant for detecting weak UV signals, e.g. in dim hollow-nests of passerines and parrots. The correlation between eye size and UV transparency of the ocular media suggests little or no lens pigmentation. Therefore, only small birds gain the full advantage from shifting pigment sensitivity from VS to UVS. On the other hand, some birds with VS pigments have unexpectedly low UV transmission of the ocular media, probably because of UV blocking lens pigmentation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014SPIE.9282E..0VY','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014SPIE.9282E..0VY"><span>Discuss the testing problems of <span class="hlt">ultraviolet</span> irradiance meters</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ye, Jun'an; Lin, Fangsheng</p> <p>2014-09-01</p> <p><span class="hlt">Ultraviolet</span> irradiance meters are widely used in many areas such as medical treatment, epidemic prevention, energy conservation and environment protection, computers, manufacture, electronics, ageing of material and photo-electric effect, for testing <span class="hlt">ultraviolet</span> irradiance intensity. So the accuracy of value directly affects the sterile control in hospital, treatment, the prevention level of CDC and the control accuracy of curing and aging in manufacturing industry etc. Because the display of <span class="hlt">ultraviolet</span> irradiance meters is easy to change, in order to ensure the accuracy, it needs to be recalibrated after being used period of time. By the comparison with the standard <span class="hlt">ultraviolet</span> irradiance meters, which are traceable to national benchmarks, we can acquire the correction factor to ensure that the instruments working under accurate status and giving the accurate measured data. This leads to an important question: what kind of testing device is more accurate and reliable? This article introduces the testing method and problems of the current testing device for <span class="hlt">ultraviolet</span> irradiance meters. In order to solve these problems, we have developed a new three-dimensional automatic testing device. We introduce structure and working principle of this system and compare the advantages and disadvantages of two devices. In addition, we analyses the errors in the testing of <span class="hlt">ultraviolet</span> irradiance meters.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://files.eric.ed.gov/fulltext/ED505572.pdf','ERIC'); return false;" href="http://files.eric.ed.gov/fulltext/ED505572.pdf"><span><span class="hlt">Bright</span> Beginnings. WWC Intervention Report</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>What Works Clearinghouse, 2009</p> <p>2009-01-01</p> <p><span class="hlt">Bright</span> Beginnings is an early childhood curriculum, based in part on High/Scope[R] and Creative Curriculum[R], with an additional emphasis on literacy skills. The curriculum consists of nine thematic units designed to enhance children's cognitive, social, emotional, and physical development, and each unit includes concept maps, literacy lessons,…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/23864600','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/23864600"><span>Colour cues proved to be more informative for dogs than <span class="hlt">brightness</span>.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Kasparson, Anna A; Badridze, Jason; Maximov, Vadim V</p> <p>2013-09-07</p> <p>The results of early studies on colour vision in dogs led to the conclusion that chromatic cues are unimportant for dogs during their normal activities. Nevertheless, the canine retina possesses two cone types which provide at least the potential for colour vision. Recently, experiments controlling for the <span class="hlt">brightness</span> information in visual stimuli demonstrated that dogs have the ability to perform chromatic discrimination. Here, we show that for eight previously untrained dogs colour proved to be more informative than <span class="hlt">brightness</span> when choosing between visual stimuli differing both in <span class="hlt">brightness</span> and chromaticity. Although <span class="hlt">brightness</span> could have been used by the dogs in our experiments (unlike previous studies), it was not. Our results demonstrate that under natural photopic lighting conditions colour information may be predominant even for animals that possess only two spectral types of cone photoreceptors.</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('http://adsabs.harvard.edu/abs/1988MNRAS.235..287D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1988MNRAS.235..287D"><span>Erratum - the Lowest Surface <span class="hlt">Brightness</span> Disc Galaxy Known</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Davies, J. I.; Phillipps, S.; Disney, M. J.</p> <p>1988-11-01</p> <p>The paper "The lowest surface <span class="hlt">brightness</span> disc galaxy known' by J.I. Davies, S. Phillipps and M.J. Disney was published in Mon. Not. R. astr. Soc. (1988), 231, 69p. The declination of the object given in section 2 of the paper is incorrect and should be changed to +19^deg^48'23". Thus the object cannot be identified with GP 1444 as in the original paper. To minimize confusion we propose to refer to the low surface <span class="hlt">brightness</span> galaxy as GP 1444A.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4786037','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4786037"><span><span class="hlt">Bright</span> solitons in non-equilibrium coherent quantum matter</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Pinsker, F.; Flayac, H.</p> <p>2016-01-01</p> <p>We theoretically demonstrate a mechanism for <span class="hlt">bright</span> soliton generation in spinor non-equilibrium Bose–Einstein condensates made of atoms or quasi-particles such as polaritons in semiconductor microcavities. We give analytical expressions for <span class="hlt">bright</span> (half) solitons as minimizing functions of a generalized non-conservative Lagrangian elucidating the unique features of inter and intra-competition in non-equilibrium systems. The analytical results are supported by a detailed numerical analysis that further shows the rich soliton dynamics inferred by their instability and mutual cross-interactions. PMID:26997892</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016PASP..128j5007W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016PASP..128j5007W"><span>A New Serial-direction Trail Effect in CCD Images of the Lunar-based <span class="hlt">Ultraviolet</span> Telescope</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wu, C.; Deng, J. S.; Guyonnet, A.; Antilogus, P.; Cao, L.; Cai, H. B.; Meng, X. M.; Han, X. H.; Qiu, Y. L.; Wang, J.; Wang, S.; Wei, J. Y.; Xin, L. P.; Li, G. W.</p> <p>2016-10-01</p> <p>Unexpected trails have been seen subsequent to relative <span class="hlt">bright</span> sources in astronomical images taken with the CCD camera of the Lunar-based <span class="hlt">Ultraviolet</span> Telescope (LUT) since its first light on the Moon’s surface. The trails can only be found in the serial-direction of CCD readout, differing themselves from image trails of radiation-damaged space-borne CCDs, which usually appear in the parallel-readout direction. After analyzing the same trail defects following warm pixels (WPs) in dark frames, we found that the relative intensity profile of the LUT CCD trails can be expressed as an exponential function of the distance i (in number of pixels) of the trailing pixel to the original source (or WP), i.e., {\\mathtt{\\exp }}(α {\\mathtt{i}}+β ). The parameters α and β seem to be independent of the CCD temperature, intensity of the source (or WP), and its position in the CCD frame. The main trail characteristics show evolution occurring at an increase rate of ˜(7.3 ± 3.6) × 10-4 in the first two operation years. The trails affect the consistency of the profiles of different <span class="hlt">brightness</span> sources, which make smaller aperture photometry have larger extra systematic error. The astrometric uncertainty caused by the trails is too small to be acceptable based on LUT requirements for astrometry accuracy. Based on the empirical profile model, a correction method has been developed for LUT images that works well for restoring the fluxes of astronomical sources that are lost in trailing pixels.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/1215320','SCIGOV-STC'); return false;" href="https://www.osti.gov/servlets/purl/1215320"><span>Analysis of <span class="hlt">Bright</span> Harvest Remote Analysis for Residential Solar Installations</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>Nangle, John; Simon, Joseph</p> <p></p> <p><span class="hlt">Bright</span> Harvest provides remote shading analysis and design products for residential PV system installers. The National Renewable Energy Laboratory (NREL) through the NREL Commercialization Assistance Program, completed comparative assessments between on-site measurements and remotely calculated values to validate the accuracy of <span class="hlt">Bright</span> Harvest’s remote shading and power generation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016AAS...22713716W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016AAS...22713716W"><span>High Precision Photometry of <span class="hlt">Bright</span> Transiting Exoplanet Hosts</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wilson, Maurice; Eastman, Jason; Johnson, John A.</p> <p>2016-01-01</p> <p>Within the past two decades, the successful search for exoplanets and the characterization of their physical properties have shown the immense progress that has been made towards finding planets with characteristics similar to Earth. For most exoplanets with a radius about the size of Earth, evaluating their physical properties, such as the mass, radius and equilibrium temperature, cannot be determined with satisfactory precision. The MINiature Exoplanet Radial Velocity Array (MINERVA) was recently built to obtain spectroscopic and photometric measurements to find, confirm, and characterize Earth-like exoplanets. MINERVA's spectroscopic survey targets the brightest, nearby stars which are well-suited to the array's capabilities, while its primary photometric goal is to search for transits around these <span class="hlt">bright</span> targets. Typically, it is difficult to find satisfactory comparison stars within a telescope's field of view when the primary target is very <span class="hlt">bright</span>. This issue is resolved by using one of MINERVA's telescopes to observe the primary <span class="hlt">bright</span> star while the other telescopes observe a distinct field of view that contains satisfactory <span class="hlt">bright</span> comparison stars. We describe the code used to identify nearby comparison stars, schedule the four telescopes, produce differential photometry from multiple telescopes, and show the first results from this effort.This work has been funded by the Ronald E. McNair Post-Baccalaureate Achievement Program, the ERAU Honors Program, the ERAU Undergraduate Research Spark Fund, and the Banneker Institute at the Harvard-Smithsonian Center for Astrophysics.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018AMT....11..611B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018AMT....11..611B"><span>Retrieval of an ice water path over the ocean from ISMAR and MARSS millimeter and submillimeter <span class="hlt">brightness</span> temperatures</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Brath, Manfred; Fox, Stuart; Eriksson, Patrick; Chawn Harlow, R.; Burgdorf, Martin; Buehler, Stefan A.</p> <p>2018-02-01</p> <p>A neural-network-based retrieval method to determine the snow ice water path (SIWP), liquid water path (LWP), and integrated water vapor (IWV) from millimeter and submillimeter <span class="hlt">brightness</span> temperatures, measured by using airborne radiometers (ISMAR and MARSS), is presented. The neural networks were trained by using atmospheric profiles from the ICON numerical weather prediction (NWP) model and by radiative transfer simulations using the Atmospheric Radiative Transfer Simulator (ARTS). The basic performance of the retrieval method was analyzed in terms of offset (bias) and the median fractional error (MFE), and the benefit of using submillimeter channels was studied in comparison to pure microwave retrievals. The retrieval is offset-free for SIWP > 0.01 kg m-2, LWP > 0.1 kg m-2, and IWV > 3 kg m-2. The MFE of SIWP decreases from 100 % at SIWP = 0.01 kg m-2 to 20 % at SIWP = 1 kg m-2 and the MFE of LWP from 100 % at LWP = 0.05 kg m-2 to 30 % at LWP = 1 kg m-2. The MFE of IWV for IWV > 3 kg m-2 is 5 to 8 %. The SIWP retrieval strongly benefits from submillimeter channels, which reduce the MFE by a factor of 2, compared to pure microwave retrievals. The IWV and the LWP retrievals also benefit from submillimeter channels, <span class="hlt">albeit</span> to a lesser degree. The retrieval was applied to ISMAR and MARSS <span class="hlt">brightness</span> temperatures from FAAM flight B897 on 18 March 2015 of a precipitating frontal system west of the coast of Iceland. Considering the given uncertainties, the retrieval is in reasonable agreement with the SIWP, LWP, and IWV values simulated by the ICON NWP model for that flight. A comparison of the retrieved IWV with IWV from 12 dropsonde measurements shows an offset of 0.5 kg m-2 and an RMS difference of 0.8 kg m-2, showing that the retrieval of IWV is highly effective even under cloudy conditions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=MSFC-9126013&hterms=photo+image&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dphoto%2Bimage','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=MSFC-9126013&hterms=photo+image&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dphoto%2Bimage"><span>Astro-1 Image Taken by the <span class="hlt">Ultraviolet</span> Imaging Telescope</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>1990-01-01</p> <p>This is a presentation of two comparison images of the Spiral Galaxy M81 in the constellation URA Major. The galaxy is about 12-million light years from Earth. The left image is the Spiral Galaxy M81 as photographed by the <span class="hlt">Ultraviolet</span> Imaging Telescope (UIT) during the Astro-1 Mission (STS-35) on December 9, 1990. This UIT photograph, made with <span class="hlt">ultraviolet</span> light, reveals regions where new stars are forming at a rapid rate. The right image is a photograph of the same galaxy in red light made with a 36-inch (0.9-meter) telescope at the Kitt Peak National Observatory near Tucson, Arizona. The Astro Observatory was designed to explore the universe by observing and measuring <span class="hlt">ultraviolet</span> radiation from celestial objects. Three instruments made up the Astro Observatory: The Hopkins <span class="hlt">Ultraviolet</span> Telescope (HUT), the <span class="hlt">Ultraviolet</span> Imaging Telescope (UIT), and the Wisconsin <span class="hlt">Ultraviolet</span> Photo-Polarimetry Experiment (WUPPE). The Marshall Space Flight Center had management responsibilities for the Astro-1 mission. The Astro-1 Observatory was launched aboard the Space Shuttle Orbiter Columbia (STS-35) on December 2, 1990.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=PIA01058&hterms=Dark+web&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3DDark%2Bweb','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=PIA01058&hterms=Dark+web&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3DDark%2Bweb"><span><span class="hlt">Bright</span> and Dark Slopes on Ganymede</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>1997-01-01</p> <p>Ridges on the edge of Ganymede's north polar cap show <span class="hlt">bright</span> east-facing slopes and dark west-facing slopes with troughs of darker material below the larger ridges. North is to the top. The <span class="hlt">bright</span> slopes may be due to grain size differences, differences in composition between the original surface and the underlying material, frost deposition, or illumination effects. The large 2.4 kilometer (1.5 mile) diameter crater in this image shows frost deposits located on the north-facing rim slope, away from the sun. A smaller 675 meter (2200 foot) diameter crater in the center of the image is surrounded by a <span class="hlt">bright</span> deposit which may be ejecta from the impact. Ejecta deposits such as this are uncommon for small craters on Ganymede. This image measures 18 by 19 kilometers (11 by 12 miles) and has a resolution of 45 meters (148 feet) per pixel. NASA's Galileo spacecraft obtained this image on September 6, 1996 during its second orbit around Jupiter.<p/>The Jet Propulsion Laboratory, Pasadena, CA manages the Galileo mission for NASA's Office of Space Science, Washington, DC. JPL is an operating division of California Institute of Technology (Caltech).<p/>This image and other images and data received from Galileo are posted on the World Wide Web, on the Galileo mission home page at URL http://galileo.jpl.nasa.gov. Background information and educational context for the images can be found at URL http://www.jpl.nasa.gov/galileo/sepo</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/2186795','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/2186795"><span><span class="hlt">Brightness</span> discrimination and contrast sensitivity in chronic glaucoma--a clinical study.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Teoh, S L; Allan, D; Dutton, G N; Foulds, W S</p> <p>1990-04-01</p> <p>The visual acuity, the difference in sensitivity of the two eyes to light (<span class="hlt">brightness</span> ratio), and contrast sensitivity were assessed in 28 patients with chronic open angle glaucoma and compared with those of 41 normal controls of similar ages and visual acuity. The results obtained were related to the results of Tübingen visual field analysis in patients with glaucoma. Twenty-four of the 28 glaucoma patients (86%) had a significant disparity in <span class="hlt">brightness</span> ratio between the two eyes. This was found to match the frequency of visual field loss. Moreover, there was a significant relationship between the interocular differences in <span class="hlt">brightness</span> sense and the difference in the degree of visual field loss between the two eyes. Of the glaucoma patients 39% had sum contrast sensitivities outside the normal range for age-matched normal controls. No significant correlation was found between the interocular difference in <span class="hlt">brightness</span> sense and the visual acuity or the interocular difference in sum contrast sensitivity. It is concluded that, in the presence of a normal visual acuity, the <span class="hlt">brightness</span> ratio test warrants evaluation as a potential screening test for chronic open angle glaucoma.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=1042064','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=1042064"><span><span class="hlt">Brightness</span> discrimination and contrast sensitivity in chronic glaucoma--a clinical study.</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Teoh, S L; Allan, D; Dutton, G N; Foulds, W S</p> <p>1990-01-01</p> <p>The visual acuity, the difference in sensitivity of the two eyes to light (<span class="hlt">brightness</span> ratio), and contrast sensitivity were assessed in 28 patients with chronic open angle glaucoma and compared with those of 41 normal controls of similar ages and visual acuity. The results obtained were related to the results of Tübingen visual field analysis in patients with glaucoma. Twenty-four of the 28 glaucoma patients (86%) had a significant disparity in <span class="hlt">brightness</span> ratio between the two eyes. This was found to match the frequency of visual field loss. Moreover, there was a significant relationship between the interocular differences in <span class="hlt">brightness</span> sense and the difference in the degree of visual field loss between the two eyes. Of the glaucoma patients 39% had sum contrast sensitivities outside the normal range for age-matched normal controls. No significant correlation was found between the interocular difference in <span class="hlt">brightness</span> sense and the visual acuity or the interocular difference in sum contrast sensitivity. It is concluded that, in the presence of a normal visual acuity, the <span class="hlt">brightness</span> ratio test warrants evaluation as a potential screening test for chronic open angle glaucoma. PMID:2186795</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018eMetN...3...28G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018eMetN...3...28G"><span>Leonids 2017 from Norway – A <span class="hlt">bright</span> surprise!</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gaarder, K.</p> <p>2018-01-01</p> <p>I am very pleased to have been able to observe near maximum activity of the Leonids, and clearly witnessed the unequal mass distribution during these hours. A lot of <span class="hlt">bright</span> Leonids were seen, followed by a short period of high activity of fainter meteors, before a sharp drop in activity. The Leonids is undoubtedly a shower to watch closely, with its many variations in activity level and magnitude distribution. I already look forward to observing the next years’ display, hopefully under a dark and clear sky, filled with <span class="hlt">bright</span> meteors!</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2005JGRD..110.9209M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2005JGRD..110.9209M"><span>Twilight sky <span class="hlt">brightness</span> measurements as a useful tool for stratospheric aerosol investigations</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Mateshvili, Nina; Fussen, Didier; Vanhellemont, Filip; Bingen, Christine; KyröLä, Erkki; Mateshvili, Iuri; Mateshvili, Giuli</p> <p>2005-05-01</p> <p>In this paper we demonstrate how twilight sky <span class="hlt">brightness</span> measurements can be used to obtain information about stratospheric aerosols. Beside this, the measurements of the distribution and the variability of the twilight sky <span class="hlt">brightness</span> may help to understand how the stratospheric aerosols affect the radiation field, which is important for correct calculations of photodissociation rates. Multispectral measurements of twilight sky <span class="hlt">brightness</span> were carried out in Abastumani Observatory (41.8°N, 42.8°E), Georgia, South Caucasus, during the period (1991-1993) when the level of stratospheric aerosols was substantially enhanced after the 1991 Mount Pinatubo eruption. The twilight sky <span class="hlt">brightness</span> was measured at 9 wavelengths (422, 474, 496, 542, 610, 642, 678, 713, and 820 nm) for solar zenith angles from 89° to 107°. There are clear indications of a growth of the stratospheric aerosol layer after the eruption of Mount Pinatubo that manifests itself by "humps" in twilight sky <span class="hlt">brightness</span> dependences versus solar zenith angle. Similar features were obtained using a radiative transfer code constrained by the SAGE II aerosol optical thicknesses. It is shown how an enhancement of stratospheric aerosol loading perturbs the twilight sky <span class="hlt">brightness</span> due to light scattering and absorption in the aerosol layer. The influence of ozone variations and background stratospheric aerosols on twilight sky <span class="hlt">brightness</span> has also been analyzed. The optical thicknesses of the stratospheric aerosol layer obtained from the twilight measurements of 1990-1993 show a good agreement with SAGE II results. The spectral variations of the stratospheric aerosol extinction for pre-Pinatubo and post-Pinatubo measurements reflect the aerosol growth after the eruption. Finally, the utilization of twilight sky <span class="hlt">brightness</span> measurements for validation of satellite-based measurements of the stratospheric aerosol is proposed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1997PASP..109..745B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1997PASP..109..745B"><span>Low-Surface-<span class="hlt">Brightness</span> Galaxies: Hidden Galaxies Revealed</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Bothun, G.; Impey, C.; McGaugh, S.</p> <p>1997-07-01</p> <p>In twenty years, low surface <span class="hlt">brightness</span> (LSB) galaxies have evolved from being an idiosyncratic notion to being one of the major baryonic repositories in the Universe. The story of their discovery and the characterization of their properties is told here. Their recovery from the noise of the night sky background is a strong testament to the severity of surface <span class="hlt">brightness</span> selection effects. LSB galaxies have a number of remarkable properties which distinguish them from the more familiar Hubble Sequence of spirals. The two most important are 1) they evolve at a significantly slower rate and may well experience star formation outside of the molecular cloud environment, 2) they are embedded in dark matter halos which are of lower density and more extended than the halos around high surface <span class="hlt">brightness</span> (HSB) disk galaxies. Compared to HSB disks, LSB disks are strongly dark matter dominated at all radii and show a systematic increase in $M/L$ with decreasing central surface <span class="hlt">brightness</span>. In addition, the recognition that large numbers of LSB galaxies actually exist has changed the form of the galaxy luminosity function and has clearly increased the space density of galaxies at z =0. Recent CCD surveys have uncovered a population of red LSB disks that may be related to the excess of faint blue galaxies detected at moderate redshifts. LSB galaxies offer us a new window into galaxy evolution and formation which is every bit as important as those processes which have produced easy to detect galaxies. Indeed, the apparent youth of some LSB galaxies suggest that galaxy formation is a greatly extended process. While the discovery of LSB galaxies have lead to new insights, it remains unwise to presume that we now have a representative sample which encompasses all galaxy types and forms. (SECTION: Invited Review Paper)</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19870004788','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19870004788"><span>Coordinated observations of X-ray <span class="hlt">bright</span> BL Lacertae objects</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Urry, C. M.</p> <p>1986-01-01</p> <p>No new International <span class="hlt">Ultraviolet</span> Explorer (IUE) observations were scheduled. The work on the spectral extraction routine was continued. The computer code was adapted from the RDAF PDP 11/44 computer to a VAX 11/750, in order that it run more quickly. A chapter on <span class="hlt">ultraviolet</span> observations of blazars for a book celebrating the scientific accomplishment of IUE was written in colloboration. A copy of the final draft is attached.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/21230954','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/21230954"><span>Stable vortex-<span class="hlt">bright</span>-soliton structures in two-component Bose-Einstein condensates.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Law, K J H; Kevrekidis, P G; Tuckerman, Laurette S</p> <p>2010-10-15</p> <p>We report the numerical realization of robust two-component structures in 2D and 3D Bose-Einstein condensates with nontrivial topological charge in one component. We identify a stable symbiotic state in which a higher-dimensional <span class="hlt">bright</span> soliton exists even in a homogeneous setting with defocusing interactions, due to the effective potential created by a stable vortex in the other component. The resulting vortex-<span class="hlt">bright</span>-solitons, generalizations of the recently experimentally observed dark-<span class="hlt">bright</span> solitons, are found to be very robust both in the homogeneous medium and in the presence of external confinement.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22086471-evidence-wide-range-ultraviolet-obscuration-approx-dusty-galaxies-from-goods-herschel-survey','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22086471-evidence-wide-range-ultraviolet-obscuration-approx-dusty-galaxies-from-goods-herschel-survey"><span>EVIDENCE FOR A WIDE RANGE OF <span class="hlt">ULTRAVIOLET</span> OBSCURATION IN z {approx} 2 DUSTY GALAXIES FROM THE GOODS-HERSCHEL SURVEY</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>Penner, Kyle; Dickinson, Mark; Dey, Arjun</p> <p></p> <p>Dusty galaxies at z {approx} 2 span a wide range of relative <span class="hlt">brightness</span> between rest-frame mid-infrared (8 {mu}m) and <span class="hlt">ultraviolet</span> wavelengths. We attempt to determine the physical mechanism responsible for this diversity. Dust-obscured galaxies (DOGs), which have rest-frame mid-IR to UV flux density ratios {approx}> 1000, might be abnormally <span class="hlt">bright</span> in the mid-IR, perhaps due to prominent emission from active galactic nuclei and/or polycyclic aromatic hydrocarbons, or abnormally faint in the UV. We use far-infrared data from the GOODS-Herschel survey to show that most DOGs with 10{sup 12} L {sub Sun} {approx}< L {sub IR} {approx}< 10{sup 13} L {submore » Sun} are not abnormally <span class="hlt">bright</span> in the mid-IR when compared to other dusty galaxies with similar IR (8-1000 {mu}m) luminosities. We observe a relation between the median IR to UV luminosity ratios and the median UV continuum power-law indices for these galaxies, and we find that only 24% have specific star formation rates that indicate the dominance of compact star-forming regions. This circumstantial evidence supports the idea that the UV- and IR-emitting regions in these galaxies are spatially coincident, which implies a connection between the abnormal UV faintness of DOGs and dust obscuration. We conclude that the range in rest-frame mid-IR to UV flux density ratios spanned by dusty galaxies at z {approx} 2 is due to differing amounts of UV obscuration. Of galaxies with these IR luminosities, DOGs are the most obscured. We attribute differences in UV obscuration to either (1) differences in the degree of alignment between the spatial distributions of dust and massive stars or (2) differences in the total dust content.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19780051917&hterms=spectrophotometer&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dspectrophotometer','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19780051917&hterms=spectrophotometer&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dspectrophotometer"><span><span class="hlt">Ultraviolet</span> spectrophotometer for measuring columnar atmospheric ozone from aircraft</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hanser, F. A.; Sellers, B.; Briehl, D. C.</p> <p>1978-01-01</p> <p>An <span class="hlt">ultraviolet</span> spectrophotometer (UVS) to measure downward solar fluxes from an aircraft or other high altitude platform is described. The UVS uses an <span class="hlt">ultraviolet</span> diffuser to obtain large angular response with no aiming requirement, a twelve-position filter wheel with narrow (2-nm) and broad (20-nm) bandpass filters, and an <span class="hlt">ultraviolet</span> photodiode. The columnar atmospheric ozone above the UVS (aircraft) is calculated from the ratios of the measured <span class="hlt">ultraviolet</span> fluxes. Comparison with some Dobson station measurements gives agreement to 2%. Some UVS measured ozone profiles over the Pacific Ocean for November 1976 are shown to illustrate the instrument's performance.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017SPIE10351E..0DM','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017SPIE10351E..0DM"><span>Aluminum nanostructures for <span class="hlt">ultraviolet</span> plasmonics</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Martin, Jérôme; Khlopin, Dmitry; Zhang, Feifei; Schuermans, Silvère; Proust, Julien; Maurer, Thomas; Gérard, Davy; Plain, Jérôme</p> <p>2017-08-01</p> <p>An electromagnetic field is able to produce a collective oscillation of free electrons at a metal surface. This allows light to be concentrated in volumes smaller than its wavelength. The resulting waves, called surface plasmons can be applied in various technological applications such as ultra-sensitive sensing, Surface Enhanced Raman Spectroscopy, or metal-enhanced fluorescence, to name a few. For several decades plasmonics has been almost exclusively studied in the visible region by using nanoparticles made of gold or silver as these noble metals support plasmonic resonances in the visible and near-infrared range. Nevertheless, emerging applications will require the extension of nano-plasmonics toward higher energies, in the <span class="hlt">ultraviolet</span> range. Aluminum is one of the most appealing metal for pushing plasmonics up to <span class="hlt">ultraviolet</span> energies. The subsequent applications in the field of nano-optics are various. This metal is therefore a highly promising material for commercial applications in the field of <span class="hlt">ultraviolet</span> nano-optics. As a consequence, aluminum (or <span class="hlt">ultraviolet</span>, UV) plasmonics has emerged quite recently. Aluminium plasmonics has been demonstrated efficient for numerous potential applications including non-linear optics, enhanced fluorescence, UV-Surface Enhanced Raman Spectroscopy, optoelectronics, plasmonic assisted solid-state lasing, photocatalysis, structural colors and data storage. In this article, different preparation methods developed in the laboratory to obtain aluminum nanostructures with different geometries are presented. Their optical and morphological characterizations of the nanostructures are given and some proof of principle applications such as fluorescence enhancement are discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018ATel11710....1F','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018ATel11710....1F"><span>ZTF <span class="hlt">Bright</span> Transient Survey classifications</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Fremling, C.; Sharma, Y.; Skulkarni, S. R.; Walters, R.; Blagorodnova, N.; Neill, J. D.; Miller, A. A.; Taggart, K.; Perley, D. A.; Goobar, A.; Graham, M. L.</p> <p>2018-06-01</p> <p>The Zwicky Transient Facility (ZTF; ATel #11266) <span class="hlt">Bright</span> Transient Survey (BTS; ATel #11688) reports classifications of the following targets. Spectra have been obtained with the Spectral Energy Distribution Machine (SEDM) (range 350-950nm, spectral resolution R 100) mounted on the Palomar 60-inch (P60) telescope (Blagorodnova et. al. 2018, PASP, 130, 5003).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25923778','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25923778"><span>The influence of the environment and clothing on human exposure to <span class="hlt">ultraviolet</span> light.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Liu, Jin; Zhang, Wei</p> <p>2015-01-01</p> <p>The aim of this study is to determine the effect of clothing and the environment on human exposure to <span class="hlt">ultraviolet</span> light. The <span class="hlt">ultraviolet</span> (<span class="hlt">ultraviolet</span> A and <span class="hlt">ultraviolet</span> B) light intensity was measured, and air quality parameters were recorded in 2014 in Beijing, China. Three types of clothing (white polyester cloth, pure cotton white T-shirt, and pure cotton black T-shirt) were individually placed on a mannequin. The <span class="hlt">ultraviolet</span> (<span class="hlt">ultraviolet</span> A and <span class="hlt">ultraviolet</span> B) light intensities were measured above and beneath each article of clothing, and the percentage of <span class="hlt">ultraviolet</span> light transmission through the clothing was calculated. (1) The <span class="hlt">ultraviolet</span> light transmission was significantly higher through white cloth than through black cloth; the transmission was significantly higher through polyester cloth than through cotton. (2) The weather significantly influenced <span class="hlt">ultraviolet</span> light transmission through white polyester cloth; transmission was highest on clear days and lowest on overcast days (<span class="hlt">ultraviolet</span> A: P=0.000; <span class="hlt">ultraviolet</span> B: P=0.008). (3) Air quality parameters (air quality index and particulate matter 2.5 and 10) were inversely related to the <span class="hlt">ultraviolet</span> light intensity that reached the earth's surface. <span class="hlt">Ultraviolet</span> B transmission through white polyester cloth was greater under conditions of low air pollution compared with high air pollution. Clothing color and material and different types of weather affected <span class="hlt">ultraviolet</span> light transmission; for one particular cloth, the transmission decreased with increasing air pollution.</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/2018ATel11546....1J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018ATel11546....1J"><span>Fermi-LAT <span class="hlt">Bright</span> Gamma-ray Detection of Nova ASASSN-18fv</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jean, P.; Cheung, C. C.; Ojha, R.; van Zyl, P.; Angioni, R.</p> <p>2018-04-01</p> <p>The Large Area Telescope (LAT), one of two instruments on the Fermi Gamma-ray Space Telescope, has observed <span class="hlt">bright</span> gamma-ray emission from a source positionally consistent with the <span class="hlt">bright</span> optical nova ASASSN-18fv (ATel #11454, #11456, #11460, #11467, #11508).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/29400543','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/29400543"><span>First Observation of <span class="hlt">Bright</span> Solitons in Bulk Superfluid ^{4}He.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Ancilotto, Francesco; Levy, David; Pimentel, Jessica; Eloranta, Jussi</p> <p>2018-01-19</p> <p>The existence of <span class="hlt">bright</span> solitons in bulk superfluid ^{4}He is demonstrated by time-resolved shadowgraph imaging experiments and density functional theory (DFT) calculations. The initial liquid compression that leads to the creation of nonlinear waves is produced by rapidly expanding plasma from laser ablation. After the leading dissipative period, these waves transform into <span class="hlt">bright</span> solitons, which exhibit three characteristic features: dispersionless propagation, negligible interaction in a two-wave collision, and direct dependence between soliton amplitude and the propagation velocity. The experimental observations are supported by DFT calculations, which show rapid evolution of the initially compressed liquid into <span class="hlt">bright</span> solitons. At high amplitudes, solitons become unstable and break down into dispersive shock waves.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018AIPC.1965f0005A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018AIPC.1965f0005A"><span>Stimulation of hair cells with <span class="hlt">ultraviolet</span> light</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Azimzadeh, Julien B.; Fabella, Brian A.; Hudspeth, A. J.</p> <p>2018-05-01</p> <p>Hair bundles are specialized organelles that transduce mechanical inputs into electrical outputs. To activate hair cells, physiologists have resorted to mechanical methods of hair-bundle stimulation. Here we describe a new method of hair-bundle stimulation, irradiation with <span class="hlt">ultraviolet</span> light. A hair bundle illuminated by <span class="hlt">ultraviolet</span> light rapidly moves towards its tall edge, a motion typically associated with excitatory stimulation. The motion disappears upon tip-link rupture and is associated with the opening of mechanotransduction channels. Hair bundles can be induced to move sinusoidally with oscillatory modulation of the stimulation power. We discuss the implications of <span class="hlt">ultraviolet</span> stimulation as a novel hair-bundle stimulus.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27377245','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27377245"><span>Ion chromatography with the indirect <span class="hlt">ultraviolet</span> detection of alkali metal ions and ammonium using imidazolium ionic liquid as <span class="hlt">ultraviolet</span> absorption reagent and eluent.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Liu, Yong-Qiang; Yu, Hong</p> <p>2016-08-01</p> <p>Indirect <span class="hlt">ultraviolet</span> detection was conducted in <span class="hlt">ultraviolet</span>-absorption-agent-added mobile phase to complete the detection of the absence of <span class="hlt">ultraviolet</span> absorption functional group in analytes. Compared with precolumn derivatization or postcolumn derivatization, this method can be widely used, has the advantages of simple operation and good linear relationship. Chromatographic separation of Li(+) , Na(+) , K(+) , and NH4 (+) was performed on a carboxylic acid base cation exchange column using imidazolium ionic liquid/acid/organic solvent as the mobile phase, in which imidazolium ionic liquids acted as <span class="hlt">ultraviolet</span> absorption reagent and eluting agent. The retention behaviors of four kinds of cations are discussed, and the mechanism of separation and detection are described. The main factors influencing the separation and detection were the background <span class="hlt">ultraviolet</span> absorption reagent and the concentration of hydrogen ion in the ion chromatography-indirect <span class="hlt">ultraviolet</span> detection. The successful separation and detection of Li(+) , Na(+) , K(+) , and NH4 (+) within 13 min was achieved using the selected chromatographic conditions, and the detection limits (S/N = 3) were 0.02, 0.11, 0.30, and 0.06 mg/L, respectively. A new separation and analysis method of alkali metal ions and ammonium by ion chromatography with indirect <span class="hlt">ultraviolet</span> detection method was developed, and the application range of ionic liquid was expanded. © 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4414538','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4414538"><span>The Influence of the Environment and Clothing on Human Exposure to <span class="hlt">Ultraviolet</span> Light</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Liu, Jin; Zhang, Wei</p> <p>2015-01-01</p> <p>Objection The aim of this study is to determine the effect of clothing and the environment on human exposure to <span class="hlt">ultraviolet</span> light. Methods The <span class="hlt">ultraviolet</span> (<span class="hlt">ultraviolet</span> A and <span class="hlt">ultraviolet</span> B) light intensity was measured, and air quality parameters were recorded in 2014 in Beijing, China. Three types of clothing (white polyester cloth, pure cotton white T-shirt, and pure cotton black T-shirt) were individually placed on a mannequin. The <span class="hlt">ultraviolet</span> (<span class="hlt">ultraviolet</span> A and <span class="hlt">ultraviolet</span> B) light intensities were measured above and beneath each article of clothing, and the percentage of <span class="hlt">ultraviolet</span> light transmission through the clothing was calculated. Results (1) The <span class="hlt">ultraviolet</span> light transmission was significantly higher through white cloth than through black cloth; the transmission was significantly higher through polyester cloth than through cotton. (2) The weather significantly influenced <span class="hlt">ultraviolet</span> light transmission through white polyester cloth; transmission was highest on clear days and lowest on overcast days (<span class="hlt">ultraviolet</span> A: P=0.000; <span class="hlt">ultraviolet</span> B: P=0.008). (3) Air quality parameters (air quality index and particulate matter 2.5 and 10) were inversely related to the <span class="hlt">ultraviolet</span> light intensity that reached the earth’s surface. <span class="hlt">Ultraviolet</span> B transmission through white polyester cloth was greater under conditions of low air pollution compared with high air pollution. Conclusion Clothing color and material and different types of weather affected <span class="hlt">ultraviolet</span> light transmission; for one particular cloth, the transmission decreased with increasing air pollution. PMID:25923778</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19740027482&hterms=background+fluorescence&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dbackground%2Bfluorescence','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19740027482&hterms=background+fluorescence&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dbackground%2Bfluorescence"><span>Fluorescence of molecular hydrogen excited by solar extreme-<span class="hlt">ultraviolet</span> radiation</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.; Fastie, W. G.</p> <p>1973-01-01</p> <p>During trans-earth coast, the Apollo 17 <span class="hlt">ultraviolet</span> spectrometer was scheduled to make observations of the far <span class="hlt">ultraviolet</span> background in selected regions of the sky. In the course of one of these observations, the spacecraft fuel cells were routinely purged of excess hydrogen and water vapor. The <span class="hlt">ultraviolet</span> fluorescence spectrum of the purged molecular hydrogen excited by solar extreme <span class="hlt">ultraviolet</span> radiation is interpreted by absorption of solar L-beta and L-gamma radiation in the nearly resonant (6, 0) and (11, 0) Lyman bands. The results are deemed significant for <span class="hlt">ultraviolet</span> spectroscopic investigations of the atmospheres of the moon and planets since Lyman-band fluorescence provides an unambiguous means of identification of molecular hydrogen in upper atmospheres.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3362352','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3362352"><span>Prediction of skin cancer occurrence by <span class="hlt">ultraviolet</span> solar index</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Rivas, Miguel; Rojas, Elisa; Calaf, Gloria M.</p> <p>2012-01-01</p> <p>An increase in the amount of solar <span class="hlt">ultraviolet</span> light that reaches the Earth is considered to be responsible for the worldwide increase in skin cancer. It has been reported that exposure to excessive levels of solar <span class="hlt">ultraviolet</span> light has multiple effects, which can be harmful to humans. Experimental <span class="hlt">ultraviolet</span> light measurements were obtained in several locations in Chile between 2006 and 2009 using wide-band solar light Biometer YES, calibrated according to World Meteorological Organization (WMO) criteria and integrated into the National Meteorological Center of Chile <span class="hlt">ultraviolet</span> network (DMC). The aim of this study was to determine skin cancer rates in relation to experimental data accumulated during one year of studying the solar <span class="hlt">ultraviolet</span> index in Chile, in order to explain the possible effect of radiation on skin cancer. The rate of skin cancer per 100,000 persons was considered in Arica, Santiago, Concepción and Valdivia and extrapolated to other cities. Results of the present study showed that the incidence of skin cancer was markedly correlated with accumulative <span class="hlt">ultraviolet</span> radiation, and rates of skin cancer could be extrapolated to other locations in Chile. There is a steady increase in the rate of skin cancer in cities located nearest to the equator (low latitude) that receive greater accumulated solar <span class="hlt">ultraviolet</span> radiation, due to the accumulative effects of this type of radiation on the skin. It can be concluded that Arica is a city at sea level that receives higher levels of <span class="hlt">ultraviolet</span> solar radiation than other locations, which may explain the higher prevalence of skin cancer in the population of this location, compared with other cities in Chile. PMID:22741013</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=PIA04584&hterms=Ripple&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DRipple','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=PIA04584&hterms=Ripple&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DRipple"><span>Large, <span class="hlt">Bright</span> Wind Ripples</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>2003-01-01</p> <p>MGS MOC Release No. MOC2-397, 20 June 2003<p/>This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows large, relatively <span class="hlt">bright</span> ripples of windblown sediment in the Sinus Sabaeus region south of Schiaparelli Basin. The surrounding substrate is thickly mantled by very dark material, possibly windblown silt that settled out of the atmosphere. The picture is located near 7.1oS, 343.7oW. Sunlight illuminates the scene from the left.<p/></p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015NIMPB.348...34M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015NIMPB.348...34M"><span>Transport of a high <span class="hlt">brightness</span> proton beam through the Munich tandem accelerator</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Moser, M.; Greubel, C.; Carli, W.; Peeper, K.; Reichart, P.; Urban, B.; Vallentin, T.; Dollinger, G.</p> <p>2015-04-01</p> <p>Basic requirement for ion microprobes with sub-μm beam focus is a high <span class="hlt">brightness</span> beam to fill the small phase space usually accepted by the ion microprobe with enough ion current for the desired application. We performed beam transport simulations to optimize beam <span class="hlt">brightness</span> transported through the Munich tandem accelerator. This was done under the constraint of a maximum ion current of 10 μA that is allowed to be injected due to radiation safety regulations and beam power constrains. The main influence of the stripper foil in conjunction with intrinsic astigmatism in the beam transport on beam <span class="hlt">brightness</span> is discussed. The calculations show possibilities for <span class="hlt">brightness</span> enhancement by using astigmatism corrections and asymmetric filling of the phase space volume in the x- and y-direction.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/872688','DOE-PATENT-XML'); return false;" href="https://www.osti.gov/servlets/purl/872688"><span>Photoresist composition for extreme <span class="hlt">ultraviolet</span> lithography</span></a></p> <p><a target="_blank" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p>Felter, T. E.; Kubiak, G. D.</p> <p>1999-01-01</p> <p>A method of producing a patterned array of features, in particular, gate apertures, in the size range 0.4-0.05 .mu.m using projection lithography and extreme <span class="hlt">ultraviolet</span> (EUV) radiation. A high energy laser beam is used to vaporize a target material in order to produce a plasma which in turn, produces extreme <span class="hlt">ultraviolet</span> radiation of a characteristic wavelength of about 13 nm for lithographic applications. The radiation is transmitted by a series of reflective mirrors to a mask which bears the pattern to be printed. The demagnified focused mask pattern is, in turn, transmitted by means of appropriate optics and in a single exposure, to a substrate coated with photoresists designed to be transparent to EUV radiation and also satisfy conventional processing methods. A photoresist composition for extreme <span class="hlt">ultraviolet</span> radiation of boron carbide polymers, hydrochlorocarbons and mixtures thereof.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016ApJ...820L..10J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016ApJ...820L..10J"><span>Extreme <span class="hlt">Brightness</span> Temperatures and Refractive Substructure in 3C273 with RadioAstron</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Johnson, Michael D.; Kovalev, Yuri Y.; Gwinn, Carl R.; Gurvits, Leonid I.; Narayan, Ramesh; Macquart, Jean-Pierre; Jauncey, David L.; Voitsik, Peter A.; Anderson, James M.; Sokolovsky, Kirill V.; Lisakov, Mikhail M.</p> <p>2016-03-01</p> <p>Earth-space interferometry with RadioAstron provides the highest direct angular resolution ever achieved in astronomy at any wavelength. RadioAstron detections of the classic quasar 3C 273 on interferometric baselines up to 171,000 km suggest <span class="hlt">brightness</span> temperatures exceeding expected limits from the “inverse-Compton catastrophe” by two orders of magnitude. We show that at 18 cm, these estimates most likely arise from refractive substructure introduced by scattering in the interstellar medium. We use the scattering properties to estimate an intrinsic <span class="hlt">brightness</span> temperature of 7× {10}12 {{K}}, which is consistent with expected theoretical limits, but which is ˜15 times lower than estimates that neglect substructure. At 6.2 cm, the substructure influences the measured values appreciably but gives an estimated <span class="hlt">brightness</span> temperature that is comparable to models that do not account for the substructure. At 1.35 {{cm}}, the substructure does not affect the extremely high inferred <span class="hlt">brightness</span> temperatures, in excess of {10}13 {{K}}. We also demonstrate that for a source having a Gaussian surface <span class="hlt">brightness</span> profile, a single long-baseline estimate of refractive substructure determines an absolute minimum <span class="hlt">brightness</span> temperature, if the scattering properties along a given line of sight are known, and that this minimum accurately approximates the apparent <span class="hlt">brightness</span> temperature over a wide range of total flux densities.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017APS..DFD.G4004K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017APS..DFD.G4004K"><span>Observation of <span class="hlt">Bright</span> Ring Phenomenon for Red Blood Cells by Lattice Boltzmann Method</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kim, Young Woo; Moon, Ji Young; Lee, Joon Sang</p> <p>2017-11-01</p> <p>RBC (Red Blood Cell) aggregation is one of interests for various biomechanical fields such as cell chip or visualization. The unique phenomenon called ``<span class="hlt">bright</span> ring'' is due to RBC aggregation in pulsatile flow of blood. Shear rate and flow acceleration on RBC causes them to repeat aggregating and scattering from center of the channel. The reason that this phenomenon is called <span class="hlt">bright</span> ring is because that when observed by ultrasound imaging, the <span class="hlt">bright</span> ring occurs periodically. Many studies tried to observe this <span class="hlt">bright</span> ring phenomenon experimentally. However, there are yet not many studies trying to make use of this phenomenon for practical purposes. <span class="hlt">Bright</span> ring phenomenon has high potential when used for cell separation or other microchip devices. In this paper, the Lattice Boltzmann method is used to control this <span class="hlt">bright</span> ring phenomenon. The purpose of this paper is to find conditions when <span class="hlt">bright</span> ring phenomenon occurs, and to control the aggregating-scattering frequency and degree. Deformability of RBC is calculated following the work of Moon JY et al. (2016). The result of this paper could be further extended to the optimization of cell-separating microchips. This work was also supported by the National Research Foundation of Korea (NRF) Grant funded by the Korean Government (MSIP) (No. 2015R1A5A1037668) and Brain Korea 21 Plus.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1412904-asas-sn-bright-supernova-catalogue','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1412904-asas-sn-bright-supernova-catalogue"><span>The ASAS-SN <span class="hlt">bright</span> supernova catalogue – I. 2013–2014</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Holoien, T. W. -S.; Stanek, K. Z.; Kochanek, C. S.; ...</p> <p>2016-09-12</p> <p>We present basic statistics for all supernovae discovered by the All-Sky Automated Survey for SuperNovae (ASAS-SN) during its first year-and-a-half of operations, spanning 2013 and 2014. We also present the same information for all other <span class="hlt">bright</span> (m V ≤ 17), spectroscopically confirmed supernovae discovered from 2014 May 1 through the end of 2014, providing a comparison to the ASAS-SN sample starting from the point where ASAS-SN became operational in both hemispheres. In addition, we present collected redshifts and near-UV through IR magnitudes, where available, for all host galaxies of the <span class="hlt">bright</span> supernovae in both samples. This work represents a comprehensivemore » catalogue of <span class="hlt">bright</span> supernovae and their hosts from multiple professional and amateur sources, allowing for population studies that were not previously possible because the all-sky emphasis of ASAS-SN redresses many previously existing biases. In particular, ASAS-SN systematically finds <span class="hlt">bright</span> supernovae closer to the centres of host galaxies than either other professional surveys or amateurs, a remarkable result given ASAS-SN's poorer angular resolution. In conclusion, this is the first of a series of yearly papers on <span class="hlt">bright</span> supernovae and their hosts that will be released by the ASAS-SN team.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19920046809&hterms=sos&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D80%26Ntt%3Dsos','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19920046809&hterms=sos&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D80%26Ntt%3Dsos"><span>A catalog of low surface <span class="hlt">brightness</span> galaxies - List II</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Schombert, James M.; Bothun, Gregory D.; Schneider, Stephen E.; Mcgaugh, Stacy S.</p> <p>1992-01-01</p> <p>A list of galaxies characterized by low surface <span class="hlt">brightness</span> (LSB) is presented which facilitates the recognition of galaxies with <span class="hlt">brightnesses</span> close to that of the sky. A total of 198 objects and 140 objects are listed in the primary and secondary catalogs respectively, and LSB galaxies are examined by means of H I redshift distributions. LSB disk galaxies are shown to have similar sizes and masses as the high-surface-<span class="hlt">brightness</span> counterparts, and ellipticals and SOs are rarely encountered. Many LSB spirals have stellarlike nuclei, and most of the galaxies in the present catalog are late-type galaxies in the Sc, Sm, and Im classes. The LSB region of observational parameter space is shown to encompass a spectrum of types as full as that of the Hubble sequence. It is suggested that studies of LSB galaxies can provide important data regarding the formation and star-formation history of all galaxies.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014SPIE.9086E..0CE','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014SPIE.9086E..0CE"><span>High-<span class="hlt">brightness</span> displays in integrated weapon sight systems</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Edwards, Tim; Hogan, Tim</p> <p>2014-06-01</p> <p>In the past several years Kopin has demonstrated the ability to provide ultra-high <span class="hlt">brightness</span>, low power display solutions in VGA, SVGA, SXGA and 2k x 2k display formats. This paper will review various approaches for integrating high <span class="hlt">brightness</span> overlay displays with existing direct view rifle sights and augmenting their precision aiming and targeting capability. Examples of overlay display systems solutions will be presented and discussed. This paper will review significant capability enhancements that are possible when augmenting the real-world as seen through a rifle sight with other soldier system equipment including laser range finders, ballistic computers and sensor systems.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/10607020','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/10607020"><span>Effects of evening <span class="hlt">bright</span> light exposure on melatonin, body temperature and sleep.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Bunnell; Treiber; Phillips; Berger</p> <p>1992-03-01</p> <p>Five male subjects were exposed to a single 2-h period of <span class="hlt">bright</span> (2500 lux) or dim (<100 lux) light prior to sleep on two consecutive nights. The two conditions were repeated the following week in opposite order. <span class="hlt">Bright</span> light significantly suppressed salivary melatonin and raised rectal temperature 0.3 degrees C (which remained elevated during the first 1.5 h of sleep), without affecting tympanic temperature. <span class="hlt">Bright</span> light also increased REM latency, NREM period length, EEG spectral power in low frequency, 0.75-8 Hz and sigma, 12-14 Hz (sleep spindle) bandwidths during the first hour of sleep, and power of all frequency bands (0.5-32 Hz) within the first NREMP. Potentiation of EEG slow wave activity (0.5-4.0 Hz) by <span class="hlt">bright</span> light persisted through the end of the second NREMP. The enhanced low-frequency power and delayed REM sleep after <span class="hlt">bright</span> light exposure could represent a circadian phase-shift and/or the effect of an elevated rectal temperature, possibly mediated by the suppression of melatonin.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25385545','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25385545"><span>Relative ordering between <span class="hlt">bright</span> and dark excitons in single-walled carbon nanotubes.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Zhou, Weihang; Nakamura, Daisuke; Liu, Huaping; Kataura, Hiromichi; Takeyama, Shojiro</p> <p>2014-11-11</p> <p>The ordering and relative energy splitting between <span class="hlt">bright</span> and dark excitons are critical to the optical properties of single-walled carbon nanotubes (SWNTs), as they eventually determine the radiative and non-radiative recombination processes of generated carriers. In this work, we report systematic high-field magneto-optical study on the relative ordering between <span class="hlt">bright</span> and dark excitons in SWNTs. We identified the relative energy position of the dark exciton unambiguously by brightening it in ultra-high magnetic field. The <span class="hlt">bright</span>-dark excitonic ordering was found to depend not only on the tube structure, but also on the type of transitions. For the 1(st) sub-band transition, the <span class="hlt">bright</span> exciton appears to be higher in energy than its dark counterpart for any chiral species and is robust against environmental effect. While for the 2(nd) sub-band, their relative ordering was found to be chirality-sensitive: the <span class="hlt">bright</span> exciton can be either higher or lower than the dark one, depending on the specific nanotube structures. These findings provide new clues for engineering the optical and electronic properties of SWNTs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017JPhCS.884a2141P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017JPhCS.884a2141P"><span>Tolerance of <span class="hlt">brightness</span> and contrast adjustments on chronic apical abscess and apical granuloma interpretation</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Purnamasari, L.; Iskandar, H. H. B.; Makes, B. N.</p> <p>2017-08-01</p> <p>In digitized radiography techniques, adjusting the image enhancement can improve the subjective image quality by optimizing the <span class="hlt">brightness</span> and contrast for diagnostic needs. To determine the value range of image enhancement (<span class="hlt">brightness</span> and contrast) on chronic apical abscess and apical granuloma interpretation. 30 periapical radiographs that diagnosed chronic apical abscess and 30 that diagnosed apical granuloma were adjusted by changing <span class="hlt">brightness</span> and contrast values. The value range of <span class="hlt">brightness</span> and contrast adjustment that can be tolerated in radiographic interpretations of chronic apical abscess and apical granuloma spans from -10 to +10. <span class="hlt">Brightness</span> and contrast adjustments on digital radiographs do not affect the radiographic interpretation of chronic apical abscess and apical granuloma if conducted within the value range.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1994AAS...185.1217D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1994AAS...185.1217D"><span>Modelling and Display of the <span class="hlt">Ultraviolet</span> Sky</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Daniels, J.; Henry, R.; Murthy, J.; Allen, M.; McGlynn, T. A.; Scollick, K.</p> <p>1994-12-01</p> <p>A computer program is currently under development to model in 3D - one dimension of which is wavelength - all the known and major speculated sources of <span class="hlt">ultraviolet</span> (900 A - 3100 A ) radiation over the celestial sphere. The software is being written in Fortran 77 and IDL and currently operates under IRIX (the operating system of the Silicon Graphics Iris Machine); all output models are in FITS format. Models along with display software will become available to the astronomical community. The <span class="hlt">Ultraviolet</span> Sky Model currently includes the Zodiacal Light, Point Sources of Emission, and the Diffuse Galactic Light. The <span class="hlt">Ultraviolet</span> Sky Model is currently displayed using SkyView: a package under development at NASA/ GSFC, which allows users to retrieve and display publically available all-sky astronomical survey data (covering many wavebands) over the Internet. We present a demonstration of the SkyView display of the <span class="hlt">Ultraviolet</span> Model. The modelling is a five year development project: the work illustrated here represents product output at the end of year one. Future work includes enhancements to the current models and incorporation of the following models: Galactic Molecular Hydrogen Fluorescence; Galactic Highly Ionized Atomic Line Emission; Integrated Extragalactic Light; and speculated sources in the intergalactic medium such as Ionized Plasma and radiation from Non-Baryonic Particle Decay. We also present a poster which summarizes the components of the <span class="hlt">Ultraviolet</span> Sky Model and outlines a further package that will be used to display the <span class="hlt">Ultraviolet</span> Model. This work is supported by United States Air Force Contract F19628-93-K-0004. Dr J. Daniels is supported with a post-doctoral Fellowship from the Leverhulme Foundation, London, United Kingdom. We are also grateful for the encouragement of Dr Stephen Price (Phillips Laboratory, Hanscomb Air Force Base, MA)</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22348338-ultraviolet-bright-slowly-declining-transient-ps1-partial-tidal-disruption-event','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22348338-ultraviolet-bright-slowly-declining-transient-ps1-partial-tidal-disruption-event"><span>The <span class="hlt">ultraviolet-bright</span>, slowly declining transient PS1-11af as a partial tidal disruption event</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>Chornock, R.; Berger, E.; Zauderer, B. A.</p> <p>2014-01-01</p> <p>We present the Pan-STARRS1 discovery of the long-lived and blue transient PS1-11af, which was also detected by Galaxy Evolution Explorer with coordinated observations in the near-<span class="hlt">ultraviolet</span> (NUV) band. PS1-11af is associated with the nucleus of an early type galaxy at redshift z = 0.4046 that exhibits no evidence for star formation or active galactic nucleus activity. Four epochs of spectroscopy reveal a pair of transient broad absorption features in the UV on otherwise featureless spectra. Despite the superficial similarity of these features to P-Cygni absorptions of supernovae (SNe), we conclude that PS1-11af is not consistent with the properties of knownmore » types of SNe. Blackbody fits to the spectral energy distribution are inconsistent with the cooling, expanding ejecta of a SN, and the velocities of the absorption features are too high to represent material in homologous expansion near a SN photosphere. However, the constant blue colors and slow evolution of the luminosity are similar to previous optically selected tidal disruption events (TDEs). The shape of the optical light curve is consistent with models for TDEs, but the minimum accreted mass necessary to power the observed luminosity is only ∼0.002 M {sub ☉}, which points to a partial disruption model. A full disruption model predicts higher bolometric luminosities, which would require most of the radiation to be emitted in a separate component at high energies where we lack observations. In addition, the observed temperature is lower than that predicted by pure accretion disk models for TDEs and requires reprocessing to a constant, lower temperature. Three deep non-detections in the radio with the Very Large Array over the first two years after the event set strict limits on the production of any relativistic outflow comparable to Swift J1644+57, even if off-axis.« 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_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://hdl.handle.net/2060/20160002400','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20160002400"><span><span class="hlt">Bright</span> Stuff on Ceres = Sulfates and Carbonates on CI Chondrites</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Zolensky, Michael; Chan, Queenie H. S.; Gounelle, Matthieu; Fries, Marc</p> <p>2016-01-01</p> <p>Recent reports of the DAWN spacecraft's observations of the surface of Ceres indicate that there are <span class="hlt">bright</span> areas, which can be explained by large amounts of the Mg sulfate hexahydrate (MgSO4•6(H2O)), although the identification appears tenuous. There are preliminary indications that water is being evolved from these <span class="hlt">bright</span> areas, and some have inferred that these might be sites of contemporary hydro-volcanism. A heat source for such modern activity is not obvious, given the small size of Ceres, lack of any tidal forces from nearby giant planets, probable age and presumed bulk composition. We contend that observations of chondritic materials in the lab shed light on the nature of the <span class="hlt">bright</span> spots on Ceres</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19720004119','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19720004119"><span>The difficulty of <span class="hlt">ultraviolet</span> emssion from supernovae</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Colgate, S. A.</p> <p>1971-01-01</p> <p>There are certain conceptual difficulties in the theory of the generation of <span class="hlt">ultraviolet</span> radiation which is presumed for the creation of the optical fluorescence mechanism of supernova light emission and ionization of a nebula as large as the Gum nebula. Requirements concerning the energy distribution of the <span class="hlt">ultraviolet</span> photons are: 1) The energy of the greater part of the photons must be sufficient to cause both helium fluorescence and hydrogen ionization. 2) If the photons are emitted in an approximate black body spectrum, the fraction of energy emitted in the optical must be no more than what is already observed. <span class="hlt">Ultraviolet</span> black body emission depends primarily on the energy source. The probability that the wide mixture of elements present in the interstellar medium and supernova ejecta results in an emission localized in a limited region with less than 0.001 emission in the visible, for either ionization or fluorescence <span class="hlt">ultraviolet</span>, is remote. Therefore transparent emission must be excluded as unlikely, and black body or at least quasi-black-body emission is more probable.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1980SPIE..229...21U','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1980SPIE..229...21U"><span>Occupational Skin Hazards From <span class="hlt">Ultraviolet</span> (UV) Exposures</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Urbach, F.; Wolbarsht, M. L.</p> <p>1980-10-01</p> <p>The various types of UV effects on the skin are classified according to the part of the spectrum and their beneficial or deleterious nature. Some hazardous <span class="hlt">ultraviolet</span> sources used in industrial processes are described, and examples of photoallergy, phototoxicity, and photosensitization resulting from UV exposures are given. The incidence of skin cancer as a function of geographical location and exposure to sunlight is discussed in relation to natural and artificial exposures to long and short wavelength UV, especially in connection with tanning booths. The conclusion is reached that there is enough <span class="hlt">ultraviolet</span> in a normal environment to propose a hazard, and additional <span class="hlt">ultraviolet</span> exposure from industrial or consumer sources is not necessary, and should be eliminated wherever possible.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1981SPIE..279..201U','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1981SPIE..279..201U"><span>Occupational Skin Hazards From <span class="hlt">Ultraviolet</span> (UV) Exposures</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Urbach, F.; Wolbarsht, M. L.</p> <p>1981-11-01</p> <p>The various types of UV effects on the skin are classified according to the part of the spectrum and their beneficial or deleterious nature. Some hazardous <span class="hlt">ultraviolet</span> sources used in industrial processes are described, and examples of photoallergy, phototoxicity, and photosensitization resulting from UV exposures are given. The incidence of skin cancer as a function of geographical location and exposure to sunlight is discussed in relation to natural and artificial exposures to long and short wavelength UV, especially in connection with tanning booths. The conclusion is reached that there is enough <span class="hlt">ultraviolet</span> in a normal environment to propose a hazard, and additional <span class="hlt">ultraviolet</span> exposure from industrial or consumer sources is not necessary, and should be eliminated wherever possible.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013DPS....4521104G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013DPS....4521104G"><span>The <span class="hlt">Ultraviolet</span> Spectrograph (UVS) on ESA’s JUICE Mission</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gladstone, Randy; Retherford, K.; Steffl, A.; Eterno, J.; Davis, M.; Versteeg, M.; Greathouse, T.; Araujo, M.; Walther, B.; Persson, K.; Persyn, S.; Dirks, G.; McGrath, M.; Feldman, P.; Bagenal, F.; Spencer, J.; Schindhelm, E.; Fletcher, L.</p> <p>2013-10-01</p> <p>The Jupiter Icy Moons Explorer (JUICE) was selected in May 2012 as the first L-class mission of ESA’s Cosmic Vision Program. JUICE will launch in 2022 on a 7.6-year journey to the Jovian system, including a Venus and multiple Earth gravity assists, before entering Jupiter orbit in January 2030. JUICE will study the entire Jovian system for 3.5 years, concentrating on Europa, Ganymede, and Callisto, with the last 10 months spent in Ganymede orbit. The <span class="hlt">Ultraviolet</span> Spectrograph (UVS) on JUICE was jointly selected by NASA and ESA as part of its ~130 kg payload of 11 scientific instruments. UVS is the fifth in a series of successful <span class="hlt">ultraviolet</span> imaging spectrographs (Rosetta-Alice, New Horizons Pluto-Alice, LRO-LAMP) and is largely based on the most recent of these, Juno-UVS. It observes photons in the 55-210 nm wavelength range, at moderate spectral and spatial resolution along a 7.5-degree slit. A main entrance “airglow port” (AP) is used for most observations (e.g., airglow, aurora, surface mapping, and stellar occultations), while a separate “solar port” (SP) allows for solar occultations. Another aperture door, with a small hole through the centre, is used as a “high-spatial-resolution port” (HP) for detailed observations of <span class="hlt">bright</span> targets. Time-tagging (pixel list mode) and programmable spectral imaging (histogram mode) allow for observational flexibility and optimal data management. As on Juno-UVS, the effects of penetrating electron radiation on electronic parts and data quality are substantially mitigated through contiguous shielding, filtering of pulse height amplitudes, management of high voltage settings, and careful use of radiation-hard, flight-tested parts. The science goals of UVS are to: 1) explore the atmospheres, plasma interactions, and surfaces of the Galilean satellites; 2) determine the dynamics, chemistry, and vertical structure of Jupiter’s upper atmosphere from equator to pole; and 3) investigate the Jupiter-Io connection by</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19770041415&hterms=opal&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dopal','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19770041415&hterms=opal&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dopal"><span>Far-<span class="hlt">ultraviolet</span> imagery of the Barnard Loop Nebula</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Carruthers, G. R.; Opal, C. B.</p> <p>1977-01-01</p> <p>An electrographic Schmidt camera carried on a sounding rocket has yielded far-<span class="hlt">ultraviolet</span> (1050-2000 A and 1230-2000 A) images of the Barnard Loop Nebula and of the general background in the Orion region due to scattering of <span class="hlt">ultraviolet</span> starlight by interstellar dust particles. The total intensity in the Barnard Loop region agrees well with OAO-2 measurements, but the discrete Loop structure contributes only some 15% of the total. The measurements are consistent with a relatively high albedo for the dust grains in the far-<span class="hlt">ultraviolet</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018JASTP.169...83D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018JASTP.169...83D"><span>Response of noctilucent cloud <span class="hlt">brightness</span> to daily solar variations</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Dalin, P.; Pertsev, N.; Perminov, V.; Dubietis, A.; Zadorozhny, A.; Zalcik, M.; McEachran, I.; McEwan, T.; Černis, K.; Grønne, J.; Taustrup, T.; Hansen, O.; Andersen, H.; Melnikov, D.; Manevich, A.; Romejko, V.; Lifatova, D.</p> <p>2018-04-01</p> <p>For the first time, long-term data sets of ground-based observations of noctilucent clouds (NLC) around the globe have been analyzed in order to investigate a response of NLC to solar UV irradiance variability on a day-to-day scale. NLC <span class="hlt">brightness</span> has been considered versus variations of solar Lyman-alpha flux. We have found that day-to-day solar variability, whose effect is generally masked in the natural NLC variability, has a statistically significant effect when considering large statistics for more than ten years. Average increase in day-to-day solar Lyman-α flux results in average decrease in day-to-day NLC <span class="hlt">brightness</span> that can be explained by robust physical mechanisms taking place in the summer mesosphere. Average time lags between variations of Lyman-α flux and NLC <span class="hlt">brightness</span> are short (0-3 days), suggesting a dominant role of direct solar heating and of the dynamical mechanism compared to photodissociation of water vapor by solar Lyman-α flux. All found regularities are consistent between various ground-based NLC data sets collected at different locations around the globe and for various time intervals. Signatures of a 27-day periodicity seem to be present in the NLC <span class="hlt">brightness</span> for individual summertime intervals; however, this oscillation cannot be unambiguously retrieved due to inevitable periods of tropospheric cloudiness.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19900001486','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19900001486"><span>X-ray <span class="hlt">bright</span> points and He I lambda 10830 dark points</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Golub, L.; Harvey, K. L.; Herant, M.; Webb, D. F.</p> <p>1989-01-01</p> <p>Using near-simultaneous full disk Solar X-ray images and He I 10830 lambda, spectroheliograms from three recent rocket flights, dark points identified on the He I maps were compared with X-ray <span class="hlt">bright</span> points identified on the X-ray images. It was found that for the largest and most obvious features there is a strong correlation: most He I dark points correspond to X-ray <span class="hlt">bright</span> points. However, about 2/3 of the X-ray <span class="hlt">bright</span> points were not identified on the basis of the helium data alone. Once an X-ray feature is identified it is almost always possible to find an underlying dark patch of enhanced He I absorption which, however, would not a priori have been selected as a dark point. Therefore, the He I dark points, using current selection criteria, cannot be used as a one-to-one proxy for the X-ray data. He I dark points do, however, identify the locations of the stronger X-ray <span class="hlt">bright</span> points.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19900037527&hterms=Lambda&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D90%26Ntt%3DLambda','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19900037527&hterms=Lambda&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D90%26Ntt%3DLambda"><span>X-ray <span class="hlt">bright</span> points and He I lambda 10830 dark points</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Golub, L.; Harvey, K. L.; Herant, M.; Webb, D. F.</p> <p>1989-01-01</p> <p>Using near-simultaneous full disk Solar X-ray images and He I 10830 lambda, spectroheliograms from three recent rocket flights, dark points identified on the He I maps were compared with x-ray <span class="hlt">bright</span> points identified on the X-ray images. It was found that for the largest and most obvious features there is a strong correlation: most He I dark points correspond to X-ray <span class="hlt">bright</span> points. However, about 2/3 of the X-ray <span class="hlt">bright</span> points were not identified on the basis of the helium data alone. Once an X-ray feature is identified it is almost always possible to find an underlying dark patch of enhanced He I absorption which, however, would not a priori have been selected as a dark point. Therefore, the He I dark points, using current selection criteria, cannot be used as a one-to-one proxy for the X-ray data. He I dark points do, however, identify the locations of the stronger X-ray <span class="hlt">bright</span> points.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018A%26A...612A..84D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018A%26A...612A..84D"><span>Mapping the solar wind HI outflow velocity in the inner heliosphere by coronagraphic <span class="hlt">ultraviolet</span> and visible-light observations</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Dolei, S.; Susino, R.; Sasso, C.; Bemporad, A.; Andretta, V.; Spadaro, D.; Ventura, R.; Antonucci, E.; Abbo, L.; Da Deppo, V.; Fineschi, S.; Focardi, M.; Frassetto, F.; Giordano, S.; Landini, F.; Naletto, G.; Nicolini, G.; Nicolosi, P.; Pancrazzi, M.; Romoli, M.; Telloni, D.</p> <p>2018-05-01</p> <p>We investigated the capability of mapping the solar wind outflow velocity of neutral hydrogen atoms by using synergistic visible-light and <span class="hlt">ultraviolet</span> observations. We used polarised <span class="hlt">brightness</span> images acquired by the LASCO/SOHO and Mk3/MLSO coronagraphs, and synoptic Lyα line observations of the UVCS/SOHO spectrometer to obtain daily maps of solar wind H I outflow velocity between 1.5 and 4.0 R⊙ on the SOHO plane of the sky during a complete solar rotation (from 1997 June 1 to 1997 June 28). The 28-days data sequence allows us to construct coronal off-limb Carrington maps of the resulting velocities at different heliocentric distances to investigate the space and time evolution of the outflowing solar plasma. In addition, we performed a parameter space exploration in order to study the dependence of the derived outflow velocities on the physical quantities characterising the Lyα emitting process in the corona. Our results are important in anticipation of the future science with the Metis instrument, selected to be part of the Solar Orbiter scientific payload. It was conceived to carry out near-sun coronagraphy, performing for the first time simultaneous imaging in polarised visible-light and <span class="hlt">ultraviolet</span> H I Lyα line, so providing an unprecedented view of the solar wind acceleration region in the inner corona. The movie (see Sect. 4.2) is available at https://www.aanda.org</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19670000589','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19670000589"><span><span class="hlt">Ultraviolet</span> microscopy aids in cytological and biomedical research</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Schlenk, F.; Svihla, B.</p> <p>1967-01-01</p> <p><span class="hlt">Ultraviolet</span> microscopy is used by cytologists and biochemists to study the morphological and physiological changes in the living cell under varied culture conditions. The yeast cell is used because of its content of <span class="hlt">ultraviolet</span> absorbing materials and its lack of motility.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4083493','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4083493"><span><span class="hlt">Bright</span> to Dim Oscillatory Response of the Neurospora Circadian Oscillator</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Gooch, Van D.; Johnson, Alicia E.; Larrondo, Luis F.; Loros, Jennifer J.; Dunlap, Jay C.</p> <p>2014-01-01</p> <p>The fungus Neurospora crassa constitutes an important model system extensively used in chronobiology. Several studies have addressed how environmental cues, such as light, can reset or synchronize a circadian system. By means of an optimized firefly luciferase reporter gene and a controllable lighting system, we show that Neurospora can display molecular circadian rhythms in dim light when cultures receive <span class="hlt">bright</span> light prior to entering dim light conditions. We refer to this behavior as the “<span class="hlt">bright</span> to dim oscillatory response” (BDOR). The <span class="hlt">bright</span> light treatment can be applied up to 76 h prior to dim exposure, and it can be as short as 15 min in duration. We have characterized this response in respect to the duration of the light pulse, the time of the light pulse before dim, the intensity of dim light, and the oscillation dynamics in dim light. Although the molecular mechanism that drives the BDOR remains obscure, these findings suggest that a long-term memory of <span class="hlt">bright</span> light exists as part of the circadian molecular components. It is important to consider the ecological significance of such dim light responses in respect to how organisms naturally maintain their timing mechanism in moonlight. PMID:24492882</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24492882','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24492882"><span><span class="hlt">Bright</span> to dim oscillatory response of the Neurospora circadian oscillator.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Gooch, Van D; Johnson, Alicia E; Larrondo, Luis F; Loros, Jennifer J; Dunlap, Jay C</p> <p>2014-02-01</p> <p>The fungus Neurospora crassa constitutes an important model system extensively used in chronobiology. Several studies have addressed how environmental cues, such as light, can reset or synchronize a circadian system. By means of an optimized firefly luciferase reporter gene and a controllable lighting system, we show that Neurospora can display molecular circadian rhythms in dim light when cultures receive <span class="hlt">bright</span> light prior to entering dim light conditions. We refer to this behavior as the "<span class="hlt">bright</span> to dim oscillatory response" (BDOR). The <span class="hlt">bright</span> light treatment can be applied up to 76 h prior to dim exposure, and it can be as short as 15 min in duration. We have characterized this response in respect to the duration of the light pulse, the time of the light pulse before dim, the intensity of dim light, and the oscillation dynamics in dim light. Although the molecular mechanism that drives the BDOR remains obscure, these findings suggest that a long-term memory of <span class="hlt">bright</span> light exists as part of the circadian molecular components. It is important to consider the ecological significance of such dim light responses in respect to how organisms naturally maintain their timing mechanism in moonlight.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/21278613','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/21278613"><span>Detecting gradual visual changes in colour and <span class="hlt">brightness</span> agnosia: a double dissociation.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Nijboer, Tanja C W; te Pas, Susan F; van der Smagt, Maarten J</p> <p>2011-03-09</p> <p>Two patients, one with colour agnosia and one with <span class="hlt">brightness</span> agnosia, performed a task that required the detection of gradual temporal changes in colour and <span class="hlt">brightness</span>. The results for these patients, who showed anaverage or an above-average performance on several tasks designed to test low-level colour and luminance (contrast) perception in the spatial domain, yielded a double dissociation; the <span class="hlt">brightness</span> agnosic patient was within the normal range for the coloured stimuli, but much slower to detect <span class="hlt">brightness</span> differences, whereas the colour agnosic patient was within the normal range for the achromatic stimuli, but much slower for the coloured stimuli. These results suggest that a modality-specific impairment in the detection of gradual temporal changes might be related to, if not underlie, the phenomenon of visual agnosia.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.dtic.mil/docs/citations/ADA002369','DTIC-ST'); return false;" href="http://www.dtic.mil/docs/citations/ADA002369"><span>Sky <span class="hlt">Brightness</span> During Eclipses: A Compendium from the Literature</span></a></p> <p><a target="_blank" href="http://www.dtic.mil/">DTIC Science & Technology</a></p> <p></p> <p>1974-08-05</p> <p>86 25. Absolute Values of Luminance of the Terrain and the Sky 88 26. Sky <span class="hlt">Brightness</span> From Film No. 1 89 27. Sky <span class="hlt">Brightness</span> From Film No. 2 89 28...these twilight equivalents when dust is present in the r.tmosphere are also difficult. Both involve the passage of light through long path lengths...purposes." Ilford-Selo, HP-3 isopan film with a sensitivity of 800 H & D was used. The measurement of the photographs was performed by means of a</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://files.eric.ed.gov/fulltext/EJ1086398.pdf','ERIC'); return false;" href="http://files.eric.ed.gov/fulltext/EJ1086398.pdf"><span>The Development of Teaching and Learning in <span class="hlt">Bright</span>-Field Microscopy Technique</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>Iskandar, Yulita Hanum P.; Mahmud, Nurul Ethika; Wahab, Wan Nor Amilah Wan Abdul; Jamil, Noor Izani Noor; Basir, Nurlida</p> <p>2013-01-01</p> <p>E-learning should be pedagogically-driven rather than technologically-driven. The objectives of this study are to develop an interactive learning system in <span class="hlt">bright</span>-field microscopy technique in order to support students' achievement of their intended learning outcomes. An interactive learning system on <span class="hlt">bright</span>-field microscopy technique was…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22482905-brightness-measurement-electron-impact-gas-ion-source-proton-beam-writing-applications','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22482905-brightness-measurement-electron-impact-gas-ion-source-proton-beam-writing-applications"><span><span class="hlt">Brightness</span> measurement of an electron impact gas ion source for proton beam writing applications</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>Liu, N.; Santhana Raman, P.; Department of Electrical and Computer Engineering, National University of Singapore, Singapore 117583</p> <p></p> <p>We are developing a high <span class="hlt">brightness</span> nano-aperture electron impact gas ion source, which can create ion beams from a miniature ionization chamber with relatively small virtual source sizes, typically around 100 nm. A prototype source of this kind was designed and successively micro-fabricated using integrated circuit technology. Experiments to measure source <span class="hlt">brightness</span> were performed inside a field emission scanning electron microscope. The total output current was measured to be between 200 and 300 pA. The highest estimated reduced <span class="hlt">brightness</span> was found to be comparable to the injecting focused electron beam reduced <span class="hlt">brightness</span>. This translates into an ion reduced <span class="hlt">brightness</span> thatmore » is significantly better than that of conventional radio frequency ion sources, currently used in single-ended MeV accelerators.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/26931964','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/26931964"><span><span class="hlt">Brightness</span> measurement of an electron impact gas ion source for proton beam writing applications.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Liu, N; Xu, X; Pang, R; Raman, P Santhana; Khursheed, A; van Kan, J A</p> <p>2016-02-01</p> <p>We are developing a high <span class="hlt">brightness</span> nano-aperture electron impact gas ion source, which can create ion beams from a miniature ionization chamber with relatively small virtual source sizes, typically around 100 nm. A prototype source of this kind was designed and successively micro-fabricated using integrated circuit technology. Experiments to measure source <span class="hlt">brightness</span> were performed inside a field emission scanning electron microscope. The total output current was measured to be between 200 and 300 pA. The highest estimated reduced <span class="hlt">brightness</span> was found to be comparable to the injecting focused electron beam reduced <span class="hlt">brightness</span>. This translates into an ion reduced <span class="hlt">brightness</span> that is significantly better than that of conventional radio frequency ion sources, currently used in single-ended MeV accelerators.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19770032365&hterms=IOTA&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3DIOTA','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19770032365&hterms=IOTA&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3DIOTA"><span>The <span class="hlt">ultraviolet</span> variations of iota Cas</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Molnar, M. R.; Mallama, A. D.; Soskey, D. G.; Holm, A. V.</p> <p>1976-01-01</p> <p>The Ap variable star iota Cas was observed with the photometers on OAO-2 covering the spectral range 1430-4250 A. The <span class="hlt">ultraviolet</span> light curves show a double wave with primary minimum and maximum at phase ? 0.00 and 0.35, respectively. Secondary minimum light is at phase ? 0.65 with secondary maximum at phase ? 0.85. The light curves longward of 3150 A vary in opposition to those shortward of this 'null region'. Ground-based coude spectra show that the Fe II and Cr II line strengths have a double-wave variation such that maximum strength occurs at minimum <span class="hlt">ultraviolet</span> light. We suggest that the strong <span class="hlt">ultraviolet</span> opacities due to photoionization and line blanketing by these metals may cause the observed photometric variations. We have also constructed an oblique-rotator model which shows iron and chromium lying in a great circle band rather than in circular spots.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016ApJ...828...26M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016ApJ...828...26M"><span>Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). I. Discovery of 15 Quasars and <span class="hlt">Bright</span> Galaxies at 5.7 < z < 6.9</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Matsuoka, Yoshiki; Onoue, Masafusa; Kashikawa, Nobunari; Iwasawa, Kazushi; Strauss, Michael A.; Nagao, Tohru; Imanishi, Masatoshi; Niida, Mana; Toba, Yoshiki; Akiyama, Masayuki; Asami, Naoko; Bosch, James; Foucaud, Sébastien; Furusawa, Hisanori; Goto, Tomotsugu; Gunn, James E.; Harikane, Yuichi; Ikeda, Hiroyuki; Kawaguchi, Toshihiro; Kikuta, Satoshi; Komiyama, Yutaka; Lupton, Robert H.; Minezaki, Takeo; Miyazaki, Satoshi; Morokuma, Tomoki; Murayama, Hitoshi; Nishizawa, Atsushi J.; Ono, Yoshiaki; Ouchi, Masami; Price, Paul A.; Sameshima, Hiroaki; Silverman, John D.; Sugiyama, Naoshi; Tait, Philip J.; Takada, Masahiro; Takata, Tadafumi; Tanaka, Masayuki; Tang, Ji-Jia; Utsumi, Yousuke</p> <p>2016-09-01</p> <p>We report the discovery of 15 quasars and <span class="hlt">bright</span> galaxies at 5.7 < z < 6.9. This is the initial result from the Subaru High-z Exploration of Low-Luminosity Quasars project, which exploits the exquisite multiband imaging data produced by the Subaru Hyper Suprime-Cam (HSC) Strategic Program survey. The candidate selection is performed by combining several photometric approaches including a Bayesian probabilistic algorithm to reject stars and dwarfs. The spectroscopic identification was carried out with the Gran Telescopio Canarias and the Subaru Telescope for the first 80 deg2 of the survey footprint. The success rate of our photometric selection is quite high, approaching 100% at the brighter magnitudes (z AB < 23.5 mag). Our selection also recovered all the known high-z quasars on the HSC images. Among the 15 discovered objects, six are likely quasars, while the other six with interstellar absorption lines and in some cases narrow emission lines are likely <span class="hlt">bright</span> Lyman-break galaxies. The remaining three objects have weak continua and very strong and narrow Lyα lines, which may be excited by <span class="hlt">ultraviolet</span> light from both young stars and quasars. These results indicate that we are starting to see the steep rise of the luminosity function of z ≥ 6 galaxies, compared with that of quasars, at magnitudes fainter than M 1450 ˜ -22 mag or z AB ˜ 24 mag. Follow-up studies of the discovered objects as well as further survey observations are ongoing.</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('http://adsabs.harvard.edu/abs/2016AGUFMOS11A1778Z','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016AGUFMOS11A1778Z"><span>Death of Darkness: Artificial Sky <span class="hlt">Brightness</span> in the Anthropocene</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Zender, C. S.</p> <p>2016-12-01</p> <p>Many species (including ours) need darkness to survive and thrive yet light pollution in the anthropocene has received scant attention in Earth System Models (ESMs). Anthropogenic aerosols can brighten background sky <span class="hlt">brightness</span> and reduce the contrast between skylight and starlight. These are both aesthetic and health-related issues due to their accompanying disruption of circadian rhythms. We quantify aerosol contributions to light pollution using a single-column night sky model, NiteLite, suitable for implementation in ESMs. NiteLite accounts for physiologcal (photopic and scotopic vision, retinal diameter/age), anthropogenic (light and aerosol pollution properties), and natural (surface albedo, trace gases) effects on background <span class="hlt">brightness</span> and threshold visibility. We find that stratospheric aerosol injection contemplated as a stop-gap measure to counter global warming would increase night-sky <span class="hlt">brightness</span> by about 25%, and thus eliminate last pristine dark sky areas on Earth. Our results suggest that ESMs incorporate light pollution so that associated societal impacts can be better quantified and included in policy deliberations.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013cos..rept....5D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013cos..rept....5D"><span>Second COS FUV Lifetime Position: Verification of FUV <span class="hlt">Bright</span> Object Aperture (BOA) Operations (FCAL4)</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Debes, John H.</p> <p>2013-05-01</p> <p>As part of the calibration of the second lifetime position on the Cosmic Origins Spectrograph (COS) far-<span class="hlt">ultraviolet</span> (FUV) detectors, observations of the external target, G191-B2B, were obtained with the G130M, G160M, and G140L gratings in combi- nation with the <span class="hlt">Bright</span> Object Aperture. The observations were designed to verify the performance of these spectroscopic modes by reproducing similar observations taken during the SM4 Servicing Mission Observatory Verification (SMOV) of COS. These observations allowed for a detailed determination of the spatial location and profile of the spectra from the three gratings, as well as a determination of the spectral resolution of the G130M grating prior to and after the lifetime move. In general, the negligi- ble differences which exist between the two lifetime positions can be attributed to slight differences in the optical path. In particular, the spectral resolution appears to be slightly improved. The stability of the absolute and relative flux calibration was investigated for G130M as well using STIS echelle data of G191-B2B. We determine that the COS ab- solute flux calibration with the BOA is accurate to 10%, and flux calibrated data are reproducible at the 1-2% level since SMOV.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=PIA10006&hterms=duck+hazard&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dduck%2Bhazard','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=PIA10006&hterms=duck+hazard&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dduck%2Bhazard"><span>At <span class="hlt">Bright</span> Band Inside Victoria Crater</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>2007-01-01</p> <p><p/> A layer of light-toned rock exposed inside Victoria Crater in the Meridiani Planum region of Mars appears to mark where the surface was at the time, many millions of years ago, when an impact excavated the crater. NASA's Mars Exploration Rover Opportunity drove to this <span class="hlt">bright</span> band as the science team's first destination for the rover during investigations inside the crater. <p/> Opportunity's left front hazard-identification camera took this image just after the rover finished a drive of 2.25 meters (7 feet, 5 inches) during the rover's 1,305th Martian day, or sol, (Sept. 25, 2007). The rocks beneath the rover and its extended robotic arm are part of the <span class="hlt">bright</span> band. <p/> Victoria Crater has a scalloped shape of alternating alcoves and promontories around the crater's circumference. Opportunity descended into the crater two weeks earlier, within an alcove called 'Duck Bay.' Counterclockwise around the rim, just to the right of the arm in this image, is a promontory called 'Cabo Frio.'</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014AAS...22314832Y','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014AAS...22314832Y"><span>Winter sky <span class="hlt">brightness</span> & cloud cover over Dome A</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Yang, Yi; Moore, A. M.; Fu, J.; Ashley, M.; Cui, X.; Feng, L.; Gong, X.; Hu, Z.; Laurence, J.; LuongVan, D.; Riddle, R. L.; Shang, Z.; Sims, G.; Storey, J.; Tothill, N.; Travouillon, T.; Wang, L.; Yang, H.; Yang, J.; Zhou, X.; Zhu, Z.; Burton, M. G.</p> <p>2014-01-01</p> <p>At the summit of the Antarctic plateau, Dome A offers an intriguing location for future large scale optical astronomical Observatories. The Gattini DomeA project was created to measure the optical sky <span class="hlt">brightness</span> and large area cloud cover of the winter-time sky above this high altitude Antarctic site. The wide field camera and multi-filter system was installed on the PLATO instrument module as part of the Chinese-led traverse to Dome A in January 2008. This automated wide field camera consists of an Apogee U4000 interline CCD coupled to a Nikon fish-eye lens enclosed in a heated container with glass window. The system contains a filter mechanism providing a suite of standard astronomical photometric filters (Bessell B, V, R), however, the absence of tracking systems, together with the ultra large field of view 85 degrees) and strong distortion have driven us to seek a unique way to build our data reduction pipeline. We present here the first measurements of sky <span class="hlt">brightness</span> in the photometric B, V, and R band, cloud cover statistics measured during the 2009 winter season and an estimate of the transparency. In addition, we present example light curves for <span class="hlt">bright</span> targets to emphasize the unprecedented observational window function available from this ground-based location. A ~0.2 magnitude agreement of our simultaneous test at Palomar Observatory with NSBM(National Sky <span class="hlt">Brightness</span> Monitor), as well as an 0.04 magnitude photometric accuracy for typical 6th magnitude stars limited by the instrument design, indicating we obtained reasonable results based on our ~7mm effective aperture fish-eye lens.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018Natur.553..189B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018Natur.553..189B"><span><span class="hlt">Bright</span> triplet excitons in caesium lead halide perovskites</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Becker, Michael A.; Vaxenburg, Roman; Nedelcu, Georgian; Sercel, Peter C.; Shabaev, Andrew; Mehl, Michael J.; Michopoulos, John G.; Lambrakos, Samuel G.; Bernstein, Noam; Lyons, John L.; Stöferle, Thilo; Mahrt, Rainer F.; Kovalenko, Maksym V.; Norris, David J.; Rainò, Gabriele; Efros, Alexander L.</p> <p>2018-01-01</p> <p>Nanostructured semiconductors emit light from electronic states known as excitons. For organic materials, Hund’s rules state that the lowest-energy exciton is a poorly emitting triplet state. For inorganic semiconductors, similar rules predict an analogue of this triplet state known as the ‘dark exciton’. Because dark excitons release photons slowly, hindering emission from inorganic nanostructures, materials that disobey these rules have been sought. However, despite considerable experimental and theoretical efforts, no inorganic semiconductors have been identified in which the lowest exciton is <span class="hlt">bright</span>. Here we show that the lowest exciton in caesium lead halide perovskites (CsPbX3, with X = Cl, Br or I) involves a highly emissive triplet state. We first use an effective-mass model and group theory to demonstrate the possibility of such a state existing, which can occur when the strong spin-orbit coupling in the conduction band of a perovskite is combined with the Rashba effect. We then apply our model to CsPbX3 nanocrystals, and measure size- and composition-dependent fluorescence at the single-nanocrystal level. The <span class="hlt">bright</span> triplet character of the lowest exciton explains the anomalous photon-emission rates of these materials, which emit about 20 and 1,000 times faster than any other semiconductor nanocrystal at room and cryogenic temperatures, respectively. The existence of this <span class="hlt">bright</span> triplet exciton is further confirmed by analysis of the fine structure in low-temperature fluorescence spectra. For semiconductor nanocrystals, which are already used in lighting, lasers and displays, these excitons could lead to materials with brighter emission. More generally, our results provide criteria for identifying other semiconductors that exhibit <span class="hlt">bright</span> excitons, with potential implications for optoelectronic devices.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/21643373','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/21643373"><span><span class="hlt">Ultraviolet</span> electroluminescence from hybrid inorganic/organic ZnO/GaN/poly(3-hexylthiophene) dual heterojunctions.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Chen, Yungting; Shih, Hanyu; Wang, Chunhsiung; Hsieh, Chunyi; Chen, Chihwei; Chen, Yangfang; Lin, Taiyuan</p> <p>2011-05-09</p> <p>Based on hybrid inorganic/organic n-ZnO nanorods/p-GaN thin film/poly(3-hexylthiophene)(P3HT) dual heterojunctions, the light emitting diode (LED) emits <span class="hlt">ultraviolet</span> (UV) radiation (370 nm - 400 nm) and the whole visible light (400 nm -700 nm) at the low injection current density. Meanwhile, under the high injection current density, the UV radiation overwhelmingly dominates the room-temperature electroluminescence spectra, exponentially increases with the injection current density and possesses a narrow full width at half maximum less than 16 nm. Comparing electroluminescence with photoluminescence spectra, an enormously enhanced transition probability of the UV luminescence in the electroluminescence spectra was found. The P3HT layer plays an essential role in helping the UV emission from p-GaN material because of its hole-conductive characteristic as well as the band alignment with respect to p-GaN. With our new finding, the result shown here may pave a new route for the development of high <span class="hlt">brightness</span> LEDs derived from hybrid inorganic/organic heterojuctions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3634108','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3634108"><span>Artificial light alters natural regimes of night-time sky <span class="hlt">brightness</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>Davies, Thomas W.; Bennie, Jonathan; Inger, Richard; Gaston, Kevin J.</p> <p>2013-01-01</p> <p>Artificial light is globally one of the most widely distributed forms of anthropogenic pollution. However, while both the nature and ecological effects of direct artificial lighting are increasingly well documented, those of artificial sky glow have received little attention. We investigated how city lights alter natural regimes of lunar sky <span class="hlt">brightness</span> using a novel ten month time series of measurements recorded across a gradient of increasing light pollution. In the city, artificial lights increased sky <span class="hlt">brightness</span> to levels six times above those recorded in rural locations, nine and twenty kilometers away. Artificial lighting masked natural monthly and seasonal regimes of lunar sky <span class="hlt">brightness</span> in the city, and increased the number and annual regime of full moon equivalent hours available to organisms during the night. The changes have potentially profound ecological consequences.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/22633808','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/22633808"><span>Melanopsin-based <span class="hlt">brightness</span> discrimination in mice and humans.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Brown, Timothy M; Tsujimura, Sei-Ichi; Allen, Annette E; Wynne, Jonathan; Bedford, Robert; Vickery, Graham; Vugler, Anthony; Lucas, Robert J</p> <p>2012-06-19</p> <p>Photoreception in the mammalian retina is not restricted to rods and cones but extends to a small number of intrinsically photoreceptive retinal ganglion cells (ipRGCs), expressing the photopigment melanopsin. ipRGCs are known to support various accessory visual functions including circadian photoentrainment and pupillary reflexes. However, despite anatomical and physiological evidence that they contribute to the thalamocortical visual projection, no aspect of visual discrimination has been shown to rely upon ipRGCs. Based on their currently known roles, we hypothesized that ipRGCs may contribute to distinguishing <span class="hlt">brightness</span>. This percept is related to an object's luminance-a photometric measure of light intensity relevant for cone photoreceptors. However, the perceived <span class="hlt">brightness</span> of different sources is not always predicted by their respective luminance. Here, we used parallel behavioral and electrophysiological experiments to first show that melanopsin contributes to <span class="hlt">brightness</span> discrimination in both retinally degenerate and fully sighted mice. We continued to use comparable paradigms in psychophysical experiments to provide evidence for a similar role in healthy human subjects. These data represent the first direct evidence that an aspect of visual discrimination in normally sighted subjects can be supported by inner retinal photoreceptors. Copyright © 2012 Elsevier Ltd. All rights reserved.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017AGUFM.P31D2856M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017AGUFM.P31D2856M"><span>Discovery of a <span class="hlt">Bright</span> Equatorial Storm on Neptune</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Molter, E. M.; De Pater, I.; Alvarez, C.; Tollefson, J.; Luszcz-Cook, S.</p> <p>2017-12-01</p> <p>Images of Neptune, taken with the NIRC2 instrument during testing of the new Twilight Zone observing program at Keck Observatory, revealed an extremely large <span class="hlt">bright</span> storm system near Neptune's equator. The storm complex is ≈9,000 km across and brightened considerably between June 26 and July 2. Historically, very <span class="hlt">bright</span> clouds have occasionally been seen on Neptune, but always in the midlatitude regions between ≈15° and ≈60° North or South. Voyager and HST observations have shown that cloud features large enough to dominate near-IR photometry are often "companion" clouds of dark anti-cyclonic vortices similar to Jupiter's Great Red Spot, interpreted as orographic clouds. In the past such clouds and their coincident dark vortices often persisted for one up to several years. However, the cloud complex we detect is unique: never before has a <span class="hlt">bright</span> cloud been seen at, or so close to, the equator. The discovery points to a drastic departure in the dynamics of Neptune's atmosphere from what has been observed for the past several decades. Detections of the complex in multiple NIRC2 filters allows radiative transfer modeling to constrain the cloud's altitude and vertical extent.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/19719260','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/19719260"><span>"<span class="hlt">Bright</span>" and "dark" excited states of an alternating at oligomer characterized by femtosecond broadband spectroscopy.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Kwok, Wai-Ming; Ma, Chensheng; Phillips, David Lee</p> <p>2009-08-20</p> <p>The nature and dynamics of DNA excited states is of pivotal importance in determining both DNA <span class="hlt">ultraviolet</span> photostability and its vulnerability toward photodamage. The complexity regarding the involvement of "<span class="hlt">bright</span>" and "dark" excited states, their molecular origin, and the roles played by these states in the course of electronic energy relaxation constitute an active and contentious area in current research of DNA excited states. As a case study, we report here a combined broadband femtosecond time-resolved fluorescence (TRF) and transient absorption (TA) study on a self-complementary d(AT)(10) oligomer and a reference system of an equal molar mixture of the constituent bases represented by adenosine and thymidine (A+T). Comparison of the spectral character and temporal evolution of the TRF and TA data for 267 nm excited d(AT)(10) and A+T provides evidence for a base-localized excitation feature for an early (< approximately 50 fs) "<span class="hlt">bright</span>" S(LE) state and its ensuing evolution within approximately 3 ps into a approximately 72 ps "dark" S(E) exciplex in d(AT)(10). Combined analysis of the d(AT)(10) TRF and TA results suggests the presence of a weakly fluorescent transient S(G) state that acts as a gateway to mediate the excitation transfer and energy elimination. A distinct base conformation-dependent model involving an ultrafast approximately 0.3 ps conversion of the S(LE) to S(G) that then evolves by approximately 3 ps into the S(E) has been proposed to account for the collective deactivation character of d(AT)(10). This presents a novel excited-state picture that can unify the seemingly conflicting time-resolved results reported previously for related AT DNAs. The direct spectral and dynamical data provided here contributes important photophysical parameters for the description of the excited states of AT oligomers. The possible connection between the energy transfer giving the S(E) and the photostability vs photodamage of A/T DNAs is briefly discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19760007490','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19760007490"><span>S193 radiometer <span class="hlt">brightness</span> temperature precision/accuracy for SL2 and SL3</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Pounds, D. J.; Krishen, K.</p> <p>1975-01-01</p> <p>The precision and accuracy with which the S193 radiometer measured the <span class="hlt">brightness</span> temperature of ground scenes is investigated. Estimates were derived from data collected during Skylab missions. Homogeneous ground sites were selected and S193 radiometer <span class="hlt">brightness</span> temperature data analyzed. The precision was expressed as the standard deviation of the radiometer acquired <span class="hlt">brightness</span> temperature. Precision was determined to be 2.40 K or better depending on mode and target temperature.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016A%26A...596A..43C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016A%26A...596A..43C"><span>Non-magnetic photospheric <span class="hlt">bright</span> points in 3D simulations of the solar atmosphere</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Calvo, F.; Steiner, O.; Freytag, B.</p> <p>2016-11-01</p> <p>Context. Small-scale <span class="hlt">bright</span> features in the photosphere of the Sun, such as faculae or G-band <span class="hlt">bright</span> points, appear in connection with small-scale magnetic flux concentrations. Aims: Here we report on a new class of photospheric <span class="hlt">bright</span> points that are free of magnetic fields. So far, these are visible in numerical simulations only. We explore conditions required for their observational detection. Methods: Numerical radiation (magneto-)hydrodynamic simulations of the near-surface layers of the Sun were carried out. The magnetic field-free simulations show tiny <span class="hlt">bright</span> points, reminiscent of magnetic <span class="hlt">bright</span> points, only smaller. A simple toy model for these non-magnetic <span class="hlt">bright</span> points (nMBPs) was established that serves as a base for the development of an algorithm for their automatic detection. Basic physical properties of 357 detected nMBPs were extracted and statistically evaluated. We produced synthetic intensity maps that mimic observations with various solar telescopes to obtain hints on their detectability. Results: The nMBPs of the simulations show a mean bolometric intensity contrast with respect to their intergranular surroundings of approximately 20%, a size of 60-80 km, and the isosurface of optical depth unity is at their location depressed by 80-100 km. They are caused by swirling downdrafts that provide, by means of the centripetal force, the necessary pressure gradient for the formation of a funnel of reduced mass density that reaches from the subsurface layers into the photosphere. Similar, frequently occurring funnels that do not reach into the photosphere, do not produce <span class="hlt">bright</span> points. Conclusions: Non-magnetic <span class="hlt">bright</span> points are the observable manifestation of vertically extending vortices (vortex tubes) in the photosphere. The resolving power of 4-m-class telescopes, such as the DKIST, is needed for an unambiguous detection of them. The movie associated to Fig. 1 is available at http://www.aanda.org</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/12191006','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/12191006"><span>Morphologic examination of CD3-CD4(<span class="hlt">bright</span>) cells in rat liver.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Yamamoto, Satoshi; Sato, Yosinobu; Abo, Toru; Hatakeyama, Katsuyosi</p> <p>2002-01-01</p> <p>Recently, we found CD3-CD4(<span class="hlt">bright</span>) cells with comparative specificity for normal rat liver. In the current study, we investigated the type and form of both CD3-CD4(<span class="hlt">bright</span>) cells and CD3-CD4(dull) cells in the rat liver. The surface phenotype of hepatic mononuclear cells in Lewis rats was identified by using monoclonal antibodies including anti-CD4, anti-CD3, and antimacrophage in conjunction with two- or three-color immunofluorescence analysis. CD3-CD4(<span class="hlt">bright</span>) cells and CD3-CD4(dull) cells were examined morphologically using May-Giemsa staining and scanning electron microscopy. The distribution of CD3-CD4(<span class="hlt">bright</span>) cells and CD3-CD4(dull) cells 48 hours after intravenous administration of liposome-encapsulated dichloromethylene diphosphate was also investigated. In comparison to CD3-CD4(dull) cells, CD3-CD4(<span class="hlt">bright</span>) cells were slightly larger macrophages with abundant cytoplasmic granules, being present with comparative specificity for normal rat liver and showing negligible effects by intravenous liposome-encapsulated dichloromethylene diphosphate administration. These data suggest that in normal young rat liver these CD3-CD4(dull) and CD3-CD4(<span class="hlt">bright</span>) cells may be dendritic cells and Kupffer cells that shift from the liver to the spleen or vice versa. These cells may also be able to locally proliferate in liver or spleen due to changes in the developing liver.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/8795756','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/8795756"><span><span class="hlt">Brightness</span> discrimination test is not useful in screening for open angle glaucoma.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Peter, E; Thomas, R; Muliyil, J</p> <p>1996-06-01</p> <p><span class="hlt">Brightness</span> discrimination test (BDT) is routinely employed to assess asymmetrical optic nerve dysfunction and has been suggested as a screening test for primary open angle glaucoma (POAG). We tested the reliability and validity of BDT in the diagnosis of POAG. The study groups included 34 patients with established primary open angle glaucoma, 20 glaucoma suspects, and 33 age-sex matched controls. Cataract was not an exclusion criterion in these groups. The normal <span class="hlt">brightness</span> score was determined to be 88% (mean score, 94%-2 SD) in a pilot study. <span class="hlt">Brightness</span> discrimination test was performed in all subjects by two observers independently. BDT showed an excellent interobserver agreement (weighted Kappa 0.84). The presence of a cataract alone increased the risk of <span class="hlt">brightness</span> impairment twofold, glaucoma alone increased the risk eightfold, and the presence of both conditions by 17 times compared to those with neither condition. BDT was not a useful test in the diagnosis of POAG (sensitivity 67% and specificity 93%); the ability to detect a significant field defect was also poor (sensitivity 53% and specificity 76%). There was poor association between decreased <span class="hlt">brightness</span> scores and asymmetrical field defects as determined by the Humphrey's field analyzer (HFA).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25215794','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25215794"><span>Generalized dark-<span class="hlt">bright</span> vector soliton solution to the mixed coupled nonlinear Schrödinger equations.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Manikandan, N; Radhakrishnan, R; Aravinthan, K</p> <p>2014-08-01</p> <p>We have constructed a dark-<span class="hlt">bright</span> N-soliton solution with 4N+3 real parameters for the physically interesting system of mixed coupled nonlinear Schrödinger equations. Using this as well as an asymptotic analysis we have investigated the interaction between dark-<span class="hlt">bright</span> vector solitons. Each colliding dark-<span class="hlt">bright</span> one-soliton at the asymptotic limits includes more coupling parameters not only in the polarization vector but also in the amplitude part. Our present solution generalizes the dark-<span class="hlt">bright</span> soliton in the literature with parametric constraints. By exploiting the role of such coupling parameters we are able to control certain interaction effects, namely beating, breathing, bouncing, attraction, jumping, etc., without affecting other soliton parameters. Particularly, the results of the interactions between the bound state dark-<span class="hlt">bright</span> vector solitons reveal oscillations in their amplitudes under certain parametric choices. A similar kind of effect was also observed experimentally in the BECs. We have also characterized the solutions with complicated structure and nonobvious wrinkle to define polarization vector, envelope speed, envelope width, envelope amplitude, grayness, and complex modulation. It is interesting to identify that the polarization vector of the dark-<span class="hlt">bright</span> one-soliton evolves on a spherical surface instead of a hyperboloid surface as in the <span class="hlt">bright-bright</span> case of the mixed coupled nonlinear Schrödinger equations.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018PhRvA..97a3629G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018PhRvA..97a3629G"><span>Three-dimensional vortex-<span class="hlt">bright</span> solitons in a spin-orbit-coupled spin-1 condensate</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gautam, Sandeep; Adhikari, S. K.</p> <p>2018-01-01</p> <p>We demonstrate stable and metastable vortex-<span class="hlt">bright</span> solitons in a three-dimensional spin-orbit-coupled three-component hyperfine spin-1 Bose-Einstein condensate (BEC) using numerical solution and variational approximation of a mean-field model. The spin-orbit coupling provides attraction to form vortex-<span class="hlt">bright</span> solitons in both attractive and repulsive spinor BECs. The ground state of these vortex-<span class="hlt">bright</span> solitons is axially symmetric for weak polar interaction. For a sufficiently strong ferromagnetic interaction, we observe the emergence of a fully asymmetric vortex-<span class="hlt">bright</span> soliton as the ground state. We also numerically investigate moving solitons. The present mean-field model is not Galilean invariant, and we use a Galilean-transformed mean-field model for generating the moving solitons.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19730000469','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19730000469"><span><span class="hlt">Ultraviolet</span> reflective coating</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Schutt, J. B.</p> <p>1974-01-01</p> <p>Composition consists of dispersion of barium sulphate in aqueous solution of water-soluble inorganic binder. Binder is selected from group consisting of alkali metal sulphates. Coating exhibits high reflectance of <span class="hlt">ultraviolet</span> light to wavelengths of approximately 200.0 nm, which compares favorably with high reflectance of virgin barium sulphate power.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/908247','SCIGOV-STC'); return false;" href="https://www.osti.gov/servlets/purl/908247"><span>Method for generating extreme <span class="hlt">ultraviolet</span> with mather-type plasma accelerators for use in Extreme <span class="hlt">Ultraviolet</span> Lithography</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>Hassanein, Ahmed; Konkashbaev, Isak</p> <p></p> <p>A device and method for generating extremely short-wave <span class="hlt">ultraviolet</span> electromagnetic wave uses two intersecting plasma beams generated by two plasma accelerators. The intersection of the two plasma beams emits electromagnetic radiation and in particular radiation in the extreme <span class="hlt">ultraviolet</span> wavelength. In the preferred orientation two axially aligned counter streaming plasmas collide to produce an intense source of electromagnetic radiation at the 13.5 nm wavelength. The Mather type plasma accelerators can utilize tin, or lithium covered electrodes. Tin, lithium or xenon can be used as the photon emitting gas source.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3843830','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3843830"><span><span class="hlt">Ultraviolet</span> vision in birds: the importance of transparent eye media</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Lind, Olle; Mitkus, Mindaugas; Olsson, Peter; Kelber, Almut</p> <p>2014-01-01</p> <p><span class="hlt">Ultraviolet</span> (UV)-sensitive visual pigments are widespread in the animal kingdom but many animals, for example primates, block UV light from reaching their retina by pigmented lenses. Birds have UV-sensitive (UVS) visual pigments with sensitivity maxima around 360–373 nm (UVS) or 402–426 nm (violet-sensitive, VS). We describe how these pigments are matched by the ocular media transmittance in 38 bird species. Birds with UVS pigments have ocular media that transmit more UV light (wavelength of 50% transmittance, λT0.5, 323 nm) than birds with VS pigments (λT0.5, 358 nm). Yet, visual models predict that colour discrimination in <span class="hlt">bright</span> light is mostly dependent on the visual pigment (UVS or VS) and little on the ocular media. We hypothesize that the precise spectral tuning of the ocular media is mostly relevant for detecting weak UV signals, e.g. in dim hollow-nests of passerines and parrots. The correlation between eye size and UV transparency of the ocular media suggests little or no lens pigmentation. Therefore, only small birds gain the full advantage from shifting pigment sensitivity from VS to UVS. On the other hand, some birds with VS pigments have unexpectedly low UV transmission of the ocular media, probably because of UV blocking lens pigmentation. PMID:24258716</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2011-title21-vol8/pdf/CFR-2011-title21-vol8-sec872-6070.pdf','CFR2011'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2011-title21-vol8/pdf/CFR-2011-title21-vol8-sec872-6070.pdf"><span>21 CFR 872.6070 - <span class="hlt">Ultraviolet</span> activator for polymerization.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2011&page.go=Go">Code of Federal Regulations, 2011 CFR</a></p> <p></p> <p>2011-04-01</p> <p>... 21 Food and Drugs 8 2011-04-01 2011-04-01 false <span class="hlt">Ultraviolet</span> activator for polymerization. 872.6070 Section 872.6070 Food and Drugs FOOD AND DRUG ADMINISTRATION, DEPARTMENT OF HEALTH AND HUMAN SERVICES... polymerization. (a) Identification. An <span class="hlt">ultraviolet</span> activator for polymerization is a device that produces...</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://www.gpo.gov/fdsys/pkg/CFR-2010-title21-vol8/pdf/CFR-2010-title21-vol8-sec872-6070.pdf','CFR'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2010-title21-vol8/pdf/CFR-2010-title21-vol8-sec872-6070.pdf"><span>21 CFR 872.6070 - <span class="hlt">Ultraviolet</span> activator for polymerization.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2010&page.go=Go">Code of Federal Regulations, 2010 CFR</a></p> <p></p> <p>2010-04-01</p> <p>... 21 Food and Drugs 8 2010-04-01 2010-04-01 false <span class="hlt">Ultraviolet</span> activator for polymerization. 872.6070 Section 872.6070 Food and Drugs FOOD AND DRUG ADMINISTRATION, DEPARTMENT OF HEALTH AND HUMAN SERVICES... polymerization. (a) Identification. An <span class="hlt">ultraviolet</span> activator for polymerization is a device that produces...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20120015410','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20120015410"><span>Soil Moisture Active/Passive (SMAP) Forward <span class="hlt">Brightness</span> Temperature Simulator</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Peng, Jinzheng; Peipmeier, Jeffrey; Kim, Edward</p> <p>2012-01-01</p> <p>The SMAP is one of four first-tier missions recommended by the US National Research Council's Committee on Earth Science and Applications from Space (Earth Science and Applications from Space: National Imperatives for the Next Decade and Beyond, Space Studies Board, National Academies Press, 2007) [1]. It is to measure the global soil moisture and freeze/thaw from space. One of the spaceborne instruments is an L-band radiometer with a shared single feedhorn and parabolic mesh reflector. While the radiometer measures the emission over a footprint of interest, unwanted emissions are also received by the antenna through the antenna sidelobes from the cosmic background and other error sources such as the Sun, the Moon and the galaxy. Their effects need to be considered accurately, and the analysis of the overall performance of the radiometer requires end-to-end performance simulation from Earth emission to antenna <span class="hlt">brightness</span> temperature, such as the global simulation of L-band <span class="hlt">brightness</span> temperature simulation over land and sea [2]. To assist with the SMAP radiometer level 1B algorithm development, the SMAP forward <span class="hlt">brightness</span> temperature simulator is developed by adapting the Aquarius simulator [2] with necessary modifications. This poster presents the current status of the SMAP forward <span class="hlt">brightness</span> simulator s development including incorporating the land microwave emission model and its input datasets, and a simplified atmospheric radiative transfer model. The latest simulation results are also presented to demonstrate the ability of supporting the SMAP L1B algorithm development.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19940011958','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19940011958"><span>Variations in the Fe mineralogy of <span class="hlt">bright</span> Martian soil</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Murchie, Scott; Mustard, John; Erard, Stephane; Geissler, Paul; Singer, Robert</p> <p>1993-01-01</p> <p><span class="hlt">Bright</span> regions on Mars are interpreted as 'soil' derived by chemical alteration of crustal rocks, whose main pigmentary component is ferric oxide or oxyhydroxide. The mineralogy and mineralogic variability of ferric iron are important evidence for the evolution of Martian soil: mineralogy of ferric phases is sensitive to chemical conditions in their genetic environments, and the spatial distributions of different ferric phases would record a history of both chemical environments and physical mixing. Reflectance spectroscopic studies provide several types of evidence that discriminate possible pigmentary phases, including the position of a crystal field absorption near 0.9 microns and position and strengths of absorptions in the UV-visible wavelength region. Recent telescopic spectra and laboratory measurements of Mars soil analogs suggest that spectral features of <span class="hlt">bright</span> soil can be explained based on a single pigmentary phase, hematite (alpha-Fe2O3), occurring in both 'nanophase' and more crystalline forms. Here we report on a systematic investigation of Martian <span class="hlt">bright</span> regions using ISM imaging spectrometer data, in which we examined spatial variations in the position and shape of the approximately 0.9 microns absorption. We found both local and regional heterogeneities that indicate differences in Fe mineralogy. These results demonstrate that <span class="hlt">bright</span> soils do not represent a single lithology that has been homogenized by eolian mixing, and suggest that weathering of soils in different geologic settings has followed different physical and chemical pathways.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017A%26C....20..120M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017A%26C....20..120M"><span>JUDE: An <span class="hlt">Ultraviolet</span> Imaging Telescope pipeline</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Murthy, J.; Rahna, P. T.; Sutaria, F.; Safonova, M.; Gudennavar, S. B.; Bubbly, S. G.</p> <p>2017-07-01</p> <p>The <span class="hlt">Ultraviolet</span> Imaging Telescope (UVIT) was launched as part of the multi-wavelength Indian AstroSat mission on 28 September, 2015 into a low Earth orbit. A 6-month performance verification (PV) phase ended in March 2016, and the instrument is now in the general observing phase. UVIT operates in three channels: visible, near-<span class="hlt">ultraviolet</span> (NUV) and far-<span class="hlt">ultraviolet</span> (FUV), each with a choice of broad and narrow band filters, and has NUV and FUV gratings for low-resolution spectroscopy. We have written a software package (JUDE) to convert the Level 1 data from UVIT into scientifically useful photon lists and images. The routines are written in the GNU Data Language (GDL) and are compatible with the IDL software package. We use these programs in our own scientific work, and will continue to update the programs as we gain better understanding of the UVIT instrument and its performance. We have released JUDE under an Apache License.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=GL-2002-001248&hterms=blue+light&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3Dblue%2Blight','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=GL-2002-001248&hterms=blue+light&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3Dblue%2Blight"><span>Saturn's E Ring in <span class="hlt">Ultraviolet</span> Light</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>2002-01-01</p> <p>Visible from Earth only at times of ring plane crossing, Saturn's tenuous E Ring was discovered during the 1966 crossings and imaged again in 1980. From these observations, its color is known to be distinctively blue. The E Ring was captured in <span class="hlt">ultraviolet</span> light for the first time in this image taken with HST's Wide Field and Planetary Camera on 9 August 1995. Five individual images taken with a broadband 3000 A filter were combined, amounting to a total exposure time of 2200 sec. Shorter exposure images were also obtained with blue, red and infrared filters in order to characterize the ring's color. The peak <span class="hlt">brightness</span> of the E Ring occurs at 3.9 Saturn radii (235,000 km), coinciding with the orbit of Enceladus. In the HST images it can be traced out to a maximum distance of approximately 8 Rs (480,000 km). The vertical thickness of the ring, on the other hand, is smallest at Enceladus' orbit, with the ring puffing up noticeably at larger distances to 15,000 km or more thick. Also visible in this image, between the E Ring and the overexposed outermost part of the main rings near the lower edge of the frame, is the tenuous, thin, 6000 km-wide G Ring at 2.8 Rs (170,000 km). This is among the first earth-based observations of the G Ring, which was discovered by the Pioneer 11 spacecraft in 1979. Noticeably thinner than the E Ring and more neutral in color, the G Ring is thought to be composed of larger, macroscopic particles, and to pose a significant hazard to spacecraft. The faint diagonal band in the lower right part of the image is due to diffracted light from the heavily-overexposed planet. Credit: Phil Nicholson (Cornell University), Mark Showalter (NASA-Ames/Stanford) and NASA</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19760019131','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19760019131"><span><span class="hlt">Ultraviolet</span> corona detection sensor study</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Schmitt, R. J.; MATHERN</p> <p>1976-01-01</p> <p>The feasibility of detecting electrical corona discharge phenomena in a space simulation chamber via emission of <span class="hlt">ultraviolet</span> light was evaluated. A corona simulator, with a hemispherically capped point to plane electrode geometry, was used to generate corona glows over a wide range of pressure, voltage, current, electrode gap length and electrode point radius. Several <span class="hlt">ultraviolet</span> detectors, including a copper cathode gas discharge tube and a UV enhanced silicon photodiode detector, were evaluated in the course of the spectral intensity measurements. The performance of both silicon target vidicons and silicon intensified target vidicons was evaluated analytically using the data generated by the spectroradiometer scans and the performance data supplied by the manufacturers.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018SuMi..115...19B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018SuMi..115...19B"><span>Investigations of dark, <span class="hlt">bright</span>, combined dark-<span class="hlt">bright</span> optical and other soliton solutions in the complex cubic nonlinear Schrödinger equation with δ-potential</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Baskonus, Haci Mehmet; Sulaiman, Tukur Abdulkadir; Bulut, Hasan; Aktürk, Tolga</p> <p>2018-03-01</p> <p>In this study, using the extended sinh-Gordon equation expansion method, we construct the dark, <span class="hlt">bright</span>, combined dark-<span class="hlt">bright</span> optical, singular, combined singular solitons and singular periodic waves solutions to the complex cubic nonlinear Schrödinger equation with δ-potential. The conditions for the existence of the obtained solutions are given. To present the physical feature of the acquired result, the 2D and 3D graphs are plotted under the choice of suitable values of the parameters.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012SPIE.8322E..2MH','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012SPIE.8322E..2MH"><span>High <span class="hlt">brightness</span> electrodeless Z-Pinch EUV source for mask inspection tools</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Horne, Stephen F.; Partlow, Matthew J.; Gustafson, Deborah S.; Besen, Matthew M.; Smith, Donald K.; Blackborow, Paul A.</p> <p>2012-03-01</p> <p>Energetiq Technology has been shipping the EQ-10 Electrodeless Z-pinchTM light source since 1995. The source is currently being used for metrology, mask inspection, and resist development. Energetiq's higher <span class="hlt">brightness</span> source has been selected as the source for pre-production actinic mask inspection tools. This improved source enables the mask inspection tool suppliers to build prototype tools with capabilities of defect detection and review down to 16nm design rules. In this presentation we will present new source technology being developed at Energetiq to address the critical source <span class="hlt">brightness</span> issue. The new technology will be shown to be capable of delivering <span class="hlt">brightness</span> levels sufficient to meet the HVM requirements of AIMS and ABI and potentially API tools. The basis of the source technology is to use the stable pinch of the electrodeless light source and have a <span class="hlt">brightness</span> of up to 100W/mm(carat)2-sr. We will explain the source design concepts, discuss the expected performance and present the modeling results for the new design.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/2068210','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/2068210"><span><span class="hlt">Bright</span> light does not alter muscarinic receptor binding parameters.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Giroux, M L; Malatynska, E; Dilsaver, S C</p> <p>1991-03-01</p> <p>Seasonal Affective Disorders (SADs) are disorders of mood characterized by recurrent episodes of illness with a fixed relationship to season. Winter depression is characterized by recurrent onset of depression in the fall or winter followed by spontaneous recovery in the spring. This syndrome is responsive to treatment with <span class="hlt">bright</span> light. The pathophysiology of depressive disorders may involve central muscarinic mechanisms. This possibility led to a series of physiological studies. The authors now report that contrary to expectation, treatment with <span class="hlt">bright</span> light did not decrease the density of muscarinic receptors in either the hypothalamus or striatum.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19790050227&hterms=Krieger&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DKrieger','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19790050227&hterms=Krieger&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DKrieger"><span>Anticorrelation of X-ray <span class="hlt">bright</span> points with sunspot number, 1970-1978</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Golub, L.; Davis, J. M.; Krieger, A. S.</p> <p>1979-01-01</p> <p>Soft X-ray observations of the solar corona over the period 1970-1978 show that the number of small short-lived bipolar magnetic features (X-ray <span class="hlt">bright</span> points) varies inversely with the sunspot index. During the entire period from 1973 to 1978 most of the magnetic flux emerging at the solar surface appeared in the form of <span class="hlt">bright</span> points. In 1970, near the peak of solar cycle 20, the contributions from <span class="hlt">bright</span> points and from active regions appear to be approximately equal. These observations strongly support an earlier suggestion that the solar cycle may be characterized as an oscillator in wave-number space with relatively little variation in the average total rate of flux emergence.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.ctio.noao.edu/noao/content/Bright-Supernova-Discovered-Nearby-Galaxy-NGC-5128','SCIGOVWS'); return false;" href="http://www.ctio.noao.edu/noao/content/Bright-Supernova-Discovered-Nearby-Galaxy-NGC-5128"><span>"A <span class="hlt">Bright</span> Supernova Discovered in the Nearby Galaxy NGC 5128" | CTIO</span></a></p> <p><a target="_blank" href="http://www.science.gov/aboutsearch.html">Science.gov Websites</a></p> <p></p> <p></p> <p>Visitor's Computer Guidelines Network Connection Request Instruments Instruments by Telescope <em>IR</em> Instruments in Cen A. In the near <em>IR</em> the luminous nucleus - the <span class="hlt">bright</span> fuzzy object - of Cen A is prominent <em>IR</em> the luminous nucleus - the <span class="hlt">bright</span> fuzzy object - of Cen A is prominent, while in the u band it is</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/22095427-statics-dynamics-atomic-dark-bright-solitons-presence-impurities','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22095427-statics-dynamics-atomic-dark-bright-solitons-presence-impurities"><span>Statics and dynamics of atomic dark-<span class="hlt">bright</span> solitons in the presence of impurities</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>Achilleos, V.; Frantzeskakis, D. J.; Kevrekidis, P. G.</p> <p>2011-11-15</p> <p>Adopting a mean-field description for a two-component atomic Bose-Einstein condensate, we study the statics and dynamics of dark-<span class="hlt">bright</span> solitons in the presence of localized impurities. We use adiabatic perturbation theory to derive an equation of motion for the dark-<span class="hlt">bright</span> soliton center. We show that, counterintuitively, an attractive (repulsive) delta-like impurity, acting solely on the <span class="hlt">bright</span>-soliton component, induces an effective localized barrier (well) in the effective potential felt by the soliton; this way, dark-<span class="hlt">bright</span> solitons are reflected from (transmitted through) attractive (repulsive) impurities. Our analytical results for the small-amplitude oscillations of solitons are found to be in good agreement with resultsmore » obtained via a Bogoliubov-de Gennes analysis and direct numerical simulations.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016A%26A...585A.100B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016A%26A...585A.100B"><span>DR Tauri: Temporal variability of the <span class="hlt">brightness</span> distribution in the potential planet-forming region</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Brunngräber, R.; Wolf, S.; Ratzka, Th.; Ober, F.</p> <p>2016-01-01</p> <p>Aims: We investigate the variability of the <span class="hlt">brightness</span> distribution and the changing density structure of the protoplanetary disk around DR Tau, a classical T Tauri star. DR Tau is known for its peculiar variations from the <span class="hlt">ultraviolet</span> (UV) to the mid-infrared (MIR). Our goal is to constrain the temporal variation of the disk structure based on photometric and MIR interferometric data. Methods: We observed DR Tau with the MID-infrared Interferometric instrument (MIDI) at the Very Large Telescope Interferometer (VLTI) at three epochs separated by about nine years, two months, respectively. We fit the spectral energy distribution and the MIR visibilities with radiative transfer simulations. Results: We are able to reproduce the spectral energy distribution as well as the MIR visibility for one of the three epochs (third epoch) with a basic disk model. We were able to reproduce the very different visibility curve obtained nine years earlier with a very similar baseline (first epoch), using the same disk model with a smaller scale height. The same density distribution also reproduces the observation made with a higher spatial resolution in the second epoch, I.e. only two months before the third epoch. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, under the programs 074.C-0342(A) and 092.C-0726(A,B).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018ApJ...855L..21B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018ApJ...855L..21B"><span>Evidence for Precursors of the Coronal Hole Jets in Solar <span class="hlt">Bright</span> Points</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Bagashvili, Salome R.; Shergelashvili, Bidzina M.; Japaridze, Darejan R.; Kukhianidze, Vasil; Poedts, Stefaan; Zaqarashvili, Teimuraz V.; Khodachenko, Maxim L.; De Causmaecker, Patrick</p> <p>2018-03-01</p> <p>A set of 23 observations of coronal jet events that occurred in coronal <span class="hlt">bright</span> points has been analyzed. The focus was on the temporal evolution of the mean <span class="hlt">brightness</span> before and during coronal jet events. In the absolute majority of the cases either single or recurrent coronal jets (CJs) were preceded by slight precursor disturbances observed in the mean intensity curves. The key conclusion is that we were able to detect quasi-periodical oscillations with characteristic periods from sub-minute up to 3–4 minute values in the <span class="hlt">bright</span> point <span class="hlt">brightness</span> that precedes the jets. Our basic claim is that along with the conventionally accepted scenario of <span class="hlt">bright</span>-point evolution through new magnetic flux emergence and its reconnection with the initial structure of the <span class="hlt">bright</span> point and the coronal hole, certain magnetohydrodynamic (MHD) oscillatory and wavelike motions can be excited and these can take an important place in the observed dynamics. These quasi-oscillatory phenomena might play the role of links between different epochs of the coronal jet ignition and evolution. They can be an indication of the MHD wave excitation processes due to the system entropy variations, density variations, or shear flows. It is very likely a sharp outflow velocity transverse gradients at the edges between the open and closed field line regions. We suppose that magnetic reconnections can be the source of MHD waves due to impulsive generation or rapid temperature variations, and shear flow driven nonmodel MHD wave evolution (self-heating and/or overreflection mechanisms).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018MNRAS.478....2C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018MNRAS.478....2C"><span>Investigating a population of infrared-<span class="hlt">bright</span> gamma-ray burst host galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Chrimes, Ashley A.; Stanway, Elizabeth R.; Levan, Andrew J.; Davies, Luke J. M.; Angus, Charlotte R.; Greis, Stephanie M. L.</p> <p>2018-07-01</p> <p>We identify and explore the properties of an infrared-<span class="hlt">bright</span> gamma-ray burst (GRB) host population. Candidate hosts are selected by coincidence with sources in WISE, with matching to random coordinates and a false alarm probability analysis showing that the contamination fraction is ˜0.5. This methodology has already identified the host galaxy of GRB 080517. We combine survey photometry from Pan-STARRS, SDSS, APASS, 2MASS, GALEX, and WISE with our own WHT/ACAM and VLT/X-shooter observations to classify the candidates and identify interlopers. Galaxy SED fitting is performed using MAGPHYS, in addition to stellar template fitting, yielding 13 possible IR-<span class="hlt">bright</span> hosts. A further seven candidates are identified from the previously published work. We report a candidate host for GRB 061002, previously unidentified as such. The remainder of the galaxies have already been noted as potential hosts. Comparing the IR-<span class="hlt">bright</span> population properties including redshift z, stellar mass M⋆, star formation rate SFR, and V-band attenuation AV to GRB host catalogues in the literature, we find that the infrared-<span class="hlt">bright</span> population is biased towards low z, high M⋆, and high AV. This naturally arises from their initial selection - local and dusty galaxies are more likely to have the required IR flux to be detected in WISE. We conclude that while IR-<span class="hlt">bright</span> GRB hosts are not a physically distinct class, they are useful for constraining existing GRB host populations, particularly for long GRBs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018MNRAS.tmp..989C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018MNRAS.tmp..989C"><span>Investigating a population of infrared-<span class="hlt">bright</span> gamma-ray burst host galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Chrimes, Ashley A.; Stanway, Elizabeth R.; Levan, Andrew J.; Davies, Luke J. M.; Angus, Charlotte R.; Greis, Stephanie M. L.</p> <p>2018-04-01</p> <p>We identify and explore the properties of an infrared-<span class="hlt">bright</span> gamma-ray burst (GRB) host population. Candidate hosts are selected by coincidence with sources in WISE, with matching to random coordinates and a false alarm probability analysis showing that the contamination fraction is ˜ 0.5. This methodology has already identified the host galaxy of GRB 080517. We combine survey photometry from Pan-STARRS, SDSS, APASS, 2MASS, GALEX and WISE with our own WHT/ACAM and VLT/X-shooter observations to classify the candidates and identify interlopers. Galaxy SED fitting is performed using MAGPHYS, in addition to stellar template fitting, yielding 13 possible IR-<span class="hlt">bright</span> hosts. A further 7 candidates are identified from previously published work. We report a candidate host for GRB 061002, previously unidentified as such. The remainder of the galaxies have already been noted as potential hosts. Comparing the IR-<span class="hlt">bright</span> population properties including redshift z, stellar mass M⋆, star formation rate SFR and V-band attenuation AV to GRB host catalogues in the literature, we find that the infrared-<span class="hlt">bright</span> population is biased toward low z, high M⋆ and high AV. This naturally arises from their initial selection - local and dusty galaxies are more likely to have the required IR flux to be detected in WISE. We conclude that while IR-<span class="hlt">bright</span> GRB hosts are not a physically distinct class, they are useful for constraining existing GRB host populations, particularly for long GRBs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=EC93-03092-7&hterms=twilight&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D90%26Ntt%3Dtwilight','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=EC93-03092-7&hterms=twilight&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D90%26Ntt%3Dtwilight"><span>SR-71 Ship #1 - <span class="hlt">Ultraviolet</span> Experiment</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>1994-01-01</p> <p>NASA's SR-71 streaks into the twilight on a night/science flight from the Dryden Flight Research Center, Edwards, California. Mounted in the nose of the SR-71 was an <span class="hlt">ultraviolet</span> video camera aimed skyward to capture images of stars, asteroids and comets. The science portion of the flight is a project of the Jet Propulsion Laboratory, Pasadena, California. Two SR-71 aircraft have been used by NASA as test beds for high-speed and high-altitude aeronautical research. One early research project flown on one of Dryden's SR-71s consisted of a proposal for a series of flights using the SR-71 as a science camera platform for the Jet Propulsion Laboratory (JPL) of the California Institute of Technology, which operates under contract to NASA in much the way that NASA centers do. In March 1993, an upward-looking <span class="hlt">ultraviolet</span> (UV) video camera placed in the SR-71's nosebay studied a variety of celestial objects in the <span class="hlt">ultraviolet</span> light spectrum. The SR-71 was proposed as a test bed for the experiment because it is capable of flying at altitudes above 80,000 feet for an extended length of time. Observation of <span class="hlt">ultraviolet</span> radiation is not possible from the Earth's surface because the atmosphere's ozone layer absorbs UV rays. Study of UV radiation is important because it is known to cause skin cancer with prolonged exposure. UV radiation is also valuable to study from an astronomical perspective. Satellite study of <span class="hlt">ultraviolet</span> radiation is very expensive. As a result, the South West Research Institute (SWRI) in Texas developed the hypothesis of using a high-flying aircraft such as the SR-71 to conduct UV observations. The SR-71 is capable of flying above 90 percent of the Earth's atmosphere. The flight program was also designed to test the stability of the aircraft as a test bed for UV observation. A joint flight program was developed between the JPL and NASA's Ames-Dryden Flight Research Facility (redesignated the Dryden Flight Research Center, Edwards, California, in 1994) in</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2011-title21-vol8/pdf/CFR-2011-title21-vol8-sec878-4635.pdf','CFR2011'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2011-title21-vol8/pdf/CFR-2011-title21-vol8-sec878-4635.pdf"><span>21 CFR 878.4635 - <span class="hlt">Ultraviolet</span> lamp for tanning.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2011&page.go=Go">Code of Federal Regulations, 2011 CFR</a></p> <p></p> <p>2011-04-01</p> <p>... 21 Food and Drugs 8 2011-04-01 2011-04-01 false <span class="hlt">Ultraviolet</span> lamp for tanning. 878.4635 Section 878.4635 Food and Drugs FOOD AND DRUG ADMINISTRATION, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL DEVICES GENERAL AND PLASTIC SURGERY DEVICES Surgical Devices § 878.4635 <span class="hlt">Ultraviolet</span> lamp for...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2012-title21-vol8/pdf/CFR-2012-title21-vol8-sec878-4635.pdf','CFR2012'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2012-title21-vol8/pdf/CFR-2012-title21-vol8-sec878-4635.pdf"><span>21 CFR 878.4635 - <span class="hlt">Ultraviolet</span> lamp for tanning.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2012&page.go=Go">Code of Federal Regulations, 2012 CFR</a></p> <p></p> <p>2012-04-01</p> <p>... 21 Food and Drugs 8 2012-04-01 2012-04-01 false <span class="hlt">Ultraviolet</span> lamp for tanning. 878.4635 Section 878.4635 Food and Drugs FOOD AND DRUG ADMINISTRATION, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL DEVICES GENERAL AND PLASTIC SURGERY DEVICES Surgical Devices § 878.4635 <span class="hlt">Ultraviolet</span> lamp for...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.gpo.gov/fdsys/pkg/CFR-2014-title21-vol8/pdf/CFR-2014-title21-vol8-sec878-4635.pdf','CFR2014'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2014-title21-vol8/pdf/CFR-2014-title21-vol8-sec878-4635.pdf"><span>21 CFR 878.4635 - <span class="hlt">Ultraviolet</span> lamp for tanning.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2014&page.go=Go">Code of Federal Regulations, 2014 CFR</a></p> <p></p> <p>2014-04-01</p> <p>... 21 Food and Drugs 8 2014-04-01 2014-04-01 false <span class="hlt">Ultraviolet</span> lamp for tanning. 878.4635 Section 878.4635 Food and Drugs FOOD AND DRUG ADMINISTRATION, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL DEVICES GENERAL AND PLASTIC SURGERY DEVICES Surgical Devices § 878.4635 <span class="hlt">Ultraviolet</span> lamp for...</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.gpo.gov/fdsys/pkg/CFR-2013-title21-vol8/pdf/CFR-2013-title21-vol8-sec878-4635.pdf','CFR2013'); return false;" href="https://www.gpo.gov/fdsys/pkg/CFR-2013-title21-vol8/pdf/CFR-2013-title21-vol8-sec878-4635.pdf"><span>21 CFR 878.4635 - <span class="hlt">Ultraviolet</span> lamp for tanning.</span></a></p> <p><a target="_blank" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2013&page.go=Go">Code of Federal Regulations, 2013 CFR</a></p> <p></p> <p>2013-04-01</p> <p>... 21 Food and Drugs 8 2013-04-01 2013-04-01 false <span class="hlt">Ultraviolet</span> lamp for tanning. 878.4635 Section 878.4635 Food and Drugs FOOD AND DRUG ADMINISTRATION, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL DEVICES GENERAL AND PLASTIC SURGERY DEVICES Surgical Devices § 878.4635 <span class="hlt">Ultraviolet</span> lamp for...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA19047.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA19047.html"><span><span class="hlt">Bright</span> Feature Appears in Titan Kraken Mare</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2014-11-10</p> <p>Two Synthetic Aperture Radar (SAR) images from the radar experiment on NASA's Cassini spacecraft show that, between May 2013 and August 2014, a <span class="hlt">bright</span> feature appeared in Kraken Mare, the largest hydrocarbon sea on Saturn's moon Titan. Researchers think the <span class="hlt">bright</span> feature is likely representative of something on the hydrocarbon sea's surface, such as waves or floating debris. A similar feature appeared in Ligea Mare, another Titan sea, and was seen to evolve in appearance between 2013 and 2014 (see PIA18430). The image at left was taken on May 23, 2013 at an incidence angle of 56 degrees; the image at right was taken on August 21, 2014 at an incidence angle of 5 degrees. Incidence angle refers to the angle at which the radar beam strikes the surface. http://photojournal.jpl.nasa.gov/catalog/PIA19047</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://cfpub.epa.gov/si/si_public_record_report.cfm?dirEntryId=115958&keyword=Corals&actType=&TIMSType=+&TIMSSubTypeID=&DEID=&epaNumber=&ntisID=&archiveStatus=Both&ombCat=Any&dateBeginCreated=&dateEndCreated=&dateBeginPublishedPresented=&dateEndPublishedPresented=&dateBeginUpdated=&dateEndUpdated=&dateBeginCompleted=&dateEndCompleted=&personID=&role=Any&journalID=&publisherID=&sortBy=revisionDate&count=50','EPA-EIMS'); return false;" href="https://cfpub.epa.gov/si/si_public_record_report.cfm?dirEntryId=115958&keyword=Corals&actType=&TIMSType=+&TIMSSubTypeID=&DEID=&epaNumber=&ntisID=&archiveStatus=Both&ombCat=Any&dateBeginCreated=&dateEndCreated=&dateBeginPublishedPresented=&dateEndPublishedPresented=&dateBeginUpdated=&dateEndUpdated=&dateBeginCompleted=&dateEndCompleted=&personID=&role=Any&journalID=&publisherID=&sortBy=revisionDate&count=50"><span><span class="hlt">ULTRAVIOLET</span> PROTECTIVE PIGMENTS AND DNA DIMER INDUCTION AS RESPONSES TO <span class="hlt">ULTRAVIOLET</span> RADIATION</span></a></p> <p><a target="_blank" href="http://oaspub.epa.gov/eims/query.page">EPA Science Inventory</a></p> <p></p> <p></p> <p>Life on Earth has evolved adaptations to many environmental stresses over the epochs. One consistent stress has been exposure to <span class="hlt">ultraviolet</span> (UV) radiation. The most basic effect of UV radiation on biological systems is damage to DNA. In response to UV radiation organisms have ad...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5288790','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5288790"><span>Cell-free measurements of <span class="hlt">brightness</span> of fluorescently labeled antibodies</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Zhou, Haiying; Tourkakis, George; Shi, Dennis; Kim, David M.; Zhang, Hairong; Du, Tommy; Eades, William C.; Berezin, Mikhail Y.</p> <p>2017-01-01</p> <p>Validation of imaging contrast agents, such as fluorescently labeled imaging antibodies, has been recognized as a critical challenge in clinical and preclinical studies. As the number of applications for imaging antibodies grows, these materials are increasingly being subjected to careful scrutiny. Antibody fluorescent <span class="hlt">brightness</span> is one of the key parameters that is of critical importance. Direct measurements of the <span class="hlt">brightness</span> with common spectroscopy methods are challenging, because the fluorescent properties of the imaging antibodies are highly sensitive to the methods of conjugation, degree of labeling, and contamination with free dyes. Traditional methods rely on cell-based assays that lack reproducibility and accuracy. In this manuscript, we present a novel and general approach for measuring the <span class="hlt">brightness</span> using antibody-avid polystyrene beads and flow cytometry. As compared to a cell-based method, the described technique is rapid, quantitative, and highly reproducible. The proposed method requires less than ten microgram of sample and is applicable for optimizing synthetic conjugation procedures, testing commercial imaging antibodies, and performing high-throughput validation of conjugation procedures. PMID:28150730</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017JBO....22f5004A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017JBO....22f5004A"><span>Inactivation of Pseudomonas aeruginosa biofilm after <span class="hlt">ultraviolet</span> light-emitting diode treatment: a comparative study between <span class="hlt">ultraviolet</span> C and <span class="hlt">ultraviolet</span> B</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Argyraki, Aikaterini; Markvart, Merete; Bjørndal, Lars; Bjarnsholt, Thomas; Petersen, Paul Michael</p> <p>2017-06-01</p> <p>The objective of this study was to test the inactivation efficiency of two different light-based treatments, namely <span class="hlt">ultraviolet</span> B (UVB) and <span class="hlt">ultraviolet</span> C (UVC) irradiation, on Pseudomonas aeruginosa biofilms at different growth stages (24, 48, and 72 h grown). In our experiments, a type of AlGaN light-emitting diodes (LEDs) was used to deliver UV irradiation on the biofilms. The effectiveness of the UVB at 296 nm and UVC at 266 nm irradiations was quantified by counting colony-forming units. The survival of less mature biofilms (24 h grown) was studied as a function of UV-radiant exposure. All treatments were performed on three different biological replicates to test reproducibility. It was shown that UVB irradiation was significantly more effective than UVC irradiation in inactivating P. aeruginosa biofilms. UVC irradiation induced insignificant inactivation on mature biofilms. The fact that the UVB at 296 nm exists in daylight and has such disinfection ability on biofilms provides perspectives for the treatment of infectious diseases.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20050091485','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20050091485"><span>Line Tunable <span class="hlt">Ultraviolet</span> Laser</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Walsh, Brian M.; Barnes, Norman P.</p> <p>2004-01-01</p> <p>An <span class="hlt">ultraviolet</span> laser is demonstrated using a dual wavelength Nd:YAG oscillator, sum frequency and second harmonic process. Synchronous pulses at 1.052 and 1.319 micrometers are amplified, mixed and subsequently doubled, producing pulses at 0.293 micrometers.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/29108645','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/29108645"><span>The bidirectional congruency effect of <span class="hlt">brightness</span>-valence metaphoric association in the Stroop-like and priming paradigms.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Huang, Yanli; Tse, Chi-Shing; Xie, Jiushu</p> <p>2017-11-04</p> <p>The conceptual metaphor theory (Lakoff & Johnson, 1980, 1999) postulates a unidirectional metaphoric association between abstract and concrete concepts: sensorimotor experience activated by concrete concepts facilitates the processing of abstract concepts, but not the other way around. However, this unidirectional view has been challenged by studies that reported a bidirectional metaphoric association. In three experiments, we tested the directionality of the <span class="hlt">brightness</span>-valence metaphoric association, using Stroop-like paradigm, priming paradigm, and Stroop-like paradigm with a go/no-go manipulation. Both mean and vincentile analyses of reaction time data were performed. We showed that the directionality of <span class="hlt">brightness</span>-valence metaphoric congruency effect could be modulated by the activation level of the <span class="hlt">brightness</span>/valence information. Both <span class="hlt">brightness</span>-to-valence and valence-to-<span class="hlt">brightness</span> metaphoric congruency effects occurred in the priming paradigm, which could be attributed to the presentation of prime that pre-activated the <span class="hlt">brightness</span> or valence information. However, in the Stroop-like paradigm the metaphoric congruency effect was only observed in the <span class="hlt">brightness</span>-to-valence direction, but not in the valence-to-<span class="hlt">brightness</span> direction. When the go/no-go manipulation was used to boost the activation of word meaning in the Stroop-like paradigm, the valence-to-<span class="hlt">brightness</span> metaphoric congruency effect was observed. Vincentile analyses further revealed that valence-to-<span class="hlt">brightness</span> metaphoric congruency effect approached significance in the Stroop-like paradigm when participants' reaction times were slower (at around 490ms). The implications of the current findings on the conceptual metaphor theory and embodied cognition are discussed. Copyright © 2017 Elsevier B.V. All rights reserved.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1992AAS...181.4913C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1992AAS...181.4913C"><span>Three <span class="hlt">Bright</span> X-ray Sources in NGC 1313</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Colbert, E.; Petre, R.; Schlegel, E.</p> <p>1992-12-01</p> <p>Three <span class="hlt">bright</span> X-ray sources were detected in a recent (April/May 1991) ROSAT PSPC observation of the nearby (D ~ 4.5 Mpc) face--on barred spiral galaxy NGC 1313. Two of the sources were at positions coincident with X-ray sources detected by Fabbiano & Trinchieri (ApJ 315, 1987) in a previous (Jan 1980) Einstein IPC observation. The position of the brightest Einstein source is near the center of NGC 1313, and the second Einstein source is ~ 7' south of the ``nuclear'' source, in the outskirts of the spiral arms. A third <span class="hlt">bright</span> X-ray source was detected in the ROSAT observation ~ 7' southwest of the ``nuclear'' source. We present X-ray spectra and X-ray images for the three <span class="hlt">bright</span> sources found in the ROSAT observation of NGC 1313, and compare with previous Einstein results. Spectral analysis of these sources require them to have very large soft X-ray luminosities ( ~ 10(40) erg s(-1) ) when compared with typical X-ray sources in our Galaxy. Feasible explanations for the X-ray emission are presented. The third X-ray source is positively identified with the recently discovered (Ryder et. al., ApJ 1992) peculiar type-II supernova 1978K.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19840010054','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19840010054"><span>Observations of emission in <span class="hlt">bright</span>, low redshift quasars</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>1983-01-01</p> <p><span class="hlt">Ultraviolet</span>, infrared, and optical spectra were combined to obtain a data set sample as broad as possible in the range of hydrogen lines in individual quasars. From the measured Lyman fluxes, coupled with Balmer and Paschen line fluxes measured in these same objects, an effort was made to establish observational constraints that would guide models of the broad emission line regions of quasars. It was found that IUE spectra were generally of sufficiently high quality to derive line profiles of the <span class="hlt">ultraviolet</span> lines Lyman alpha and CIV 1550 A, which were compared to the Balmer line profiles. The objects observed and the line fluxes are tabulated. Plots of line profiles are included.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/16171276','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/16171276"><span>The treatment of early-morning awakening insomnia with 2 evenings of <span class="hlt">bright</span> light.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Lack, Leon; Wright, Helen; Kemp, Kristyn; Gibbon, Samantha</p> <p>2005-05-01</p> <p>To assess the effectiveness of brief <span class="hlt">bright</span>-light therapy for the treatment of early-morning awakening insomnia. Twenty-four healthy adults with early-morning awakening insomnia were assigned to either the <span class="hlt">bright</span>-light condition (2,500-lux white light) or the control (dim red light) condition. The circadian phase of rectal temperature and urinary melatonin rhythms were assessed with 26-hour constant routines before and after 2 evenings of light therapy. Sleep and daytime functioning were monitored using sleep diaries, activity monitors, and mood scales before light therapy and for 4 weeks during the follow-up period. While there were no significant circadian phase changes in the dim-light control group, the <span class="hlt">bright</span>-light group had significant 2-hour phase delays of circadian temperature and melatonin rhythm. Compared to pretreatment measures, over the 4-week follow-up period, the <span class="hlt">bright</span>-light group had a greater reduction of time awake after sleep onset, showed a trend toward waking later, and had a greater increase of total sleep time. Participants in the <span class="hlt">bright</span>-light condition also tended to report greater reductions of negative daytime symptoms, including significantly fewer days of feeling depressed at the 4-week follow-up, as compared with the control group. Two evenings of <span class="hlt">bright</span>-light exposure phase delayed the circadian rhythms of early-morning awakening insomniacs. It also improved diary and actigraphy sleep measures and improved some indexes of daytime functioning for up to 1 month after light exposure. The study suggests that a brief course of evening <span class="hlt">bright</span>-light therapy can be an effective treatment for early-morning awakening insomniacs who have relatively phase advanced circadian rhythms.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=PIA01179&hterms=Dark+web&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3DDark%2Bweb','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=PIA01179&hterms=Dark+web&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3DDark%2Bweb"><span>Dark and <span class="hlt">Bright</span> Ridges on Europa</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>1998-01-01</p> <p>This high-resolution image of Jupiter's moon Europa, taken by NASA's Galileo spacecraft camera, shows dark, relatively smooth region at the lower right hand corner of the image which may be a place where warm ice has welled up from below. The region is approximately 30 square kilometers in area. An isolated <span class="hlt">bright</span> hill stands within it. The image also shows two prominent ridges which have different characteristics; youngest ridge runs from left to top right and is about 5 kilometers in width (about 3.1 miles). The ridge has two <span class="hlt">bright</span>, raised rims and a central valley. The rims of the ridge are rough in texture. The inner and outer walls show <span class="hlt">bright</span> and dark debris streaming downslope, some of it forming broad fans. This ridge overlies and therefore must be younger than a second ridge running from top to bottom on the left side of the image. This dark 2 km wide ridge is relatively flat, and has smaller-scale ridges and troughs along its length.<p/>North is to the top of the picture, and the sun illuminates the surface from the upper left. This image, centered at approximately 14 degrees south latitude and 194 degrees west longitude, covers an area approximately 15 kilometers by 20 kilometers (9 miles by 12 miles). The resolution is 26 meters (85 feet) per picture element. This image was taken on December 16, 1997 at a range of 1300 kilometers (800 miles) by Galileo's solid state imaging system.<p/>The Jet Propulsion Laboratory, Pasadena, CA manages the Galileo mission for NASA's Office of Space Science, Washington, DC. JPL is an operating division of California Institute of Technology (Caltech).<p/>This image and other images and data received from Galileo are posted on the World Wide Web, on the Galileo mission home page at URL http://www.jpl.nasa.gov/ galileo.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19800016766','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19800016766"><span>The Barnes-Evans color-surface <span class="hlt">brightness</span> relation: A preliminary theoretical interpretation</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Shipman, H. L.</p> <p>1980-01-01</p> <p>Model atmosphere calculations are used to assess whether an empirically derived relation between V-R and surface <span class="hlt">brightness</span> is independent of a variety of stellar paramters, including surface gravity. This relationship is used in a variety of applications, including the determination of the distances of Cepheid variables using a method based on the Beade-Wesselink method. It is concluded that the use of a main sequence relation between V-R color and surface <span class="hlt">brightness</span> in determining radii of giant stars is subject to systematic errors that are smaller than 10% in the determination of a radius or distance for temperature cooler than 12,000 K. The error in white dwarf radii determined from a main sequence color surface <span class="hlt">brightness</span> relation is roughly 10%.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20120009384','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20120009384"><span>A Swift Look at SN 2011fe: The Earliest <span class="hlt">Ultraviolet</span> Observations of a Type Ia Supernova</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Oates, Samantha; Holland, Stephen; Immler, Stefan; Brown, Peter J.; Dawson, Kyle S.; DePasquale, Massimiliano; Gronwall, Caryl; Kuin, Paul; Mazzali, Paolo; Miline, Peter; <a style="text-decoration: none; " href="javascript:void(0); " onClick="displayelement('author_20120009384'); toggleEditAbsImage('author_20120009384_show'); toggleEditAbsImage('author_20120009384_hide'); "> <img style="display:inline; width:12px; height:12px; " src="images/arrow-up.gif" width="12" height="12" border="0" alt="hide" id="author_20120009384_show"> <img style="width:12px; height:12px; display:none; " src="images/arrow-down.gif" width="12" height="12" border="0" alt="hide" id="author_20120009384_hide"></p> <p>2012-01-01</p> <p>We present the earliest <span class="hlt">ultraviolet</span> (UV) observations of the <span class="hlt">bright</span> Type Ia supernova SN 2011fe/PTF11kly in the nearby galaxy M101 at a distance of only 6.4 Mpc. It was discovered shortly after explosion by the Palomar Transient Factory and first observed by Swift/UVOT about a day after explosion. The early UV light is well-defined, with approx. 20 data points per filter in the 5 days after explosion. With these early UV observations, we extend the near-UV template of SNe Ia to earlier times for comparison with observations at low and high redshift and report fits from semiempirical models of the explosion. We find the early UV count rates to be well fit by the superposition of two parabolic curves. Finally, we use the early UV flux measurements to examine a possible shock interaction with a non-degenerate companion. We find that even a solar mass companion at a distance of a few solar radii is unlikely at more than 95% confidence.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017JApSp..84..657K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017JApSp..84..657K"><span>Energy and Emission Characteristics of a Short-Arc Xenon Flash Lamp Under "Saturated" Optical <span class="hlt">Brightness</span> Conditions</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kamrukov, A. S.; Kireev, S. G.; Kozlov, N. P.; Shashkovskii, S. G.</p> <p>2017-09-01</p> <p>We present the results of a study of the electrical, energy, and spectral <span class="hlt">brightness</span> characteristics of an experimental three-electrode high-pressure xenon flash lamp under conditions ensuring close to maximum possible spectral <span class="hlt">brightness</span> for the xenon emission. We show that under saturated optical <span class="hlt">brightness</span> conditions (<span class="hlt">brightness</span> temperature in the visible region of the spectrum 30,000 K), emission of a pulsed discharge in xenon is quite different from the emission from an ideal blackbody: the maximum <span class="hlt">brightness</span> temperatures are 24,000 K in the short-wavelength UV region and 19,000 K in the near IR range. The relative fraction of UV radiation in the emission spectrum of the lamp is >50%, which lets us consider such lamps as promising broadband sources of radiation with high spectral <span class="hlt">brightness</span> for many important practical applications.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010SPIE.7580E..1LJ','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010SPIE.7580E..1LJ"><span><span class="hlt">Brightness</span> enhancement limits in pulsed cladding-pumped fiber Raman amplifiers</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ji, Junhua; Codemard, Christophe A.; Nilsson, Johan</p> <p>2010-02-01</p> <p>We analyze theoretically limitations on <span class="hlt">brightness</span> enhancement of a multimode pump beam into a diffraction-limited Stokes beam in efficient cladding-pumped fiber Raman amplifiers. Firstly, the power-scaling of the 1st Stokes (hence the <span class="hlt">brightness</span> enhancement) is limited by the generation of the 2nd order Stokes. Thus using a spectral waveguide filter such as a W-type fiber core, it is possible to improve this limit to nearly five times that of a normal fiber without spectral filter. Secondly, we analyze limits set by glass damage, propagation loss, and pump-signal pulse walk-off in the multimode fiber. We show that a well-designed fiber with a propagation loss of 3.5 dB/km allows for a pump-to-signal <span class="hlt">brightness</span> improvement of over 1000 times for pulses longer than 40 ns and up to 3500 times in the cw regime.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018AcSpA.192..228Z','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018AcSpA.192..228Z"><span>A high <span class="hlt">brightness</span> probe of polymer nanoparticles for biological imaging</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Zhou, Sirong; Zhu, Jiarong; Li, Yaping; Feng, Liheng</p> <p>2018-03-01</p> <p>Conjugated polymer nanoparticles (CPNs) with high <span class="hlt">brightness</span> in long wavelength region were prepared by the nano-precipitation method. Based on fluorescence resonance energy transfer (FRET) mechanism, the high <span class="hlt">brightness</span> property of the CPNs was realized by four different emission polymers. Dynamic light scattering (DLS) and scanning electron microscopy (SEM) displayed that the CPNs possessed a spherical structure and an average diameter of 75 nm. Analysis assays showed that the CPNs had excellent biocompatibility, good photostability and low cytotoxicity. The CPNs were bio-modified with a cell penetrating peptide (Tat, a targeted element) through covalent link. Based on the entire wave fluorescence emission, the functionalized CPNs1-4 can meet multichannel and high throughput assays in cell and organ imaging. The contribution of the work lies in not only providing a new way to obtain a high <span class="hlt">brightness</span> imaging probe in long wavelength region, but also using targeted cell and organ imaging.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018PhRvS..21e0703M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018PhRvS..21e0703M"><span><span class="hlt">Brightness</span> analysis of an electron beam with a complex profile</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Maesaka, Hirokazu; Hara, Toru; Togawa, Kazuaki; Inagaki, Takahiro; Tanaka, Hitoshi</p> <p>2018-05-01</p> <p>We propose a novel analysis method to obtain the core <span class="hlt">bright</span> part of an electron beam with a complex phase-space profile. This method is beneficial to evaluate the performance of simulation data of a linear accelerator (linac), such as an x-ray free electron laser (XFEL) machine, since the phase-space distribution of a linac electron beam is not simple, compared to a Gaussian beam in a synchrotron. In this analysis, the <span class="hlt">brightness</span> of undulator radiation is calculated and the core of an electron beam is determined by maximizing the <span class="hlt">brightness</span>. We successfully extracted core electrons from a complex beam profile of XFEL simulation data, which was not expressed by a set of slice parameters. FEL simulations showed that the FEL intensity was well remained even after extracting the core part. Consequently, the FEL performance can be estimated by this analysis without time-consuming FEL simulations.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016DPS....4840202G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016DPS....4840202G"><span>Juno <span class="hlt">Ultraviolet</span> Spectrograph (Juno-UVS) Observations of Jupiter during Approach</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gladstone, Randy; Versteeg, Maarten; Greathouse, Thomas K.; Hue, Vincent; Davis, Michael; Gerard, Jean-Claude; Grodent, Denis; Bonfond, Bertrand</p> <p>2016-10-01</p> <p>We present the initial results from Juno <span class="hlt">Ultraviolet</span> Spectrograph (Juno-UVS) observations of Jupiter obtained during approach in June 2016. Juno-UVS is an imaging spectrograph with a bandpass of 70<λ<205 nm. This wavelength range includes all important <span class="hlt">ultraviolet</span> (UV) emissions from the H2 bands and the H Lyman series which are produced in Jupiter's auroras, and also the absorption signatures of aurorally-produced hydrocarbons. The Juno-UVS instrument telescope has a 4 x 4 cm2 input aperture and uses an off-axis parabolic primary mirror. A flat scan mirror situated near the entrance of the telescope is used to observe at up to ±30° perpendicular to the Juno spin plane. The light is focused onto the spectrograph entrance slit, which has a "dog-bone" shape 7.2° long, in three sections of 0.2°, 0.025°, and 0.2° width (as projected onto the sky). Light entering the slit is dispersed by a toroidal grating which focuses UV light onto a curved microchannel plate (MCP) cross delay line (XDL) detector with a solar blind UV-sensitive CsI photocathode. Tantalum surrounds the spectrograph assembly to shield the detector and its electronics from high-energy electrons. All other electronics are located in Juno's spacecraft vault, including redundant low-voltage and high-voltage power supplies, command and data handling electronics, heater/actuator electronics, scan mirror electronics, and event processing electronics. The purpose of Juno-UVS is to remotely sense Jupiter's auroral morphology and <span class="hlt">brightness</span> to provide context for in situ measurements by Juno's particle instruments. Prior to Jupiter Orbit Insertion (JOI) on July 5, Juno approach observations provide a rare opportunity to correlate local solar wind conditions with Jovian auroral emissions. Some of Jupiter's auroral emissions (e.g., polar emissions) may be controlled or at least affected by the solar wind. Here we compare synoptic Juno-UVS observations of Jupiter's auroral emissions (~40 minutes per hour</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19780040454&hterms=attention+size&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Dattention%2Bsize','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19780040454&hterms=attention+size&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Dattention%2Bsize"><span>Effects of cloud size and cloud particles on satellite-observed reflected <span class="hlt">brightness</span></span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Reynolds, D. W.; Mckee, T. B.; Danielson, K. S.</p> <p>1978-01-01</p> <p>Satellite observations allowed obtaining data on the visible <span class="hlt">brightness</span> of cumulus clouds over South Park, Colorado, while aircraft observations were made in cloud to obtain the drop size distributions and liquid water content of the cloud. Attention is focused on evaluating the relationship between cloud <span class="hlt">brightness</span>, horizontal dimension, and internal microphysical structure. A Monte Carlo cloud model for finite clouds was run using different distributions of drop sizes and numbers, while varying the cloud depth and width to determine how theory would predict what the satellite would view from its given location in space. Comparison of these results to the satellite observed reflectances is presented. Theoretical results are found to be in good agreement with observations. For clouds of optical thickness between 20 and 60, monitoring cloud <span class="hlt">brightness</span> changes in clouds of uniform depth and variable width gives adequate information about a cloud's liquid water content. A cloud having a 10:1 width to depth ratio is almost reaching its maximum <span class="hlt">brightness</span> for a specified optical thickness.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/16679716','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/16679716"><span>Influences of diurnal <span class="hlt">bright</span> or dim light exposure on urine volume in humans.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Hyun, Ki-Ja; Nishimura, Shinya; Tokura, Hiromi</p> <p>2006-03-01</p> <p>We investigated with eight healthy females if 8 hr diurnal (0700 to 1500 h) <span class="hlt">bright</span> rather than dim light (5,000 vs. 80 lx) influenced urine volume. Environmental illuminance was made identical at all other times besides 07:00 to 15:00 h. The participants spent time at strictly regulated schedules in a bioclimatic chamber (26 degrees C, relative humidity 60%) for 57 h. Blood was drawn (2 ml) just before lunch in order to calculate Creatinine clearance (Ccr). Urine volume was significantly higher during wakefulness and the 8-h sleep period with <span class="hlt">bright</span> rather than dim light. Ccr was significantly higher after <span class="hlt">bright</span> light. The results were discussed in terms of suppression of the sympathetic nerve system under the influence of diurnal <span class="hlt">bright</span> light exposure. We also discussed these in terms of physiological polymorphisms.</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('https://www.osti.gov/biblio/21392570-new-fe-ix-line-identifications-using-solar-heliospheric-observatory-solar-ultraviolet-measurement-emitted-radiation-hinode-eis-joint-observations-quiet-sun','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/21392570-new-fe-ix-line-identifications-using-solar-heliospheric-observatory-solar-ultraviolet-measurement-emitted-radiation-hinode-eis-joint-observations-quiet-sun"><span>NEW Fe IX LINE IDENTIFICATIONS USING SOLAR AND HELIOSPHERIC OBSERVATORY/SOLAR <span class="hlt">ULTRAVIOLET</span> MEASUREMENT OF EMITTED RADIATION AND HINODE/EIS JOINT OBSERVATIONS OF THE QUIET SUN</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>Landi, E.; Young, P. R.</p> <p>2009-12-20</p> <p>In this work, we study joint observations of Hinode/EUV Imaging Spectrometer (EIS) and Solar and Heliospheric Observatory/Solar <span class="hlt">Ultraviolet</span> Measurement of Emitted Radiation of Fe IX lines emitted by the same level of the high energy configuration 3s {sup 2}3p {sup 5}4p. The intensity ratios of these lines are dependent on atomic physics parameters only and not on the physical parameters of the emitting plasma, so that they are excellent tools to verify the relative intensity calibration of high-resolution spectrometers that work in the 170-200 A and 700-850 A wavelength ranges. We carry out extensive atomic physics calculations to improve themore » accuracy of the predicted intensity ratio, and compare the results with simultaneous EIS-SUMER observations of an off-disk quiet Sun region. We were able to identify two <span class="hlt">ultraviolet</span> lines in the SUMER spectrum that are emitted by the same level that emits one <span class="hlt">bright</span> line in the EIS wavelength range. Comparison between predicted and measured intensity ratios, wavelengths and energy separation of Fe IX levels confirms the identifications we make. Blending and calibration uncertainties are discussed. The results of this work are important for cross-calibrating EIS and SUMER, as well as future instrumentation.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017AGUFM.P23F..04I','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017AGUFM.P23F..04I"><span>Exploring Mercury's Surface in <span class="hlt">UltraViolet</span> from Orbit</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Izenberg, N.</p> <p>2017-12-01</p> <p>The MESSENGER Mission's <span class="hlt">Ultraviolet</span> and Visible Spectrometer (UVVS) component of its Mercury Atmosphere and Surface Composition Spectrometer (MASCS) instrument obtained approximately 4600 point observations of Mercury's surface in middle <span class="hlt">ultraviolet</span> (MUV; 210 nm - 300 nm) and far <span class="hlt">ultraviolet</span> (FUV; 119.1 - 122.5 nm and 129.2 - 131.5 nm) wavelengths over the course of its orbital mission, mostly in Mercury's southern hemisphere. Given the very low (<1 to 2 wt %) average abundance of iron in the silicates of Mercury observed by multiple MESSENGER instruments, the near- to middle-<span class="hlt">ultraviolet</span> wavelengths encompassing the oxygen metal charge transfer band (<400 nm), which is more sensitive to the presence of iron than the classic 1 micron absorption band, provides potentially useful additional compositional insight into the top layer of Mercury's regolith. The presence of nano- and microphase carbon also has potentially significant expression in the <span class="hlt">ultraviolet</span>, and the interplay and variation between carbon and iron in mercury surface materials is an active area of investigation. Analysis of middle-UV surface reflectance and parameters appear to support the presence of varying amounts of carbon in different spectral or geologic units on Mercury. Far-UV reflectance data is currently under-utilized, but analysis of lunar surface by the Lunar Reconnaissance Orbiter (LRO) Lyman Alpha Mapping Project (LAMP) indicate that the data are sensitive to both composition and space weathering. The far-UV reflectance from MASCS may provide similar information for the Mercury surface, complementing results from longer wavelengths. MESSENGER data products for surface reflectance include middle-UV reflectance spectra, <span class="hlt">ultraviolet</span> far-UV reflectance values, combined middle-UV through near-infrared spectra (210 nm - 1450 nm), a global `spectral cube' of near-UV to near-IR, and an upcoming UV spectral cube.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19920000300&hterms=Reactivity&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DReactivity','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19920000300&hterms=Reactivity&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DReactivity"><span><span class="hlt">Ultraviolet</span> Spectrum And Chemical Reactivity Of CIO Dimer</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Demore, William B.; Tschuikow-Roux, E.</p> <p>1992-01-01</p> <p>Report describes experimental study of <span class="hlt">ultraviolet</span> spectrum and chemical reactivity of dimer of chlorine monoxide (CIO). Objectives are to measure absorption cross sections of dimer at near-<span class="hlt">ultraviolet</span> wavelengths; determine whether asymmetrical isomer (CIOCIO) exists at temperatures relevant to Antarctic stratosphere; and test for certain chemical reactions of dimer. Important in photochemistry of Antarctic stratosphere.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017ATel10710....1J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017ATel10710....1J"><span>ASAS-SN Discovery of a <span class="hlt">Bright</span> Be Star Undergoing a Possible Outburst</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jayasinghe, T.; Stanek, K. Z.; Kochanek, C. S.; Thorstensen, J.; Rupert, J.; Prieto, J. L.; Shields, J. V.; Thompson, T. A.; Holoien, T. W.-S.; Shappee, B. J.; Dong, Subo</p> <p>2017-09-01</p> <p>As part of an ongoing effort by ASAS-SN project (Shappee et al. 2014; Kochanek et al. 2017) to characterize and catalog all <span class="hlt">bright</span> variable stars (e.g., Jayasinghe et al. 2017, ATel #10634, #10677), we report the discovery of a <span class="hlt">bright</span> Be star undergoing a possible outburst.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017SPIE10461E..1RW','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017SPIE10461E..1RW"><span>Analysis and design of the <span class="hlt">ultraviolet</span> warning optical system based on interference imaging</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wang, Wen-cong; Hu, Hui-jun; Jin, Dong-dong; Chu, Xin-bo; Shi, Yu-feng; Song, Juan; Liu, Jin-sheng; Xiao, Ting; Shao, Si-pei</p> <p>2017-10-01</p> <p><span class="hlt">Ultraviolet</span> warning technology is one of the important methods for missile warning. It provides a very effective way to detect the target for missile approaching alarm. With the development of modern technology, especially the development of information technology at high speed, the <span class="hlt">ultraviolet</span> early warning system plays an increasingly important role. Compared to infrared warning, the <span class="hlt">ultraviolet</span> warning has high efficiency and low false alarm rate. In the modern warfare, how to detect the threats earlier, prevent and reduce the attack of precision-guided missile has become a new challenge of missile warning technology. Because the <span class="hlt">ultraviolet</span> warning technology has high environmental adaptability, the low false alarm rate, small volume and other advantages, in the military field applications it has been developed rapidly. For the <span class="hlt">ultraviolet</span> warning system, the optimal working waveband is 250 nm 280 nm (Solar Blind UV) due to the strong absorption of ozone layer. According to current application demands for solar blind <span class="hlt">ultraviolet</span> detection and warning, this paper proposes <span class="hlt">ultraviolet</span> warning optical system based on interference imaging, which covers solar blind <span class="hlt">ultraviolet</span> (250nm-280nm) and dual field. This structure includes a primary optical system, an <span class="hlt">ultraviolet</span> reflector array, an <span class="hlt">ultraviolet</span> imaging system and an <span class="hlt">ultraviolet</span> interference imaging system. It makes use of an <span class="hlt">ultraviolet</span> beam-splitter to achieve the separation of two optical systems. According to the detector and the corresponding application needs of two visual field of the optical system, the calculation and optical system design were completed. After the design, the MTF of the two optical system is more than 0.8@39lp/mm.A single pixel energy concentration is greater than 80%.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/5765605-luminosity-function-faint-galaxies-ultraviolet-continuum','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/5765605-luminosity-function-faint-galaxies-ultraviolet-continuum"><span>Luminosity function of faint galaxies with <span class="hlt">ultraviolet</span> continuum</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>Stepanyan, D.A.</p> <p>1985-05-01</p> <p>The spatial density of faint galaxies with <span class="hlt">ultraviolet</span> continuum in the Second Survey of the Byurakan Astrophysical Observatory is determined. The luminosity function of galaxies with <span class="hlt">ultraviolet</span> continuum can be extended to objects fainter by 1-1.5 magnitudes. The spatial density of such galaxies in the interval of luminosities -16 /sup m/ .5 to -21 /sup m/ .5 is on the average 0.08 of the total density of field galaxies in the same interval of absolute magnitudes. The spatial density of low-luminosity galaxies with <span class="hlt">ultraviolet</span> continuum is very high. In the interval from -12 /sup m/ .5 to -15 /sup m/more » .5 it is 0.23 Mpc/sup -3/.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017SoSyR..51..592S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017SoSyR..51..592S"><span>Web-Resources for Astronomical Data in the <span class="hlt">Ultraviolet</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sachkov, M. E.; Malkov, O. Yu.</p> <p>2017-12-01</p> <p>In this paper we describe databases of space projects that are operating or have operated in the <span class="hlt">ultraviolet</span> spectral region. We give brief descriptions and links to major sources for UV data on the web: archives, space mission sites, databases, catalogues. We pay special attention to the World Space Observatory—<span class="hlt">Ultraviolet</span> mission that will be launched in 2021.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19720021675','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19720021675"><span>Microwave <span class="hlt">brightness</span> temperature of a windblown sea</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hall, F. G.</p> <p>1972-01-01</p> <p>A mathematical model is developed for the apparent temperature of the sea at all microwave frequencies. The model is a numerical model in which both the clear water structure and white water are accounted for as a function of wind speed. The model produces results similar to Stogryn's model at 19.35 GHz for wind speeds less than 8 m/sec; it can use radiosonde data to calculate atmospheric effects and can incorporate an empirically determined antenna gain pattern. The corresponding computer program is of modular design and the logic of the main program is capable of treating a horizontally inhomogeneous surface or atmosphere. It is shown that a variation of microwave <span class="hlt">brightness</span> temperature with zenith angle is necessary to produce the wind sensitivity of the horizontally polarized <span class="hlt">brightness</span> temperature; the variation of sky temperature with frequency is sufficient to produce a frequency dependent wind sensitivity.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19860012987','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19860012987"><span>A search for outflows from X-ray <span class="hlt">bright</span> points in coronal holes</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Mullan, D. J.; Waldron, W. L.</p> <p>1986-01-01</p> <p>Properties of X-ray <span class="hlt">bright</span> points using two of the instruments on Solar Maximum Mission were investigated. The mass outflows from magnetic regions were modeled using a two dimensional MHD code. It was concluded that mass can be detected from X-ray <span class="hlt">bright</span> points provided that the magnetic topology is favorable.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19860015840','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19860015840"><span>Metallicity and the level of the <span class="hlt">ultraviolet</span> rising branch in elliptical galaxies</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Faber, S. M.</p> <p>1986-01-01</p> <p>This final report concerns a project to study the systematics of the <span class="hlt">ultraviolet</span> flux level in elliptical galaxies. Prior to the inception of this work, the systematic behavior of the <span class="hlt">ultraviolet</span> flux level was basically unknown and <span class="hlt">ultraviolet</span> fluxes were observed to vary greatly from galaxy to galaxy. There was a suggestion, however, that there might be a dependence of <span class="hlt">ultraviolet</span> flux on galaxy metallicity, but the correlation was based on just six galaxies. IUE spectra of elliptical galaxies have been reanalyzed and placed on a consistent, homogenous flux system. The major conclusion is a confirmation of the original hypothesis: galaxies with stronger Mg2 lines show enhanced <span class="hlt">ultraviolet</span> flux.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2018TCry...12..921R','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2018TCry...12..921R"><span>Arctic sea ice signatures: L-band <span class="hlt">brightness</span> temperature sensitivity comparison using two radiation transfer models</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Richter, Friedrich; Drusch, Matthias; Kaleschke, Lars; Maaß, Nina; Tian-Kunze, Xiangshan; Mecklenburg, Susanne</p> <p>2018-03-01</p> <p>Sea ice is a crucial component for short-, medium- and long-term numerical weather predictions. Most importantly, changes of sea ice coverage and areas covered by thin sea ice have a large impact on heat fluxes between the ocean and the atmosphere. L-band <span class="hlt">brightness</span> temperatures from ESA's Earth Explorer SMOS (Soil Moisture and Ocean Salinity) have been proven to be a valuable tool to derive thin sea ice thickness. These retrieved estimates were already successfully assimilated in forecasting models to constrain the ice analysis, leading to more accurate initial conditions and subsequently more accurate forecasts. However, the <span class="hlt">brightness</span> temperature measurements can potentially be assimilated directly in forecasting systems, reducing the data latency and providing a more consistent first guess. As a first step towards such a data assimilation system we studied the forward operator that translates geophysical parameters provided by a model into <span class="hlt">brightness</span> temperatures. We use two different radiative transfer models to generate top of atmosphere <span class="hlt">brightness</span> temperatures based on ORAP5 model output for the 2012/2013 winter season. The simulations are then compared against actual SMOS measurements. The results indicate that both models are able to capture the general variability of measured <span class="hlt">brightness</span> temperatures over sea ice. The simulated <span class="hlt">brightness</span> temperatures are dominated by sea ice coverage and thickness changes are most pronounced in the marginal ice zone where new sea ice is formed. There we observe the largest differences of more than 20 K over sea ice between simulated and observed <span class="hlt">brightness</span> temperatures. We conclude that the assimilation of SMOS <span class="hlt">brightness</span> temperatures yields high potential for forecasting models to correct for uncertainties in thin sea ice areas and suggest that information on sea ice fractional coverage from higher-frequency <span class="hlt">brightness</span> temperatures should be used simultaneously.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1997IJBm...41...90A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1997IJBm...41...90A"><span>Exposure to <span class="hlt">bright</span> light for several hours during the daytime lowers tympanic temperature</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Aizawa, Seika; Tokura, H.</p> <p></p> <p>The present study investigates the effect on thympanic temperature of exposure to different light intensities for several hours during the daytime. Nine healthy young adult volunteers (two male, seven female) were exposed to <span class="hlt">bright</span> light of 4000 lx or dim light of 100 lx during the daytime from 0930 to 1800 hours; the light condition was then kept at 100 lx for a further hour. Tympanic temperature was measured continuously at a neutral condition (28° C, 60% relative humidity) from 1000 to 1800 hours. Urinary samples were collected from 1100 to 1900 hours every 2 h, and melatonin excretion rate was measured by enzyme immunoassay. Of nine subjects, six showed clearly lower tympanic temperatures in the <span class="hlt">bright</span> compared with the dim condition from 1400 to 1800 hours. Average tympanic temperatures were significantly lower in the <span class="hlt">bright</span> than in the dim condition from 1645 to 1800 hours. Melatonin excretion rate tended to be higher in the <span class="hlt">bright</span> than in the dim condition. It was concluded that exposure to <span class="hlt">bright</span> light of 4000 lx during the daytime for several hours could reduce tympanic temperature, compared with that measured in dim light of 100 lx.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/9429342','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/9429342"><span>Exposure to <span class="hlt">bright</span> light for several hours during the daytime lowers tympanic temperature.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Aizawa, S; Tokura, H</p> <p>1997-11-01</p> <p>The present study investigates the effect on thympanic temperature of exposure to different light intensities for several hours during the daytime. Nine healthy young adult volunteers (two male, seven female) were exposed to <span class="hlt">bright</span> light of 4000 lx or dim light of 100 lx during the daytime from 0930 to 1800 hours; the light condition was then kept at 100 lx for a further hour. Tympanic temperature was measured continuously at a neutral condition (28 degrees C, 60% relative humidity) from 1000 to 1800 hours. Urinary samples were collected from 1100 to 1900 hours every 2 h, and melatonin excretion rate was measured by enzyme immunoassay. Of nine subjects, six showed clearly lower tympanic temperatures in the <span class="hlt">bright</span> compared with the dim condition from 1400 to 1800 hours. Average tympanic temperatures were significantly lower in the <span class="hlt">bright</span> than in the dim condition from 1645 to 1800 hours. Melatonin excretion rate tended to be higher in the <span class="hlt">bright</span> than in the dim condition. It was concluded that exposure to <span class="hlt">bright</span> light of 4000 lx during the daytime for several hours could reduce tympanic temperature, compared with that measured in dim light of 100 lx.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=PIA01515&hterms=gardening&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dgardening','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=PIA01515&hterms=gardening&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dgardening"><span><span class="hlt">Bright</span> Ray Craters in Ganymede's Northern Hemisphere</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>1979-01-01</p> <p>GANYMEDE COLOR PHOTOS: This color picture as acquired by Voyager 1 during its approach to Ganymede on Monday afternoon (the 5th of March). At ranges between about 230 to 250 thousand km. The images show detail on the surface with a resolution of four and a half km. This picture is of a region in the northern hemisphere near the terminator. It shows a variety of impact structures, including both razed and unrazed craters, and the odd, groove-like structures discovered by Voyager in the lighter regions. The most striking features are the <span class="hlt">bright</span> ray craters which have a distinctly 'bluer' color appearing white against the redder background. Ganymede's surface is known to contain large amounts of surface ice and it appears that these relatively young craters have spread <span class="hlt">bright</span> fresh ice materials over the surface. Likewise, the lighter color and reflectivity of the grooved areas suggests that here, too, there is cleaner ice. We see ray craters with all sizes of ray patterns, ranging from extensive systems of the crater in the southern part of this picture, which has rays at least 300-500 kilometers long, down to craters which have only faint remnants of <span class="hlt">bright</span> ejects patterns (such as several of the craters in the southern half of PIA01516; P21262). This variation suggests that, as on the Moon, there are processes which act to darken ray material, probably 'gardening' by micrometeoroid impact. JPL manages and controls the Voyager project for NASA's Office of Space Science.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012SPIE.8383E..0QW','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012SPIE.8383E..0QW"><span>Ultra-high resolution and high-<span class="hlt">brightness</span> AMOLED</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wacyk, Ihor; Ghosh, Amal; Prache, Olivier; Draper, Russ; Fellowes, Dave</p> <p>2012-06-01</p> <p>As part of its continuing effort to improve both the resolution and optical performance of AMOLED microdisplays, eMagin has recently developed an SXGA (1280×3×1024) microdisplay under a US Army RDECOM CERDEC NVESD contract that combines the world's smallest OLED pixel pitch with an ultra-high <span class="hlt">brightness</span> green OLED emitter. This development is aimed at next-generation HMD systems with "see-through" and daylight imaging requirements. The OLED pixel array is built on a 0.18-micron CMOS backplane and contains over 4 million individually addressable pixels with a pixel pitch of 2.7 × 8.1 microns, resulting in an active area of 0.52 inches diagonal. Using both spatial and temporal enhancement, the display can provide over 10-bits of gray-level control for high dynamic range applications. The new pixel design also enables the future implementation of a full-color QSXGA (2560 × RGB × 2048) microdisplay in an active area of only 1.05 inch diagonal. A low-power serialized low-voltage-differential-signaling (LVDS) interface is integrated into the display for use as a remote video link for tethered systems. The new SXGA backplane has been combined with the high-<span class="hlt">brightness</span> green OLED device developed by eMagin under an NVESD contract. This OLED device has produced an output <span class="hlt">brightness</span> of more than 8000fL with all pixels on; lifetime measurements are currently underway and will presented at the meeting. This paper will describe the operational features and first optical and electrical test results of the new SXGA demonstrator microdisplay.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19920061973&hterms=micro+macro+evolution&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dmicro%2Bmacro%2Bevolution','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19920061973&hterms=micro+macro+evolution&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dmicro%2Bmacro%2Bevolution"><span>Galileo <span class="hlt">Ultraviolet</span> Spectrometer experiment</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hord, C. W.; Mcclintock, W. E.; Stewart, A. I. F.; Barth, C. A.; Esposito, L. W.; Thomas, G. E.; Sandel, B. R.; Hunten, D. M.; Broadfoot, A. L.; Shemansky, D. E.</p> <p>1992-01-01</p> <p>The Galileo <span class="hlt">ultraviolet</span> spectrometer experiment uses data obtained by the <span class="hlt">Ultraviolet</span> Spectrometer (UVS) mounted on the pointed orbiter scan platform and from the Extreme <span class="hlt">Ultraviolet</span> Spectrometer (EUVS) mounted on the spinning part of the orbiter with the field of view perpendicular to the spin axis. The UVS is a Ebert-Fastie design that covers the range 113-432 nm with a wavelength resolution of 0.7 nm below 190 and 1.3 nm at longer wavelengths. The UVS spatial resolution is 0.4 deg x 0.1 deg for illuminated disk observations and 1 deg x 0.1 deg for limb geometries. The EUVS is a Voyager design objective grating spectrometer, modified to cover the wavelength range from 54 to 128 nm with wavelength resolution 3.5 nm for extended sources and 1.5 nm for point sources and spatial resolution of 0.87 deg x 0.17 deg. The EUVS instrument will follow up on the many Voyager UVS discoveries, particularly the sulfur and oxygen ion emissions in the Io torus and molecular and atomic hydrogen auroral and airglow emissions from Jupiter. The UVS will obtain spectra of emission, absorption, and scattering features in the unexplored, by spacecraft, 170-432 nm wavelength region. The UVS and EUVS instruments will provide a powerful instrument complement to investigate volatile escape and surface composition of the Galilean satellites, the Io plasma torus, micro- and macro-properties of the Jupiter clouds, and the composition structure and evolution of the Jupiter upper atmosphere.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2009SPIE.7325E..0TP','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2009SPIE.7325E..0TP"><span>High <span class="hlt">brightness</span> diode laser module development at nLIGHT Photonics</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Price, Kirk; Karlsen, Scott; Brown, Aaron; Reynolds, Mitch; Mehl, Ron; Leisher, Paul; Patterson, Steve; Bell, Jake; Martinsen, Rob</p> <p>2009-05-01</p> <p>We report on the development of ultra-high <span class="hlt">brightness</span> laser diode modules at nLIGHT Photonics. This paper demonstrates a laser diode module capable of coupling over 100W at 976 nm into a 105 μm, 0.15 NA fiber with fiber coupling efficiency greater than 85%. The high <span class="hlt">brightness</span> module has an optical excitation under 0.13 NA, is virtually free of cladding modes, and has been wavelength stabilized with the use of volume holographic gratings for narrow-band operation. Utilizing nLIGHT's Pearl product architecture, these modules are based on hard soldered single emitters packaged into a compact and passively-cooled package. These modules are designed to be compatible with high power 7:1 fused fiber combiners, enabling over 500W power coupled into a 220 μm, 0.22 NA fiber. These modules address the need in the market for high <span class="hlt">brightness</span> and wavelength stabilized diode lasers for pumping fiber lasers and solid-state laser systems.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017OptEn..56k4103K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017OptEn..56k4103K"><span>On correct evaluation techniques of <span class="hlt">brightness</span> enhancement effect measurement data</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kukačka, Leoš; Dupuis, Pascal; Motomura, Hideki; Rozkovec, Jiří; Kolář, Milan; Zissis, Georges; Jinno, Masafumi</p> <p>2017-11-01</p> <p>This paper aims to establish confidence intervals of the quantification of <span class="hlt">brightness</span> enhancement effects resulting from the use of pulsing <span class="hlt">bright</span> light. It is found that the methods used so far may yield significant bias in the published results, overestimating or underestimating the enhancement effect. The authors propose to use a linear algebra method called the total least squares. Upon an example dataset, it is shown that this method does not yield biased results. The statistical significance of the results is also computed. It is concluded over an observation set that the currently used linear algebra methods present many patterns of noise sensitivity. Changing algorithm details leads to inconsistent results. It is thus recommended to use the method with the lowest noise sensitivity. Moreover, it is shown that this method also permits one to obtain an estimate of the confidence interval. This paper neither aims to publish results about a particular experiment nor to draw any particular conclusion about existence or nonexistence of the <span class="hlt">brightness</span> enhancement effect.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19930001910','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19930001910"><span><span class="hlt">Ultraviolet</span> radiation changes</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Mckenzie, Richard L.; Frederick, John E.; Ilyas, Mohammad; Filyushkin, V.; Wahner, Andreas; Stamnes, K.; Muthusubramanian, P.; Blumthaler, M.; Roy, Colin E.; Madronich, Sasha</p> <p>1991-01-01</p> <p>A major consequence of ozone depletion is an increase in solar <span class="hlt">ultraviolet</span> (UV) radiation received at the Earth's surface. This chapter discusses advances that were made since the previous assessment (World Meteorological Organization (WMO)) to our understanding of UV radiation. The impacts of these changes in UV on the biosphere are not included, because they are discussed in the effects assessment.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010cosp...38.1352G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010cosp...38.1352G"><span><span class="hlt">Ultraviolet</span> aurorae and dayglow in the upper atmospheres of terrestrial planets</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gerard, Jean-Claude; Hubert, Benoit; Gustin, J.; Cox, Cedric</p> <p></p> <p>Since its discovery in 2005 with the SPICAM spectrograph on board Mars Express, the Mars aurora has been further investigated. It is caused by sporadic soft electron precipitation whose signature is clearly observed in the FUV nightglow spectrum. The characteristics of the auroral electrons have been documented with parallel observations. Dayglow UV spectra have been collected with SPICAM over several seasons. The dependence of the intensity and peak altitude of the CO Cameron bands and CO2 + doublet emissions on latitude, local time and solar activity level have been investigated and compared with the results of a FUV Mars dayglow model. Far and Extreme <span class="hlt">ultraviolet</span> spectra have been collected with the UVIS instrument during the flyby of Venus by Cassini, in a period a high solar activity. Their analysis shows the presence of OI, OII, NI, CI, CO and CO2 + emissions, some of them not previously identified in the Venus spectrum. The intensities will be compared with those observed with the HUT spectrograph during a period of low solar activity. The excitation processes of the observed features will be discussed. Scans of the intensity variation of several EUV <span class="hlt">bright</span> emissions such as OII 83.4 nm, OI 98.9 nm and NI 120.0 nm multiplets across the sunlit disc will be compared with the calculations of a Venus dayglow model, including multiple scattering of optically thick transitions.</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('https://www.osti.gov/biblio/22667474-subaru-high-exploration-low-luminosity-quasars-shellqs-discovery-quasars-bright-galaxies','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/22667474-subaru-high-exploration-low-luminosity-quasars-shellqs-discovery-quasars-bright-galaxies"><span>SUBARU HIGH- z EXPLORATION OF LOW-LUMINOSITY QUASARS (SHELLQs). I. DISCOVERY OF 15 QUASARS AND <span class="hlt">BRIGHT</span> GALAXIES AT 5.7 < z < 6.9</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>Matsuoka, Yoshiki; Kashikawa, Nobunari; Imanishi, Masatoshi</p> <p></p> <p>We report the discovery of 15 quasars and <span class="hlt">bright</span> galaxies at 5.7 < z < 6.9. This is the initial result from the Subaru High- z Exploration of Low-Luminosity Quasars project, which exploits the exquisite multiband imaging data produced by the Subaru Hyper Suprime-Cam (HSC) Strategic Program survey. The candidate selection is performed by combining several photometric approaches including a Bayesian probabilistic algorithm to reject stars and dwarfs. The spectroscopic identification was carried out with the Gran Telescopio Canarias and the Subaru Telescope for the first 80 deg{sup 2} of the survey footprint. The success rate of our photometric selectionmore » is quite high, approaching 100% at the brighter magnitudes (z {sub AB} < 23.5 mag). Our selection also recovered all the known high- z quasars on the HSC images. Among the 15 discovered objects, six are likely quasars, while the other six with interstellar absorption lines and in some cases narrow emission lines are likely <span class="hlt">bright</span> Lyman-break galaxies. The remaining three objects have weak continua and very strong and narrow Ly α lines, which may be excited by <span class="hlt">ultraviolet</span> light from both young stars and quasars. These results indicate that we are starting to see the steep rise of the luminosity function of z ≥ 6 galaxies, compared with that of quasars, at magnitudes fainter than M {sub 1450} ∼ −22 mag or z {sub AB} ∼ 24 mag. Follow-up studies of the discovered objects as well as further survey observations are ongoing.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19930017533','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19930017533"><span>Wide-field direct CCD observations supporting the Astro-1 Space Shuttle mission's <span class="hlt">Ultraviolet</span> Imaging Telescope</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hintzen, Paul; Angione, Ron; Talbert, Freddie; Cheng, K.-P.; Smith, Eric; Stecher, Theodore P.</p> <p>1993-01-01</p> <p>Wide field direct CCD observations are being obtained to support and complement the vacuum-<span class="hlt">ultraviolet</span> (VUV) images provided by Astro's <span class="hlt">Ultraviolet</span> Imaging Telescope (UIT) during a Space Shuttle flight in December 1990. Because of the wide variety of projects addressed by UIT, the fields observed include (1) galactic supernova remnants such as the Cygnus Loop and globular clusters such as Omega Cen and M79; (2) the Magellanic Clouds, M33, M81, and other galaxies in the Local Group; and (3) rich clusters of galaxies, principally the Perseus cluster and Abell 1367. Ground-based observations have been obtained for virtually all of the Astro-1 UIT fields. The optical images allow identification of individual UV sources in each field and provide the long baseline in wavelength necessary for accurate analysis of UV-<span class="hlt">bright</span> sources. To facilitate use of our optical images for analysis of UIT data and other projects, we plan to archive them, with the UIT images, at the National Space Science Data Center (NSSDC), where they will be universally accessible via anonymous FTP. The UIT, one of three telescopes comprising the Astro spacecraft, is a 38-cm f/9 Ritchey-Chretien telescope on which high quantum efficiency, solar-blind image tubes are used to record VUV images on photographic film. Five filters with passbands centered between 1250A and 2500A provide both VUV colors and a measurement of extinction via the 2200A dust feature. The resulting calibrated VUV pictures are 40 arcminutes in diameter at 2.5 arcseconds resolution. The capabilities of UIT, therefore, complement HST's WFPC: the latter has 40 times greater collecting area, while UIT's usable field has 170 times WFPC's field area.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/biblio/5545797-psoriasis-ultraviolet-radiation','SCIGOV-STC'); return false;" href="https://www.osti.gov/biblio/5545797-psoriasis-ultraviolet-radiation"><span>Psoriasis and <span class="hlt">ultraviolet</span> radiation</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>Farber, E.M.; Nall, L.</p> <p>1993-09-01</p> <p>Prevention and detection screening programs as a public health service in curtailing the ever-increasing incidence of all forms of skin cancer are reviewed. The effect of solar and artificial <span class="hlt">ultraviolet</span> radiation on the general population and persons with psoriasis is examined. 54 refs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19800005501','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19800005501"><span>Photosynthetic carbon reduction by seagrasses exposed to <span class="hlt">ultraviolet</span> A radiation</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>1979-01-01</p> <p>The seagrasses Halophila engelmannii, Halodule wrightii, and Syringodium filiforme were examined for their intrinsic sensitivity to <span class="hlt">ultraviolet</span>-A-UV-A and <span class="hlt">ultraviolet</span>-B-UV-B radiation. The effect of UV-A on photosynthetically active radiation (PAR) was also determined. <span class="hlt">Ultraviolet</span>-A and <span class="hlt">ultraviolet</span>-B were studied with emphasis on the greater respective environmental consequence in terms of seagrass distribution and abundance. Results indicate that an intrinsic sensitivity to UV-A alone is apparent only in Halophila, while net photosynthesis in Halodule and Syringodium seems unaffected by the level of UV-A provided. The sensitivity of Halophila to UV-A in the absense of (PAR) indicates that the photosynthetic reaction does not need to be in operation for damage to occur. Other significant results are reported.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/872784','DOE-PATENT-XML'); return false;" href="https://www.osti.gov/servlets/purl/872784"><span>Method for extreme <span class="hlt">ultraviolet</span> lithography</span></a></p> <p><a target="_blank" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p>Felter, T. E.; Kubiak, Glenn D.</p> <p>1999-01-01</p> <p>A method of producing a patterned array of features, in particular, gate apertures, in the size range 0.4-0.05 .mu.m using projection lithography and extreme <span class="hlt">ultraviolet</span> (EUV) radiation. A high energy laser beam is used to vaporize a target material in order to produce a plasma which in turn, produces extreme <span class="hlt">ultraviolet</span> radiation of a characteristic wavelength of about 13 nm for lithographic applications. The radiation is transmitted by a series of reflective mirrors to a mask which bears the pattern to be printed. The demagnified focused mask pattern is, in turn, transmitted by means of appropriate optics and in a single exposure, to a substrate coated with photoresists designed to be transparent to EUV radiation and also satisfy conventional processing methods.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/servlets/purl/873452','DOE-PATENT-XML'); return false;" href="https://www.osti.gov/servlets/purl/873452"><span>Method for extreme <span class="hlt">ultraviolet</span> lithography</span></a></p> <p><a target="_blank" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p>Felter, T. E.; Kubiak, G. D.</p> <p>2000-01-01</p> <p>A method of producing a patterned array of features, in particular, gate apertures, in the size range 0.4-0.05 .mu.m using projection lithography and extreme <span class="hlt">ultraviolet</span> (EUV) radiation. A high energy laser beam is used to vaporize a target material in order to produce a plasma which in turn, produces extreme <span class="hlt">ultraviolet</span> radiation of a characteristic wavelength of about 13 nm for lithographic applications. The radiation is transmitted by a series of reflective mirrors to a mask which bears the pattern to be printed. The demagnified focused mask pattern is, in turn, transmitted by means of appropriate optics and in a single exposure, to a substrate coated with photoresists designed to be transparent to EUV radiation and also satisfy conventional processing methods.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://cfpub.epa.gov/si/si_public_record_report.cfm?dirEntryId=83629&Lab=NHEERL&keyword=maca&actType=&TIMSType=+&TIMSSubTypeID=&DEID=&epaNumber=&ntisID=&archiveStatus=Both&ombCat=Any&dateBeginCreated=&dateEndCreated=&dateBeginPublishedPresented=&dateEndPublishedPresented=&dateBeginUpdated=&dateEndUpdated=&dateBeginCompleted=&dateEndCompleted=&personID=&role=Any&journalID=&publisherID=&sortBy=revisionDate&count=50','EPA-EIMS'); return false;" href="https://cfpub.epa.gov/si/si_public_record_report.cfm?dirEntryId=83629&Lab=NHEERL&keyword=maca&actType=&TIMSType=+&TIMSSubTypeID=&DEID=&epaNumber=&ntisID=&archiveStatus=Both&ombCat=Any&dateBeginCreated=&dateEndCreated=&dateBeginPublishedPresented=&dateEndPublishedPresented=&dateBeginUpdated=&dateEndUpdated=&dateBeginCompleted=&dateEndCompleted=&personID=&role=Any&journalID=&publisherID=&sortBy=revisionDate&count=50"><span><span class="hlt">ULTRAVIOLET</span> RADIATION DOWN-REGULATES ALLERGY IN BALB/C MICE</span></a></p> <p><a target="_blank" href="http://oaspub.epa.gov/eims/query.page">EPA Science Inventory</a></p> <p></p> <p></p> <p><span class="hlt">ULTRAVIOLET</span> RADIATION SUPPRESSES ALLERGY IN BALB/C MICE<br>Marsha D.W. Ward+ *, Denise M. Sailstad+, Debora L. Andrews, Elizabeth H. Boykin, and MaryJane K. Selgrade<br><br>ABSTRACT<br>The immunosuppressive effects of exposure to <span class="hlt">ultraviolet</span> radiation (UVR) are well known and the...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28651468','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28651468"><span>Human Adolescent Phase Response Curves to <span class="hlt">Bright</span> White Light.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Crowley, Stephanie J; Eastman, Charmane I</p> <p>2017-08-01</p> <p>Older adolescents are particularly vulnerable to circadian misalignment and sleep restriction, primarily due to early school start times. Light can shift the circadian system and could help attenuate circadian misalignment; however, a phase response curve (PRC) to determine the optimal time for receiving light and avoiding light is not available for adolescents. We constructed light PRCs for late pubertal to postpubertal adolescents aged 14 to 17 years. Participants completed 2 counterbalanced 5-day laboratory sessions after 8 or 9 days of scheduled sleep at home. Each session included phase assessments to measure the dim light melatonin onset (DLMO) before and after 3 days of free-running through an ultradian light-dark (wake-sleep) cycle (2 h dim [~20 lux] light, 2 h dark). In one session, intermittent <span class="hlt">bright</span> white light (~5000 lux; four 20-min exposures) was alternated with 10 min of dim room light once per day for 3 consecutive days. The time of light varied among participants to cover the 24-h day. For each individual, the phase shift to <span class="hlt">bright</span> light was corrected for the free-run derived from the other laboratory session with no <span class="hlt">bright</span> light. One PRC showed phase shifts in response to light start time relative to the DLMO and another relative to home sleep. Phase delay shifts occurred around the hours corresponding to home bedtime. Phase advances occurred during the hours surrounding wake time and later in the afternoon. The transition from delays to advances occurred at the midpoint of home sleep. The adolescent PRCs presented here provide a valuable tool to time <span class="hlt">bright</span> light in adolescents.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.fs.usda.gov/treesearch/pubs/3773','TREESEARCH'); return false;" href="https://www.fs.usda.gov/treesearch/pubs/3773"><span><span class="hlt">Ultraviolet</span> radiation, human health, and the urban forest</span></a></p> <p><a target="_blank" href="http://www.fs.usda.gov/treesearch/">Treesearch</a></p> <p>Gordon M. Heisler; Richard H. Grant</p> <p>2000-01-01</p> <p>Excess exposure to <span class="hlt">ultraviolet</span> (UV) radiation from the sun, particularly the <span class="hlt">ultraviolet</span> B (UVB) portion, has been linked with adverse effects on human health ranging from skin cancers to eye diseases such as cataracts. Trees may prevent even greater disease rates in humans by reducing UV exposure. Tree shade greatly reduces UV irradiance when both the sun and sky are...</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19990028291&hterms=Cluster+analysis&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DCluster%2Banalysis','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19990028291&hterms=Cluster+analysis&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DCluster%2Banalysis"><span>Analysis of Mass Profiles and Cooling Flows of <span class="hlt">Bright</span>, Early-Type Galaxies AO2, AO3 and Surface <span class="hlt">Brightness</span> Profiles and Energetics of Intracluster Gas in Cool Galaxy Clusters AO3</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>White, Raymond E., III</p> <p>1998-01-01</p> <p>This final report uses ROSAT observations to analyze two different studies. These studies are: Analysis of Mass Profiles and Cooling Flows of <span class="hlt">Bright</span>, Early-Type Galaxies; and Surface <span class="hlt">Brightness</span> Profiles and Energetics of Intracluster Gas in Cool Galaxy Clusters.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015JMOp...62..536J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015JMOp...62..536J"><span>Image contrast enhancement with <span class="hlt">brightness</span> preservation using an optimal gamma correction and weighted sum approach</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jiang, G.; Wong, C. Y.; Lin, S. C. F.; Rahman, M. A.; Ren, T. R.; Kwok, Ngaiming; Shi, Haiyan; Yu, Ying-Hao; Wu, Tonghai</p> <p>2015-04-01</p> <p>The enhancement of image contrast and preservation of image <span class="hlt">brightness</span> are two important but conflicting objectives in image restoration. Previous attempts based on linear histogram equalization had achieved contrast enhancement, but exact preservation of <span class="hlt">brightness</span> was not accomplished. A new perspective is taken here to provide balanced performance of contrast enhancement and <span class="hlt">brightness</span> preservation simultaneously by casting the quest of such solution to an optimization problem. Specifically, the non-linear gamma correction method is adopted to enhance the contrast, while a weighted sum approach is employed for <span class="hlt">brightness</span> preservation. In addition, the efficient golden search algorithm is exploited to determine the required optimal parameters to produce the enhanced images. Experiments are conducted on natural colour images captured under various indoor, outdoor and illumination conditions. Results have shown that the proposed method outperforms currently available methods in contrast to enhancement and <span class="hlt">brightness</span> preservation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://images.nasa.gov/#/details-PIA14723.html','SCIGOVIMAGE-NASA'); return false;" href="https://images.nasa.gov/#/details-PIA14723.html"><span>Dark Murky Clouds in the <span class="hlt">Bright</span> Milky Way</span></a></p> <p><a target="_blank" href="https://images.nasa.gov/">NASA Image and Video Library</a></p> <p></p> <p>2011-08-24</p> <p>This infrared image from NASA Wide-field Infrared Survey Explorer shows exceptionally cold, dense cloud cores seen in silhouette against the <span class="hlt">bright</span> diffuse infrared glow of the plane of the Milky Way galaxy.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1336139-laser-ion-source-high-brightness-heavy-ion-beam','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1336139-laser-ion-source-high-brightness-heavy-ion-beam"><span>Laser ion source for high <span class="hlt">brightness</span> heavy ion beam</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Okamura, M.</p> <p>2016-09-01</p> <p>A laser ion source is known as a high current high charge state heavy ion source. But, we place great emphasis on the capability to realize a high <span class="hlt">brightness</span> ion source. A laser ion source has a pinpoint small volume where materials are ionized and can achieve quite uniform low temperature ion beam. Those features may enable us to realize very small emittance beams. Furthermore, a low charge state high <span class="hlt">brightness</span> laser ion source was successfully commissioned in Brookhaven National Laboratory in 2014. Now most of all the solid based heavy ions are being provided from the laser ion sourcemore » for regular operation.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016Natur.535..416C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016Natur.535..416C"><span><span class="hlt">Bright</span> spots among the world’s coral reefs</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Cinner, Joshua E.; Huchery, Cindy; MacNeil, M. Aaron; Graham, Nicholas A. J.; McClanahan, Tim R.; Maina, Joseph; Maire, Eva; Kittinger, John N.; Hicks, Christina C.; Mora, Camilo; Allison, Edward H.; D'Agata, Stephanie; Hoey, Andrew; Feary, David A.; Crowder, Larry; Williams, Ivor D.; Kulbicki, Michel; Vigliola, Laurent; Wantiez, Laurent; Edgar, Graham; Stuart-Smith, Rick D.; Sandin, Stuart A.; Green, Alison L.; Hardt, Marah J.; Beger, Maria; Friedlander, Alan; Campbell, Stuart J.; Holmes, Katherine E.; Wilson, Shaun K.; Brokovich, Eran; Brooks, Andrew J.; Cruz-Motta, Juan J.; Booth, David J.; Chabanet, Pascale; Gough, Charlie; Tupper, Mark; Ferse, Sebastian C. A.; Sumaila, U. Rashid; Mouillot, David</p> <p>2016-07-01</p> <p>Ongoing declines in the structure and function of the world’s coral reefs require novel approaches to sustain these ecosystems and the millions of people who depend on them. A presently unexplored approach that draws on theory and practice in human health and rural development is to systematically identify and learn from the ‘outliers’—places where ecosystems are substantially better (‘<span class="hlt">bright</span> spots’) or worse (‘dark spots’) than expected, given the environmental conditions and socioeconomic drivers they are exposed to. Here we compile data from more than 2,500 reefs worldwide and develop a Bayesian hierarchical model to generate expectations of how standing stocks of reef fish biomass are related to 18 socioeconomic drivers and environmental conditions. We identify 15 <span class="hlt">bright</span> spots and 35 dark spots among our global survey of coral reefs, defined as sites that have biomass levels more than two standard deviations from expectations. Importantly, <span class="hlt">bright</span> spots are not simply comprised of remote areas with low fishing pressure; they include localities where human populations and use of ecosystem resources is high, potentially providing insights into how communities have successfully confronted strong drivers of change. Conversely, dark spots are not necessarily the sites with the lowest absolute biomass and even include some remote, uninhabited locations often considered near pristine. We surveyed local experts about social, institutional, and environmental conditions at these sites to reveal that <span class="hlt">bright</span> spots are characterized by strong sociocultural institutions such as customary taboos and marine tenure, high levels of local engagement in management, high dependence on marine resources, and beneficial environmental conditions such as deep-water refuges. Alternatively, dark spots are characterized by intensive capture and storage technology and a recent history of environmental shocks. Our results suggest that investments in strengthening fisheries</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017Icar..296..289Z','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017Icar..296..289Z"><span>Aqueous origins of <span class="hlt">bright</span> salt deposits on Ceres</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Zolotov, Mikhail Yu.</p> <p>2017-11-01</p> <p><span class="hlt">Bright</span> materials have been reported in association with impact craters on Ceres. The abundant Na2CO3 and some ammonium salts, NH4HCO3 and/or NH4Cl, were detected in <span class="hlt">bright</span> deposits within Occator crater with Dawn near infrared spectroscopy. The composition and appearance of the salts suggest their aqueous mobilization and emplacement after formation of the crater. Here we consider origins of the <span class="hlt">bright</span> deposits through calculation of speciation in the H-C-N-O-Na-Cl water-salt type system constrained by the mass balance of observed salts. Calculations of chemical equilibria show that initial solutions had the pH of ∼10. The temperature and salinity of solutions could have not exceeded ∼273 K and ∼100 g per kg H2O, respectively. Freezing models reveal an early precipitation of Na2CO3·10H2O followed by minor NaHCO3. Ammonium salts precipitate near eutectic from brines enriched in NH4+, Cl- and Na+. A late-stage precipitation of NaCl·2H2O is modeled for solution compositions with added NaCl. Calculated eutectics are above 247 K. The apparently unabundant ammonium and chloride salts in Occator's deposits imply a rapid emplacement without a compositional evolution of solution. Salty ice grains could have deposited from post-impact ballistic plumes formed through low-pressure boiling of subsurface solutions. Hydrated and ammonium salts are unstable at maximum temperatures of Ceres' surface and could decompose through space weathering. Occator's ice-free salt deposits formed through a post-depositional sublimation of ice followed by dehydration of Na2CO3·10H2O and NaHCO3 to Na2CO3. In other regions, excavated and exposed <span class="hlt">bright</span> materials could be salts initially deposited from plumes and accumulated at depth via post-impact boiling. The lack of detection of sulfates and an elevated carbonate/chloride ratio in Ceres' materials suggest an involvement of compounds abundant in the outer solar system.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25299950','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25299950"><span>A <span class="hlt">brightness</span>-referenced star identification algorithm for APS star trackers.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Zhang, Peng; Zhao, Qile; Liu, Jingnan; Liu, Ning</p> <p>2014-10-08</p> <p>Star trackers are currently the most accurate spacecraft attitude sensors. As a result, they are widely used in remote sensing satellites. Since traditional charge-coupled device (CCD)-based star trackers have a limited sensitivity range and dynamic range, the matching process for a star tracker is typically not very sensitive to star <span class="hlt">brightness</span>. For active pixel sensor (APS) star trackers, the intensity of an imaged star is valuable information that can be used in star identification process. In this paper an improved <span class="hlt">brightness</span> referenced star identification algorithm is presented. This algorithm utilizes the k-vector search theory and adds imaged stars' intensities to narrow the search scope and therefore increase the efficiency of the matching process. Based on different imaging conditions (slew, <span class="hlt">bright</span> bodies, etc.) the developed matching algorithm operates in one of two identification modes: a three-star mode, and a four-star mode. If the reference <span class="hlt">bright</span> stars (the stars brighter than three magnitude) show up, the algorithm runs the three-star mode and efficiency is further improved. The proposed method was compared with other two distinctive methods the pyramid and geometric voting methods. All three methods were tested with simulation data and actual in orbit data from the APS star tracker of ZY-3. Using a catalog composed of 1500 stars, the results show that without false stars the efficiency of this new method is 4~5 times that of the pyramid method and 35~37 times that of the geometric method.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19910008572&hterms=malina&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Dmalina','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19910008572&hterms=malina&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Dmalina"><span>The extreme <span class="hlt">ultraviolet</span> explorer</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Bowyer, Stuart; Malina, Roger F.</p> <p>1990-01-01</p> <p>The Extreme <span class="hlt">Ultraviolet</span> Explorer (EUVE) mission, currently scheduled for launch in September 1991, is described. The primary purpose of the mission is to survey the celestial sphere for astronomical sources of Extreme <span class="hlt">Ultraviolet</span> (EUV) radiation. The survey will be accomplished with the use of three EUV telescopes, each sensitive to a different segment of the EUV band. A fourth telescope will perform a high sensitivity search of a limited sample of the sky in the shortest wavelength bands. The all sky survey will be carried out in the first six months of the mission and will be made in four bands, or colors. The second phase of the mission, conducted entirely by guest observers selected by NASA, will be devoted to spectroscopic observations of EUV sources. The performance of the instrument components is described. An end to end model of the mission, from a stellar source to the resulting scientific data, was constructed. Hypothetical data from astronomical sources processed through this model are shown.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1996OptCo.125..377K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1996OptCo.125..377K"><span>Properties of <span class="hlt">bright</span> solitons in averaged and unaveraged models for SDG fibres</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kumar, Ajit; Kumar, Atul</p> <p>1996-04-01</p> <p>Using the slowly varying envelope approximation and averaging over the fibre cross-section the evolution equation for optical pulses in semiconductor-doped glass (SDG) fibres is derived from the nonlinear wave equation. <span class="hlt">Bright</span> soliton solutions of this equation are obtained numerically and their properties are studied and compared with those of the <span class="hlt">bright</span> solitons in the unaveraged model.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/29855075','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/29855075"><span>Effect of <span class="hlt">ultraviolet</span> light on mood, depressive disorders and well-being.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Veleva, Bistra I; van Bezooijen, Rutger L; Chel, Victor G M; Numans, Mattijs E; Caljouw, Monique A A</p> <p>2018-06-01</p> <p>Human and animal studies have shown that exposure to <span class="hlt">ultraviolet</span> light can incite a chain of endocrine, immunologic, and neurohumoral reactions that might affect mood. This review focuses on the evidence from clinical trials and observational studies on the effect of <span class="hlt">ultraviolet</span> light on mood, depressive disorders, and well-being. A search was made in PubMed, Embase, Web of Science, Cochrane, Psychinfo, CINAHL, Academic Search Premier and Science Direct, and the references of key papers, for clinical trials and observational studies describing the effect of <span class="hlt">ultraviolet</span> light applied to skin or eyes on mood, depressive disorders, and well-being. Of the seven studies eligible for this review, the effect of <span class="hlt">ultraviolet</span> light on mood, depressive symptoms and seasonal affective disorders was positive in six of them. Of the seven studies, six demonstrated benefit of exposure to <span class="hlt">ultraviolet</span> radiation and improvement in mood which supports a positive effect of <span class="hlt">ultraviolet</span> light on mood. Because of the small number of the studies and their heterogeneity, more research is warranted to confirm and document this correlation. © 2018 The Authors. Photodermatology, Photoimmunology & Photomedicine Published by John Wiley & Sons Ltd.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25679698','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25679698"><span>Dark-<span class="hlt">bright</span> solitons in coupled nonlinear Schrödinger equations with unequal dispersion coefficients.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Charalampidis, E G; Kevrekidis, P G; Frantzeskakis, D J; Malomed, B A</p> <p>2015-01-01</p> <p>We study a two-component nonlinear Schrödinger system with equal, repulsive cubic interactions and different dispersion coefficients in the two components. We consider states that have a dark solitary wave in one component. Treating it as a frozen one, we explore the possibility of the formation of <span class="hlt">bright</span>-solitonic structures in the other component. We identify bifurcation points at which such states emerge in the <span class="hlt">bright</span> component in the linear limit and explore their continuation into the nonlinear regime. An additional analytically tractable limit is found to be that of vanishing dispersion of the <span class="hlt">bright</span> component. We numerically identify regimes of potential stability, not only of the single-peak ground state (the dark-<span class="hlt">bright</span> soliton), but also of excited states with one or more zero crossings in the <span class="hlt">bright</span> component. When the states are identified as unstable, direct numerical simulations are used to investigate the outcome of the instability development. Although our principal focus is on the homogeneous setting, we also briefly touch upon the counterintuitive impact of the potential presence of a parabolic trap on the states of interest.</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. Their policies may differ from this site.</div> </div><!-- container --> <footer><a id="backToTop" href="#top"> </a><nav><a id="backToTop" href="#top"> </a><ul class="links"><a id="backToTop" href="#top"> </a><li><a id="backToTop" href="#top"></a><a href="/sitemap.html">Site Map</a></li> <li><a href="/members/index.html">Members Only</a></li> <li><a href="/website-policies.html">Website Policies</a></li> <li><a href="https://doe.responsibledisclosure.com/hc/en-us" target="_blank">Vulnerability Disclosure Program</a></li> <li><a href="/contact.html">Contact Us</a></li> </ul> <div class="small">Science.gov is maintained by the U.S. Department of Energy's <a href="https://www.osti.gov/" target="_blank">Office of Scientific and Technical Information</a>, in partnership with <a href="https://www.cendi.gov/" target="_blank">CENDI</a>.</div> </nav> </footer> <script type="text/javascript"><!-- // var lastDiv = ""; function showDiv(divName) { // hide last div if (lastDiv) { document.getElementById(lastDiv).className = "hiddenDiv"; } //if value of the box is not nothing and an object with that name exists, then change the class if (divName && document.getElementById(divName)) { document.getElementById(divName).className = "visibleDiv"; lastDiv = divName; } } //--> </script> <script> /** * Function that tracks a click on an outbound link in Google Analytics. * This function takes a valid URL string as an argument, and uses that URL string * as the event label. */ var trackOutboundLink = function(url,collectionCode) { try { h = window.open(url); setTimeout(function() { ga('send', 'event', 'topic-page-click-through', collectionCode, url); }, 1000); } catch(err){} }; </script> <!-- Google Analytics --> <script> (function(i,s,o,g,r,a,m){i['GoogleAnalyticsObject']=r;i[r]=i[r]||function(){ (i[r].q=i[r].q||[]).push(arguments)},i[r].l=1*new Date();a=s.createElement(o), m=s.getElementsByTagName(o)[0];a.async=1;a.src=g;m.parentNode.insertBefore(a,m) })(window,document,'script','//www.google-analytics.com/analytics.js','ga'); ga('create', 'UA-1122789-34', 'auto'); ga('send', 'pageview'); </script> <!-- End Google Analytics --> <script> showDiv('page_1') </script> </body> </html>