Science.gov

Sample records for multisite spectroscopic observations

  1. Coordinated Multi-Site and Multi-Wavelength Observing Campaigns

    NASA Astrophysics Data System (ADS)

    Butler, C. J.

    1994-03-01

    A brief description is given of: (1) a newsletter which has been established to notify interested observers of future collaborative programmes, (2) MUSICOS, a group which organizes multisite, continuous spectroscopy, and (3) a computer program which has been written to assist in the coordination of simultaneous observations from ground-based and satellite telescopes.

  2. Multisite spectroscopic seismic study of the β Cep star V2052 Ophiuchi: inhibition of mixing by its magnetic field

    NASA Astrophysics Data System (ADS)

    Briquet, M.; Neiner, C.; Aerts, C.; Morel, T.; Mathis, S.; Reese, D. R.; Lehmann, H.; Costero, R.; Echevarria, J.; Handler, G.; Kambe, E.; Hirata, R.; Masuda, S.; Wright, D.; Yang, S.; Pintado, O.; Mkrtichian, D.; Lee, B. C.; Han, I.; Bruch, A.; De Cat, P.; Uytterhoeven, K.; Lefever, K.; Vanautgaerden, J.; de Batz, B.; Frémat, Y.; Henrichs, H.; Geers, V. C.; Martayan, C.; Hubert, A. M.; Thizy, O.; Tijani, A.

    2012-11-01

    We used extensive ground-based multisite and archival spectroscopy to derive observational constraints for a seismic modelling of the magnetic β Cep star V2052 Ophiuchi. The line-profile variability is dominated by a radial mode (f1 = 7.148 46 d-1) and by rotational modulation (Prot = 3.638 833 d). Two non-radial low-amplitude modes (f2 = 7.756 03 d-1 and f3 = 6.823 08 d-1) are also detected. The four periodicities that we found are the same as the ones discovered from a companion multisite photometric campaign and known in the literature. Using the photometric constraints on the degrees ℓ of the pulsation modes, we show that both f2 and f3 are prograde modes with (ℓ, m) = (4, 2) or (4, 3). These results allowed us to deduce ranges for the mass (M ∈ [8.2, 9.6] M⊙) and central hydrogen abundance (Xc ∈ [0.25, 0.32]) of V2052 Oph, to identify the radial orders n1 = 1, n2 = -3 and n3 = -2, and to derive an equatorial rotation velocity veq ∈ [71, 75] km s-1. The model parameters are in full agreement with the effective temperature and surface gravity deduced from spectroscopy. Only models with no or mild core overshooting (αov ∈ [0, 0.15] local pressure scale heights) can account for the observed properties. Such a low overshooting is opposite to our previous modelling results for the non-magnetic β Cep star θ Oph having very similar parameters, except for a slower surface rotation rate. We discuss whether this result can be explained by the presence of a magnetic field in V2052 Oph that inhibits mixing in its interior.

  3. A gridded multisite weather generator and synchronization to observed weather data

    NASA Astrophysics Data System (ADS)

    Wilks, Daniel S.

    2009-10-01

    Procedures are described for constructing a daily multisite weather generator at a collection of arbitrary (e.g., gridded) locations and for synchronizing the gridded generator to observed weather series at a set of reference stations. The gridded generator is constructed by interpolating conventional single-station weather generator parameters using locally weighted regressions and producing coherent simulations of daily weather from them using spatial correlation functions. When implemented, the synchronization algorithm results in simulated spatial weather fields at the grid points that are consistent with daily weather observations at nearby locations for particular years. The synchronization is achieved by exploiting the latent multivariate Gaussian structure of the spatially distributed weather generator and making use of well-known statistical results that define conditional multivariate Gaussian distributions given known values for a subset of variables from the larger joint distribution. The primary focus is on precipitation, but the nonprecipitation variables in the weather generator are also amenable to gridding and to synchronization with nearby observed weather series. The motivating idea is to allow calibration of spatially distributed hydrological models consistent with the climate of the spatial weather generator, potentially allowing more realistic hydrological simulation, but the procedure may also be useful for interpolation of missing daily weather data.

  4. AstroNet: A Tool Set for Simultaneous, Multi-Site Observations of Astronomical Objects

    NASA Technical Reports Server (NTRS)

    Chakrabarti, Supriya

    1995-01-01

    Earth-based, fully automatic "robotic" telescopes have been in routine operation for a number of years. As their number grows and their distribution becomes global, increasing attention is being given to forming networks of various sorts that will allow them, as a group, to make observations 24 hours a day in both hemispheres. We have suggested that telescopes based in space be part of this network. We further suggested that any telescope on this network be capable of asking, almost in real time, that other robotic telescopes perform support observations for them. When a target of opportunity required support observations, the system would determine which telescope(s) in the network would be most appropriate to make the observations and formulate a request to do so. Because the network would be comprised of telescopes located in widely distributed regions, this system would guarantee continuity of observations This report summarizes our efforts under this contract. We proposed to develop a set of data collection and display tools to aid simultaneous observation of astronomical targets from a number of observing sites. We planned to demonstrate the usefulness of this toolset for simultaneous multi-site observation of astronomical targets. Possible candidates or the proposed demonstration included the Extreme Ultraviolet Explorer (EUVE), International Ultraviolet Explorer (IUE), and ALEXIS, sounding rocket experiments. Ground-based observatories operated by the University of California, Berkeley, the Jet Propulsion Laboratory, and Fairborn Observatory in Mesa, Arizona were to be used to demonstrate the proposed concept. Although the demonstration was to have involved astronomical investigations, the tools were to have been applicable to a large number of scientific disciplines. The software tools and systems developed as a result of the work were to have been made available to the scientific community.

  5. Spectroscopic observations of cool degenerate star candidates

    NASA Technical Reports Server (NTRS)

    Hintzen, P.

    1986-01-01

    Spectroscopic observations are reported for 23 Luyten Half-Second degenerate star candidates and for 13 Luyten-Palomar common proper-motion pairs containing possible degenerate star components. Twenty-five degenerate stars are identified, 20 of which lack previous spectroscopy. Most of these stars are cool - Luyten color class g or later. One star, LP 77-57, shows broad continuum depressions similar to those in LHS 1126, which Liebert and Dahn attributed to pressure-shifted C2. A second degenerate star, LHS 290, exhibits apparent strong Swan bands which are blueshifted about 75 A. Further observations, including polarimetry and photometry, are required to appraise the spectroscopic peculiarities of these stars. Finally, five cool, sharp-lined DA white dwarfs have been observed to detect lines of metals and to determine line strengths. None of these DAs show signs of Mg b or the G band, and four show no evidence of Ca II K. The attempt to detect Ca MI in the fifth star, G199-71, was inconclusive.

  6. The first spectroscopic observation of germanium carbide

    NASA Astrophysics Data System (ADS)

    Ruiz, Jose I.

    Electronic spectroscopy was used to obtain gas phase spectrum of the germanium carbide molecule in emission from a corona excited supersonic expansion source. The (2) 3pi -- X 3pi electronic transition was observed around the 21250 cm-1 region. In this system, vibrational bands and the rotational lines of the O = 0, 1, and 2 components were obtained and analyzed. The equilibrium transition energy is found at 21120.3 cm-1 and the fundamental vibrational frequency for the lowest energy ground state O = 2 component is 795.3 cm -1. This is the first spectroscopic observation of germanium carbide. An unsuccessful attempt to obtain the first electronic emission spectrum of aluminum boride is also described.

  7. Spectroscopic Observations of Nearby Low Mass Stars

    NASA Astrophysics Data System (ADS)

    Vican, Laura; Zuckerman, B. M.; Rodriguez, D.

    2014-01-01

    Young low-mass stars are known to be bright in X-ray and UV due to a high level of magnetic activity. By cross-correlating the GALEX Catalog with the WISE and 2MASS Point Source Catalogs, we have identified more than 2,000 stars whose UV excesses suggest ages in the 10-100 Myr range. We used the Shane 3-m telescope at Lick Observatory on Mount Hamilton, California to observe some of these 2,000 stars spectroscopically. We measured the equivalent width of lithium at 6708 A absorption and H-alpha emission lines. Out of a total of 122 stars observed with the Kast grating spectrometer, we find that roughly 10% have strong lithium absorption features. The high percentage of stars with lithium present is further evidence of the importance of UV emission as a youth indicator for low-mass stars. In addition, we used high-resolution spectra obtained with the Hamilton echelle spectrograph to determine radial velocities for several UV-bright stars. These radial velocities will be useful for the calculation of Galactic UVW space velocities for determination of possible moving group membership. This work is supported by NASA Astrophysics Data Analysis Program award NNX12AH37G to RIT and UCLA and Chilean FONDECYT grant 3130520 to Universidad de Chile. This submission presents work for the GALNYSS project and should be linked to abstracts submitted by David Rodriguez, Laura Vican, and Joel Kastner.

  8. Using a Two-Staged Propensity Score Matching Strategy and Multilevel Modeling to Estimate Treatment Effects in a Multisite Observational Study

    ERIC Educational Resources Information Center

    Rickles, Jordan H.

    2012-01-01

    The study is designed to demonstrate and test the utility of the proposed two-stage matching method compared to other analytic methods traditionally employed for multisite observational studies. More specifically, the study addresses the following research questions: (1) How do different specifications of the matching method influence covariate…

  9. Correlations of experimental isotope shifts with spectroscopic and mass observables

    SciTech Connect

    Cakirli, R. B.; Casten, R. F.; Blaum, K.

    2010-12-15

    Experimental differential observables relating to mean square charge radii, spectroscopic, and mass observables of even-even nuclei are presented for different regions in the nuclear chart. They exhibit remarkable correlations, not heretofore recognized, that provide a new perspective on structural evolution, especially in exotic nuclei. This can also be a guide for future measurements of charge radii, spectroscopic observables, and masses, as well as for future theoretical approaches.

  10. A Two-Stage Propensity Score Matching Strategy for Treatment Effect Estimation in a Multisite Observational Study

    ERIC Educational Resources Information Center

    Rickles, Jordan H.; Seltzer, Michael

    2014-01-01

    When nonrandom treatments occur across sites, within-site matching (WM) is often desirable. This approach, however, can significantly reduce treatment group sample size and exclude substantively important subgroups. To limit these drawbacks, we extend a matching approach developed by Stuart and Rubin to a multisite study. We demonstrate the…

  11. GROUND-BASED MULTISITE OBSERVATIONS OF TWO TRANSITS OF HD 80606b

    SciTech Connect

    Shporer, A.; Winn, J. N.; Dreizler, S.; Colon, K. D.; Wood-Vasey, W. M.; Cerutti, S.; Coban, L.; Costello, K.; Choi, P. I.; Morley, C.; Adams, E.; Moutou, C.; Welsh, W. F.; Pollaco, D.; Barros, S. C. C.; Starkey, D.; Bouchy, F.; DIaz, R. F.; Cabrera-Lavers, A.; Deeg, H.

    2010-10-10

    We present ground-based optical observations of the 2009 September and 2010 January transits of HD 80606b. Based on three partial light curves of the 2009 September event, we derive a midtransit time of T{sub c} [HJD] = 2455099.196 {+-} 0.026, which is about 1{sigma} away from the previously predicted time. We observed the 2010 January event from nine different locations, with most phases of the transit being observed by at least three different teams. We determine a midtransit time of T{sub c} [HJD] = 2455210.6502 {+-} 0.0064, which is within 1.3{sigma} of the time derived from a Spitzer observation of the same event.

  12. Patient compliance with postoperative analgesia after day case surgery: a multisite observational study of patients in North East London

    PubMed Central

    Fahmy, Nisreen; Siah, Julian; Umo-Etuk, Joanna

    2016-01-01

    Background: Pain is the commonest reason for delayed discharge and readmission post day surgery with up to 45% of patients reported to suffer moderate-to-severe post-surgical pain 24 hours after discharge. The importance of post-surgical pain management extends beyond the acute phase when one considers that all chronic post-surgical pain was once acute. Although much focus is given to perioperative analgesia, a patient’s pain management once discharged can be overlooked, whilst at this time the patient’s pain management is within their own hands. Methods: We conducted this multisite observational study of adult patients undergoing day case surgery. After obtaining patient consent data was collected on the operation, intra- and postoperative analgesia administered and discharge analgesia prescribed. Patients were then contacted at home by telephone 48 hours after discharge and asked about their postoperative pain and analgesia requirements. Results: Of 150 patients consented for the enrolment, we were able to obtain postoperative analgesia data on 100. A total of 68% of patients reported pain following discharge with 26% reporting severe pain, defined as a pain score of ⩾7. A total 68% of patients were prescribed and dispensed analgesia, and of those, 83% were compliant with their analgesia. Thus, we conclude that in this patient group, the incidence of postoperative pain was not due to lack of patient compliance, but inadequate analgesia prescription. Discussion: We recognise that our data reflect a patient population in North East London but suggest that the results may still be relevant to a wider patient group across the United Kingdom as the incidence of postoperative pain in our study was similar to published figures. Better patient satisfaction with postoperative analgesia may be obtained with more patient- and surgery-specific analgesic prescription. PMID:27551418

  13. Using and Experiencing the Academic Library: A Multisite Observational Study of Space and Place

    ERIC Educational Resources Information Center

    May, Francine; Swabey, Alice

    2015-01-01

    This study examines how students are using academic library spaces and the role these spaces are playing in the campus community. Data were collected on five campuses (two community colleges, two undergraduate universities, and one technical institute) via observational seating sweeps and questionnaires. The study found remarkably similar usage…

  14. The first spectroscopic observation of germanium carbide

    NASA Astrophysics Data System (ADS)

    Brazier, Christopher R.; Ruiz, José I.

    2011-11-01

    The gas phase spectrum of the germanium carbide radical has been observed at low temperature in emission from a corona excited supersonic expansion source. Many vibrational bands involving the Ω = 0, 1, and 2 components of the (2) 3Π-X 3Π system were recorded and analyzed. The equilibrium transition energy is found at 21120.3 cm -1, in good agreement with theoretical predictions. The fundamental vibrational frequency for the lowest energy ground state Ω = 2 component is 795.3 cm -1.

  15. Seasonal Variation of Methane Emissions in California's Urban and Rural Regions Using Multi-site Observations

    NASA Astrophysics Data System (ADS)

    Jeong, S.; Hsu, Y.; Andrews, A. E.; Bianco, L.; Newman, S.; Cui, X.; Bagley, J.; Graven, H. D.; Salameh, P.; Sloop, C.; LaFranchi, B.; Michelsen, H. A.; Bambha, R.; Weiss, R. F.; Keeling, R. F.; Fischer, M. L.

    2014-12-01

    California's commitment (Assembly Bill 32) to reduce total greenhouse gas (GHG) emissions to 1990 levels by 2020 requires quantification of current GHG emissions. We present seasonal variation of California's total CH4 emissions for summer 2013 - spring 2014, using data from a dozen sites covering urban and rural areas of California that include South Coast Air Basin (SoCAB), Central Valley, and San Francisco Bay Area. We apply a Bayesian inverse model to estimate CH4 emissions from discrete regions of California and source sectors by combining atmospheric measurements, upstream background, updated high-resolution prior emission maps developed for California, and predicted atmospheric transport from WRF-STILT. We quantify site-specific model-measurement uncertainties due to transport using simulated and observed meteorology, background estimated from oceanic and aircraft observations, and the prior emissions. In particular, we evaluate predicted transport variables in WRF with networks of surface and upper air observations. Preliminary inversion results during summer of 2013 suggest that state total CH4 emissions are 1.2 - 1.7 times higher than the current CARB inventory. Here, we extend and improve upon earlier analyses to provide a full seasonal cycle of CH4 emissions across all major urban and rural regions in California.

  16. Spectroscopic observations of spatial and temporal variations on Venus

    NASA Technical Reports Server (NTRS)

    Young, A. T.; Young, L. G.; Woszczyk, A.

    1974-01-01

    Details of the Table Mountain spectroscopic patrol of Venus in September-October 1972 are given. The data indicate systematic variation over the disc, with more CO2 absorption near the terminator than at the limb, and slightly more in the southern than in the northern hemisphere. The semiregular four-day variation, reported to occur simultaneously over the disk at 8689 A by Young et al. (1973), is confirmed by observations of the 7820 A and 7883 A CO2 bands.

  17. Spectroscopic Observations of Fe XVIII in Solar Active Regions

    NASA Astrophysics Data System (ADS)

    Teriaca, Luca; Warren, Harry P.; Curdt, Werner

    2012-08-01

    The large uncertainties associated with measuring the amount of high temperature emission in solar active regions (ARs) represents a significant impediment to making progress on the coronal heating problem. Most current observations at temperatures of 3 MK and above are taken with broadband soft X-ray instruments. Such measurements have proven difficult to interpret unambiguously. Here, we present the first spectroscopic observations of the Fe XVIII 974.86 Å emission line in an on-disk AR taken with the SUMER instrument on SOHO. Fe XVIII has a peak formation temperature of 7.1 MK and provides important constraints on the amount of impulsive heating in the corona. Detailed evaluation of the spectra and comparison of the SUMER data with soft X-ray images from the X-Ray Telescope on Hinode confirm that this line is unblended. We also compare the spectroscopic data with observations from the Atmospheric Imaging Assembly (AIA) 94 Å channel on the Solar Dynamics Observatory. The AIA 94 Å channel also contains Fe XVIII, but is blended with emission formed at lower temperatures. We find that it is possible to remove the contaminating blends and form relatively pure Fe XVIII images that are consistent with the spectroscopic observations from SUMER. The observed spectra also contain the Ca XIV 943.63 Å line that, although a factor 2-6 weaker than the Fe XVIII 974.86 Å line, allows us to probe the plasma around 3.5 MK. The observed ratio between the two lines indicates (isothermal approximation) that most of the plasma in the brighter Fe XVIII AR loops is at temperatures between 3.5 and 4 MK.

  18. Spectroscopic Observations of the Recent M33 Nova Candidate

    NASA Astrophysics Data System (ADS)

    Shafter, A. W.; Ciardullo, R.; Bode, M. F.; Darnley, M. J.; Misselt, K. A.

    2010-10-01

    We report spectroscopic observations of the recent M33 nova candidate (M33N 2010-10a?), which was discovered by K. Nishiyama and F. Kabashima (Miyaki-Argenteus Observatory, Japan) on 2010 Oct. 26.65 UT. At our request a spectrum (410-950 nm) of the nova candidate was obtained by John Caldwell on 2010 Oct. 28.37 UT (~2 days post discovery) with the Marcario Low-Resolution Spectrograph on the 9.2m Hobby-Eberly Telescope.

  19. Carnegie Supernova Project: Spectroscopic Observations of Core Collapse Supernovae

    NASA Astrophysics Data System (ADS)

    Morrell, Nidia I.

    2012-09-01

    The Carnegie Supernova Project (CSP) has performed, during the period 2004-2009, the optical and NIR follow up of 253 supernovae (SNe) of all types. Among those, 124 were core collapse events, comprising 93 SNe of type II and 31 of types Ib/Ic/IIb. Our follow up consisted of photometric observations suitable to build detailed light curves and a considerable amount of optical spectroscopy. The bulk of our observations is carried out at Las Campanas Observatory, while access to other facilities is also provided thanks to our strong collaboration with the Millennium Center for Supernova Studies (MCSS). Our spectroscopic observations were primarily aimed at typing possible new SNe, and follow-up the evolution of CSP targets. One of the goals of the follow-up of type II SNe is the application of independent distance indicators such as the Standard Candle (SCM) and the Expanding Photosphere (EPM) methods. Moreover, through the study of the spectroscopic evolution of these objects, from as early as possible after explosion to the nebular phases, we hope to contribute to their further understanding. Specific analysis of particular objects is underway by members of the CSP and an extended collaboration.

  20. Employing Multiple Spectroscopic Techniques Simultaneously to Observe Protein Unfolding

    NASA Astrophysics Data System (ADS)

    Crowe, Michael; Kelty, Ben; Link, Justin

    2015-03-01

    A protein's function is directly related to its native, folded structure. In order to study the structure of proteins, the unfolding process may be characterized. In our study, by using the spectroscopic techniques of circular dichroism (CD), absorption, and fluorescence simultaneously, we examined the unfolding of horse heart cytochrome c, a well-studied, model protein by gradually increasing the concentration of the chemical denaturant, guanidine hydrochloride. The signal changes from these modalities over the course of the unfolding reaction provides some of the thermodynamic properties like Gibbs free energy for insight into the stability of the protein. This allows us to compare the three techniques under the exact same conditions. The objective of this session is to present recent work in developing a protocol to observe the unfolding of cytochrome c using fluorescence, absorbance, and CD simultaneously.

  1. Spectroscopic observations of the dwarf nova IP Pegasi

    SciTech Connect

    Hessman, F.V. )

    1989-08-01

    Time-resolved spectroscopic measurements of IP Peg were obtained immediately after a dwarf nova eruption. The radio-velocity amplitude of the white dwarf (118 + or - 10 km/s) implied by measurements from the wings of the Balmer emission lines is different from that found previously. The results suggest a mass ratio M1/M2 of 0.435 + or - 0.052 and that the narrow component is due to unusually strong chromospheric emission from the late-type star. The low value for the radial-velocity amplitude of this narrow emission (about 200 km/s) is consistent with the observed absorption-line amplitude of 331 km/s if the irradiated surface of the M dwarf produces little line absorption. 40 refs.

  2. Spectroscopic and video observations of fullerene production arcs

    SciTech Connect

    Lorents, D.C.; Stalder, K.R.; Keegan, D.M.; Ruoff, R.S.; Malhotra, R.M.

    1993-12-01

    Spatially resolved spectroscopic studies of a carbon arc operating under fullerene production conditions have been made across the visible wavelength range using an imaging Optical Multichannel Analyzer. C{sub 2} Swan bands are observed to be the major visible emissions although strong CI and CII as well as He I atomic lines are also observed. Video and photographic studies of the arc characteristics show the Swan-band emissions to be concentrated most intensely near the anode but also to appear strongly in regions well outside the electrode gap region. Vibrational and rotational temperatures of these bands provide information on the temperatures in various regions of the arc. The characteristic spatial structure of the arcs observed in the Swan-band light suggests that they are excited by electrons whose trajectories are controlled by the local electric and magnetic fields. The arc exhibits complex and interesting temporal behavior that has been observed with a video camera using short exposure times. Video film taken through a Swan-band filter clearly shows the dominant spatial features of the C{sub 2} emissions.

  3. Spectroscopic observations and analysis of the peculiar SN1999aa

    SciTech Connect

    Garavini, G.; Folatelli, G.; Goobar, A.; Nobili, S.; Aldering,G.; Amadon, A.; Amanullah, R.; Astier, P.; Balland, C.; Blanc, G.; Burns,M.S.; Conley, A.; Dahlen, T.; Deustua, S.E.; Ellis, R.; Fabbro, S.; Fan,X.; Frye, B.; Gates, E.L.; Gibbons, R.; Goldhaber, G.; Goldman, B.; Groom, D.E.; Haissinski, J.; Hardin, D.; Hook, I.M.; Howell, D.A.; Kasen,D.; Kent, S.; Kim, A.G.; Knop, R.A.; Lee, B.C.; Lidman, C.; Mendez, J.; Miller, G.J.; Moniez, M.; Mourao, A.; Newberg, H.; Nugent, P.E.; Pain,R.; Perdereau, O.; Perlmutter, S.; Prasad, V.; Quimby, R.; Raux, J.; Regnault, N.; Rich, J.; Richards, G.T.; Ruiz-Lapuente, P.; Sainton, G.; Schaefer, B.E.; Schahmaneche, K.; Smith, E.; Spadafora, A.L.; Stanishev,V.; Walton, N.A.; Wang, L.; Wood-Vasey, W.M.

    2003-12-10

    We present an extensive new time series of spectroscopic data of the peculiar SN 1999aa in NGC 2595. Our data set includes 25 optical spectra between -11 and +58 days with respect to B-band maximum light, providing an unusually complete time history. The early spectra resemble those of an SN 1991T-like object but with a relatively strong CaH and K absorption feature. The first clear sign of Si II lambda 6355, characteristic of Type Ia supernovae, is found at day -7, and its velocity remains constant up to at least the first month after B-band maximum light. The transition to normal-looking spectra is found to occur earlier than in SN 1991T, suggesting SN 1999aa as a possible link between SN 1991T-like and Branch-normal supernovae. Comparing the observations with synthetic spectra, doubly ionized Fe, Si, and Ni are identified at early epochs. These are characteristic of SN 1991 T-like objects. Furthermore, in the day -11 spectrum, evidence is found for an absorption feature that could be identified as high velocity C II lambda 6580 or H alpha. At the same epoch C III lambda 4648.8 at photospheric velocity is probably responsible for the absorption feature at 4500 8. High-velocity Ca is found around maximum light together with Si II and Fe II confined in a narrow velocity window. Implied constraints on supernovae progenitor systems and explosion hydrodynamic models are briefly discussed.

  4. Spectroscopic Observations of Propagating Disturbances in Polar Coronal Hole

    NASA Astrophysics Data System (ADS)

    Gupta, Girjesh R.; Marsch, Eckart; Solanki, Sami K.; Banerjee, Dipankar; Teriaca, Luca

    2012-07-01

    We focus on long duration spectroscopic observations of the south polar coronal hole taken on 1997 February 25 by the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) spectrometer aboard SOHO. We analyze the data in the on-disk part of the coronal hole to find any signature of propagating waves or high speed up-flows. We find the clear presence of propagating disturbances in intensity and Doppler velocity with a projected propagation speed of about 60~km~s^{-1} and a periodicity of ≈14.5~min. During the propagation, the intensity enhancement is associated with a blue-shifted Doppler velocity. These disturbances are clearly seen in intensity at higher latitudes (i.e. closer to the limb), whereas disturbances in Doppler velocity becomes faint there. We study average spectral line profiles at the roots of these disturbances and along the propagating ridge. Based on our analysis, we interpret these disturbances in terms of propagating slow magneto-acoustic waves.

  5. LBT/LUCI Spectroscopic Observations of z≃7 Galaxies

    NASA Astrophysics Data System (ADS)

    Bian, Fuyan; Stark, Daniel P.; Fan, Xiaohui; Jiang, Linhua; Clément, Benjamin; Egami, Eiichi; Frye, Brenda; Green, Richard F.; McGreer, Ian D.; Cai, Zheng

    2015-06-01

    We present deep near-infrared spectroscopic observations of 13 luminous z≃ 7 Lyman break galaxies (LBGs) ({{M}UV}≃ -21) and a z≃ 9.6 lensed LBG candidate, MACS1149-JD1, using the LBT/LUCI spectrograph in the multi-object mode and long-slit mode, respectively. The z˜ 7 galaxies are selected in one of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey/WIDE survey observations, the UKIRT Infrared Deep Sky Survey Ultra Deep Survey field, and MACS1159-JD1 is selected from the Cluster Lensing And Supernova survey with Hubble survey observations. With ˜4-5 hr integrations, the LBT spectra are sensitive to Lyα emission, with rest-frame equivalent width greater than 55 Å (E{{W}0}\\gt 55 Å) at z˜ 7 and 90 Å (E{{W}0}\\gt 90 Å) at z˜ 9.5. No Lyα emission is observed in any of the z≃ 7 LBGs. After correcting the spectroscopic incompleteness, our measurements place an upper limit on the Lyα emission fraction of {{X}Lyα }(E{{W}0}\\gt 55 { {\\mathring{{A}} }},z≃ 7)\\lt 9.8% in luminous LBGs at z≃ 7. This result is consistent with the lack of Lyα emission in z\\gt 7 LBGs in previous studies. Together with other measurements of the Lyα emission fraction in LBGs at z≃ 7, this study puts a strong constraint on the fraction of luminous z≃ 7 LBGs with large EW Lyα, {{X}Lyα }(E{{W}0}\\gt 55 { {\\mathring{{A}} }},z≃ 7)=2.6-2.6+3.2%. We estimate the expected Lyα emission fraction at z≃ 7 by extrapolating the evolution of the fraction at low redshifts and find that the observed Lyα emission fraction is lower than the expected Lyα emission fraction at the 89% significance level, consistent with expectations if Lyα emission in z≃ 7 LBGs has been suppressed by neutral hydrogen in the intergalactic medium or optically thick absorbers around the galaxies. We do not find any strong Lyα emission feature at the redshift range of z ≃ 7.3-9.7 in the MACSJ1159-JD1 spectrum, either. This is consistent with the conclusion that Lyα emission in

  6. Spectroscopic Observations of the Star Formation Regions in Nearby Galaxies

    NASA Astrophysics Data System (ADS)

    Kong, X.; Lin, L.; Li, J. R.; Zhou, X.; Zou, H.; Li, H. Y.; Chen, F. Z.; Du, W.; Fan, Z.; Mao, Y. W.; Wang, J.; Zhu, Y. N.; Zhou, Z. M.

    2014-01-01

    During the late 1990s and the first decade of the 21st century, the 8˜10 m scale ground-based telescopes are helping astronomers learn much more about how galaxies develop. The existing 2˜4 m scale telescopes become less important for astrophysical researches. To use the existing 2˜4 m scale telescopes to address important issues in cosmology and extragalactic and galactic astronomy, we have to consider very carefully which kind of things we can do, and which we can not. For this reason, the Time Allocation Committee (TAC) of the National Astronomical Observatories of China (NAOC) 2.16 m telescope decides to support some key projects since 2013. Nearby galaxies supply us with the opportunity to study galaxy dynamics and star formation on large scales, yet are close enough to reveal the details. Star formation regions in nearby galaxies provide an excellent laboratory to study the star formation processes, the evolution of massive stars, and the properties of the surrounding interstellar medium. A wealth of information can be obtained from the spectral analysis of the bright emission lines and the stellar continuum. Considering these, we proposed a long-term project ``Spectroscopic Observations of the Star Formation Regions in Nearby Galaxies'', and it becomes the key project of the NAOC 2.16 m telescope since 2013, supported with 30 dark/grey nights per year. The primary goal of this project is to observe the spectroscopy of star formation regions in 20 nearby galaxies, with the NAOC 2.16 m telescope and the Hectospec/MMT (Multiple Mirror Telescope) multifiber spectrograph by Telescope Access Program (TAP). With the spectra of a large sample of star formation regions, combining multi-wavelength data from UV to IR, we can investigate, understand, and quantify the nature of the deviation from the starbursts' IRX-β (the IR/UV ratio ``IRX'' versus the UV color ``β'') correlation. It will be important for a better understanding of the interaction of dust and

  7. Using a Two-Stage Propensity Score Matching Strategy and Multilevel Modeling to Estimate Treatment Effects in a Multisite Observational Study

    ERIC Educational Resources Information Center

    Rickles, Jordan Harry

    2012-01-01

    In this study I present, demonstrate, and test a method that extends the Stuart and Rubin (2008) multiple control group matching strategy to a multisite setting. Three primary phases define the proposed method: (1) a design phase, in which one uses a two-stage matching strategy to construct treatment and control groups that are well balanced along…

  8. Statistical multisite simulations of summertime precipitation over South Korea and its future change based on observational data

    NASA Astrophysics Data System (ADS)

    Kim, Ji-Won; Kim, Kwang-Yul; Kim, Maeng-Ki; Cho, Chun-Ho; Lee, Youngjo; Lee, Jaeyong

    2013-11-01

    In this study, a weather generator for summer (May 19 - September 15) precipitation over South Korea is developed. Precipitation data for 33 years (1979-2011) observed at 57 stations of Korea Meteorological Administration (KMA) are used to develop a new weather generator. Using the cyclostationary empirical orthogonal function (CSEOF) technique, the observed precipitation data is described as a linear combination of deterministic evolution patterns and corresponding stochastic amplitude (principal component) time series. An autoregressive-moving average (ARMA) model is used to generate one hundred sets of synthetic amplitude time series for the period of 1979-2061 (83 years) with similar statistical properties of the original amplitude time series. Based on these synthetic time series and the annually repeating evolution patterns, one hundred sets of synthetic summer precipitation were generated. Statistical characteristics of the synthetic datasets are examined in comparison with those of the KMA observational record for the period of the observational record. Characteristic changes of synthetic precipitations for a future period are also examined. The seasonal cycle in the synthetic precipitation is reproduced faithfully with typical bimodal peaks of summer precipitation. The spatial correlation patterns of the synthetic precipitation are fairly similar to that of the observational data. The frequency-intensity relationship of the synthetic precipitation also looks similar to that of the observational data. In the future period, precipitation amount increases except in the precipitation range of (0,10) mm day-1 with nearly no change in the frequency of no-rain days; frequency increase is particularly conspicuous in the range of (100,500) mm day-1.

  9. Spectroscopic Observation of Chemical Interaction Between Impact-induced Vapor Clouds and the Ambient Atmosphere

    NASA Technical Reports Server (NTRS)

    Sugita, S.; Heineck, J. T.; Schultz, P. H.

    2000-01-01

    Chemical reactions within impact-induced vapor clouds were observed in laboratory experiments using a spectroscopic method. The results indicate that projectile-derived carbon-rich vapor reacts intensively with atmospheric nitrogen.

  10. Estimating CH4 and CO Emissions in California's Urban and Rural Regions Using Multi-site Observations

    NASA Astrophysics Data System (ADS)

    Jeong, S.; Andrews, A. E.; Bianco, L.; Graven, H. D.; Hsu, Y.; Newman, S.; Novakovskaia, E.; Vaca, P.; Salameh, P.; Sloop, C.; Weiss, R. F.; Keeling, R. F.; Fischer, M. L.

    2013-12-01

    California's commitment (Assembly Bill 32) to reduce total greenhouse gas (GHG) emissions to 1990 levels by 2020 (~20% reduction) requires quantification of current GHG emissions. We will present atmospheric inversion estimates of California's total CH4 emissions for summer 2013, using data from multiple sites covering urban and rural areas of California's South Coast Air Basin (SoCAB), Central Valley, and San Francisco Bay Area. We will also use measured CO from two tall-tower sites (Central Valley and SoCAB) to quantify CO emissions as well as to evaluate atmospheric transport. We use Bayesian inverse modeling to estimate the CH4 and CO emissions from discrete regions of California by combining the atmospheric measurements, upstream background, high-resolution prior emission maps, and predicted atmospheric transport from WRF-STILT. We quantify site-specific model-measurement uncertainties due to transport using meteorological data from a network of atmospheric profilers and in-situ sensors, due to background using oceanic and aircraft observations, and the prior emissions. To reduce the uncertainty in transport, we assimilate available meteorological measurements from surface and upper air stations, and wind profilers into the WRF model. Preliminary inversion results during September 2010 - June 2011 and summer of 2012 suggest that state total CH4 emissions are 1.2 - 1.8 times higher than the current CARB inventory and we will update these estimates. We expect the results of this study will significantly improve upon existing work in quantifying CH4 and CO emissions in California's urban and rural regions.

  11. Spectroscopic observations of X-ray selected late type stars

    NASA Technical Reports Server (NTRS)

    Takalo, L. O.

    1988-01-01

    A spectroscopic survey of nine X-ray selected late type stars was conducted. These stars are serendipitously discovered EINSTEIN X-ray sources, selected from two large x-ray surveys: the Columbia Astrophysical Laboratory survey (five stars) and the CFA Medium Sensitivity survey (four stars). Four of the Columbia survey stars were found to be short period binaries. The fifth was found to be an active single G dwarf. None of the Medium Sensitivity survey stars were found to be either binaries or active stars. Activity was measured by comparing the H-alpha and the CaII infrared triplet (8498, 8542) lines in these stars to the lines in inactive stars of similar spectral type. A correlation was found between the excess H-alpha lime emission and V sin(i) and between the excess H-alpha line emission and X-ray luminosity. No correlation was found between the infrared line emission and any other measured quantity.

  12. Spectroscopic and photometric observations of M supergiants in Carina.

    NASA Technical Reports Server (NTRS)

    Humphreys, R. M.; Strecker, D. W.; Ney, E. P.

    1972-01-01

    Spectroscopic study of 30 Southern-Hemisphere M supergiants mostly in Carina in the blue and near-infrared, and photometrical study of these stars from 0.4 to 18 microns. The uncertainties in the determinations of interstellar extinction are discussed, and the spatial distribution of the M supergiants in the Carina arm is shown. The presence of the 11-micron excess attributed to silicate dust is a common feature. Stars of the same spectral type and luminosity class are remarkably homogeneous in their long-wave behavior. The silicate feature becomes more prominent in the more luminous stars and in stars of later spectral type. Four composite systems show little long-wave excess. The two VV Cephei objects have excesses probably produced by gas emission, and the other two have little or no excess - supporting the suggestion that the presence of the early star prohibits the formation of a dust envelope. Three stars - VY CMa, VX Sgr, and HD 9767 - appear to be extreme examples of stars with large excesses over the entire long-wave region. It is suggested that these objects are surrounded by large amounts of particulate material over a great range of distances from the stars.

  13. NMR spectroscopic observation of a metal-free acetylide anion.

    PubMed

    Tanaka, Yoshiyuki; Arakawa, Makoto; Yamaguchi, Yohei; Hori, Chieko; Ueno, Masahiro; Tanaka, Takeyuki; Imahori, Tatsushi; Kondo, Yoshinori

    2006-10-20

    A metal-free acetylide was observed by using NMR spectroscopy. Metal-free acetylides are closely related to reactive intermediates (carbanions) in solution; therefore, they have been regarded as unobservable species. However, we generated this highly reactive and unstable species through the deprotonation of phenylacetylene by using the strong nonmetallic phosphazene base tBu-P4. In the presence of tBu-P4, the J coupling between the ethynyl carbon and hydrogen nuclei (1J(C,H)) of phenylacetylene disappeared; this indicates the deprotonation of the alkyne terminal. Furthermore, a large low-field shift (approximately 90 ppm) of the alkyne carbon resonance was observed. We concluded that we have observed a metal-free carbanion with a formal charge on an sp-hybridized carbon atom for the first time. PMID:17441096

  14. Herschel Spectroscopic Observations of Little Things Dwarf Galaxies

    NASA Astrophysics Data System (ADS)

    Cigan, Phil; Young, Lisa; Cormier, Diane; Lebouteiller, Vianney; Madden, Suzanne; Hunter, Deidre; Brinks, Elias; Elmegreen, Bruce; Schruba, Andreas; Heesen, Volker; the Little Things Team

    2016-01-01

    We present far-infrared (FIR) spectral line observations of five galaxies from the Little Things sample: DDO 69, DDO 70, DDO 75, DDO 155, and WLM. While most studies of dwarfs focus on bright systems or starbursts due to observational constraints, our data extend the observed parameter space into the regime of low surface brightness dwarf galaxies with low metallicities and moderate star formation rates. Our targets were observed with Herschel at the [C ii] 158 μm, [O i] 63 μm, [O iii] 88 μm, and [N ii] 122 μm emission lines using the PACS Spectrometer. These high-resolution maps allow us for the first time to study the FIR properties of these systems on the scales of larger star-forming complexes. The spatial resolution in our maps, in combination with star formation tracers, allows us to identify separate photodissociation regions (PDRs) in some of the regions we observed. Our systems have widespread [C ii] emission that is bright relative to continuum, averaging near 0.5% of the total infrared (TIR) budget—higher than in solar-metallicity galaxies of other types. [N ii] is weak, suggesting that the [C ii] emission in our galaxies comes mostly from PDRs instead of the diffuse ionized interstellar medium (ISM). These systems exhibit efficient cooling at low dust temperatures, as shown by ([O i]+[C ii])/TIR in relation to 60 μm/100 μm, and low [O i]/[C ii] ratios which indicate that [C ii] is the dominant coolant of the ISM. We observe [O iii]/[C ii] ratios in our galaxies that are lower than those published for other dwarfs, but similar to levels noted in spirals.

  15. Spectroscopic observation of nitrogen anions N(-) in solid matrices.

    PubMed

    Boltnev, R E; Bykhalo, I B; Krushinskaya, I N; Pelmenev, A A; Mao, S; Meraki, A; McColgan, P T; Lee, D M; Khmelenko, V V

    2016-06-21

    Analysis of old and recent experiments on thermoluminescence of cryocrystals and nanoclusters of N2, Ne, Ar, and Kr containing stabilized nitrogen atoms, suggests that the so-called γ-line may correspond to the bound-bound transition (1)D-(3)P of nitrogen anions N(-) formed in solids by the association of delocalized electrons and metastable nitrogen atoms N((2)D). The recent observations of the γ-line were accompanied by simultaneous luminescence of metastable nitrogen N((2)D) atoms and exoelectron emission. The fine structure of the γ-line at 793 nm has been experimentally observed and investigated for the first time. PMID:27241627

  16. SOHO/UVCS spectroscopic observations of coronal oscillations

    NASA Astrophysics Data System (ADS)

    Mancuso, Salvatore; Raymond, John C.; Rubinetti, Sara; Taricco, Carla

    2016-06-01

    We analyzed the temporal evolution of the intensities and Doppler shifts of two sets of high-cadence sit-and-stare observations acquired with the Ultraviolet Coronagraph Spectrometer (UVCS) on board the Solar and Heliospheric Observatory (SOHO) satellite to detect the possible signature of wave and oscillatory motions in the solar corona. The first set of data consisted of H I Lyα observations collected on 1997 December 14 at 1.43 RS above the eastern limb of the Sun. Spectral analysis of the data revealed clear Doppler-shift oscillations with period P = 14.3 min over a portion of the UVCS slit. The origin of these oscillations is attributable to the excitation of propagating fast-mode magnetoacoustic kink waves along a narrow, jet-like ejection observed higher up in the white-light corona. The second set of data consisted of O VI 1032 Å observations collected on 1996 December 19 at 1.38 RS above the north polar coronal hole. In this case, clear intensity oscillations (P = 19.5 min) and Doppler-shift oscillations (P = 7.2 min) over two different portions of the UVCS slit were detected. The origin of these oscillations is attributable to the excitation of slow-mode magnetoacoustic waves propagating along polar plumes that may partially account for heating of the plasma in the corona.

  17. Spectroscopic Observations of the 2011 Draconids Meteor Shower

    NASA Astrophysics Data System (ADS)

    Rudawska, Regina; Zender, Joe; Jenniskens, Peter; Vaubaillon, Jeremie; Koten, Pavel; Margonis, Anastasios; Tóth, Juraj; McAuliffe, Jonathan; Koschny, Detlef

    2014-08-01

    Some past October Draconid shower meteoroids fell apart in a spray of fragments at the end of their trajectory before slowing down, from which it was concluded that these were among the most fragile meteoroids known. In those instances, the dust could not be reliably traced to a particular return of the parent comet 21P/Giaconini-Zinner. On October 8th, 2011, Earth was predicted to transverse the 1900 A.D. dust ejecta of the comet. In 1900, the comet's perihelion distance first moved significantly inwards to the Sun and ejection conditions could have been unusual. An airborne observing campaign was organized, with several teams contributing imaging and spectrographic cameras to study the manner in which these meteoroids released the volatile element sodium during the ablation process in the Earth's atmosphere. IMCCE, ESA, and the SETI Institute contributed spectrographic cameras based on low-light WATEC 902H2 Ultimate, low-light LCC1, and GenII XX1332 image intensified cameras. An outburst was observed, much as predicted. Despite a lack of bright meteors, a total of 15 Draconid spectra were recorded. All show evidence of an early release of sodium. The loss of sodium was observed to coincide with the formation of a distinct wake of fragments. The observations show that 21P/Giacobini-Zinner ejected fragile meteoroids during the return in 1900. Those grains may have lost some sodium even before impacting Earth.

  18. Spectroscopic observations of D-type symbiotic stars

    NASA Astrophysics Data System (ADS)

    Pereira, C. B.; Landaberry, S. J. C.; Junqueira, S.

    1998-05-01

    Observations of five D-type symbiotics are presented: three oxygen Mira (He2-38, H2-38 and H1-36) and two carbon Mira symbiotics (AS 210 and SS 38). The observations in the spectral range between 3200Angstroms, and 7400Angstroms, show the presence of several emission lines in various states of excitation. A line list is provided with their suggested identifications. Several parameters were derived for each object: interstellar reddening as determined from Balmer decrement and Heii lines, temperature and electronic density, abundance ratios of Ne/O, Ar/O, Fe/Ne, N/O and He/H. We found nitrogen enrichment while for the other elements their abundances are compatible with solar, except iron which is depleted. We did not detect significant changes in the line and in the continuos spectra of the stars analyzed here, except for He2-38, which increased its degree of excitation compared to Allen's (1984) catalogue. Based on observations made with the 1.52m telescope at the European Southern Observatory (La Silla, Chile) under the agreement with the CNPq-Observatório Nacional (Brazil)

  19. Rotational Spectroscopic Studies and Observational Searches for HO3

    NASA Astrophysics Data System (ADS)

    Widicus Weaver, Susanna

    Interstellar chemistry is largely driven by reactions of unstable molecules that serve as reaction intermediates in terrestrial chemistry. One such class of compounds are weakly-bound clusters. These clusters could form in interstellar environments through radiative association reactions, but their identification and characterization in interstellar environments is limited by a lack of rotational spectral information. One such species is HO3, which could be formed in the interstellar medium from O2 and OH. HO3 has been studied extensively in the infrared, and there are a few microwave spectral studies that have also been reported. However, no millimeter or submillimeter spectral information is available to guide astronomical observations. In this talk, we will present the laboratory characterization of trans -HO3 and trans -DO3 from 70 to 450 GHz using our newly developed fast sweeping technique. The molecular constants have been significantly refined, and additional higher order centrifugal distortion constants have been determined. We will also present an initial observational search for HO3 in 32 star forming regions. Although no HO3 lines have been detected thus far, strict upper limits can be placed on the HO3 column density in these sources based on this analysis. Additional Authors: Luyao Zou, Brian M. Hays.

  20. Herschel FIR Spectroscopic Observations of L1448-MM

    NASA Astrophysics Data System (ADS)

    Lee, Jinhee; Lee, J.; DIGIT Team

    2012-01-01

    We present the FIR (continuum and line) maps and spectra of L1448-MM at 55 to 210 micron observed with the range scan mode of PACS on the Herschel Space Observatory, as part of the DIGIT key program. L1448-MM was previously known as an embedded Class 0 and prominent outflow source, and a secondary YSO was claimed by the Spitzer images and confirmed by submm interferometric observations. The PACS detected various CO, OH, H2O, and OI lines. The PACS line and continuum maps show that the emission at shorter wavelengths peaks at the central spatial pixel (the primary YSO position) although the line emission of low energy levels distributes along the outflow direction. According to our excitation analysis, the CO gas has two temperature components (warm and hot) that are tentatively attributed to PDR and shock, respectively. However, the H2O gas with the rotational temperature of 200 K seems to trace the shock. Interestingly, the relative strength of OH transitions suggests the IR pumping process dominates in L1448-MM. The gas along the outflow cavities in L1448-MM seems to be heated mainly by shock and UV photons, and relative line luminosities indicate that H2O and CO are the main coolants of this gas, although cooling by OI and OH cannot be ignored.

  1. Spectroscopic observations of the optical counterpart of Centaurus X-4

    NASA Technical Reports Server (NTRS)

    Van Paradijs, J.; Verbunt, F.; Van Der Linden, T.; Pedersen, H.; Wamsteker, W.

    1980-01-01

    The optical spectrum of the transient X-ray burst source Centaurus X-4 was observed about 5 weeks after the source reached its maximum. The brightness of the optical counterpart had decreased to V = 18.2, and the star had become appreciably redder (B - V = 0.7) compared to its color at maximum. The spectrum of Centaurus X-4 is similar to that of cataclysmic variables showing strong emission lines of H-1 and weaker lines of He-1 and He-2. The N03 lambda 4640 line is not visible. The continuum energy distribution of Centaurus X-4 shows the presence of a main-sequence star in the system, with spectral type between K3 and K7. This is consistent with the orbital period of 8.2 hr proposed by Kaluzienski et al (1980), if the main-sequence star is close to filling its Roche lobe.

  2. Spectroscopic observations of the symbiotic binary RW Hydrae

    NASA Technical Reports Server (NTRS)

    Kenyon, Scott J.; Fernandez-Castro, Telmo

    1987-01-01

    Ultraviolet/optical spectrophotometry and infrared photometry show that the symbiotic binary RW Hya is comprised of an M giant (with L of about 1000 solar luminosities) and a compact object (with L of about 200 solar luminosities) which resembles the central star of a planetary nebula. The luminosity of the hot component is produced by a nuclear shell source which is replenished by the wind of the red giant at a rate of about 10 to the -8th solar mass/yr. Results indicate that the binary is surrounded by an H II region (of radius of about 10 AU) which gives rise to the observed emission lines and radio emission. The He(2+) and O(2+) regions are found to be confined to the immediate vicinity of the hot component.

  3. Preliminary results of V440 Per and α UMi observations with the Poznan Spectroscopic Telescope

    NASA Astrophysics Data System (ADS)

    Fagas, M.; Baranowski, R.; Bartczak, P.; Borczyk, W.; Dimitrow, W.; Kaminski, K.; Kwiatkowski, T.; Ratajczak, R.; Rozek, A.; Schwarzenberg-Czerny, A.

    2009-03-01

    Presented herein are preliminary radial velocity results for two classical Cepheids: V440 Per and α UMi (Polaris). Both stars have been observed with the Poznan Spectroscopic Telescope (PST), operational since Aug 2007 at the Borowiec Station of Poznań Astronomical Observatory in Poland. Data obtained for V440 Per suggest the presence of a low-amplitude secondary mode of pulsations. Results of α UMi observations confirm further pulsation amplitude growth, as observed during the last decades.

  4. Spectroscopic observations of the detached binary PG 1413 + 015

    NASA Technical Reports Server (NTRS)

    Fulbright, Michael S.; Liebert, James; Bergeron, P.; Green, Richard

    1993-01-01

    We present improved estimates of the stellar parameters of the eclipsing, precataclysmic binary system PG 1413 + 015 (GH Vir), which has an orbital period of only 8h16m. Model atmosphere fits a Balmer line profiles yield T(eff) = 48,800 +/- 1200 K and log g = 7.70 +/- 0.11 for the DAO white dwarf primary star, from which a mass of 0.51 +/- 0.04 solar mass is inferred using evolutionary models. An ultraviolet spectrum obtained with the IUE Observatory has a slope consistent with this temperature and the assumption of no interstellar extinction. A red CCD spectrum of the secondary star during the 12-minute total eclipse indicates a spectral type of M3 V-M5 V. Reanalysis of the eclipse light curve leads to an inferred radius of 0.15 solar radius and a mass of 0.10 solar mass for the secondary, the latter being marginally consistent with the spectral type. Reprocessing on the facing side of the secondary produces phase-dependent Balmer line emission and detectable variations in the continuum from 6500-9000 A. The observed levels of reprocessing are consistent with expectations based on the above stellar parameters.

  5. Spitzer mid-infrared spectroscopic observations of planetary nebulae

    NASA Astrophysics Data System (ADS)

    Mata, H.; Ramos-Larios, G.; Guerrero, M. A.; Nigoche-Netro, A.; Toalá, J. A.; Fang, X.; Rubio, G.; Kemp, S. N.; Navarro, S. G.; Corral, L. J.

    2016-06-01

    We present Spitzer Space Telescope archival mid-infrared (mid-IR) spectroscopy of a sample of 11 planetary nebulae (PNe). The observations, acquired with the Spitzer Infrared Spectrograph (IRS), cover the spectral range 5.2-14.5 μm that includes the H2 0-0 S(2) to S(7) rotational emission lines. This wavelength coverage has allowed us to derive the Boltzmann distribution and calculate the H2 rotational excitation temperature (Tex). The derived excitation temperatures have consistent values ≃900 ± 70 K for different sources despite their different structural components. We also report the detection of mid-IR ionic lines of [Ar III], [S IV], and [Ne II] in most objects, and polycyclic aromatic hydrocarbon features in a few cases. The decline of the [Ar III]/[Ne II] line ratio with the stellar effective temperature can be explained either by a true neon enrichment or by high density circumstellar regions of PNe that presumably descend from higher mass progenitor stars.

  6. Spectroscopic observations of low-lying gas clouds: sensitivity of detection by method of covariance matrix

    NASA Astrophysics Data System (ADS)

    Margolis, Jack S.; Liu, Karen Y.; Moynihan, Philip I.

    1999-01-01

    The sensitivity of spectroscopic detection of low-lying gas clouds by an arbitrary spectrometer may be determined by simulating the observation using a high spectral resolution radiative transfer code. The instrumental characteristics may be superimposed on the simulation and the accuracy of the retrieval of the desired parameters may be estimated by use of the covariance matrix.

  7. Photoelectric and Spectroscopic Observations Related to a Possible Optical Counterpart for Pulsar CP 1919+21.

    PubMed

    Lynds, R; Maran, S P; Trumbo, D E

    1968-07-01

    Spectroscopic observations of the two stars near the pulsar CP 1919+21 are not sufficiently conclusive to permit an identification of either object with the source of the radio pulses. However, our most extensive series of photometric observations of a region of sky near the radio source position, which region includes the brighter of the two stars, suggests an approximately sinusoidal variation. It is significant that the period of the variation is double the period of the radio pulsations. PMID:17756510

  8. Optical Spectroscopic Observations of Gamma-Ray Blazar Candidates. VI. Further Observations from TNG, WHT, OAN, SOAR, and Magellan Telescopes

    NASA Astrophysics Data System (ADS)

    Álvarez Crespo, N.; Massaro, F.; Milisavljevic, D.; Landoni, M.; Chavushyan, V.; Patiño-Álvarez, V.; Masetti, N.; Jiménez-Bailón, E.; Strader, J.; Chomiuk, L.; Katagiri, H.; Kagaya, M.; Cheung, C. C.; Paggi, A.; D'Abrusco, R.; Ricci, F.; La Franca, F.; Smith, Howard A.; Tosti, G.

    2016-04-01

    Blazars, one of the most extreme classes of active galaxies, constitute so far the largest known population of γ-ray sources, and their number is continuously growing in the Fermi catalogs. However, in the latest release of the Fermi catalog there is still a large fraction of sources that are classified as blazar candidates of uncertain type (BCUs) for which optical spectroscopic observations are necessary to confirm their nature and their associations. In addition, about one-third of the γ-ray point sources listed in the Third Fermi-LAT Source Catalog (3FGL) are still unassociated and lacking an assigned lower-energy counterpart. Since 2012 we have been carrying out an optical spectroscopic campaign to observe blazar candidates to confirm their nature. In this paper, the sixth of the series, we present optical spectroscopic observations for 30 γ-ray blazar candidates from different observing programs we carried out with the Telescopio Nazionale Galileo, William Herschel Telescope, Observatorio Astronómico Nacional, Southern Astrophysical Research Telescope, and Magellan Telescopes. We found that 21 out of 30 sources investigated are BL Lac objects, while the remaining targets are classified as flat-spectrum radio quasars showing the typical broad emission lines of normal quasi-stellar objects. We conclude that our selection of γ-ray blazar candidates based on their multifrequency properties continues to be a successful way to discover potential low-energy counterparts of the Fermi unidentified gamma-ray sources and to confirm the nature of BCUs.

  9. Massive Young Stellar Objects in the Galactic Center. 1; Spectroscopic Identification from Spitzer/IRS Observations

    NASA Technical Reports Server (NTRS)

    An, Deokkeun; Ramirez, Solange V.; Sellgren, Kris; Arendt, Richard G.; Boogert, A. C. Adwin; Robitaille, Thomas P.; Schultheis, Mathias; Cotera, Angela S.; Smith, Howard A.; Stolovy, Susan R.

    2011-01-01

    We present results from our spectroscopic study, using the Infrared Spectrograph (IRS) onboard the Spitzer Space Telescope, designed to identify massive young stellar objects (YSOs) in the Galactic Center (GC). Our sample of 107 YSO candidates was selected based on IRAC colors from the high spatial resolution, high sensitivity Spitzer/IRAC images in the Central Molecular Zone (CMZ), which spans the central approximately 300 pc region of the Milky Way Galaxy. We obtained IRS spectra over 5 micron to 35 micron using both high- and low-resolution IRS modules. We spectroscopically identify massive YSOs by the presence of a 15.4 micron shoulder on the absorption profile of 15 micron CO2 ice, suggestive of CO2 ice mixed with CH30H ice on grains. This 15.4 micron shoulder is clearly observed in 16 sources and possibly observed in an additional 19 sources. We show that 9 massive YSOs also reveal molecular gas-phase absorption from C02, C2H2, and/or HCN, which traces warm and dense gas in YSOs. Our results provide the first spectroscopic census of the massive YSO population in the GC. We fit YSO models to the observed spectral energy distributions and find YSO masses of 8 - 23 solar Mass, which generally agree with the masses derived from observed radio continuum emission. We find that about 50% of photometrically identified YSOs are confirmed with our spectroscopic study. This implies a preliminary star formation rate of approximately 0.07 solar mass/yr at the GC.

  10. MASSIVE YOUNG STELLAR OBJECTS IN THE GALACTIC CENTER. I. SPECTROSCOPIC IDENTIFICATION FROM SPITZER INFRARED SPECTROGRAPH OBSERVATIONS

    SciTech Connect

    An, Deokkeun; RamIrez, Solange V.; Boogert, A. C. Adwin; Sellgren, Kris; Arendt, Richard G.; Schultheis, Mathias; Cotera, Angela S.; Stolovy, Susan R.

    2011-08-01

    We present results from our spectroscopic study, using the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope, designed to identify massive young stellar objects (YSOs) in the Galactic center (GC). Our sample of 107 YSO candidates was selected based on Infrared Array Camera (IRAC) colors from the high spatial resolution, high sensitivity Spitzer/IRAC images in the Central Molecular Zone, which spans the central {approx}300 pc region of the Milky Way. We obtained IRS spectra over 5-35 {mu}m using both high- and low-resolution IRS modules. We spectroscopically identify massive YSOs by the presence of a 15.4 {mu}m shoulder on the absorption profile of 15 {mu}m CO{sub 2} ice, suggestive of CO{sub 2} ice mixed with CH{sub 3}OH ice on grains. This 15.4 {mu}m shoulder is clearly observed in 16 sources and possibly observed in an additional 19 sources. We show that nine massive YSOs also reveal molecular gas-phase absorption from CO{sub 2}, C{sub 2}H{sub 2}, and/or HCN, which traces warm and dense gas in YSOs. Our results provide the first spectroscopic census of the massive YSO population in the GC. We fit YSO models to the observed spectral energy distributions and find YSO masses of 8-23 M{sub sun}, which generally agree with the masses derived from observed radio continuum emission. We find that about 50% of photometrically identified YSOs are confirmed with our spectroscopic study. This implies a preliminary star formation rate of {approx}0.07 M{sub sun} yr{sup -1} at the GC.

  11. The source regions of the solar wind revealed by UV/EUV spectroscopic observations

    NASA Astrophysics Data System (ADS)

    Xia, L.

    2012-06-01

    The heating of the solar corona and the origin and acceleration of the solar wind are among the important unsolved problems of space plasma and solar physics. During the SOHO era, coronal holes as source regions of the fast solar wind have been investigated by using UV/EUV spectroscopic data observed with high-resolution spectrometers. At the base of the coronal hole, a detailed picture concerning the origin of the fast solar wind was first obtained by SUMER observations. For example, the Dopplergram deduced from the line profile of Ne VIII and other transition-region lines showed strong evidence that the wind originates in the chromospheric network and starts flowing out of the corona in magnetic funnels. Solar wind mass is suggested to be supplied through supergranule-scale magnetoconvection in the chromosphere and transition region. However, the spectral lines used in these studies are mainly obtained in the transition region and the behaviours of the nascent solar wind at higher temperatures have not yet been understood. Recent spectroscopic and imaging observations with instruments on Hinode and SDO provide further information about the coronal holes seen in EUV lines formed in the solar corona. Some interesting results, e.g., ubiquitous episodic outflow (jets) and enhanced emission in the blue wing of coronal line profiles, are found from the new observations. The purpose of this presentation is to review recent research progress on solar-wind source regions revealed by UV/EUV spectroscopic and imaging observations. Such observational studies and further interpretations of the data may provide crucial constraints and implications for future studies on both observations and theoretical models concerning coronal heating and acceleration of the nascent solar wind.

  12. Spectroscopic and photometric observations of the M31 nova candidate PTF12ahb

    NASA Astrophysics Data System (ADS)

    Shafter, A. W.; Darnley, M. J.; Bode, M. F.; Ciardullo, R.; Hornoch, K.; Cao, Y.; Kasliwal, M. M.

    2012-02-01

    We report spectroscopic and photometric observations of the M31 nova candidate PTF12ahb (tentatively designated M31N 2012-02a) discovered by Cao et al. (ATel #3905) on 2012 Feb 01.117 UT at R = 19.1. At our request, a spectrum (410-900 nm) was obtained by J. Caldwell on 2012 Feb. 03.08 UT with the 9.2m Hobby-Eberly Telescope (+ Marcario Low-Resolution Spectrograph). The spectrum reveals narrow (marginally resolved) Balmer and Fe II emission lines (FWHM Hα ~ 600 km/s; EW Hα ~ -9.0 nm) superimposed on a slightly blue continuum.

  13. Spectroscopic observations of the counterpart of IGR J00291+5934

    NASA Astrophysics Data System (ADS)

    Roelofs, G.; Jonker, P. G.; Steeghs, D.; Torres, M.; Nelemans, G.

    2004-12-01

    Spectroscopic observations of the optical counterpart of the millisecond X-ray pulsar IGR J00291+5934 (Atel #352, 353) reported in an Atel by Fox & Kulkarni were obtained (Dec 5 00:29-01:15 UT) with the ISIS spectrograph mounted on the 4.2m William Herschel Telescope on La Palma. Weather conditions were not optimal with a seeing of ~2" and thin clouds. The spectra show weak evidence for broad emission line features near the HeII line at 4686 Angstrom and near the Halpha line at 6563 Angstrom.

  14. Clinical Utility of an Observation and Response Chart With Human Factors Design Characteristics and a Track and Trigger System: Study Protocol for a Two-Phase Multisite Multiple-Methods Design

    PubMed Central

    McKinley, Sharon; Perry, Lin; Duffield, Christine; Iedema, Rick; Gallagher, Robyn; Fry, Margaret; Roche, Michael; Allen, Emily

    2014-01-01

    Background Clinical deterioration of adult patients in acute medical-surgical wards continues to occur, despite a range of systems and processes designed to minimize this risk. In Australia, a standardized template for adult observation charts using human factors design principles and decision-support characteristics was developed to improve the detection of and response to abnormal vital signs. Objective To describe the study protocol for the clinical testing of these observation and response charts (ORCs). Methods We propose a two-phase multisite multiple-methods design to test the initial clinical utility of the charts in 10 hospitals of differing types and sizes across state jurisdictions in Australia. Data collection in the first phase includes user surveys, observations and field notes by project officers, handover de-briefs (short interviews with small groups of staff), and an audit of ORC documentation completion compared to the site’s existing observation chart. For the second phase, data will be collected using a retrospective audit of observation documentation from the previous hospital observation chart, prospective audit of observation documentation following implementation of the selected ORC, user focus groups, observational field notes, and patient outcome data from routinely collected organizational data sources. Results Site selection and preparation, project officer training, chart selection and implementation, participant recruitment, and data collection has been completed and the analysis of these results are in progress. Conclusions This detailed description of these study methods and data collection approaches will enable a comprehensive assessment of the clinical utility of these newly developed track and trigger charts and will be useful for clinicians and researchers when planning and implementing similar studies. Potential methodological limitations are also noted. PMID:25116446

  15. Low X-Ray Luminosity Galaxy Clusters: Main Goals, Sample Selection, Photometric and Spectroscopic Observations

    NASA Astrophysics Data System (ADS)

    Nilo Castellón, José Luis; Alonso, M. Victoria; García Lambas, Diego; Valotto, Carlos; O’ Mill, Ana Laura; Cuevas, Héctor; Carrasco, Eleazar R.; Ramírez, Amelia; Astudillo, José M.; Ramos, Felipe; Jaque Arancibia, Marcelo; Ulloa, Natalie; Órdenes, Yasna

    2016-06-01

    We present our study of 19 low X-ray luminosity galaxy clusters (L{}X ∼ 0.5–45 × 1043 erg s‑1), selected from the ROSAT Position Sensitive Proportional Counters Pointed Observations and the revised version of Mullis et al. in the redshift range of 0.16–0.7. This is the introductory paper of a series presenting the sample selection, photometric and spectroscopic observations, and data reduction. Photometric data in different passbands were taken for eight galaxy clusters at Las Campanas Observatory; three clusters at Cerro Tololo Interamerican Observatory; and eight clusters at the Gemini Observatory. Spectroscopic data were collected for only four galaxy clusters using Gemini telescopes. Using the photometry, the galaxies were defined based on the star-galaxy separation taking into account photometric parameters. For each galaxy cluster, the catalogs contain the point-spread function and aperture magnitudes of galaxies within the 90% completeness limit. They are used together with structural parameters to study the galaxy morphology and to estimate photometric redshifts. With the spectroscopy, the derived galaxy velocity dispersion of our clusters ranged from 507 km s‑1 for [VMF98]022 to 775 km s‑1 for [VMF98]097 with signs of substructure. Cluster membership has been extensively discussed taking into account spectroscopic and photometric redshift estimates. In this sense, members are the galaxies within a projected radius of 0.75 Mpc from the X-ray emission peak and with clustercentric velocities smaller than the cluster velocity dispersion or 6000 km s‑1, respectively. These results will be used in forthcoming papers to study, among the main topics, the red cluster sequence, blue cloud and green populations, the galaxy luminosity function, and cluster dynamics.

  16. Near-Infrared Spectroscopic Study of AA Tau: Water and OH Observations

    NASA Astrophysics Data System (ADS)

    Brown, Logan Ryan; Gibb, Erika

    2014-06-01

    To understand our own solar origins, we must investigate the composition of the protoplanetary disk from which the solar system formed. To infer this, we study analogs to the early solar system called T Tauri stars. These objects are low-mass, pre-main sequence stars surrounded by circumstellar disks of material from which planets are believed to form. We present high-resolution (λ/Δλ˜25,000), near-infrared spectroscopic data from the T Tauri star AA Tau using NIRSPEC at the Keck II telescope, located on Mauna Kea, HI, taken in 2009 and 2010. AA Tau has a close to edge-on geometry, with an inclination of 70° ± 10° (Donati et al. 2010). Objects must have a nearly edge-on inclination for the disk to be sampled via absorption line spectroscopy. We observed strong absorption lines of both water and OH to which a spectroscopic model was fit in order for us to determine column density and rotational temperature. These near-infrared observations complement the work being done with ALMA, allowing us to probe the inner most disk regions and the chemistry contained within while ALMA primarily samples and is most sensitive to the outer disk.

  17. Chemical Nature Of Titan’s Organic Aerosols Constrained from Spectroscopic and Mass Spectrometric Observations

    NASA Astrophysics Data System (ADS)

    Imanaka, Hiroshi; Cruikshank, D. P.

    2012-10-01

    The Cassini-Huygens observations greately extend our knowledge about Titan’s organic aerosols. The Cassini INMS and CAPS observations clearly demonstrate the formation of large organic molecules in the ionosphere [1, 2]. The VIMS and CIRS instruments have revealed spectral features of the haze covering the mid-IR and far-IR wavelengths [3, 4, 5, 6]. This study attempts to speculate the possible chemical nature of Titan’s aerosols by comparing the currently available observations with our laboratory study. We have conducted a series of cold plasma experiment to investigate the mass spectrometric and spectroscopic properties of laboratory aerosol analogs [7, 8]. Titan tholins and C2H2 plasma polymer are generated with cold plasma irradiations of N2/CH4 and C2H2, respectively. Laser desorption mass spectrum of the C2H2 plasma polymer shows a reasonable match with the CAPS positive ion mass spectrum. Furthermore, spectroscopic features of the the C2H2 plasma polymer in mid-IR and far-IR wavelegths qualitatively show reasonable match with the VIMS and CIRS observations. These results support that the C2H2 plasma polymer is a good candidate material for Titan’s aerosol particles at the altitudes sampled by the observations. We acknowledge funding supports from the NASA Cassini Data Analysis Program, NNX10AF08G, and from the NASA Exobiology Program, NNX09AM95G, and the Cassini Project. [1] Waite et al. (2007) Science 316, 870-875. [2] Crary et al. (2009) Planet. Space Sci. 57, 1847-1856. [3] Bellucci et al. (2009) Icarus 201, 198-216. [4] Anderson and Samuelson (2011) Icarus 212, 762-778. [5] Vinatier et al. (2010) Icarus 210, 852-866. [6] Vinatier et al. (2012) Icarus 219, 5-12. [7] Imanaka et al. (2004) Icarus 168, 344-366. [8] Imanaka et al. (2012) Icarus 218, 247-261.

  18. Direct Spectroscopic Observation of a Shallow Hydrogenlike Donor State in Insulating SrTiO3

    NASA Astrophysics Data System (ADS)

    Salman, Z.; Prokscha, T.; Amato, A.; Morenzoni, E.; Scheuermann, R.; Sedlak, K.; Suter, A.

    2014-10-01

    We present a direct spectroscopic observation of a shallow hydrogenlike muonium state in SrTiO3 which confirms the theoretical prediction that interstitial hydrogen may act as a shallow donor in this material. The formation of this muonium state is temperature dependent and appears below ˜70 K. From the temperature dependence we estimate an activation energy of ˜50 meV in the bulk and ˜23 meV near the free surface. The field and directional dependence of the muonium precession frequencies further supports the shallow impurity state with a rare example of a fully anisotropic hyperfine tensor. From these measurements we determine the strength of the hyperfine interaction and propose that the muon occupies an interstitial site near the face of the oxygen octahedron in SrTiO3. The observed shallow donor state provides new insight for tailoring the electronic and optical properties of SrTiO3-based oxide interface systems.

  19. High-Resolution Spectroscopic Database for the NASA Earth Observing System Program

    NASA Technical Reports Server (NTRS)

    Rothman, Laurence S.; Starr, David (Technical Monitor)

    2002-01-01

    The purpose of this project is to develop and enhance the HITRAN molecular spectroscopic database and associated software to support the observational programs of the Earth Observing System (EOS). In particular, the focus is on the EOS projects: the Atmospheric Infrared Sounder (AIRS), the High-Resolution Dynamics Limb Sounder (HIRDLS), Measurements of Pollution in the Troposphere (MOPITT), the Tropospheric Emission Spectrometer (TES), and the Stratospheric Aerosol and Gas Experiment (SAGE III). The data requirements of these programs in terms of spectroscopy are varied, but usually call for additional spectral parameters or improvements to existing molecular bands. In addition, cross-section data for heavier molecular species must be expanded and made amenable to modeling in remote sensing. The effort in the project also includes developing software and distribution to make access, manipulation, and use of HITRAN functional to the EOS program.

  20. Optical spectroscopic observations of γ-ray blazar candidates. I. Preliminary results

    SciTech Connect

    Paggi, A.; Milisavljevic, D.; D'Abrusco, R.; Smith, H. A.; Margutti, R.; Martínez-Galarza, J. R.; Landoni, M.; Grindlay, J. E.; Masetti, N.; Giroletti, M.; Jiménez-Bailón, E.; Otí-Floranes, H.; Chavushyan, V.; Massaro, F.; Funk, S.; Tosti, G.

    2014-05-01

    A significant fraction (∼30%) of the γ-ray sources listed in the second Fermi/LAT (2FGL) catalog is still of unknown origin, being not yet associated with counterparts at lower energies. Using the available information at lower energies and optical spectroscopy on the selected counterparts of these γ-ray objects, we can pinpoint their exact nature. Here, we present a pilot project pointing to assess the effectiveness of the several classification methods developed to select γ-ray blazar candidates. To this end, we report optical spectroscopic observations of a sample of five γ-ray blazar candidates selected on the basis of their infrared Wide-field Infrared Survey Explorer (WISE) colors or of their low-frequency radio properties. Blazars come in two main classes, BL Lac objects and FSRQs, showing similar optical spectra except for the stronger emission lines of the latter. For three of our sources, the almost featureless optical spectra obtained confirm their BL Lac nature, while for the source WISEJ022051.24+250927.6 we observe emission lines with equivalent width EW ∼ 31 Å, identifying it as a FSRQ with z = 0.48. The source WISEJ064459.38+603131.7, although not featuring a clear radio counterpart, shows a blazar-like spectrum with weak emission lines with EW ∼ 7 Å, yielding a redshift estimate of z = 0.36. In addition, we report optical spectroscopic observations of four WISE sources associated with known γ-ray blazars without a firm classification or redshift estimate. For the latter sources, we confirm a BL Lac classification, with a tentative redshift estimate for the source WISEJ100800.81+062121.2 of z = 0.65.

  1. Submillimetric spectroscopic observations of volatiles in comet C/2004 Q2 (Machholz)

    NASA Astrophysics Data System (ADS)

    de Val-Borro, M.; Hartogh, P.; Jarchow, C.; Rengel, M.; Villanueva, G. L.; Küppers, M.; Biver, N.; Bockelée-Morvan, D.; Crovisier, J.

    2012-09-01

    Context. Submillimeter spectroscopic observations of comets provide an important tool for understanding their chemical composition and enable a taxonomic classification. Aims: We aim to determine the production rates of several parent- and product volatiles and the 12C/13C isotopic carbon ratio in the long-period comet C/2004 Q2 (Machholz), which is likely to originate from the Oort Cloud. Methods: The line emission from several molecules in the coma was measured with high signal-to-noise ratio in January 2005 at heliocentric distance of 1.2 AU by means of high-resolution spectroscopic observations using the Submillimeter Telescope (SMT) at the Arizona Radio Observatory (ARO). Results: We have obtained production rates of several volatiles (CH3OH, HCN, H13CN, HNC, H2CO, CO, and CS) by comparing the observed and simulated line-integrated intensities. We calculated the synthetic profiles using a radiative transfer code that includes collisions between neutrals and electrons, and the effects of radiative pumping of the fundamental vibrational levels by solar infrared radiation. Furthermore, multiline observations of the CH3OH J = 7-6 series allow us to estimate the rotational temperature using the rotation diagram technique. We find that the CH3OH population distribution of the levels sampled by these lines can be described by a rotational temperature of 40 ± 3 K. Derived mixing ratios relative to hydrogen cyanide are CO/CH3OH/H2CO/CS/HNC/H13CN/HCN = 30.9/24.6/4.8/0.57/0.031/0.013/1 assuming a pointing offset of 8'' due to the uncertain ephemeris at the time of the observations and the telescope pointing error. Conclusions: The measured relative molecular abundances in C/2004 Q2 (Machholz) are between low- to typical values of those obtained in Oort Cloud comets, suggesting that it has visited the inner solar system previously and undergone thermal processing. The HNC/HCN abundance ratio of ~3.1% is comparable to that found in other comets, accounting for the

  2. Implementation of Multiple Spectroscopic Techniques to Simultaneously Observe Native and Mutated Protein Unfolding

    NASA Astrophysics Data System (ADS)

    Cull, Brennan; Ben, Kelty; Link, Justin

    A protein's natural, correctly folded structure can determine the protein's ability to carry out its function. If the unfolding process of proteins can be observed, then the relative stability can be better understood between native and mutated proteins. A global picture of the unfolding process may be completed through the studies of strategically mutated proteins using tryptophan as a probe. Horse heart cytochrome c, a thoroughly studied, model protein was used in our investigation to explore this idea. Various spectroscopic techniques such as circular dichroism (CD), absorbance, and fluorescence were simultaneously applied while slowly unfolding our protein by increasing the concentration of a chemical denaturant, guanidine hydrochloride. This provided us information about the thermodynamic properties of the protein and several mutants which can then be interpreted to gain relative stability information among mutations. Efforts to utilize these techniques on native and mutated proteins in comparison to current scientific unfolding theories will be presented in this session.

  3. Vibrational Spectroscopic Observation of Atomic-Scale Local Surface Sites Using Site-Selective Signal Enhancement.

    PubMed

    Hu, Jian; Hoshi, Nagahiro; Uosaki, Kohei; Ikeda, Katsuyoshi

    2015-12-01

    Molecule-substrate interactions are sensitively affected by atomic-scale surface structures. Unique activity in heterogeneous catalysts or electrocatalysts is often related with local surface sites with specific structures. We demonstrate that adsorption geometry of a model molecule with an isocyanide anchor is drastically varied among one-fold atop, two-fold bridge, and three-fold hollow configurations with increasing the size of atomic-scale local surface sites of Pd islands on an Au(111) model surface. The vibrational spectroscopic observation of such local information is realized by site-selective and self-assembled formation of hotspots, where Raman scattering intensity is significantly enhanced via excitation of localized surface plasmons. PMID:26551000

  4. Photometric Observations of the η Carinae 2009.0 Spectroscopic Event

    NASA Astrophysics Data System (ADS)

    Landes, H.; Fitzgerald, M.

    2010-09-01

    We have observed η Carinae over 34 nights between 2009 January 4 and 2009 March 27 covering the estimated timeframe for a predicted spectroscopic event related to a suspected binary system concealed within the homunculus nebula. A photometric minimum feature was confirmed to be periodic and comparison to a previous event indicated that the period to within our error was 2022.6+/-1.0d. Using the E-region standard star system, the apparent V magnitudes determined for the local comparison stars were HD 303308 8.14+/-0.02, HD 93205 7.77+/-0.03, and HD 93162 8.22+/-0.05. The latter star was found to be dimmer than previously reported.

  5. Submillimetric Spectroscopic Observations of Volatiles in Comet C-2004 Q2 (Machholz)

    NASA Technical Reports Server (NTRS)

    DeVal-Borro, M.; Hartogh, P.; Jarchow, C.; Rengel, M.; Villanueva, G. L.; Kueppers, M.; Biver, N.; Bockelee-Morvan, D.; Crovisier, J.

    2012-01-01

    Submillimeter spectroscopic observations of comets provide an important tool for understanding their chemical composition and enable a taxonomic classification. Aims. We aim to determine the production rates of several parent- and product volatiles and the C-12/C-13 isotopic carbon ratio in the long-period comet C/2004 Q2 (Machholz), which is likely to originate from the Oort Cloud. Methods. The line emission from several molecules in the coma was measured with high signal-to-noise ratio in January 2005 at heliocentric distance of 1.2 AU by means of high-resolution spectroscopic observations using the Submillimeter Telescope (SMT) at the Arizona Radio Observatory (ARO). Results. We have obtained production rates of several volatiles (CH3OH, HCN, H(sup 13)CN, HNC, H2CO, CO, and CS) by comparing the observed and simulated line-integrated intensities. We calculated the synthetic profiles using a radiative transfer code that includes collisions between neutrals and electrons, and the effects of radiative pumping of the fundamental vibrational levels by solar infrared radiation. Furthermore, multiline observations of the CH3OH J = 7-6 series allow us to estimate the rotational temperature using the rotation diagram technique. We find that the CH3OH population distribution of the levels sampled by these lines can be described by a rotational temperature of 40 +/- 3 K. Derived mixing ratios relative to hydrogen cyanide are CO/CH3OH/H2CO/CS/HNC/HC-13N/HCN= 30.9/24.6/4.8/0.57/0.031/0.013/1 assuming a pointing offset of 8" due to the uncertain ephemeris at the time of the observations and the telescope pointing error. Conclusions. The measured relative molecular abundances in C/2004 Q2 (Machholz) are between low- to typical values of those obtained in Oort Cloud comets, suggesting that it has visited the inner solar system previously and undergone thermal processing. The HNC/HCN abundance ratio of approx 3.1% is comparable to that found in other comets, accounting for the

  6. High-dispersion infrared spectroscopic observations of comet 8P/Tuttle with VLT/CRIRES

    NASA Astrophysics Data System (ADS)

    Kobayashi, H.; Bockelée-Morvan, D.; Kawakita, H.; Dello Russo, N.; Jehin, E.; Manfroid, J.; Smette, A.; Hutsemékers, D.; Stüwe, J.; Weiler, M.; Arpigny, C.; Biver, N.; Cochran, A.; Crovisier, J.; Magain, P.; Sana, H.; Schulz, R.; Vervack, R. J.; Weaver, H.; Zucconi, J.-M.

    2010-01-01

    We report on the composition of the Halley-family comet (HFC) 8P/Tuttle investigated with high-dispersion near-infrared spectroscopic observations. The observations were carried out at the ESO VLT (Very Large Telescope) with the CRIRES instrument as part of a multi-wavelength observation campaign of 8P/Tuttle performed in late January and early February 2008. Radar observations suggested that 8P/Tuttle is a contact binary, and it was proposed that these components might be heterogeneous in chemistry. We determined mixing ratios of organic volatiles with respect to H2O and found that mixing ratios were consistent with previous near infrared spectroscopic observations obtained in late December 2007 and in late January 2008. It has been suggested that because 8P/Tuttle is a contact binary, it might be chemically heterogeneous. However, we find no evidence for chemical heterogeneity within the nucleus of 8P/Tuttle. We also compared the mixing ratios of organic molecules in 8P/Tuttle with those of both other HFCs and long period comets (LPCs) and found that HCN, C2H2, and C2H6 are depleted whereas CH4 and CH3OH have normal abundances. This may indicate that 8P/Tuttle was formed in a different region of the early solar nebula than other HFCs and LPCs. We estimated the conversion efficiency from C2H2 to C2H6 by hydrogen addition reactions on cold grains by employing the C2H6/(C2H6+C2H2) ratio. The C2H6/(C2H6+C2H2) ratio in 8P/Tuttle is consistent with the ratios found in other HFCs and LPCs within the error bars. We also discuss the source of C2 and CN based on our observations and conclude that the abundances of C2H2 and C2H6 are insufficient to explain the C2 abundances in comet 8P/Tuttle and that the abundance of HCN is insufficient to explain the CN abundances in the comet, so at least one additional parent is needed for each species, as pointed out in previous study. Based on observations collected at the European Southern Observatory, Paranal, Chile (ESO Prog. 080.C

  7. Revised spectroscopic parameters of SH(+) from ALMA and IRAM 30m observations.

    PubMed

    Müller, Holger S P; Goicoechea, Javier R; Cernicharo, José; Agúndez, Marcelino; Pety, Jérôme; Cuadrado, Sara; Gerin, Maryvonne; Dumas, Gaëlle; Chapillon, Edwige

    2014-09-19

    Hydrides represent the first steps of interstellar chemistry. Sulfanylium (SH(+)), in particular, is a key tracer of energetic processes. We used ALMA and the IRAM 30 m telescope to search for the lowest frequency rotational lines of SH(+) toward the Orion Bar, the prototypical photo-dissociation region illuminated by a strong UV radiation field. On the basis of previous Herschel/HIFI observations of SH(+), we expected to detect emission of the two SH(+) hyperfine structure (HFS) components of the NJ = 10-01 fine structure (FS) component near 346 GHz. While we did not observe any lines at the frequencies predicted from laboratory data, we detected two emission lines, each ~15 MHz above the SH(+) predictions and with relative intensities and HFS splitting expected for SH(+). The rest frequencies of the two newly detected lines are more compatible with the remainder of the SH(+) laboratory data than the single line measured in the laboratory near 346 GHz and previously attributed to SH(+). Therefore, we assign these new features to the two SH(+) HFS components of the NJ = 10-01 FS component and re-determine its spectroscopic parameters, which will be useful for future observations of SH(+), in particular if its lowest frequency FS components are studied. Our observations demonstrate the suitability of these lines for SH(+) searches at frequencies easily accessible from the ground. PMID:26525172

  8. Solar Flares Observed with the Ramaty High Energy Solar Spectroscopic Imager (RHESSI)

    NASA Technical Reports Server (NTRS)

    Holman, Gordon D.

    2004-01-01

    Solar flares are impressive examples of explosive energy release in unconfined, magnetized plasma. It is generally believed that the flare energy is derived from the coronal magnetic field. However, we have not been able to establish the specific energy release mechanism(s) or the relative partitioning of the released energy between heating, particle acceleration (electrons and ions), and mass motions. NASA's RHESSI Mission was designed to study the acceleration and evolution of electrons and ions in flares by observing the X-ray and gamma-ray emissions these energetic particles produce. This is accomplished through the combination of high-resolution spectroscopy and spectroscopic imaging, including the first images of flares in gamma rays. RHESSI has observed over 12,000 solar flares since its launch on February 5, 2002. I will demonstrate how we use the RHESSI spectra to deduce physical properties of accelerated electrons and hot plasma in flares. Using images to estimate volumes, w e typically find that the total energy in accelerated electrons is comparable to that in the thermal plasma. I will also present flare observations that provide strong support for the presence of magnetic reconnection in a large-scale, vertical current sheet in the solar corona. RHESSI observations such as these are allowing us to probe more deeply into the physics of solar flares.

  9. IMAGING AND SPECTROSCOPIC OBSERVATIONS OF MAGNETIC RECONNECTION AND CHROMOSPHERIC EVAPORATION IN A SOLAR FLARE

    SciTech Connect

    Tian, Hui; Reeves, Katharine K.; Raymond, John C.; Chen, Bin; Murphy, Nicholas A.; Li, Gang; Guo, Fan; Liu, Wei

    2014-12-20

    Magnetic reconnection is believed to be the dominant energy release mechanism in solar flares. The standard flare model predicts both downward and upward outflow plasmas with speeds close to the coronal Alfvén speed. Yet, spectroscopic observations of such outflows, especially the downflows, are extremely rare. With observations of the newly launched Interface Region Imaging Spectrograph (IRIS), we report the detection of a greatly redshifted (∼125 km s{sup –1} along the line of sight) Fe XXI 1354.08 Å emission line with a ∼100 km s{sup –1} nonthermal width at the reconnection site of a flare. The redshifted Fe XXI feature coincides spatially with the loop-top X-ray source observed by RHESSI. We interpret this large redshift as the signature of downward-moving reconnection outflow/hot retracting loops. Imaging observations from both IRIS and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory also reveal the eruption and reconnection processes. Fast downward-propagating blobs along these loops are also found from cool emission lines (e.g., Si IV, O IV, C II, Mg II) and images of AIA and IRIS. Furthermore, the entire Fe XXI line is blueshifted by ∼260 km s{sup –1} at the loop footpoints, where the cool lines mentioned above all exhibit obvious redshift, a result that is consistent with the scenario of chromospheric evaporation induced by downward-propagating nonthermal electrons from the reconnection site.

  10. High-Resolution Spectroscopic Database for the NASA Earth Observing System Program

    NASA Technical Reports Server (NTRS)

    Rothman, Laurence

    2003-01-01

    The purpose of this project is to develop and enhance the HITRAN molecular spectroscopic database and associated software to support the observational programs of the Earth Observing System (EOS). In particular, the focus is on the EOS projects: the Atmospheric Infrared Sounder (AIRS), the High-Resolution Dynamics Limb Sounder (HIRDLS), Measurements of Pollution in the Troposphere (MOPITT), the Tropospheric Emission Spectrometer (TES), and the Stratospheric Aerosol and Gas Experiment (SAGE III). The HITRAN program is also involved in the Ozone Monitoring Experiment (OMI). The data requirements of these programs in terms of spectroscopy are varied with respect to constituents being observed, required remote-sensing parameters, and spectral coverage. A general requisite is for additional spectral parameters and improvements to existing molecular bands sufficient for the simulation of the observations leading to retrieval of the atmospheric state. In addition, cross-section data for heavier molecular species must be expanded and made amenable to modeling in remote sensing. The effort in the project also includes developing software and distribution to make access, manipulation, and use of HITRAN functional to the EOS program.

  11. High-Resolution Spectroscopic Database for the NASA Earth Observing System Program

    NASA Technical Reports Server (NTRS)

    Rothman, Laurence S.

    2004-01-01

    The purpose of this project is to develop and enhance the HITRAN molecular spectroscopic database and associated - software to support the observational programs of the Earth observing System (EOS). In particular, the focus is on the EOS projects: the Atmospheric Infrared Sounder (AIRS), the High-Resolution Dynamics Limb Sounder (HIRDLS), Measurements of Pollution in the Troposphere (MOPITT), the Tropospheric Emission Spectrometer (TES), and the Stratospheric Aerosol and Gas Experiment (SAGE III). The HITRAN program is also involved in the Ozone Monitoring Experiment (OMI). The data requirements of these programs in terms of spectroscopy are varied with respect to constituents being observed, required remote-sensing parameters, and spectral coverage. A general requisite is for additional spectral parameters and improvements to existing molecular bands sufficient for the simulation of the observations leading to retrieval of the atmospheric state. In addition cross-section data for heavier molecular species must be expanded and made amenable to modeling in remote sensing. The effort in the project also includes developing software and distribution to make access, manipulation, and use HITRAN functional to the EOS program.

  12. High Resolution Spectroscopic Database for the NASA Earth Observing System Program

    NASA Technical Reports Server (NTRS)

    Rothman, Laurence

    2004-01-01

    The purpose of this project has been to develop and enhance the HITRAN molecular spectroscopic database and associated software to support the observational programs of the Earth Observing System (EOS). Emphasis has been on the EOS projects: the Atmospheric Infrared Sounder (AIRS), the High-Resolution Dynamics Limb Sounder (HIRDLS), Measurements of Pollution in the Troposphere (MOPITT), the Tropospheric Emission Spectrometer (TES), and the Stratospheric Aerosol and Gas Experiment (SAGE III). The HITRAN program is also involved in the Ozone Monitoring Experiment (OMI). The data requirements of these programs in terms of spectroscopy are varied with respect to constituents being observed, required remote-sensing parameters, and spectral coverage. A general requisite is for additional spectral parameters and improvements to existing molecular bands sufficient for the simulation of the observations leading to retrieval of the atmospheric state. In addition, cross-section data for heavier molecular species must be expanded and made amenable to modeling in remote sensing. The effort in the project also includes developing software and distribution to make access, manipulation, and use of HITRAN functional to the EOS program.

  13. Identifying the Young Low-mass Stars within 25 pc. I. Spectroscopic Observations

    NASA Astrophysics Data System (ADS)

    Shkolnik, Evgenya; Liu, Michael C.; Reid, I. Neill

    2009-07-01

    We have completed a high-resolution (R ≈ 60,000) optical spectroscopic survey of 185 nearby M dwarfs identified using ROSAT data to select active, young objects with fractional X-ray luminosities comparable to or greater than Pleiades members. Our targets are drawn from the NStars 20 pc census and the Moving-M sample with distances determined from parallaxes or spectrophotometric relations. We limited our sample to 25 pc from the Sun, prior to correcting for pre-main-sequence overluminosity or binarity. Nearly half of the resulting M dwarfs are not present in the Gliese catalog and have no previously published spectral types. We identified 30 spectroscopic binaries (SBs) from the sample, which have strong X-ray emission due to tidal spin-up rather than youth. This is equivalent to a 16% SB fraction, with at most a handful of undiscovered SBs. We estimate upper limits on the age of the remaining M dwarfs using spectroscopic youth indicators such as surface gravity-sensitive indices (CaH and K I). We find that for a sample of field stars with no metallicity measurements, a single CaH gravity index may not be sufficient, as higher metallicities mimic lower gravity. This is demonstrated in a subsample of metal-rich radial velocity (RV) standards, which appear to have low surface gravity as measured by the CaH index, yet show no other evidence of youth. We also use additional youth diagnostics such as lithium absorption and strong Hα emission to set more stringent age limits. Eleven M dwarfs with no Hα emission or absorption are likely old (>400 Myr) and were caught during an X-ray flare. We estimate that our final sample of the 144 youngest and nearest low-mass objects in the field is less than 300 Myr old, with 30% of them being younger than 150 Myr and four very young (lap10 Myr), representing a generally untapped and well-characterized resource of M dwarfs for intensive planet and disk searches. Based on observations collected at the W. M. Keck Observatory and

  14. Possibility of Detecting the H2O Snowline in Protoplanetary Disks Using Spectroscopic Observations

    NASA Astrophysics Data System (ADS)

    Notsu, Shota; Nomura, Hideko; Ishimoto, Daiki; Walsh, Catherine; Honda, Mitsuhiko; Millar, Thomas J.

    2015-08-01

    Inside the H2O snowline in protoplanetary disks, H2O evaporates from grain surfaces into the gas. On the other hand, it is frozen out on the grain surface in the cold region beyond the H2O snowline. The H2O snowline is thought to divide the regions of rocky planet and gas giant planet formation. Observationally measuring the position of the H2O snowline in protoplanetary disks in exoplanetary systems will constrain modern theories of planet formation. In disks around solar-mass T-tauri stars, the H2O snowline is thought to exist at a few AU from the central star. Therefore, it is difficult to detect the H2O snowline of exoplanetary systems by direct imaging, since the spatial resolution of existing telescopes is insufficient. In this work, we propose a method of detecting the H2O snowline directly by analyzing the velocity profiles of H2O line spectra which can be obtained by high dispersion spectroscopic observations in the near future.First, we use self-consistent physical models of protoplanetary disks (e.g., Nomura & Millar 2005, Nomura et al. 2007, Walsh et al. 2010, 2012) to investigate the abundance distribution of H2O gas and the position of the snowline. We confirm that the abundance of H2O gas is high not only inside the H2O snowline near the equatorial plane but also in the hot surface layer of the outer disk. Second, we calculate the emergent intensity of H2O emission lines from protoplanetary disks that are assumed to rotate with Keplerian velocity profiles. We can find information on the H2O snowline through investigating the profiles of emission lines that have small Einstein A coefficients and large excitation energies. The wavelengths of the useful H2O emission lines range from mid-infrared to sub-millimeter wavelengths. These lines will be observable with future high dispersion spectroscopic observations (e.g., ALMA, TMT).

  15. Generation and evolution of impact-induced vapor clouds: Spectroscopic observations and hydrodynamic calculations

    NASA Astrophysics Data System (ADS)

    Sugita, Seiji

    1999-11-01

    behind the vaporization phenomena during hypervelocity impacts. I developed a new spectroscopic technique to observe thermodynamical quantities of highly transient impact vapor clouds. Finally, I returned to the problem of the interaction between impact-induced vapor clouds and an atmosphere with the newly developed spectroscopic technique. Extensive comparison was made between the experimental results and theoretical calculations in order to find processes overlooked in previous theoretical considerations.

  16. Spectroscopic observations and modelling of impulsive Alfvén waves along a polar coronal jet

    NASA Astrophysics Data System (ADS)

    Jelínek, P.; Srivastava, A. K.; Murawski, K.; Kayshap, P.; Dwivedi, B. N.

    2015-09-01

    Context. The magnetic reconnection in the solar corona results in impulsively generated Alfvén waves, which drive a polar jet. Aims: Using the Hinode/EIS 2'' spectroscopic observations, we study the intensity, velocity, and full width at half maximum (FWHM) variations of the strongest Fe XII 195.12 Å line along the jet to find the signature of Alfvén waves. We numerically simulate the impulsively generated Alfvén waves within the vertical Harris current sheet, forming the jet plasma flows, and mimicking their observational signatures. Methods: Using the FLASH code and an atmospheric model with an embedded, weakly expanding magnetic field configuration within a vertical Harris current sheet, we solve the 2.5-dimensional (2.5D) ideal magnetohydrodynamic (MHD) equations to study the evolution of Alfvén waves and vertical flows forming the plasma jet. Results: At a height of ~5 Mm from the base of the jet, the red-shifted velocity component of Fe XII 195.12 Å line attains its maximum (5 km s-1), which converts into a blue-shifted velocity component between the altitude of 5-10 Mm. The spectral intensity continuously increases up to 10 Mm, while the FWHM still exhibits low values with an almost constant trend. This indicates that the reconnection point within the jet's magnetic field topology lies in the corona 5-10 Mm from its footpoint anchored in the Sun's surface. Beyond this height, the FWHM shows a growing trend. This may be the signature of Alfvén waves that impulsively evolve, due to reconnection, and propagate along the jet. From our numerical data, we evaluate space- and time- averaged Alfvén waves velocity amplitudes at different heights in the jet's current sheet, which contribute to the non-thermal motions and spectral line broadening. The synthetic width of Fe XII 195.12 Å line exhibits a similar trend of increment as in the observational data, possibly proving the existence of Alfvén waves, impulsively generated by reconnection, that propagate

  17. Visible Spectroscopic Observation Of Asteroid 162173 (1999ju3) With The Gemini-s Telescope

    NASA Astrophysics Data System (ADS)

    Sugita, Seiji; Kuroda, D.; Kameda, S.; Hasegawa, S.; Kamata, S.; Abe, M.; Ishiguro, M.; Takato, N.; Yoshikawa, M.

    2012-10-01

    Asteroid 162173 (1999JU3; hereafter JU3) is the target of the Hayabusa-2 mission. Its visible reflectance spectra have been observed a few times [1,2], and obtained spectra exhibit a wide variety of spectral patterns ranging from a spectra with absorption in the UV region (May 1999) to a flat spectrum with a faint broad absorption centered around 0.6 microns (September 2007) and that with UV absorption and strong broad absorption centered around 0.7 micron (July 2007). The apparent large spectral variation may be due to variegation on the asteroid surface. Such variegation would make a large influence on remote sensing strategy for Hayabusa-2 before its sampling operations. In order to better constraint the spectral properties of JU3, we conducted visible spectroscopic observations at the GEMINI-South observatory 8.1-m telescope with the GMOS instrument. We could obtain three different sets of data in June and July 2012. Although the JU3 rotation phases of two of the observation are close to each other, the other is about 120 degrees away from the two. Our preliminary analyses indicate that these three spectra are slightly reddish but generally flat across the observed wavelength range (0.47 - 0.89 microns). The observed flat spectra are most similar to the spectrum obtained in September 2007, which probably has the highest signal-to-noise ratio among the previous three spectra. This result suggests that material with a flat spectrum probably covers a dominant proportion of the JU3 surface and that the other two types of previously obtained spectra may not cover a very large fraction of the JU3 surface. [1] Binzel, R. P. et al. (2001) Icarus, 151, 139-149; [2] Vilas, F. (2008) AJ, 135, 1101-1105.

  18. Revised spectroscopic parameters of SH+ from ALMA and IRAM 30 m observations

    NASA Astrophysics Data System (ADS)

    Müller, Holger S. P.; Goicoechea, Javier R.; Cernicharo, José; Agúndez, Marcelino; Pety, Jérôme; Cuadrado, Sara; Gerin, Maryvonne; Dumas, Gaëlle; Chapillon, Edwige

    2014-09-01

    Hydrides represent the first steps of interstellar chemistry. Sulfanylium (SH+), in particular, is a key tracer of energetic processes. We used ALMA and the IRAM 30 m telescope to search for the lowest frequency rotational lines of SH+ toward the Orion Bar, the prototypical photo-dissociation region illuminated by a strong UV radiation field. On the basis of previous Herschel/HIFI observations of SH+, we expected to detect emission of the two SH+ hyperfine structure (HFS) components of the NJ = 10-01 fine structure (FS) component near 346 GHz. While we did not observe any lines at the frequencies predicted from laboratory data, we detected two emission lines, each ~15 MHz above the SH+ predictions and with relative intensities and HFS splitting expected for SH+. The rest frequencies of the two newly detected lines are more compatible with the remainder of the SH+ laboratory data than the single line measured in the laboratory near 346 GHz and previously attributed to SH+. Therefore, we assign these new features to the two SH+ HFS components of the NJ = 10-01 FS component and re-determine its spectroscopic parameters, which will be useful for future observations of SH+, in particular if its lowest frequency FS components are studied. Our observations demonstrate the suitability of these lines for SH+ searches at frequencies easily accessible from the ground. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2012.1.00352.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ.This paper makes use of observations obtained with the IRAM 30 m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).Appendix A is available in electronic form at http://www.aanda.org

  19. A SURVEY OF FAR ULTRAVIOLET SPECTROSCOPIC EXPLORER OBSERVATIONS OF CATACLYSMIC VARIABLES

    SciTech Connect

    Froning, Cynthia S.; Long, Knox S.; Gaensicke, Boris; Szkody, Paula E-mail: long@stsci.edu E-mail: szkody@alicar.astro.washington.edu

    2012-03-01

    During its lifetime, the Far Ultraviolet Spectroscopic Explorer (FUSE) was used to observe 99 cataclysmic variables (CVs) in 211 separate observations. Here, we present a survey of the moderate-resolution (R {approx_equal} 10, 000), far-ultraviolet (905-1188 A), time-averaged FUSE spectra of CVs. The FUSE spectra are morphologically diverse. They show contributions from the accretion disk, the disk chromosphere, disk outflows, and the white dwarf (WD), but the relative contribution of each component varies widely as a function of CV subtype, orbital period and evolutionary state, inclination, mass accretion rate, and magnetic field strength of the WD. The data reveal information about the structure, temperature, density and mass flow rates of the disk and disk winds, the temperature of the WD and the effects of ongoing accretion on its structure, and the long-term response of the systems to disk outbursts. The complete atlas of time-averaged FUSE spectra of CVs is available at the Multimission Archive at Space Telescope Science Institute as a High Level Science Product.

  20. Direct spectroscopic observation of a shallow hydrogenlike donor state in insulating SrTiO3.

    PubMed

    Salman, Z; Prokscha, T; Amato, A; Morenzoni, E; Scheuermann, R; Sedlak, K; Suter, A

    2014-10-10

    We present a direct spectroscopic observation of a shallow hydrogenlike muonium state in SrTiO(3) which confirms the theoretical prediction that interstitial hydrogen may act as a shallow donor in this material. The formation of this muonium state is temperature dependent and appears below ∼ 70K. From the temperature dependence we estimate an activation energy of ∼ 50 meV in the bulk and ∼ 23 meV near the free surface. The field and directional dependence of the muonium precession frequencies further supports the shallow impurity state with a rare example of a fully anisotropic hyperfine tensor. From these measurements we determine the strength of the hyperfine interaction and propose that the muon occupies an interstitial site near the face of the oxygen octahedron in SrTiO(3). The observed shallow donor state provides new insight for tailoring the electronic and optical properties of SrTiO(3)-based oxide interface systems. PMID:25375730

  1. Additional spectroscopic observations and Swift monitoring of the M31 nova iPTF16bqy (ASASSN-16hf)

    NASA Astrophysics Data System (ADS)

    Chinetti, K.; Darnley, M. J.; Page, K. L.; Williams, S. C.

    2016-08-01

    We report additional spectroscopic observations of the M31 nova, iPTF16bqy (ASASSN-16hf, ATels #9245, #9248). iPTF16bqy was initially classified as a Fe II nova based on spectra obtained 2016 July 14 and 15 (ATel #9248), about two days after discovery.

  2. Psychological factors, beliefs about medication, and adherence of youth with human immunodeficiency virus in a multisite directly observed therapy pilot study.

    PubMed

    Garvie, Patricia A; Flynn, Patricia M; Belzer, Marvin; Britto, Paula; Hu, Chengcheng; Graham, Bobbie; Neely, Michael; McSherry, George D; Spector, Stephen A; Gaur, Aditya H

    2011-06-01

    This study examined psychological functioning and beliefs about medicine in adolescents with human immunodeficiency virus (HIV) on highly active antiretroviral therapy in a community-based directly observed therapy (DOT) pilot feasibility study. Participants were youth with behaviorally acquired HIV (n = 20; 65% female; median age, 21 years) with adherence problems, who received once-daily DOT. Youth were assessed at baseline, week 12 (post-DOT), and week 24 (follow-up). At baseline, 55% of youth reported having clinical depressive symptoms compared to 27% at week 12 with sustained improvements at week 24. At baseline, substance use was reported within the borderline clinical range (T(score) = 68), with clinical but statistically nonsignificant improvement (T(score) = 61) at week 12. Hopelessness scores reflected optimism for the future. Coping strategies showed significantly decreased cognitive avoidance (p = .02), emotional discharge (p = .004), and acceptance/resignation ("nothing I can do," p = .004), whereas positive reappraisal and seeking support emerged. With the exception of depressive symptoms, week 12 improvements were not sustained at week 24. DOT adherence was predicted by higher baseline depression (p = .05), beliefs about medicine (p = .006) and perceived threat of illness scores (p = .03). Youth with behaviorally acquired HIV and adherence problems who participated in a community-based DOT intervention reported clinically improved depressive symptoms, and temporarily reduced substance use and negative coping strategies. Depressive symptoms, beliefs about medicine, and viewing HIV as a potential threat predicted better DOT adherence. PMID:21575827

  3. A spectroscopic survey for lambda Bootis stars. II. The observational data

    NASA Astrophysics Data System (ADS)

    Paunzen, E.; Duffee, B.; Heiter, U.; Kuschnig, R.; Weiss, W. W.

    2001-07-01

    lambda Bootis stars comprise only a small number of all A-type stars and are characterized as nonmagnetic, Population i, late B to early F-type dwarfs which show significant underabundances of metals whereas the light elements (C, N, O and S) are almost normal abundant compared to the Sun. In the second paper on a spectroscopic survey for lambda Bootis stars, we present the spectral classifications of all program stars observed. These stars were selected on the basis of their Strömgren uvbybeta colors as lambda Bootis candidates. In total, 708 objects in six open clusters, the Orion OB1 association and the Galactic field were classified. In addition, 9 serendipity non-candidates in the vicinity of our program stars as well as 15 Guide Star Catalogue stars were observed resulting in a total of 732 classified stars. The 15 objects from the Guide Star Catalogue are part of a program for the classification of apparent variable stars from the Fine Guidance Sensors of the Hubble Space Telescope. A grid of 105 MK standard as well as ``pathological'' stars guarantees a precise classification. A comparison of our spectral classification with the extensive work of Abt & Morrell (\\cite{Abt95}) shows no significant differences. The derived types are 0.23 +/- 0.09 (rms error per measurement) subclasses later and 0.30 +/- 0.08 luminosity classes more luminous than those of Abt & Morrell (\\cite{Abt95}) based on a sample of 160 objects in common. The estimated errors of the means are +/- 0.1 subclasses. The characteristics of our sample are discussed in respect to the distribution on the sky, apparent visual magnitudes and Strömgren uvbybeta colors. Based on observations from the Observatoire de Haute-Provence, Osservatorio Astronomico di Padova-Asiago, Observatório do Pico dos Dias-LNA/CNPq/MCT, Chews Ridge Observatory (MIRA) and University of Toronto Southern Observatory (Las Campanas).

  4. NIR SPECTROSCOPIC OBSERVATION OF MASSIVE GALAXIES IN THE PROTOCLUSTER AT z = 3.09

    SciTech Connect

    Kubo, Mariko; Yamada, Toru; Ichikawa, Takashi; Kajisawa, Masaru; Matsuda, Yuichi; Tanaka, Ichi

    2015-01-20

    We present the results of near-infrared spectroscopic observations of the K-band-selected candidate galaxies in the protocluster at z = 3.09 in the SSA22 field. We observed 67 candidates with K {sub AB} < 24 and confirmed redshifts of the 39 galaxies at 2.0 < z {sub spec} < 3.4. Of the 67 candidates, 24 are certainly protocluster members with 3.04 ≤ z {sub spec} ≤ 3.12, which are massive red galaxies that have been unidentified in previous optical observations of the SSA22 protocluster. Many distant red galaxies (J – K {sub AB} > 1.4), hyper extremely red objects (J – K {sub AB} > 2.1), Spitzer MIPS 24 μm sources, active galactic nuclei (AGNs) as well as the counterparts of Lyα blobs and the AzTEC/ASTE 1.1 mm sources in the SSA22 field are also found to be protocluster members. The mass of the SSA22 protocluster is estimated to be ∼2-5 × 10{sup 14} M {sub ☉}, and this system is plausibly a progenitor of the most massive clusters of galaxies in the current universe. The reddest (J – K {sub AB} ≥ 2.4) protocluster galaxies are massive galaxies with M {sub star} ∼ 10{sup 11} M {sub ☉} showing quiescent star formation activities and plausibly dominated by old stellar populations. Most of these massive quiescent galaxies host moderately luminous AGNs detected by X-ray. There are no significant differences in the [O III] λ5007/Hβ emission line ratios and [O III] λ5007 line widths and spatial extents of the protocluster galaxies from those of massive galaxies at z ∼ 2-3 in the general field.

  5. NIR Spectroscopic Observation of Massive Galaxies in the Protocluster at z = 3.09

    NASA Astrophysics Data System (ADS)

    Kubo, Mariko; Yamada, Toru; Ichikawa, Takashi; Kajisawa, Masaru; Matsuda, Yuichi; Tanaka, Ichi

    2015-01-01

    We present the results of near-infrared spectroscopic observations of the K-band-selected candidate galaxies in the protocluster at z = 3.09 in the SSA22 field. We observed 67 candidates with K AB < 24 and confirmed redshifts of the 39 galaxies at 2.0 < z spec < 3.4. Of the 67 candidates, 24 are certainly protocluster members with 3.04 <= z spec <= 3.12, which are massive red galaxies that have been unidentified in previous optical observations of the SSA22 protocluster. Many distant red galaxies (J - K AB > 1.4), hyper extremely red objects (J - K AB > 2.1), Spitzer MIPS 24 μm sources, active galactic nuclei (AGNs) as well as the counterparts of Lyα blobs and the AzTEC/ASTE 1.1 mm sources in the SSA22 field are also found to be protocluster members. The mass of the SSA22 protocluster is estimated to be ~2-5 × 1014 M ⊙, and this system is plausibly a progenitor of the most massive clusters of galaxies in the current universe. The reddest (J - K AB >= 2.4) protocluster galaxies are massive galaxies with M star ~ 1011 M ⊙ showing quiescent star formation activities and plausibly dominated by old stellar populations. Most of these massive quiescent galaxies host moderately luminous AGNs detected by X-ray. There are no significant differences in the [O III] λ5007/Hβ emission line ratios and [O III] λ5007 line widths and spatial extents of the protocluster galaxies from those of massive galaxies at z ~ 2-3 in the general field.

  6. Near-Simultaneous Spectroscopic and Broadband Polarimetric Observations of Be Stars

    NASA Technical Reports Server (NTRS)

    Ghosh, K.; Iyengar, K. V. K.; Ramsey, B. D.; Austin, R. A.

    1999-01-01

    Near simultaneous optical spectroscopic (on four nights) and broadband linear continuum (B, V, R, and I bands) polarimetric (on seven nights) observations of 29 Be stars were carried out during 1993 November-December. The program Be stars displayed wavelength dependence of intrinsic polarizations with no frequency dependence of polarimetric position angles. Some of the Be stars displayed long-term polarization variability. The Be and Be-shell stars could not be distinguished from one another solely on the basis of their polarization values. Full widths at half-maximum of the H.alpha profiles and the intrinsic linear continuum polarizations are closely correlated with the projected rotational velocities of the program stars. Photospheric-absorption-corrected equivalent widths of H.alpha profiles [W(alpha)] and the radii of H.alpha-emitting or -absorbing envelopes (R(sub e) or R(sub a)) are nonlinearly correlated with the intrinsic continuum polarizations of these stars. However, W(alpha) and R(sub e) are linearly correlated. With large uncertainties, there is a trend of spectral dependence of polarization. Detailed discussion of these results is presented in this paper.

  7. New spectroscopic and photometric observations of CV J0644+3344

    NASA Astrophysics Data System (ADS)

    Hernández Santisteban, J. V.

    We report photometric and simultaneous spectroscopic observations of the cataclysmic variable J0644+3344 and present calibrated Doppler tomography results of the object. We have calibrated the spectra for slit losses using simultaneous photometry. This has been used to construct reliable Doppler images in the Halpha , Hbeta and He II 4686 Å@ emission lines. We have also performed a radial velocity analysis using these emission lines to derive the primary semi-amplitude and used a cophasing method to determine the secondary K_2 best value. We have improved the ephemeris of the object based on the published and our new photometric eclipse timings to obtain HJD=254474.7927+0.26937446E. We derived a K_1=123.2±6.6 {km s}-1 and K_2=205.4±6.7. Assuming a i>76, the orbital parameters are M_1=0.91±0.04 M⊙, M_2=0.83±0.04 M⊙ and a=2.10±0.03 R⊙. Based on the Doppler tomography we conclude that J0644+3344 is a nova-like SW Sex type system.

  8. Spectroscopic Observations and Analysis of the Unusual Type Ia SN1999ac

    SciTech Connect

    Garavini, G.; Aldering, G.; Amadon, A.; Amanullah, R.; Astier,P.; Balland, C.; Blanc, G.; Conley, A.; Dahlen, T.; Deustua, S.E.; Ellis,R.; Fabbro, S.; Fadeyev, V.; Fan, X.; Folatelli, G.; Frye, B.; Gates,E.L.; Gibbons, R.; Goldhaber, G.; Goldman, B.; Goobar, A.; Groom, D.E.; Haissinski, J.; Hardin, D.; Hook, I.; Howell, D.A.; Kent, S.; Kim, A.G.; Knop, R.A.; Kowalski, M.; Kuznetsova, N.; Lee, B.C.; Lidman, C.; Mendez,J.; Miller, G.J.; Moniez, M.; Mouchet, M.; Mourao, A.; Newberg, H.; Nobili, S.; Nugent, P.E.; Pain, R.; Perdereau, O.; Perlmutter, S.; Quimby, R.; Regnault, N.; Rich, J.; Richards, G.T.; Ruiz-Lapuente, P.; Schaefer, B.E.; Schahmaneche, K.; Smith, E.; Spadafora, A.L.; Stanishev,V.; Thomas, R.C.; Walton, N.A.; Wang, L.; Wood-Vasey, W.M.

    2005-07-12

    The authors present optical spectra of the peculiar Type Ia supernova (SN Ia) 1999ac. The data extend from -15 to +42 days with respect to B-band maximum and reveal an event that is unusual in several respects. prior to B-band maximum, the spectra resemble those of SN 1999aa, a slowly declining event, but possess stronger Si II and Ca II signatures (more characteristic of a spectroscopically normal SN). Spectra after B-band maximum appear more normal. The expansion velocities inferred from the Iron lines appear to be lower than average; whereas, the expansion velocity inferred from Calcium H and K are higher than average. The expansion velocities inferred from the Iron lines appear to be lower than average; whereas, the expansion velocity inferred from Calcium H and K are higher than average. The expansion velocities inferred from Si II are among the slowest ever observed, though SN 1999ac is not particularly dim. The analysis of the parameters v{sub 10}(Si II), R(Si II), v, and {Delta}m{sub 15} further underlines the unique characteristics of SN 1999ac. They find convincing evidence of C II {lambda}6580 in the day -15 spectrum with ejection velocity v > 16,000 km s{sup -1}, but this signature disappears by day -9. This rapid evolution at early times highlights the importance of extremely early-time spectroscopy.

  9. Vertical profiling of methane and carbon dioxide using high resolution near-infrared heterodyne spectroscopic observations

    NASA Astrophysics Data System (ADS)

    Rodin, Alexander; Klimchuk, Artem; Churbanov, Dmitry; Pereslavtseva, Anastasia; Spiridonov, Maxim; Nadezhdinskyi, Alexander

    2014-05-01

    We present new method of monitoring greenhouse gases using spectroscopic observations of solar radiation passed through the atmosphere with spectral resolution ΛvδΛ up to 108. Such a high resolution is achieved by heterodyne technique and allows to retrieve full information about spectral line shape which, in turn, is used to distinguish contribution of different atmospheric layers to the resulting absorption. Weak absorption line at 6056.5 cm-1 was selected for CO2 measurements and a quartet of lines centered at 6057 cm-1for CH4. The instrument setup includes Sun tracker with a microtelescope and chopper, diode DFB laser used as a local oscillator, a bundle of single mode optical fibers that provides medium for radiation transfer and beam coupling, reference cell with depressurized methane for LO frequency stabilization, and Fabry-Perot etalon for LO frequency calibration. A commercial p-i-n diode with squared detector replaces a mixer and IF spectrometer, providing measurement of heterodyne beating within a bandpass of few MHz, which determines the effective spectral resolution of the instrument. Spectral coverage within narrow range (about 1 cm-1) is provided by ramping the LO frequency based on feedback from the reference channel. Observations of Sun in the Moscow region have resulted for the first time in measurements of the atmospheric transmission near 1.65 μm with sub-Doppler spectral resolution. In order to retrieve vertical profiles of methane and carbon dioxide we developed the inversion algorithm implementing Tikhonov regularization approach. With measured transmission having S/N ratio of 100 or higher, the uncertainty of CH4 profile is about 10 ppb, with the uncertainty of CO2 profile at 1 ppm. This techniques is promising an affordable opportunity or widespread monitoring of greenhouse gases and may be implemented on existing ground-based stations. This work has been supported by the grant of Russian Ministry of education and science #11.G34.31.0074

  10. Near-infrared spectroscopic observations of Comets by Japanese Infrared Satellite

    NASA Astrophysics Data System (ADS)

    Kobayashi, Hitomi; Yamaguchi, Mitsuru; Ootsubo, Takafumi; Kawakita, Hideyo; Hamada, Saki

    Comets are thought to be one of the primeordial bodies in the solar system. Chemical abun-dances of the cometary icy materials are precious clue to the conditions in the early solar system. H2O is the most abundant species of the cometry nucleus, but CO and CO2 are also abundant with diversities. Especially, CO2 cannot be directly observed by ground-based ob-servations because of the strong absorption by telluric CO2. Thus, only the space observatory (or spacecraft) can access CO2 in comets directly. We observed some comets by "AKARI", Japanese infrared satellite. It has 68.5 cm telescope with InfraRed Camera (IRC). The IRC also has a spectroscopic capability (both grism and prism were available for disperser). The data we present were taken by the IRC in the grism mode. The IRC with grism can cover the wavelength range from 2.5 to 5 microns where vibrational fundamental bands of H2O, CO2, and CO (at 2.7, 4.3, and 4.7 microns) are usually recognized as emission in cometary spectra. We determined the mixng ratios of CO and CO2 relative to H2O for 5 comets: C/2006 W3, C/2006 OF2, C/2006 W3, /2007 N3, and C/2007 W1. These comets were observed at various heliocetric distances, so their mixing ratios can not be compared directly among these comets. We tried to convert the obtained mixing ratios at various heliocentric distancees to the mixing ratios at 1 AU from the Sun. Previous studies of mixing ratios of CO2 and CO relative to H2O were carried out by the Vega space craft (1P/Halley), ISO (C/1995 O1 and 103P/Hartley 2) and Deep Impcat spacecraft (9P/Tempel 1). We also applied the conversion factors to those prvious works. We will discuss about the diversity of mixing ratios of CO2 and CO in these comets.

  11. GEMINI near-infrared spectroscopic observations of young massive stars embedded in molecular clouds

    NASA Astrophysics Data System (ADS)

    Roman-Lopes, A.; Abraham, Z.; Ortiz, R.; Rodriguez-Ardila, A.

    2009-03-01

    K-band spectra of young stellar candidates in four Southern hemisphere clusters have been obtained with the Gemini Near-Infrared Spectrograph in Gemini South. The clusters are associated with IRAS sources that have colours characteristic of ultracompact HII regions. Spectral types were obtained by comparison of the observed spectra with those of a near-infrared (NIR) library; the results include the spectral classification of nine massive stars and seven objects confirmed as background late-type stars. Two of the studied sources have K-band spectra compatible with those characteristic of very hot stars, as inferred from the presence of CIV, NIII and NV emission lines at 2.078, 2.116 and 2.100 μm, respectively. One of them, I16177_IRS1, has a K-band spectrum similar to that of Cyg OB2 7, an O3If* supergiant star. The nebular K-band spectrum of the associated Ultra-Compact (UC) HII region shows the s-process [KrIII] and [SeIV] high excitation emission lines, previously identified only in planetary nebula. One young stellar object was found in each cluster, associated with either the main IRAS source or a nearby resolved Midecourse Space eXperiment (MSX) component, confirming the results obtained from previous NIR photometric surveys. The distances to the stars were derived from their spectral types and previously determined JHK magnitudes; they agree well with the values obtained from the kinematic method, except in the case of IRAS 15408-5356, for which the spectroscopic distance is about a factor of 2 smaller than the kinematic value.

  12. Far Ultraviolet Spectroscopic Explorer Observation of the Nonradiative Collisionless Shock in the Remnant of SN 1006

    NASA Astrophysics Data System (ADS)

    Korreck, K. E.; Raymond, J. C.; Zurbuchen, T. H.; Ghavamian, P.

    2004-11-01

    The appearance of the young supernova remnant SN 1006 is dominated by emission from nonradiative shocks in the northeast and northwest regions. At X-ray energies the northeast shock exhibits predominantly nonthermal synchrotron emission, while the northwest shock exhibits a thermal spectrum. We present far-ultraviolet spectra of the northeast (NE) and northwest (NW) portions of SN 1006 acquired with the Far Ultraviolet Spectroscopic Explorer (FUSE). We have detected emission lines of O VI λλ1032, 1038 and broad Lyβ λ1025 in the NW filament but detect no emission lines in the NE region down to a level of 4.7×10-17 ergs cm-2 s-1 arcsec-2. We observed in the NW an O VI intensity of 2.0+/-0.2×10-16 ergs cm-2 s-1 arcsec-2 and measured an O VI line width of 2100+/-200 km s-1 at a position where the Hα width was measured to be 2290+/-80 km s-1. This implies less than mass-proportional heating of the ions. Using the ratio of intensities I(NW)/I(NE)~n(NW)/n(NE), the density ratio of the two regions is found to be >=4, a value that is consistent with the uncertainties of the ratio of 2.5 measured in 2003 by Long and coworkers. The derived O VI kinetic temperature is compared to previous estimates of electron, proton, and ion temperatures in the remnant to study the relative heating efficiency of various species at the shock front. The degree of postshock temperature equilibration may be crucial to particle acceleration, since the temperature of each species determines the number of high-speed particles available for injection into an acceleration process that could produce Galactic cosmic rays.

  13. Unveiling the nature of two unidentified EGRET blazar candidates through spectroscopic observations

    NASA Astrophysics Data System (ADS)

    Nkundabakura, P.; Meintjes, P. J.

    2012-11-01

    Studies using the Energetic Gamma-Ray Experiment Telescope (EGRET) revealed that blazars [flat-spectrum radio quasars (FSRQs) and BL Lac objects] emit most of their luminosity in the high-energy gamma-ray (E > 100 MeV) range. From the 271 sources observed by EGRET, 131 are still unidentified. A systematic search is conducted to identify possible high-energy gamma-ray blazars among the unidentified EGRET population. Based upon multiwavelength emission properties, 13 extragalactic radio sources were selected in the EGRET error boxes for further investigation. From the above-mentioned sample, results of a multiwavelength follow-up of two EGRET sources, 3EG J0821-5814 and 3EG J0706-3837, are presented. These sources are associated with their radio counterparts PKS J0820-5705 and PMN J0710-3850, respectively. Spectroscopic observations utilizing the SOAR/Goodman spectrograph at the Cerro Tololo Inter-American Observatory in Chile reveal a spectrum of PKS J0820-5705 that corresponds to that of a radio-loud active galactic nucleus (FSRQ) with redshift z = 0.06 ± 0.01, while the visibility of wide and narrow emission lines in the spectrum of PMN J0710-3850 resembles that of a low-ionization nuclear emission-line region (LINER) or type 1 Seyfert galaxy at z = 0.129 ± 0.001. The observed Ca II K&H lines depression ratio at 4000 Å showed a shallow depression of 8.8 ± 2.5 per cent for PKS J0820-5705 and 80 ± 1 per cent for PMN J0710-3850, suggesting the presence of a strong non-thermal optical contribution in PKS J0820-5705, which clearly distinguishes its spectrum from that of a radio galaxy. The weaker optical non-thermal contribution for PMN J0710-3850 is in accordance with that expected of a LINER. For PMN J0710-3850 the line flux ratios [O III] λ5007/Hβ < 3 and [N II] λ6583/Hα > 0.6 which are in agreement with the expected ratios of LINERs. However, the absence of [O II] λ3727 implies an anomalously low [O II]/[O III] < 0.5 ratio for a LINER, and agrees more

  14. The B0.5 IVe CoRoT target HD 49330. II. Spectroscopic ground-based observations

    NASA Astrophysics Data System (ADS)

    Floquet, M.; Hubert, A.-M.; Huat, A.-L.; Frémat, Y.; Janot-Pacheco, E.; Gutiérrez-Soto, J.; Neiner, C.; de Batz, B.; Leroy, B.; Poretti, E.; Amado, P.; Catala, C.; Rainer, M.; Diaz, D.; Uytterhoeven, K.; Andrade, L.; Diago, P. D.; Emilio, M.; Espinosa Lara, F.; Fabregat, J.; Martayan, C.; Semaan, T.; Suso, J.

    2009-10-01

    Context: We present spectroscopic ground-based observations of the early Be star HD 49330 obtained simultaneously with the CoRoT-LRA1 run just before the burst observed in the CoRoT data. Aims: Ground-based spectroscopic observations of the early Be star HD 49330 obtained during the precursor phase and just before the start of an outburst allow us to disantangle stellar and circumstellar contributions and identify modes of stellar pulsations in this rapidly rotating star. Methods: Time series analysis (TSA) is performed on photospheric line profiles of He I and Si III by means of the least squares method. Results: We find two main frequencies f1 = 11.86 c d-1 and f2 = 16.89 c d-1 which can be associated with high order p-mode pulsations. We also detect a frequency f3 = 1.51 c d-1 which can be associated with a low order g-mode. Moreover we show that the stellar line profile variability changed over the spectroscopic run. These results are in agreement with the results of the CoRoT data analysis, as shown in Huat et al. (2009). Conclusions: Our study of mid- and short-term spectroscopic variability allows the identification of p- and g-modes in HD 49330. It also allows us to display changes in the line profile variability before the start of an outburst. This brings new constraints for the seimic modelling of this star. Based on observations made with ESO Telescopes at La Silla Observatory under the ESO Large Programme: LP178.D-0361, and on data collected with the TBL at Pic du Midi Observatory (France).

  15. VizieR Online Data Catalog: Spectroscopic observations of globular clusters (Sharina+, 2010)

    NASA Astrophysics Data System (ADS)

    Sharina, M. E.; Chandar, R.; Puzia, T. H.; Goudfrooij, P.; Davoust, E.

    2012-03-01

    The spectroscopic data were obtained with the SCORPIO spectrograph installed at the prime focus of the SAO 6-m telescope of the Russian Academy of Sciences in two modes: with long-slit (LS) and multislit (MS) units. (5 data files).

  16. Photometric and spectroscopic observations, and abundance tomography modelling of the Type Ia supernova SN 2014J located in M82

    NASA Astrophysics Data System (ADS)

    Ashall, C.; Mazzali, P.; Bersier, D.; Hachinger, S.; Phillips, M.; Percival, S.; James, P.; Maguire, K.

    2014-12-01

    Spectroscopic and photometric observations of the nearby Type Ia Supernova (SN Ia) SN 2014J are presented. Spectroscopic observations were taken -8 to +10 d relative to B-band maximum, using FRODOSpec, a multipurpose integral-field unit spectrograph. The observations range from 3900 to 9000 Å. SN 2014J is located in M82 which makes it the closest SN Ia studied in at least the last 28 yr. It is a spectroscopically normal SN Ia with high-velocity features. We model the spectra of SN 2014J with a Monte Carlo radiative transfer code, using the abundance tomography technique. SN 2014J is highly reddened, with a host galaxy extinction of E(B - V) = 1.2 (RV = 1.38). It has a Δm15(B) of 1.08 ± 0.03 when corrected for extinction. As SN 2014J is a normal SN Ia, the density structure of the classical W7 model was selected. The model and photometric luminosities are both consistent with B-band maximum occurring on JD 245 6690.4 ± 0.12. The abundance of the SN 2014J behaves like other normal SN Ia, with significant amounts of silicon (12 per cent by mass) and sulphur (9 per cent by mass) at high velocities (12 300 km s-1) and the low-velocity ejecta (v < 6500 km s-1) consists almost entirely of 56Ni.

  17. Far Ultraviolet Spectroscopic Explorer (FUSE) observations of emitting and absorbing gas in the Local Interstellar Chimney

    NASA Astrophysics Data System (ADS)

    Welsh, B. Y.; Sallmen, S.; Sfeir, D.; Shelton, R. L.; Lallement, R.

    2002-11-01

    We present Far Ultraviolet Spectroscopic Explorer (FUSE) satellite measurements of the absorption and emission characteristics of interstellar gas associated with the Local Interstellar Chimney, which is an extension of the rarefied Local Bubble cavity that extends outward from the galactic disk towards the lower galactic halo. Far ultraviolet (FUV) diffuse background emission has been detected in the high ionization line of O VI (lambda 1032 Å) for two lines-of-sight (l = 162.7deg, b = +57.0deg) and (l = 156.3deg, b = +57.8deg) at emission levels of 2500+/-700 photons cm-2 s-1 sr-1 (LU) and 3300+/-1100 LU respectively. These levels of O VI emission are very similar to those found for four other lines-of-sight sampled thus far by the FUSE satellite, implying a fairly constant level of average O VI surface brightness emission at high galactic latitudes of about 2700 LU with a standard deviation of 450 LU. These emission-line data are supplemented by FUV interstellar absorption line measurements taken towards the hot DA white dwarf star, REJ 1032+532 (l = 157.5deg, b = +53.2deg), whose distance of 116 pc places it within the Local Bubble region. No high ionization interstellar O VI lambda 1032 Å absorption has been detected (N(O VI) < 13.0 cm-2), which is consistent with the non-detections of interstellar C IV and Si IV absorption reported towards this star by Holberg et al. (\\cite{holberg99a}). Taken together, our FUV absorption and emission data may be explained by a scenario in which the O VI emission and absorption lines are both formed at the conductive interface of the neutral boundary to the Local Bubble. For the presently sampled sight-lines we have found no correlation between the OVI emission line intensity and the associated 0.25 keV soft X-ray background flux as measured in the R1 and R2 bands by the ROSAT satellite. The OVI line intensities also show no correlation with the soft X-ray background flux attributable to emission from the million degree K

  18. How Can Multi-Site Evaluations Be Participatory?

    ERIC Educational Resources Information Center

    Lawrenz, Frances; Huffman, Douglas

    2003-01-01

    Multi-site evaluations are becoming increasingly common in federal funding portfolios. Although much thought has been given to multi-site evaluation, there has been little emphasis on how it might interact with participatory evaluation. Therefore, this paper reviews several National Science Foundation educational, multi-site evaluations for the…

  19. Optical Spectroscopic Observations of Gamma-ray Blazar Candidates. IV. Results of the 2014 Follow-up Campaign

    NASA Astrophysics Data System (ADS)

    Ricci, F.; Massaro, F.; Landoni, M.; D'Abrusco, R.; Milisavljevic, D.; Stern, D.; Masetti, N.; Paggi, A.; Smith, Howard A.; Tosti, G.

    2015-05-01

    The extragalactic γ-ray sky is dominated by the emission arising from blazars, one of the most peculiar classes of radio-loud active galaxies. Since the launch of Fermi several methods were developed to search for blazars as potential counterparts of unidentified γ-ray sources (UGSs). To confirm the nature of the selected candidates, optical spectroscopic observations are necessary. In 2013 we started a spectroscopic campaign to investigate γ-ray blazar candidates selected according to different procedures. The main goals of our campaign are: (1) to confirm the nature of these candidates, and (2) whenever possible, determine their redshifts. Optical spectroscopic observations will also permit us to verify the robustness of the proposed associations and check for the presence of possible source class contaminants to our counterpart selection. This paper reports the results of observations carried out in 2014 in the northern hemisphere with Kitt Peak National Observatory and in the southern hemisphere with the Southern Astrophysical Research telescopes. We also report three sources observed with the Magellan and Palomar telescopes. Our selection of blazar-like sources that could be potential counterparts of UGSs is based on their peculiar infrared colors and on their combination with radio observations both at high and low frequencies (i.e., above and below ˜1 GHz) in publicly available large radio surveys. We present the optical spectra of 27 objects. We confirm the blazar-like nature of nine sources that appear to be potential low-energy counterparts of UGSs. Then we present new spectroscopic observations of 10 active galaxies of uncertain type associated with Fermi sources, classifying all of them as blazars. In addition, we present the spectra for five known γ-ray blazars with uncertain redshift estimates and three BL Lac candidates that were observed during our campaign. We also report the case for WISE J173052.85-035247.2, candidate counterpart of the

  20. Ab initio study of the O4H(+) novel species: spectroscopic fingerprints to aid its observation.

    PubMed

    Xavier, F George D; Hernández-Lamoneda, Rámon

    2015-06-28

    A detailed ab initio characterization of the structural, energetic and spectroscopic properties of the novel O4H(+) species is presented. The equilibrium structures and relative energies of all multiplet states have been determined systematically by analyzing static and dynamical correlation effects. The two and three body dissociation processes have been studied and indicate the presence of conical intersections in various states including the ground state. Comparison with available thermochemical data is very good, supporting the applied methodology. The reaction, H3(+) + O4→ O4H(+) + H2, was found to be exothermic ΔH = -19.4 kcal mol(-1) and therefore, it is proposed that the product in the singlet state could be formed in the interstellar medium (ISM) via collision processes. To aid in its laboratory or radioastronomy detection in the interstellar medium we determined spectroscopic fingerprints. It is estimated for the most stable geometry of O4H(+) dipole allowed electronic transitions in the visible region at 429 nm and 666 nm, an intense band at 1745 cm(-1) in the infrared and signals at 40.6, 81.2 and 139.2 GHz in the microwave region at 10, 50 and 150 K respectively, relevant for detection in the ISM. PMID:26028209

  1. FIRST SPECTROSCOPIC IMAGING OBSERVATIONS OF THE SUN AT LOW RADIO FREQUENCIES WITH THE MURCHISON WIDEFIELD ARRAY PROTOTYPE

    SciTech Connect

    Oberoi, Divya; Matthews, Lynn D.; Lonsdale, Colin J.; Benkevitch, Leonid; Cairns, Iver H.; Lobzin, Vasili; Emrich, David; Wayth, Randall B.; Arcus, Wayne; Morgan, Edward H.; Williams, Christopher; Prabu, T.; Vedantham, Harish; Williams, Andrew; White, Stephen M.; Allen, G.; Barnes, David; Bernardi, Gianni; Bowman, Judd D.; Briggs, Frank H.

    2011-02-20

    We present the first spectroscopic images of solar radio transients from the prototype for the Murchison Widefield Array, observed on 2010 March 27. Our observations span the instantaneous frequency band 170.9- 201.6 MHz. Though our observing period is characterized as a period of 'low' to 'medium' activity, one broadband emission feature and numerous short-lived, narrowband, non-thermal emission features are evident. Our data represent a significant advance in low radio frequency solar imaging, enabling us to follow the spatial, spectral, and temporal evolution of events simultaneously and in unprecedented detail. The rich variety of features seen here reaffirms the coronal diagnostic capability of low radio frequency emission and provides an early glimpse of the nature of radio observations that will become available as the next generation of low-frequency radio interferometers come online over the next few years.

  2. A study of non-Keplerian velocities in observations of spectroscopic binary stars

    NASA Astrophysics Data System (ADS)

    Hearnshaw, J. B.; Komonjinda, Siramas; Skuljan, J.; Kilmartin, P. M.

    2012-11-01

    This paper presents an orbital analysis of six southern single-lined spectroscopic binary systems. The systems selected were shown to have circular or nearly circular orbits (e < 0.1) from earlier published solutions of only moderate precision. The purpose was to obtain high-precision orbital solutions in order to investigate the presence of small non-Keplerian velocity effects in the data and hence the reality of the small eccentricities found for most of the stars. The Hercules spectrograph and 1-m McLellan telescope at Mt John Observatory, New Zealand, were used to obtain over 450 CCD spectra between 2004 October and 2007 August. Radial velocities were obtained by cross-correlation. These data were used to achieve high-precision orbital solutions for all the systems studied, sometimes with solutions up to about 50 times more precise than those from the earlier literature. However, the precision of the solutions is limited in some cases by the rotational velocity or chromospheric activity of the stars. The data for the six binaries analysed here are combined with those for six stars analysed earlier by Komonjinda, Hearnshaw and Ramm. We have performed tests using the prescription of Lucy on all 12 binaries, and conclude that, with one exception, none of the small eccentricities found by fitting Keplerian orbits to the radial-velocity data can be supported. Instead we conclude that small non-Keplerian effects, which are clearly detectable for six of our stars, make impossible the precise determination of spectroscopic binary orbital eccentricities for many late-type stars to better than about 0.03 in eccentricity, unless the systematic perturbations are also carefully modelled. The magnitudes of the non-Keplerian velocity variations are given quantitatively.

  3. Culture and Influence in Multisite Evaluation

    ERIC Educational Resources Information Center

    Kirkhart, Karen E.

    2011-01-01

    Understanding the influence of multisite evaluation requires careful consideration of cultural context. The author illustrates dimensions of influence and culture with excerpts from four National Science Foundation evaluation case studies and summarizes what influence teaches everyone about culture and what culture teaches everyone about…

  4. Multisite functional connectivity MRI classification of autism: ABIDE results

    PubMed Central

    Nielsen, Jared A.; Zielinski, Brandon A.; Fletcher, P. Thomas; Alexander, Andrew L.; Lange, Nicholas; Bigler, Erin D.; Lainhart, Janet E.; Anderson, Jeffrey S.

    2013-01-01

    Background: Systematic differences in functional connectivity MRI metrics have been consistently observed in autism, with predominantly decreased cortico-cortical connectivity. Previous attempts at single subject classification in high-functioning autism using whole brain point-to-point functional connectivity have yielded about 80% accurate classification of autism vs. control subjects across a wide age range. We attempted to replicate the method and results using the Autism Brain Imaging Data Exchange (ABIDE) including resting state fMRI data obtained from 964 subjects and 16 separate international sites. Methods: For each of 964 subjects, we obtained pairwise functional connectivity measurements from a lattice of 7266 regions of interest covering the gray matter (26.4 million “connections”) after preprocessing that included motion and slice timing correction, coregistration to an anatomic image, normalization to standard space, and voxelwise removal by regression of motion parameters, soft tissue, CSF, and white matter signals. Connections were grouped into multiple bins, and a leave-one-out classifier was evaluated on connections comprising each set of bins. Age, age-squared, gender, handedness, and site were included as covariates for the classifier. Results: Classification accuracy significantly outperformed chance but was much lower for multisite prediction than for previous single site results. As high as 60% accuracy was obtained for whole brain classification, with the best accuracy from connections involving regions of the default mode network, parahippocampaland fusiform gyri, insula, Wernicke Area, and intraparietal sulcus. The classifier score was related to symptom severity, social function, daily living skills, and verbal IQ. Classification accuracy was significantly higher for sites with longer BOLD imaging times. Conclusions: Multisite functional connectivity classification of autism outperformed chance using a simple leave-one-out classifier

  5. Multisite Reliability of Cognitive BOLD Data

    PubMed Central

    Brown, Gregory G.; Mathalon, Daniel H.; Stern, Hal; Ford, Judith; Mueller, Bryon; Greve, Douglas N.; McCarthy, Gregory; Voyvodic, Jim; Glover, Gary; Diaz, Michele; Yetter, Elizabeth; Burak Ozyurt, I.; Jorgensen, Kasper W.; Wible, Cynthia G.; Turner, Jessica A.; Thompson, Wesley K.; Potkin, Steven G.

    2010-01-01

    Investigators perform multi-site functional magnetic resonance imaging studies to increase statistical power, to enhance generalizability, and to improve the likelihood of sampling relevant subgroups. Yet undesired site variation in imaging methods could off-set these potential advantages. We used variance components analysis to investigate sources of variation in the blood oxygen level dependent (BOLD) signal across four 3T magnets in voxelwise and region of interest (ROI) analyses. Eighteen participants traveled to four magnet sites to complete eight runs of a working memory task involving emotional or neutral distraction. Person variance was more than 10 times larger than site variance for five of six ROIs studied. Person-by-site interactions, however, contributed sizable unwanted variance to the total. Averaging over runs increased between-site reliability, with many voxels showing good to excellent between-site reliability when eight runs were averaged and regions of interest showing fair to good reliability. Between-site reliability depended on the specific functional contrast analyzed in addition to the number of runs averaged. Although median effect size was correlated with between-site reliability, dissociations were observed for many voxels. Brain regions where the pooled effect size was large but between-site reliability was poor were associated with reduced individual differences. Brain regions where the pooled effect size was small but between-site reliability was excellent were associated with a balance of participants who displayed consistently positive or consistently negative BOLD responses. Although between-site reliability of BOLD data can be good to excellent, acquiring highly reliable data requires robust activation paradigms, ongoing quality assurance, and careful experimental control. PMID:20932915

  6. Bias and Bias Correction in Multi-Site Instrumental Variables Analysis of Heterogeneous Mediator Effects

    ERIC Educational Resources Information Center

    Reardon, Sean F.; Unlu, Faith; Zhu, Pei; Bloom, Howard

    2013-01-01

    We explore the use of instrumental variables (IV) analysis with a multi-site randomized trial to estimate the effect of a mediating variable on an outcome in cases where it can be assumed that the observed mediator is the only mechanism linking treatment assignment to outcomes, as assumption known in the instrumental variables literature as the…

  7. Bias and Bias Correction in Multisite Instrumental Variables Analysis of Heterogeneous Mediator Effects

    ERIC Educational Resources Information Center

    Reardon, Sean F.; Unlu, Fatih; Zhu, Pei; Bloom, Howard S.

    2014-01-01

    We explore the use of instrumental variables (IV) analysis with a multisite randomized trial to estimate the effect of a mediating variable on an outcome in cases where it can be assumed that the observed mediator is the only mechanism linking treatment assignment to outcomes, an assumption known in the IV literature as the exclusion restriction.…

  8. Near Infrared photometric and spectroscopic observations of the bright optical transient J212444.87+321738.3

    NASA Astrophysics Data System (ADS)

    Mondal, Soumen; Das, Ramkrishna; Ashok, N. M.; Banerjee, D. P. K.; Dutta, Somnath; Ghosh, Supriyo; Mondal, Anindita

    2013-04-01

    We report near infrared JHK-band photometry and spectroscopic observations of the recently reported bright optical transient J212444.87+321738.3 using the Near-IR Imager cum spectrograph (NICMOS-3) installed on the Mount Abu 1.2-m telescope of the Physical Research Laboratory, India following the outburst announcement by Tiurina et al. in ATel #4888. The photometric observations were carried out on 2013 March 21.020 UT and 23.010 UT yielding magnitudes of J = 5.85 +/- 0.06, H = 4.47 +/- 0.06, K = 3.77 +/- 0.05; and J= 5.64 +/- 0.04, H= 4.48 +/- 0.04, K = 3.77 +/- 0.03 respectively.

  9. Thermal treatment effects imposed on solid DNA cationic lipid complex with hexadecyltrimethylammonium chloride, observed by variable angle spectroscopic ellipsometry

    SciTech Connect

    Nizioł, Jacek

    2014-12-21

    DNA cationic lipid complexes are materials of properties required for applications in organic electronics and optoelectronics. Often, their thermal stability demonstrated by thermogravimetry is cited in the literature as important issue. However, little is known about processes occurring in heated solid DNA cationic lipid complexes. In frame of this work, thin films of Deoxyribonucleic acid-hexadecyltrimethylammonium chloride (DNA-CTMA) were deposited on silicon wafers. Samples were thermally annealed, and simultaneously, their optical functions were measured by spectroscopic ellipsometry. At lower temperatures, thermal expansion coefficient of solid DNA-CTMA was negative, but at higher temperatures positive. Thermally induced modification of absorption spectrum in UV-vis was observed. It occurred at a range of temperatures higher than this of DNA denaturation in solution. The observed phenomenon was irreversible, at least in time scale of the experiment (one day)

  10. Spectroscopic observations of bright and dark emission features on the night side of venus.

    PubMed

    Bell, J F; Crisp, D; Lucey, P G; Ozoroski, T A; Sinton, W M; Willis, S C; Campbell, B A

    1991-05-31

    Near-infrared spectra of a bright and a dark thermal emission feature on the night side of Venus have been obtained from 2.2 to 2.5 micrometers (microm) at a spectral resolution of 1200 to 1500. Both bright and dark features show numerous weak absorption bands produced by CO(2), CO, water vapor, and other gases. The bright feature (hot spot) emits more radiation than the dark feature (cold spot) throughout this spectral region, but the largest contrasts occur between 2.21 and 2.32 microm, where H(2)SO(4) clouds and a weak CO(2) band provide the only known sources of extinction. The contrast decreases by 55 to 65 percent at wavelengths longer than 2.34 microm, where CO, clouds, and water vapor also absorb and scatter upwelling radiation. This contrast reduction may provide direct spectroscopic evidence for horizontal variations in the water vapor concentrations in the Venus atmosphere at levels below the cloud tops. PMID:17842954

  11. Radial-velocity observations of pulsating stars with a new Poznan Spectroscopic Telescope

    NASA Astrophysics Data System (ADS)

    Dimitrow, W.

    2008-12-01

    We present results of radial velocity measurements of classical cepheids, δ Scuti and β Cephei stars. The spectra were obtained with Poznan Spectroscopic Telescope (PST). The telescope has been operating since August 2007. The PST is equipped with two 40cm diameter mirrors of Newtonian focus, connected by an optic fiber with an echelle spectrograph. The PSTs design aimed at the best cooperation with the spectrograph as well as limiting light looses. It allows us to measure radial velocity of stars as faint as 11.5 magnitudes. The peltier-liquid cooled CCD camera covers 64 echelle orders with spectral range from 4480 to 9250˚A. The dispersion of the obtained radial velocity measurements is on the level of 150 m/s. Echelle spectra reduction and RV measu- rements are performed with Image Reduction and Analysis Facility (IRAF). We have achived sufficient phase coverage for 28 And, γ Peg, Polaris and V440 Per. Further data acquirement for other pulsating stars is currently held.

  12. Multi-site, multivariate weather generator using maximum entropy bootstrap

    NASA Astrophysics Data System (ADS)

    Srivastav, Roshan K.; Simonovic, Slobodan P.

    2014-05-01

    Weather generators are increasingly becoming viable alternate models to assess the effects of future climate change scenarios on water resources systems. In this study, a new multisite, multivariate maximum entropy bootstrap weather generator (MEBWG) is proposed for generating daily weather variables, which has the ability to mimic both, spatial and temporal dependence structure in addition to other historical statistics. The maximum entropy bootstrap (MEB) involves two main steps: (1) random sampling from the empirical cumulative distribution function with endpoints selected to allow limited extrapolation and (2) reordering of the random series to respect the rank ordering of the original time series (temporal dependence structure). To capture the multi-collinear structure between the weather variables and between the sites, we combine orthogonal linear transformation with MEB. Daily weather data, which include precipitation, maximum temperature and minimum temperature from 27 years of record from the Upper Thames River Basin in Ontario, Canada, are used to analyze the ability of MEBWG based weather generator. Results indicate that the statistics from the synthetic replicates were not significantly different from the observed data and the model is able to preserve the 27 CLIMDEX indices very well. The MEBWG model shows better performance in terms of extrapolation and computational efficiency when compared to multisite, multivariate K-nearest neighbour model.

  13. Submillimeter Continuum Observations of the T Tauri Spectroscopic Binary GW Orionis

    NASA Astrophysics Data System (ADS)

    Mathieu, R. D.; Adams, F. C.; Fuller, G. A.; Jensen, E. L.

    1993-05-01

    We have used the James Clerk Maxwell Telescope to detect strong submillimeter (350 microns - 1100 microns) continuum emission from the classical T Tauri star GW Orionis. GW Ori is a spectroscopic binary with a period of 242 days and a separation of 1 AU (Mathieu, Adams and Latham, 1991, AJ 101, 2184; MAL). It is the first pre-main sequence short-period binary system to show submillimeter emission. The submillimeter luminosity is comparable to the largest among both T Tauri and Herbig Ae stars. The emission is confined within a radius of 5 arcsec (2000 AU). We show that the origin of the emission must be circumbinary. With an optically thin, isothermal approximation we place a lower limit of 0.1 M_⊙ on the mass of circumbinary material, assuming a maximum temperature of 150 K. Using the pure-disk models of MAL, we find disk masses between a few tenths of a solar mass and a few solar masses, depending on choice of submillimeter opacity. These values are a significant fraction of the total stellar mass (2.8 M_⊙ to 3.8 M_⊙, depending on inclination) and possibly comparable to the secondary mass alone (0.3 M_⊙ to 1.3 M_⊙). Our fluxes are inconsistent with the disk-envelope model of MAL, for typically adopted opacities. Other extended distributions of material need to be considered, particularly since GW Ori lies near the birthline. If the circumbinary material is in a disk, then the derived masses are sufficient to drive rapid evolution of the binary orbital elements, including exciting eccentricity into the orbit. As such, the low eccentricity of GW Ori (e=0.04+/-0.06) may indicate that the disk matter does not populate the strong resonances near the secondary. In addition, the case of GW Ori suggests that massive circumbinary disks can survive the binary formation process, placing constraints on the degree of disk consumption and/or replenishment (e.g., if formation is the result of disk instabilities) or circuminary disk disruption (e.g.,in a disk

  14. Optical Spectroscopic Observations of γ-Ray Blazar Candidates. III. The 2013/2014 Campaign in the Southern Hemisphere

    NASA Astrophysics Data System (ADS)

    Landoni, M.; Massaro, F.; Paggi, A.; D'Abrusco, R.; Milisavljevic, D.; Masetti, N.; Smith, H. A.; Tosti, G.; Chomiuk, L.; Strader, J.; Cheung, C. C.

    2015-05-01

    We report the results of our exploratory program carried out with the southern Astrophysical Research telescope aimed at associating counterparts and establishing the nature of the Fermi Unidentified γ-ray Sources (UGSs). We selected the optical counterparts of six UGSs from the Fermi catalog on the basis of our recently discovered tight connection between infrared and γ-ray emission found for the γ-ray blazars detected by the Wide-Field Infrared Survey Explorer in its all-sky survey. We perform for the first time a spectroscopic study of the low-energy counterparts of the Fermi UGSs, in the optical band, confirming the blazar-like nature of the whole sample. We also present new spectroscopic observations of six active galaxies of uncertain type associated with Fermi sources which appear to be BL Lac objects. Finally, we report the spectra collected for six known γ-ray blazars belonging to the Roma BZCAT that were obtained to establish their nature or better estimate their redshifts. Two interesting cases of high redshift and extremely luminous BL Lac objects (z ≥ 1.18 and z ≥ 1.02, based on the detection of Mg ii intervening systems) are also discussed. Based on observations obtained at the southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia, e Inovação (MCTI) da República Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU).

  15. Spectroscopic Observations of Steep Spectrum Narrow-Line Seyfert 1 Galaxies

    NASA Technical Reports Server (NTRS)

    Leighly, Karen

    1999-01-01

    ROSAT observations of narrow-line Seyfert 1s found consistently steep spectra and rapid variability, but ASCA observations show more diversity, very different to classical Seyfert 1s. However, in 3 NLS1s, ASCA finds common characteristics of these exciting new class of AGN (active galactic nuclei): a very strong high temperature soft excess, weak hard tail, a possible blue shifted ionized oxygen edge, and rapid large amplitude variability characterized by flares and quiescent periods. It is necessary to observe many more such objects in order to understand the physical processes underlying the different phenomenology in ASCA. ASCA observations of two NLS1s discovered by ROSAT's all sky survey were proposed and an observation of one of these objects, RX J0439-45, was awarded. The results of spectral and variability analysis are included in Leighly 1999ab, and preliminary results are found in Leighly 1998ab.

  16. Detection of High-Frequency Oscillations and Damping from Multi-slit Spectroscopic Observations of the Corona

    NASA Astrophysics Data System (ADS)

    Samanta, T.; Singh, J.; Sindhuja, G.; Banerjee, D.

    2016-01-01

    During the total solar eclipse of 11 July 2010, multi-slit spectroscopic observations of the solar corona were performed from Easter Island, Chile. To search for high-frequency waves, observations were taken at a high cadence in the green line at 5303 Å that is due to [Fe xiv] and the red line at 6374 Å that is due to [Fe x]. The data were analyzed to study the periodic variations in intensity, Doppler velocity, and line width using wavelet analysis. The data with high spectral and temporal resolution enabled us to study the rapid dynamical changes within coronal structures. We find that at certain locations, each parameter shows significant oscillation with periods ranging from 6 - 25 s. For the first time, we were able to detect damping of high-frequency oscillations with periods of about 10 s. If the observed damped oscillations are due to magnetohydrodynamic waves, then they can contribute significantly to the heating of the corona. From a statistical study we try to characterize the nature of the observed oscillations while considering the distribution of power in different line parameters.

  17. Time Series Spectroscopic and Photometric Observations of the Massive DAV BPM 37093

    NASA Astrophysics Data System (ADS)

    Nitta, Atsuko; Kepler, S. O.; Chene, Andre–Nicolas; Koester, D.; Provencal, J. L.; Sullivan, D. J.; Chote, Paul; Safeko, Ramotholo; Kanaan, Antonio; Romero, Alejandra; Corti, Mariela; Corti, Mariela; Kilic, Mukremin; Winget, D. E.

    2015-06-01

    BPM 37093 was the first of only a handful of massive (1.05+/-0.05 M⊙; Bergeron 2004;Koester & Allard 2000) white dwarf pulsators discovered (Kanaan et al. 1992). These stars are particularly interesting because the crystallized mass-fraction as a function of mass and temperature is poorly constrained by observation, yet this process adds 1-2 Gyr uncertainty in ages of the oldest white dwarf stars observed and hence, in the ages of associations that contain them (Abrikosov 1960; Kirzhnits 1960; Salpeter 1961). Last year, we discovered that ESO uses BPM 37093 as a standard star and extracted corresponding spectra from the public archive. The data suggested a large variation in the observed hydrogen line profiles that could potentially be due to pulsations, but the measurement did not reach a detection-quality threshold. To further explore this possibility, though, we obtained 4hrs of continuous time series spectroscopy of BPM 37093 with Gemini in the Northern Spring of 2014. We present our preliminary results from these data along with those from the accompanying time series photometric observations we gathered from Mt. John (New Zealand), South African Astronomical Observatory (SAAO), Panchromatic Robotic optical Monitoring and Polarimetry Telescopes (PROMPT) in Chile, and Complejo Astronomico El Leoncito (Argentina) to support the Gemini observations.

  18. Non-LTE Inversion of Spectropolarimetric and Spectroscopic Observations of a Small Active-region Filament Observed at the VTT

    NASA Astrophysics Data System (ADS)

    Schwartz, P.; Balthasar, H.; Kuckein, C.; Koza, J.; Gömöry, P.; Rybák, J.; Kučera, A.; Heinzel, P.

    2016-04-01

    An active region mini-filament was observed by VTT simultaneously in the HeI 10 830 Å triplet by the TIP 1 spectropolarimeter, in Hα by the TESOS Fabry-Pérot interferometer, and in Ca II 8542 Å by the VTT spectrograph. The spectropolarimetric data were inverted using the HAZEL code and Hα profiles were modelled solving a NLTE radiative transfer in a simple isobaric and isothermal 2D slab irradiated both from bottom and sides. It was found that the mini-filament is composed of horizontal fluxtubes, along which the cool plasma of T˜10 000 K can flow by very large - even supersonic - velocities.

  19. Spectroscopic observations of the Uranus' satellite Miranda in Near-IR

    NASA Astrophysics Data System (ADS)

    Gourgeot, F.; Dumas, C.; Merlin, F.; Vernazza, P.; Alvarez-Candal, A.

    2013-09-01

    We present new Near-IR spectra of the Uranus' icy satellite Miranda. This body is probably the most remarkable of all satellites of Uranus, displaying series of surface features such as faults, craters and largescale upwelling, remnant of a geologically very active past. The observations were performed first at the Palomar Observatory with the PHARO instrument (Palomar High Angular Resolution Observer) and then at the Mauna Kea Observatory with SpeX instrument based on the IRTF (Infra-Red Telescope Facility). Water ice is clearly visible in K-band (large 2.0 μm absorption band) and crystalline water ice (at 1.65 μm) seems to cover the most part of the satellite's surface. We focused the study in H band on the 1.42-1.72 μm range at observations dates corresponding to the leading and trailing hemispheres of Miranda. Contrary to the other outer Uranus' moons (Grundy et al. 2006), we did not found any significative differences between both hemispheres in this spectral range. We also studied the possible presence of volatiles like ammonia hydrate and do not exclude the possible presence of a tiny 2.22 μm band yet observed by Bauer et al. 2002. No significant features of carbon dioxide were identified on any spectra. We performed spectral models, based on bi-hemispherical reflectance theory (Hapke 1993) in order to obtain more details on the chemical compounds possibly present on the surface of this Uranian satellite.

  20. Inferential monitoring of chlorinated solvents through Raman spectroscopic observation of the vibrational modes of water.

    PubMed

    Sinfield, Joseph V; Monwuba, Chike

    2016-02-01

    Recent improvements in diode laser, fiber optic, and data acquisition technology have rejuvenated interest in field applications of Raman spectroscopy in a wide range of settings. One such application involves the observation of chlorinated solvents to facilitate the practice of "monitored natural attenuation." In this context, this manuscript focuses on means to improve the sensitivity of in-situ Raman analysis of chlorinated solvents. In particular, the work explores the performance limits of a Time-Resolved Raman Spectroscopy (TRRS) system employed to observe chlorinated solvents in aqueous samples via laboratory tests conducted on both liquid standards of trichloroethylene (TCE) and simulated biodegraded field samples. Quantitative assessment of TCE in solution is carried out through both direct observation of TCE Raman functional groups (381 cm(-1) (δ skeletal), 840 cm(-1) (νCCl) and 1242 cm(-1) (δCH)) and indirect observation of the broad OH stretching (2700-3800 cm(-1)) Raman modes of water. Results from tests on simple solutions show that the TRRS system can detect TCE at aqueous concentrations as low as 70 ppm by directly monitoring the 381 cm(-1) TCE line, whereas observation of the OH stretching line of water (3393 cm(-1)) provides an indirect indication of TCE presence with nearly a 9× improvement in detection level. This unique and counterintuitive mechanism to detect the presence of chlorinated compounds in solution takes advantage of the influence of chlorine on the vibrational modes of water. This influence, which is believed to be attributed to the formation of hydrogen bonds and their resultant interactions with the solvation shell, may serve as a more sensitive and robust indication of the presence of aggregate chlorinated solvent contamination in aqueous systems. Tests performed on simulated biodegraded field samples demonstrate that the indirect detection mechanism is apparent even in complex samples representative of typical field

  1. The composition of M-type asteroids II: Synthesis of spectroscopic and radar observations

    NASA Astrophysics Data System (ADS)

    Neeley, J. R.; Clark, B. E.; Ockert-Bell, M. E.; Shepard, M. K.; Conklin, J.; Cloutis, E. A.; Fornasier, S.; Bus, S. J.

    2014-08-01

    This work updates and expands on results of our long-term radar-driven observational campaign of main-belt asteroids (MBAs) focused on Bus-DeMeo Xc- and Xk-type objects (Tholen X and M class asteroids) using the Arecibo radar and NASA Infrared Telescope Facilities (Ockert-Bell, M.E., Clark, B.E., Shepard, M.K., Rivkin, A.S., Binzel, R.P., Thomas, C.A., DeMeo, F.E., Bus, S.J., Shah, S. [2008]. Icarus 195, 206-219; Ockert-Bell, M.E., Clark, B.E., Shepard, M.K., Issacs, R.A., Cloutis, E.A., Fornasier, S., Bus, S.J. [2010]. Icarus 210, 674-692; Shepard, M.K. et al. [2008a]. Icarus 193, 20-38; Shepard, M.K. et al. [2008b]. Icarus 195, 184-205; Shepard, M.K. et al. [2010]. Icarus 215, 547-551). Eighteen of our targets were near-simultaneously observed with radar and those observations are described in Shepard et al. (Shepard, M.K. et al. [2010]. Icarus 215, 547-551). We combine our near-infrared data with available visible wavelength data for a more complete compositional analysis of our targets. Compositional evidence is derived from our target asteroid spectra using two different methods, a χ2 search for spectral matches in the RELAB database and parametric comparisons with meteorites. We present four new methods of parametric comparison, including discriminant analysis. Discriminant analysis identifies meteorite type with 85% accuracy. This paper synthesizes the results of these two analog search algorithms and reconciles those results with analogs suggested from radar data (Shepard, M.K. et al. [2010]. Icarus 215, 547-551). We have observed 29 asteroids, 18 in conjunction with radar observations. For eighteen out of twenty-nine objects observed (62%) our compositional predictions are consistent over two or more methods applied. We find that for our Xc and Xk targets the best fit is an iron meteorite for 34% of the samples. Enstatite chondrites were best fits for 6 of our targets (21%). Stony-iron meteorites were best fits for 2 of our targets (7%). A discriminant

  2. Evidence for CO in Jupiter's atmosphere from airborne spectroscopic observations at 5 microns

    NASA Technical Reports Server (NTRS)

    Larson, H. P.; Fink, U.; Treffers, R. R.

    1978-01-01

    High-altitude (12.4 km) spectra of Jupiter recorded at the Kuiper Airborne Observatory are analyzed for the presence of CO absorption lines. A line-by-line comparison of Jupiter's spectrum with that of carbon monoxide is presented, as well as a correlation analysis that includes the influence of other gases present in Jupiter's atmosphere (CH4, NH3, H2O, PH3, and GeH4). The resulting evidence points strongly to the presence of carbon monoxide in Jupiter's atmosphere, thus strengthening Beer's evidence for it. Possible explanations for the existence and observability of Jovian CO, including convection from hotter, deeper layers or decomposition of organic molecules, are explored. A recent suggestion that the Jovian CO is restricted to stratospheric levels is not supported by the observations.

  3. SPECTROSCOPIC OBSERVATIONS OF PLANETARY NEBULAE IN THE NORTHERN SPUR OF M31

    SciTech Connect

    Fang, X.; Liu, X.-W.; Zhang, Y.; Garcia-Benito, R.

    2013-09-10

    We present spectroscopy of three planetary nebulae (PNe) in the Northern Spur of the Andromeda galaxy (M31) obtained with the Double Spectrograph on the 5.1 m Hale Telescope at the Palomar Observatory. The samples were selected from the observations of Merrett et al. Our purpose is to investigate the formation of the substructures of M31 using PNe as a tracer of chemical abundances. The [O III] {lambda}4363 line is detected in the spectra of two objects, enabling temperature determinations. Ionic abundances are derived from the observed collisionally excited lines, and elemental abundances of nitrogen, oxygen, neon, sulfur, and argon are estimated. We study the correlations between oxygen and the {alpha}-element abundance ratios using our sample and the M31 disk and bulge PNe from the literature. In one of the three PNe, we observed a relatively higher oxygen abundance compared to the disk sample of M31 at similar galactocentric distances. The results of at least one of the three Northern Spur PNe might be in line with the proposed possible origin of the Northern Spur substructure of M31, i.e., the Northern Spur is connected to the Southern Stream and both substructures comprise the tidal debris of the satellite galaxies of M31.

  4. Impact of Spectroscopic Line Parameters on Carbon Monoxide Column Density Retrievals from Shortwave Infrared Nadir Observations

    NASA Astrophysics Data System (ADS)

    Schmidt, Denise; Gimeno Garcia, Sebastian; Schreier, Franz; Lichtenberg, Gunter

    2015-06-01

    Among the various input data required for the retrieval of atmospheric state parameters from infrared remote sensing observations molecular spectroscopy line data have a central role, because their quality is critical for the quality of the final product. Here we discuss the impact of the line parameters on vertical column densities (VCD) estimated from short wave infrared nadir observations. Using BIRRA (the Beer InfraRed Retrieval Algorithm) comprising a line-by-line radiative transfer code (forward model) and a separable nonlinear least squares solver for inversion we retrieve carbon monoxide from observations of SCIAMACHY aboard Envisat. Retrievals using recent versions of HITRAN und GEISA have been performed and the results are compared in terms of residual norms, molecular density scaling factors, their corresponding errors, and the final VCD product. The retrievals turn out to be quite similar for all three databases, so a definite recommendation in favor of one of these databases is difficult for the considered spectral range around 2:3 μm . Nevertheless, HITRAN 2012 appears to be advantageous when evaluating the different quality criteria.

  5. The composition of M-type asteroids: Synthesis of spectroscopic and radar observations

    NASA Astrophysics Data System (ADS)

    Ockert-Bell, M. E.; Clark, B. E.; Shepard, M. K.; Isaacs, R. A.; Cloutis, E. A.; Fornasier, S.; Bus, S. J.

    2010-12-01

    We have conducted a radar-driven observational campaign of 22 main-belt asteroids (MBAs) focused on Bus-DeMeo Xc- and Xk-type objects (Tholen X and M class asteroids) using the Arecibo radar and NASA Infrared Telescope Facilities (IRTF). Sixteen of our targets were near-simultaneously observed with radar and those observations are described in a companion paper (Shepard, M.K., and 19 colleagues [2010]. Icarus, in press). We find that most of the highest metal-content asteroids, as suggested by radar, tend to exhibit silicate absorption features at both 0.9 and 1.9 μm, and the lowest metal-content asteroids tend to exhibit either no bands or only the 0.9 μm band. Eleven of the asteroids were observed at several rotational longitudes in the near-infrared and significant variations in continuum slope were found for nine in the spectral regions 1.1-1.45 μm and 1.6-2.3 μm. We utilized visible wavelength data (Bus, S.J., Binzel, R.P. [2002b]. Icarus 158, 146-177; Fornasier, S., Clark, B.E., Dotto, E., Migliorini, A., Ockert-Bell, M., Barucci, M.A. [2010]. Icarus 210, 655-673.) for a more complete compositional analysis of our targets. Compositional evidence is derived from our target asteroid spectra using two different methods: (1) a χ2 search for spectral matches in the RELAB database, and (2) parametric comparisons with meteorites. This paper synthesizes the results of the RELAB search and the parametric comparisons with compositional suggestions based on radar observations. We find that for six of the seven asteroids with the highest iron abundances, our spectral results are consistent with the radar evidence (16 Psyche, 216 Kleopatra, 347 Pariana, 758 Mancunia, 779 Nina, and 785 Zwetana). Three of the seven asteroids with the lowest metal abundances, our spectral results are consistent with the radar evidence (21 Lutetia, 135 Hertha, 497 Iva). The remaining seven asteroids (22 Kalliope, 97 Klotho, 110 Lydia, 129 Antigone, 224 Oceana, 678 Fredegundis, and 771

  6. In Situ Spectroscopic Observation of Activation and Transformation of Tantalum Suboxides

    SciTech Connect

    Wang, Ke; Liu, Zhi; Cruz, Tirma Herranz; Salmeron, Miquel; Liang, Hong

    2009-12-16

    Using ambient pressure X-ray Photoelectron Spectroscopy (AP-XPS), we were able to observe the process of oxidation of tantalum with different morphological parameters. Being able to trace surface evolution during oxidation, we evaluated activation energy of oxidation under the influence of strain and grain boundaries. It was found that the metal oxidized through three different stages and there was a transition stage where the phase transformation from suboxides to the equilibrium state of pentoxide. The applied stress and surface defects reduced the activation energy oxidation.

  7. SULFUR CHEMISTRY. Gas phase observation and microwave spectroscopic characterization of formic sulfuric anhydride.

    PubMed

    Mackenzie, Rebecca B; Dewberry, Christopher T; Leopold, Kenneth R

    2015-07-01

    We report the observation of a covalently bound species, formic sulfuric anhydride (FSA), that is produced from formic acid and sulfur trioxide under supersonic jet conditions. FSA has been structurally characterized by means of microwave spectroscopy and further investigated by using density functional theory and ab initio calculations. Theory indicates that a π2 + π2 + σ2 cycloaddition reaction between SO3 and HCOOH is a plausible pathway to FSA formation and that such a mechanism would be effectively barrierless. We speculate on the possible role that FSA may play in the Earth's atmosphere. PMID:26138972

  8. High-dispersion Spectroscopic Observations Of 8P/Tuttle With VLT/CRIRES

    NASA Astrophysics Data System (ADS)

    Kobayashi, Hitomi; Bockelee-Morvan, D.; Dello Russo, N.; Kawakita, H.; Verback, R. J.; Weaver, H.; Jehin, E.; Manfroid, J.; Smette, A.; Cochran, A.; Hutsemekers, D.; Schulz, R.; Stuwe, J.; Weiler, M.; Zucconi, J.; Arpigny, C.; Biver, N.; Crovisier, J.; Magain, P.; Rauer, H.; Sana, H.

    2008-09-01

    We present near-infrared observations of organic molecules in comet 8P/Tuttle. Comet 8P/Tuttle is a Halley-type comet and its last perihelion was in early January 2008. Our observations were carried out on January 28 and February 4 using CRIRES (CRyogenic high-resolution InfraRed Echelle Spectrograph) at the Very Large Telescope (VLT). We used a 0.2" slit which provided a spectral resolving power of 80,000. We detected H2O, OH, HCN, C2H2 on Jan 28, and H2O, OH, CH4, C2H6, and CH3OH on Feb 4. We find that 8P/Tuttle is depleted in HCN, C2H2 and C2H6 relative to H2O compared with most other Oort cloud comets studied to date. Perhaps these depletions suggest that 8P/Tuttle formed in a different region from most Oort cloud comets, but it is also possible that the depletions are caused by repeated passages through the inner solar system.

  9. The "Cool Algol" BD+05 706 : Photometric observations of a new eclipsing double-lined spectroscopic binary

    NASA Astrophysics Data System (ADS)

    Marschall, L. A.; Torres, G.; Neuhauser, R.

    1998-05-01

    BVRI Observations of the star BD+05 706, carried out between January, 1997, and April 1998 using the 0.4m reflector and Photometrics CCD camera at the Gettysburg College Observatory, show that the star is an eclipsing binary system with a light curve characteristic of a class of semi-detached binaries known as the "cool Algols". These results are in good agreement with the previous report of BD+05 706 as a cool Algol by Torres, Neuhauser, and Wichmann,(Astron. J., 115, May 1998) who based their classification on the strong X-ray emission detected by Rosat and on a series of spectroscopic observations of the radial velocities of both components of the system obtained at the Oak Ridge Observatory, the Fred L. Whipple Observatory, and the Multiple Mirror Telescope. Only 10 other examples of cool Algols are known, and the current photometric light curve, together with the radial velocity curves obtained previously, allows us to derive a complete solution for the physical parameters of each component, providing important constraints on models for these interesting systems.

  10. Imaging and spectroscopic observations of a filament channel and the implications for the nature of counter-streamings

    SciTech Connect

    Chen, P. F.; Fang, C.; Harra, L. K.

    2014-03-20

    The dynamics of a filament channel are observed with imaging and spectroscopic telescopes before and during the filament eruption on 2011 January 29. The extreme ultraviolet (EUV) spectral observations reveal that there are no EUV counterparts of the Hα counter-streamings in the filament channel, implying that the ubiquitous Hα counter-streamings found by previous research are mainly due to longitudinal oscillations of filament threads, which are not in phase between each other. However, there exist larger-scale patchy counter-streamings in EUV along the filament channel from one polarity to the other, implying that there is another component of unidirectional flow (in the range of ±10 km s{sup –1}) inside each filament thread in addition to the implied longitudinal oscillation. Our results suggest that the flow direction of the larger-scale patchy counter-streaming plasma in the EUV is related to the intensity of the plage or active network, with the upflows being located at brighter areas of the plage and downflows at the weaker areas. We propose a new method to determine the chirality of an erupting filament on the basis of the skewness of the conjugate filament drainage sites. This method suggests that the right-skewed drainage corresponds to sinistral chirality, whereas the left-skewed drainage corresponds to dextral chirality.

  11. Spectroscopic observation of jet-cooled 2,5-dichlorobenzyl radical generated by corona discharge

    NASA Astrophysics Data System (ADS)

    Yi, Eun Hye; Yoon, Young Wook; Lee, Sang Kuk

    2014-07-01

    Vibronically excited but jet-cooled 2,5-dichlorobenzyl radical was generated from 2,5-dichlorotoluene precursor in a large excess of helium carrier gas, from which the visible vibronic emission spectrum was recorded. From an analysis of the spectrum observed, it was found that the origin band shows larger shift to red than those expected from mono-substitutions, which has been discussed in terms of orientation of substituents. Also, the electronic energy of the D1 → D0 transition and vibrational mode frequencies at the ground electronic state of the 2,5-dichlorobenzyl radical were determined in comparison with the known vibrational data of precursor and ab initio calculations.

  12. Spectroscopic Observation of Resonant Electric Dipole-Dipole Interactions between Cold Rydberg Atoms

    NASA Astrophysics Data System (ADS)

    Afrousheh, K.; Bohlouli-Zanjani, P.; Vagale, D.; Mugford, A.; Fedorov, M.; Martin, J. D.

    2004-11-01

    Resonant electric dipole-dipole interactions between cold Rydberg atoms were observed using microwave spectroscopy. Laser-cooled 85Rb atoms in a magneto-optical trap were optically excited to 45d5/2 Rydberg states using a pulsed laser. A microwave pulse transferred a fraction of these Rydberg atoms to the 46p3/2 state. A second microwave pulse then drove atoms in the 45d5/2 state to the 46d5/2 state, and was used as a probe of interatomic interactions. The spectral width of this two-photon probe transition was found to depend on the presence of the 46p3/2 atoms, and is due to the resonant electric dipole-dipole interaction between 45d5/2 and 46p3/2 Rydberg atoms.

  13. Extreme-Ultraviolet Spectroscopic Observation of Direct Coronal Heating During a C-Class Solar Flare

    NASA Technical Reports Server (NTRS)

    Brosius, Jeffrey W.

    2012-01-01

    With the Coronal Diagnostic Spectrometer operating in rapid cadence (9.8 s) stare mode during a C6.6 flare on the solar disk, we observed a sudden brightening of Fe xix line emission (formed at temperature T ˜ 8 MK) above the pre-flare noise without a corresponding brightening of emission from ions formed at lower temperatures, including He i (0.01 MK), Ov (0.25 MK), and Si xii (2 MK). The sudden brightening persisted as a plateau of Fe xix intensity that endured more than 11 minutes. The Fe xix emission at the rise and during the life of the plateau showed no evidence of significant bulk velocity flows, and hence cannot be attributed to chromospheric evaporation. However, the line width showed a significant broadening at the rise of the plateau, corresponding to nonthermal velocities of at least 89 km s-1 due to reconnection outflows or turbulence. During the plateau He i, Ov, and Si xii brightened at successively later times starting about 3.5 minutes after Fe xix, which suggests that these brightenings were produced by thermal conduction from the plasma that produced the Fe xix line emission; however, we cannot rule out the possibility that they were produced by a weak beam of nonthermal particles. We interpret an observed shortening of the Ov wavelength for about 1.5 minutes toward the middle of the plateau to indicate new upward motions driven by the flare, as occurs during gentle chromospheric evaporation; relative to a quiescent interval shortly before the flare, the Ov upward velocity was around -10 km s-1.

  14. Herschel spectroscopic observations of Zw 049.057 and Arp 299

    NASA Astrophysics Data System (ADS)

    Falstad, Niklas; Aalto, Susanne; González-Alfonso, Eduardo

    2015-08-01

    Luminous infrared galaxies (LIRGs) are extreme examples of star-forming galaxies or galaxies with active galactic nuclei (AGN), often interacting or merging systems, whose high infrared luminosities are powered by their intense star formation or AGN activity. Through studying molecular species that are mainly excited by warm dust emission (i.e. OH, H2O) it is possible to probe the nuclear source of far-IR radiation and gain insights in its physical conditions and chemistry.We present the results and analysis of Herschel observations of the compact obscured nucleus in the extremely H2O luminous LIRG Zw 049.057. We model the H2O and OH lines and continuum using a spherically symmetric radiative transfer code. We find that the far-IR absorption lines are primarily formed in a Compton-thick warm (Tdust>100 K) core with high columns of H2O and OH (similar to the nuclear regions of the ULIRG Arp 220). We also find an enhancement of 18O in the core component, suggesting that the ISM has been enriched by ejecta from massive stars.One of the low excited H2O lines exhibit an emission feature extending up to 500 km/s, suggesting an outflow. At the same time, we find a prominent infall signature in the [O I] 63 µm line, implying that the gas reservoir in the central region of Zw 049.057 is being replenished. The presence of both outflowing and infalling gas suggests that the nucleus is in a state of rapid evolution.We also present observations of the luminous merger Arp 299. This is another source with prominent H2O and OH lines, but preliminary results suggest that its nuclear activity is in a different evolutionary state compared to Zw 049.057.

  15. SHRINE: Enabling Nationally Scalable Multi-Site Disease Studies

    PubMed Central

    McMurry, Andrew J.; Murphy, Shawn N.; MacFadden, Douglas; Weber, Griffin; Simons, William W.; Orechia, John; Bickel, Jonathan; Wattanasin, Nich; Gilbert, Clint; Trevvett, Philip; Churchill, Susanne; Kohane, Isaac S.

    2013-01-01

    Results of medical research studies are often contradictory or cannot be reproduced. One reason is that there may not be enough patient subjects available for observation for a long enough time period. Another reason is that patient populations may vary considerably with respect to geographic and demographic boundaries thus limiting how broadly the results apply. Even when similar patient populations are pooled together from multiple locations, differences in medical treatment and record systems can limit which outcome measures can be commonly analyzed. In total, these differences in medical research settings can lead to differing conclusions or can even prevent some studies from starting. We thus sought to create a patient research system that could aggregate as many patient observations as possible from a large number of hospitals in a uniform way. We call this system the ‘Shared Health Research Information Network’, with the following properties: (1) reuse electronic health data from everyday clinical care for research purposes, (2) respect patient privacy and hospital autonomy, (3) aggregate patient populations across many hospitals to achieve statistically significant sample sizes that can be validated independently of a single research setting, (4) harmonize the observation facts recorded at each institution such that queries can be made across many hospitals in parallel, (5) scale to regional and national collaborations. The purpose of this report is to provide open source software for multi-site clinical studies and to report on early uses of this application. At this time SHRINE implementations have been used for multi-site studies of autism co-morbidity, juvenile idiopathic arthritis, peripartum cardiomyopathy, colorectal cancer, diabetes, and others. The wide range of study objectives and growing adoption suggest that SHRINE may be applicable beyond the research uses and participating hospitals named in this report. PMID:23533569

  16. A Mixed Methods Sampling Methodology for a Multisite Case Study

    ERIC Educational Resources Information Center

    Sharp, Julia L.; Mobley, Catherine; Hammond, Cathy; Withington, Cairen; Drew, Sam; Stringfield, Sam; Stipanovic, Natalie

    2012-01-01

    The flexibility of mixed methods research strategies makes such approaches especially suitable for multisite case studies. Yet the utilization of mixed methods to select sites for these studies is rarely reported. The authors describe their pragmatic mixed methods approach to select a sample for their multisite mixed methods case study of a…

  17. The Role of Involvement and Use in Multisite Evaluations

    ERIC Educational Resources Information Center

    Lawrenz, Frances; King, Jean A.; Ooms, Ann

    2011-01-01

    A cross-case analysis of four National Science Foundation (NSF) case studies identified both unique details and common themes related to promoting the use and influence of multisite evaluations. The analysis provided evidence of diverse evaluation use by stakeholders and suggested that people taking part in the multisite evaluations perceived…

  18. Building a Community of Evaluation Practice within a Multisite Program

    ERIC Educational Resources Information Center

    Goodyear, Leslie K.

    2011-01-01

    New and novel uses of evaluation processes and findings are possible when a community of practice develops as evaluation stakeholders participate in multisite evaluations in multiple ways. Developing such communities takes advantage of what makes multisite evaluations special. This chapter uses the example of the Innovative Technology Experiences…

  19. OH populations and temperatures from simultaneous spectroscopic observations of 25 bands

    NASA Astrophysics Data System (ADS)

    Noll, S.; Kausch, W.; Kimeswenger, S.; Unterguggenberger, S.; Jones, A. M.

    2015-04-01

    OH rotational temperatures are widely used to derive mesopause temperatures and their variations. Since most data sets are only based on a fixed set of lines of a single band, it is important to know possible systematic uncertainties related to the choice of lines. Therefore, a comprehensive study of as many OH bands as possible is desirable. For this purpose, astronomical echelle spectrographs at large telescopes are the most suitable instruments. They offer a wide wavelength coverage, relatively high spectral resolution, and high sensitivity. Moreover, since each ground-based astronomical observation has an imprint of the Earth's atmosphere, the data archives of large astronomical facilities are a treasure for atmospheric studies. For our project, we used archival data of the medium-resolution X-shooter echelle spectrograph operated by the European Southern Observatory at Cerro Paranal in Chile. The instrument can simultaneously observe all OH bands that are accessible from ground. We reduced and analysed a set of 343 high-quality spectra taken between 2009 and 2013 to measure OH line intensities and to derive rotational and vibrational temperatures of 25 bands between 0.58 and 2.24 μm. We studied the influence of the selected line set, OH band, upper vibrational level v', and the molecular data on the derived level populations and temperatures. The rotational temperature results indicate differences by several degrees depending on the selection. The temperatures for bands of even and odd v' show deviations which increase with v'. A study of the temporal variations revealed that the nocturnal variability pattern changes for v' from 2 to 9. In particular, the spread of temperatures tends to increase during the night, and the time of the minimum temperature depends on v'. The vibrational temperatures depend on the range of v' used for their determination, since the higher vibrational levels from 7 to 9 seem to be overpopulated compared to the lower levels. The

  20. Direct spectroscopic observation of multiple-charged-ion acceleration by an intense femtosecond-pulse laser.

    PubMed

    Zhidkov, A G; Sasaki, A; Tajima, T; Auguste, T; D'Olivera, P; Hulin, S; Monot, P; Faenov, A Y; Pikuz, T A; Skobelev, I Y

    1999-09-01

    We have observed evidence of the emission of energetic He-and H-like ions of fluorine more than 1 MeV produced via the optical field ionization (OFI) from a solid target irradiated by an intense I=(2-4)x10(18) W/cm(2) (60 fs, lambda=800 nm), obliquely incident p-polarized pulse laser. The measured blue wing of He(alpha), He(beta), and Ly(alpha) lines of fluorine shows a feature of the Doppler-shifted spectrum due to the self-similar ion expansion dominated by superthermal electrons with the temperature T(h) approximately 100 keV. Using a collisional particle-in-cell simulation, which incorporates the nonlocal-thermodynamic-equilibrium ionization including OFI, we have obtained the plasma temperature, line shape, and maximal energy of accelerated ions, which agree well with those determined from the experimental spectra. The red wing of ion spectra gives the temperature of bulk plasma electrons. PMID:11970139

  1. Spectroscopic Coronal Observations During the Total Solar Eclipse of 11 July 2010

    NASA Astrophysics Data System (ADS)

    Voulgaris, A. G.; Gaintatzis, P. S.; Seiradakis, J. H.; Pasachoff, J. M.; Economou, T. E.

    2012-05-01

    The flash spectra of the solar chromosphere and corona were measured with a slitless spectrograph before, after, and during the totality of the solar eclipse of 11 July 2010, at Easter Island, Chile. This eclipse took place at the beginning of Solar Cycle 24, after an extended minimum of solar activity. The spectra taken during the eclipse show a different intensity ratio of the red and green coronal lines compared with those taken during the total solar eclipse of 1 August 2008, which took place toward the end of Solar Cycle 23. The characteristic coronal emission line of forbidden Fe xiv (5303 Å) was observed on the east and west solar limbs in four areas relatively symmetrically located with respect to the solar rotation axis. Subtraction of the continuum flash-spectrum background led to the identification of several extremely weak emission lines, including forbidden Ca xv (5694 Å), which is normally detected only in regions of very high excitation, e.g., during flares or above large sunspots. The height of the chromosphere was measured spectrophotometrically, using spectral lines from light elements and compared with the equivalent height of the lower chromosphere measured using spectral lines from heavy elements.

  2. High-Dispersion Spectroscopic Observations of Comet C/2012 S1 (ISON) with the Subaru Telescope

    NASA Astrophysics Data System (ADS)

    Shinnaka, Yoshiharu; Kawakita, Hideyo; Nagashima, Masayoshi; Hitomi, Kobayashi; Decock, Alice; Jehin, Emmanuel; Boice, Daniel C.

    2014-11-01

    Comet C/2012 S1 (ISON) was one of the Oort cloud comets and dynamically new. This comet was broken at its perihelion passage on UT 2013 November 28.1 (at Rh ~ 17 solar radius). We observed the comet C/2012 S1 (ISON) on UT 2013 November 15 with the High Dispersion Spectrograph (HDS) mounted on the Subaru Telescope atop Mauna Kea, Hawaii. Its heliocentric and geocentric distances were 0.601 and 0.898 AU, respectively. We selected the slit size of 0”.5 x 9”.0 on the sky to achieve the spectral resolution of R = 72,000 from 550 to 830 nm. The total exposure time of comet C/2012 S1 (ISON) was 1200 seconds. We detected many emission lines caused from radicals (e.g., CN, C2, NH2), ions (H2O+), atoms ([OI] and Na I) and also many unidentified lines in the spectra. We report the (1) the ortho-to-para abundance ratios (OPRs) of water and ammonia estimated from the high-dispersion spectra of H2O+ and NH2, (2) the green-to-red line ratio of forbidden oxygen emissions, (3) the isotopic ratios of C2 (the carbon isotopic ratio from Swan band) and CN (the carbon and nitrogen isotopic ratios from red band), (4) the sodium-to-continuum ratio of comet C/2012 S1 (ISON).

  3. Direct spectroscopic observation of ion deceleration accompanying laser plasma-wall interaction

    NASA Astrophysics Data System (ADS)

    Renner, O.; Krouský, E.; Liska, R.; Šmíd, M.; Larroche, O.; Dalimier, E.; Rosmej, F. B.

    2010-08-01

    Interactions of plasma jets with solid surfaces are extensively studied in context with development of future fusion devices. In experiments carried out on the iodine laser system PALS, the energetic ions were produced at double-foil Al/Mg targets irradiated by one or two counter-propagating laser beams. The plasma jets from the rear surface of the laser-exploded Al foil streamed towards the Mg target representing the wall preheated by the action of the high-energy photons, particle and/or laser beams. Instead of being trapped by the cold secondary-target material, the forward-accelerated Al ions collided with the counter-propagating matter ejected from the wall. The environmental conditions in near-wall plasmas were analyzed with the high-resolution x-ray spectroscopy and temporally-resolved x-ray imaging. The deceleration of the incident Al ions in the near-wall region was directly observed and quantitatively characterized via Doppler shifts of the J-satellite from the Al Lya spectral group. The interaction scenario was modelled using the 2D arbitrary Lagrangian Eulerian hydrocode PALE and the multifluid code MULTIF.

  4. A multisite validity study of self-reported anesthesia outcomes.

    PubMed

    Walker, Peter; Pekmezaris, Renee; Lesser, Martin L; Nouryan, Christian N; Rosinia, Frank; Pratt, Kathy; LaVopa, Catherine

    2012-01-01

    The purpose of this study was to assess the validity of a multisite anesthesia voluntary adverse event reporting process. A data validation methodology was used through medical chart review on live records at 3 facilities (N = 600). The per-item aggregated error rate among all 42 data items was 0.3%: 0.1% for quality indicators, 1.3% for demographic/status variables, and 1.7% for administrative items. The per-patient error rate among all 42 data items was 6.3%: 3.0% for quality indicators, 1.7% for demographic/status variables, and 3.0% for administrative items. Trends such as better accuracy for more serious events continue, but observed error rates were lower than those found in previous surveys-an indication that, while further study is needed, nonpunitive voluntary reporting may reduce errors in anesthesia care. PMID:22326979

  5. Spectroscopic properties of explosive volcanism within the Caloris basin with MESSENGER observations

    NASA Astrophysics Data System (ADS)

    Besse, S.; Doressoundiram, A.; Benkhoff, J.

    2015-12-01

    Volcanism on Mercury has been indisputably identified at various locations on the surface, by means of both effusive and explosive volcanism. Its characterization is crucial to understand the evolution of the planet, in particular the thermal evolution of the mantle, and the volatile content of the planet. This analysis presents a detailed view of the pyroclastic deposits of the Caloris basin. Observations from the Mercury Atmospheric and Surface Composition Spectrometer (MASCS) are used to understand the spectral characteristics of the pyroclastic deposits, both in the visible and near-infrared. Additional calibration steps are proposed to reconcile the difference of absolute reflectance between the visible (VIS) and near-infrared (NIR) detectors. These calibration steps allow the use of the full spectral range of the MASCS instrument. Pyroclastic deposits exhibit a redder spectral slope in the VIS and NIR. This spectral slope diminishes toward the edge of the deposits to match that of Mercury's average surface. Spectral properties in the ultraviolet (UV) also change as a function of distance to the vent. Only the UV properties unambiguously separate the pyroclastic deposits from Mercury's average spectra. The spectral variations are consistent with a lower iron content of the pyroclastic deposits with respect to the average surface of Mercury, similar to what has been proposed for pyrolcastic deposits on the lunar surface. Nonetheless, given the limited illumination conditions diversity of the MASCS instrument, other causes such as grain size, space weathering, and bulk composition could also be accounted for the spectral variations. Variability of the pyroclastic deposits' properties within the entire basin are potentially identified between the three main clusters, and could be related to space weathering of deposits of different ages.

  6. X-Ray Spectroscopic Observations with ASCA and BeppoSAX

    NASA Astrophysics Data System (ADS)

    Kaastra, J. S.

    Introduction X-ray spectroscopy The ASCA and BeppoSAX missions The most prominent spectral features observable with ASCA and - BeppoSAX A Few Notes on Spectral Data Fitting Introduction Data binning Model binning Calibration uncertainties Spectral deconvolution Statistics Low count rates Data presentation Plasma models Stellar Coronae Introduction Differential emission measure distribution techniques Temperature structure Abundances Flares Stellar evolution Hot Stars Introduction Normal O and B stars Luminous blue variables Wolf-Rayet stars Protostars and T Tauri Stars Introduction X-ray emission from protostars X-ray emission from T Tauri stars Cataclysmic Variables Introduction Non-magnetic cataclysmic variables Intermediate polars Polars High-Mass X-Ray Binaries Introduction Vela X-1 Cyg X-3 Cen X-3 SS 433 Other cases Low-Mass X-Ray Binaries Introduction 4U 1626-67 Cir X-1 Supernova Remnants Introduction Oxygen-ricg remnats: Cas A Young type Ia remnants Old shell-like remnants Synchrotron X-ray emission from SNRs Crab-like remnants Center-filled thermal remnants Jets interacting with SNRs Isolated pulsars The Magellanic Cloud SNRs Supernova explosions in distant galaxies Extended X-Ray Emission from Normal Galaxies The galactic ridge The galactic center X-ray emission from other normal galaxies Seyfert 1 Galaxies The iron line Warm absorbers The power law component Soft components Low-luminosity AGN Broad-line radio galaxies Seyfert 2 Galaxies Introduction NGC 1068 NGC 6552 NGC 4945 NGC 1808 Other cases Intermediate cases: narrow-line emission galaxies and others Quasars Radio-quiet quasars Radio-loud quasars Type 2 quasars BL Lac objects Clusters of Galaxies Temperature distribtuion of the hot medium The cooling flow and the central temperature distribtuion Mass distribution Groups of galaxies Cluster mergers and dynamical evolution Optical-depth effects The quest for the Hubble constant Abundances in nearby clusters Abundances in distant clusters Abundances

  7. Herschel spectroscopic observations of the compact obscured nucleus in Zw 049.057

    NASA Astrophysics Data System (ADS)

    Falstad, N.; González-Alfonso, E.; Aalto, S.; van der Werf, P. P.; Fischer, J.; Veilleux, S.; Meléndez, M.; Farrah, D.; Smith, H. A.

    2015-08-01

    Context. The luminous infrared galaxy Zw 049.057 contains a compact obscured nucleus where a considerable amount of the galaxy's luminosity is generated. This nucleus contains a dusty environment that is rich in molecular gas. One approach to probing this kind of environment and to revealing what is hidden behind the dust is to study the rotational lines of molecules that couple well with the infrared radiation emitted by the dust. Aims: We probe the physical conditions in the core of Zw 049.057 and establish the nature of its nuclear power source (starburst or active galactic nucleus). Methods: We observed Zw 049.057 with the Photodetector Array Camera and Spectrometer (PACS) and the Spectral and Photometric Imaging Receiver (SPIRE) onboard the Herschel Space Observatory in rotational lines of H2O, H218O, OH, 18OH, and [O I]. We modeled the unresolved core of the galaxy using a spherically symmetric radiative transfer code. To account for the different excitation requirements of the various molecular transitions, we use multiple components and different physical conditions. Results: We present the full high-resolution SPIRE FTS spectrum of Zw 049.057, along with relevant spectral scans in the PACS range. We find that a minimum of two different components (nuclear and extended) are required in order to account for the rich molecular line spectrum of Zw 049.057. The nuclear component has a radius of 10-30 pc, a very high infrared surface brightness (~1014L⊙kpc-2), warm dust (Td > 100 K), and a very large H2 column density (NH2 = 1024-1025 cm-2). The modeling also indicates high nuclear H2O (~5 × 10-6) and OH (~4 × 10-6) abundances relative to H2 as well as a low 16O/18O-ratio of 50-100. We also find a prominent infall signature in the [O I] line. We tentatively detect a 500 km s-1 outflow in the H2O 313 → 202 line. Conclusions: The high surface brightness of the core indicates the presence of either a buried active galactic nucleus or a very dense nuclear

  8. Spectroscopic observation of Lyα emitters at z ∼ 7.7 and implications on re-ionization

    SciTech Connect

    Faisst, A. L.; Carollo, C. M.; Capak, P.; Scarlata, C.; Scoville, N.

    2014-06-10

    We present spectroscopic follow-up observations on two bright Lyα emitter (LAE) candidates originally found by Krug et al. at a redshift of z ∼ 7.7 using the Multi-Object Spectrometer for Infra-Red Exploration at Keck. We rule out any line emission at the >5σ level for both objects, putting on solid ground a previous null result for one of the objects. The limits inferred from the non-detections rule out the previous claim of no or even reversed evolution between 5.7 < z < 7.7 in the Lyα luminosity function (LF) and suggest a drop in the Lyα LF consistent with that seen in Lyman break galaxy (LBG) samples. We model the redshift evolution of the LAE LF using the LBG UV-continuum LF and the observed rest-frame equivalent width distribution. From the comparison of our empirical model with the observed LAE distribution, we estimate lower limits of the neutral hydrogen fraction to be 50%-70% at z ∼ 7.7. Together with this, we find a strong evolution in the Lyα optical depth characterized by (1 + z){sup 2.2} {sup ±} {sup 0.5} beyond z = 6, indicative of a strong evolution of the intergalactic medium. Finally, we extrapolate the LAE LF to z ∼ 9 using our model and show that it is unlikely that large area surveys, like UltraVISTA or Euclid, pick up LAEs at this redshift assuming the current depths and area.

  9. Detection of optical path in spectroscopic space-based observations of greenhouse gases: Application to GOSAT data processing

    NASA Astrophysics Data System (ADS)

    Oshchepkov, Sergey; Bril, Andrey; Maksyutov, Shamil; Yokota, Tatsuya

    2011-07-01

    We present a method to detect optical path modification due to atmospheric light scattering in space-based greenhouse gas spectroscopic sounding. This method, which was applied to the analysis of radiance spectra measured by the Greenhouse Gases Observing Satellite (GOSAT), is based on the path length probability density function (PPDF) and on retrieval of PPDF parameters from radiance spectra in the oxygen A-band of absorption at 0.76 μm. We show that these parameters can be effectively used to characterize the impact of atmospheric light scattering on carbon dioxide retrieval in the atmospheric carbon dioxide (CO2) absorption bands at 1.6 μm and 2.0 μm. The threshold for PPDF parameters is set so that the optical-path modification is negligible, and these settings are recommended as a basic guideline for selecting the clearest atmospheric scenarios. An example of data processing for six global GOSAT repeat cycles in April and July 2009 shows that PPDF-based selection efficiently removes CO2 retrieval biases associated with subvisible cirrus and sandstorm activities.

  10. Polarimetric and spectroscopic optical observations of the ultra-compact X-ray binary 4U 0614+091

    NASA Astrophysics Data System (ADS)

    Baglio, M. C.; Mainetti, D.; D'Avanzo, P.; Campana, S.; Covino, S.; Russell, D. M.; Shahbaz, T.

    2014-12-01

    Aims: We present a polarimetric and spectroscopic study of the persistent ultra-compact X-ray binary 4U 0614+091 aimed at searching for the emission of a relativistic particle jet and at unveiling the orbital period Porb of the system. Methods: We obtained r-band polarimetric observations with the Telescopio Nazionale Galileo (TNG) equipped with the PAOLO polarimeter and with the Nordic Optical Telescope (NOT) equipped with the ALFOSC instrument, covering ~2 h and ~0.5 h observations, respectively. We carried out low resolution spectroscopy of the system using the ESO Very Large Telescope equipped with FORS1 for ~1.5 h (16 spectra covering the range 4300-8000 Å). Results: The polarimetric analysis performed starting from the TNG dataset revealed a polarisation degree in the r-band of 3% ± 1%. From the NOT dataset, due to the lower signal-to-noise ratio, we could obtain only a 3σ upper limit of 3.4%. From the joining of a spectroscopic and photometric analysis, through the study of the equivalent width variations of the CII 7240 Å line and the r-band light curve, we could find a hint of a ~45 min periodicity. Conclusions: A polarisation degree P of ~3% in the r-band is consistent with the emission of a relativistic particle jet, which is supposed to emit intrinsically linearly polarised synchrotron radiation. Since no variations of P with time have been detected, and the accretion disc of the system does not contain ionised hydrogen, scattering by free electrons in the accretion disc has been rejected. The period of ~45 min obtained through the analysis of the system light curve and of the equivalent width variations of the selected spectral line is probably linked to the presence of a hot spot or a superhump in the accretion disc, and lead to an orbital period ≳1 h for the binary system. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto

  11. Spectroscopically resolved far-IR observations of the massive star-forming region G5.89-0.39

    NASA Astrophysics Data System (ADS)

    Leurini, S.; Wyrowski, F.; Wiesemeyer, H.; Gusdorf, A.; Güsten, R.; Menten, K. M.; Gerin, M.; Levrier, F.; Hübers, H. W.; Jacobs, K.; Ricken, O.; Richter, H.

    2015-12-01

    Context. The fine-structure line of atomic oxygen at 63 μm ([OI]63μm) is an important diagnostic tool in different fields of astrophysics: it is for example predicted to be the main coolant in several environments of star-forming regions (SFRs). However, our knowledge of this line relies on observations with low spectral resolution, and the real contribution of each component (photon-dominated region, jet) in the complex environment of SFRs to its total flux is poorly understood. Aims: We investigate the contribution of jet and photon-dominated region emission, and of absorption to the [OI]63μm line towards the hot gas around the ultra-compact Hii region G5.89-0.39 and study the far-IR line luminosity of the source in different velocity regimes through spectroscopically resolved spectra of atomic oxygen, [CII], CO, OH, and H2O. Methods: We mapped G5.89-0.39 in [OI]63μm and in CO(16-15) with the GREAT receiver onboard SOFIA. We also observed the central position of the source in the ground-state OH 2Π3/2 J = 5/2 → J = 3/2 triplet and in the excited OH 2Π1/2 J = 3/2 → J = 1/2 triplets with SOFIA. These data were complemented with APEX CO(6-5) and CO(7-6) maps and with Herschel/HIFI maps and single-pointing observations in lines of [CII], H2O, and HF. Results: The [OI] spectra in G5.89-0.39 are severely contaminated by absorptions from the source envelope and from different clouds along the line of sight. Emission is detected only at high velocities, and it is clearly associated with the compact north-south outflows traced by extremely high-velocity emission in low-J CO lines. The mass-loss rate and the energetics of the jet system derived from the [OI]63μm line agree well with previous estimates from CO, thus suggesting that the molecular outflows in G5.89-0.39 are driven by the jet system seen in [OI]. The far-IR line luminosity of G5.89-0.39 is dominated by [OI] at high-velocities; the second coolant in this velocity regime is CO, while [CII], OH and H2O

  12. Spectroscopic observation of Mars

    NASA Technical Reports Server (NTRS)

    Singer, R. B.

    1985-01-01

    A review is given of what is known about the surface of Mars from reflectance spectroscopy, including some new results and providing an overview of the principles involved. While some form of bound water and/or OH has been known on Mars for many years, a new result presented is the identification of structural OH in a dilute or poorly crystalline magnesian clay. The detection of water ice in the residual north polar cap is noted. Also considered is the role that reflectance spectroscopy will play in the future, from earth and as an important part of the NASA Mars Geosciences/Climatology Orbiter mission.

  13. Far Ultraviolet Spectroscopic Explorer Observations of the Seyfert 1.5 Galaxy NGC 5548 in a Low State

    NASA Technical Reports Server (NTRS)

    Brotherton, M. S.; Green, R. F.; Kriss, G. A.; Oegerle, W.; Kaiser, M. E.; Zheng, W.; Hutchings, J. B.; Fisher, Richard R. (Technical Monitor)

    2001-01-01

    We present far-ultraviolet spectra of the Seyfert 1.5 galaxy NGC 5548 obtained in 2000 June with the Far Ultraviolet Spectroscopic Explorer (FUSE). Our data span the observed wavelength range 915-1185 A at a resolution of approximately 20 km s(exp -1). The spectrum shows a weak continuum and emission from O VI (lambda)(lambda)1032, 1038, C III (lambda)977, and He II (lambda)1085. The FUSE data were obtained when the AGN (Active Galactic Nuclei) was in a low state, which has revealed strong, narrow O VI emission lines. We also resolve intrinsic, associated absorption lines of O VI and the Lyman series. Several distinct kinematic components are present, spanning a velocity range of approximately 0 to -1300 km s(exp -1) relative to systemic, with kinematic structure similar to that seen in previous observations of longer wavelength ultraviolet (UV) lines. We explore the relationships between the far-UV (ultraviolet) absorbers and those seen previously in the UV and X-rays. We find that the high-velocity UV absorption component is consistent with being low-ionization, contrary to some previous claims, and is consistent with its non-detection in high-resolution X-ray spectra. The intermediate velocity absorbers, at -300 to -400 km s(exp -1), show H I and O VI column densities consistent with having contributions from both a high-ionization X-ray absorber and a low-ionization UV absorber. No single far-UV absorbing component can be solely identified with the X-ray absorber.

  14. Long-term dynamics of multisite phosphorylation.

    PubMed

    Rubinstein, Boris Y; Mattingly, Henry H; Berezhkovskii, Alexander M; Shvartsman, Stanislav Y

    2016-07-15

    Multisite phosphorylation cycles are ubiquitous in cell regulation systems and are studied at multiple levels of complexity, from molecules to organisms, with the ultimate goal of establishing predictive understanding of the effects of genetic and pharmacological perturbations of protein phosphorylation in vivo. Achieving this goal is essentially impossible without mathematical models, which provide a systematic framework for exploring dynamic interactions of multiple network components. Most of the models studied to date do not discriminate between the distinct partially phosphorylated forms and focus on two limiting reaction regimes, distributive and processive, which differ in the number of enzyme-substrate binding events needed for complete phosphorylation or dephosphorylation. Here we use a minimal model of extracellular signal-related kinase regulation to explore the dynamics of a reaction network that includes all essential phosphorylation forms and arbitrary levels of reaction processivity. In addition to bistability, which has been studied extensively in distributive mechanisms, this network can generate periodic oscillations. Both bistability and oscillations can be realized at high levels of reaction processivity. Our work provides a general framework for systematic analysis of dynamics in multisite phosphorylation systems. PMID:27226482

  15. Optical Spectroscopic Observations of Gamma-ray Blazar Candidates. V. TNG, KPNO, and OAN Observations of Blazar Candidates of Uncertain Type in the Northern Hemisphere

    NASA Astrophysics Data System (ADS)

    Álvarez Crespo, N.; Masetti, N.; Ricci, F.; Landoni, M.; Patiño-Álvarez, V.; Massaro, F.; D'Abrusco, R.; Paggi, A.; Chavushyan, V.; Jiménez-Bailón, E.; Torrealba, J.; Latronico, L.; La Franca, F.; Smith, Howard A.; Tosti, G.

    2016-02-01

    The extragalactic γ-ray sky is dominated by emission from blazars, a peculiar class of active galactic nuclei. Many of the γ-ray sources included in the Fermi-Large Area Telescope Third Source catalog (3FGL) are classified as blazar candidates of uncertain type (BCUs) because there are no optical spectra available in the literature to confirm their nature. In 2013, we started a spectroscopic campaign to look for the optical counterparts of the BCUs and of the unidentified γ-ray sources to confirm their blazar nature. Whenever possible we also determine their redshifts. Here, we present the results of the observations carried out in the northern hemisphere in 2013 and 2014 at the Telescopio Nazionale Galileo, Kitt Peak National Observatory, and Observatorio Astronómico Nacional in San Pedro Mártir. In this paper, we describe the optical spectra of 25 sources. We confirmed that all of the 15 BCUs observed in our campaign and included in our sample are blazars and we estimated the redshifts for three of them. In addition, we present the spectra for three sources classified as BL Lacs in the literature but with no optical spectra available to date. We found that one of them is a quasar (QSO) at a redshift of z = 0.208 and the other two are BL Lacs. Moreover, we also present seven new spectra for known blazars listed in the Roma-BZCAT that have an uncertain redshift or are classified as BL Lac candidates. We found that one of them, 5BZB J0724+2621, is a “changing look” blazar. According to the spectrum available in the literature, it was classified as a BL Lac, but in our observation we clearly detected a broad emission line that led us to classify this source as a QSO at z = 1.17.

  16. Spectroscopic observations of propagating disturbances in a polar coronal hole: evidence of slow magneto-acoustic waves

    NASA Astrophysics Data System (ADS)

    Gupta, G. R.; Teriaca, L.; Marsch, E.; Solanki, S. K.; Banerjee, D.

    2012-10-01

    Aims: We focus on detecting and studying quasi-periodic propagating features that have been interpreted in terms of both slow magneto-acoustic waves and of high-speed upflows. Methods: We analyzed long-duration spectroscopic observations of the on-disk part of the south polar coronal hole taken on 1997 February 25 by the SUMER spectrometer onboard SOHO. We calibrated the velocity with respect to the off-limb region and obtained time-distance maps in intensity, Doppler velocity, and line width. We also performed a cross-correlation analysis on different time series curves at different latitudes. We studied average spectral line profiles at the roots of propagating disturbances and along the propagating ridges, and performed a red-blue asymmetry analysis. Results: We clearly find propagating disturbances in intensity and Doppler velocity with a projected propagation speed of about 60 ± 4.8 km s-1 and a periodicity of ≈14.5 min. To our knowledge, this is the first simultaneous detection of propagating disturbances in intensity as well as in Doppler velocity in a coronal hole. During the propagation, an intensity enhancement is associated with a blueshifted Doppler velocity. These disturbances are clearly seen in intensity also at higher latitudes (i.e., closer to the limb), while disturbances in Doppler velocity become faint there. The spectral line profiles averaged along the propagating ridges are found to be symmetric, to be well fitted by a single Gaussian, and have no noticeable red-blue asymmetry. Conclusions: Based on our analysis, we interpret these disturbances in terms of propagating slow magneto-acoustic waves.

  17. Latent Variable Regression 4-Level Hierarchical Model Using Multisite Multiple-Cohorts Longitudinal Data. CRESST Report 801

    ERIC Educational Resources Information Center

    Choi, Kilchan

    2011-01-01

    This report explores a new latent variable regression 4-level hierarchical model for monitoring school performance over time using multisite multiple-cohorts longitudinal data. This kind of data set has a 4-level hierarchical structure: time-series observation nested within students who are nested within different cohorts of students. These…

  18. OBSERVING THE FINE STRUCTURE OF LOOPS THROUGH HIGH-RESOLUTION SPECTROSCOPIC OBSERVATIONS OF CORONAL RAIN WITH THE CRISP INSTRUMENT AT THE SWEDISH SOLAR TELESCOPE

    SciTech Connect

    Antolin, P.; Rouppe van der Voort, L. E-mail: v.d.v.l.rouppe@astro.uio.no

    2012-02-01

    Observed in cool chromospheric lines, such as H{alpha} or Ca II H, coronal rain corresponds to cool and dense plasma falling from coronal heights. Considered as a peculiar sporadic phenomenon of active regions, it has not received much attention since its discovery more than 40 years ago. Yet, it has been shown recently that a close relationship exists between this phenomenon and the coronal heating mechanism. Indeed, numerical simulations have shown that this phenomenon is most likely due to a loss of thermal equilibrium ensuing from a heating mechanism acting mostly toward the footpoints of loops. We present here one of the first high-resolution spectroscopic observations of coronal rain, performed with the CRisp Imaging Spectro Polarimeter (CRISP) instrument at the Swedish Solar Telescope. This work constitutes the first attempt to assess the importance of coronal rain in the understanding of the coronal magnetic field in active regions. With the present resolution, coronal rain is observed to literally invade the entire field of view. A large statistical set is obtained in which dynamics (total velocities and accelerations), shapes (lengths and widths), trajectories (angles of fall of the blobs), and thermodynamic properties (temperatures) of the condensations are derived. Specifically, we find that coronal rain is composed of small and dense chromospheric cores with average widths and lengths of {approx}310 km and {approx}710 km, respectively, average temperatures below 7000 K, displaying a broad distribution of falling speeds with an average of {approx}70 km s{sup -1}, and accelerations largely below the effective gravity along loops. Through estimates of the ion-neutral coupling in the blobs we show that coronal rain acts as a tracer of the coronal magnetic field, thus supporting the multi-strand loop scenario, and acts as a probe of the local thermodynamic conditions in loops. We further elucidate its potential in coronal heating. We find that the cooling

  19. Follow-up spectroscopic observations of HD 107148 B: A new white dwarf companion of an exoplanet host star

    NASA Astrophysics Data System (ADS)

    Mugrauer, M.; Dinçel, B.

    2016-07-01

    We report on our follow-up spectroscopy of HD 1071478 B, a recently detected faint co-moving companion of the exoplanet host star HD 107148 A. The companion is separated from its primary star by about 35 arcsec (or 1790 AU of projected separation) and its optical and near infrared photometry is consistent with a white dwarf, located at the distance of HD 107148 A. In order to confirm the white dwarf nature of the co-moving companion, we obtained follow-up spectroscopic observations of HD 107148 B with CAFOS at the CAHA 2.2 m telescope. According to our CAFOS spectroscopy HD 107148 B is a DA white dwarf with an effective temperature in the range between 5900 and 6400 K. The properties of HD 107148 B can further be constrained with the derived effective temperature and the known visual and infrared photometry of the companion, using evolutionary models of DA white dwarfs. We obtain for HD 107148 B a mass of 0.56±0.05 M_ȯ, a luminosity of (2.0±0.2)×10-4 L_ȯ, log g [cm s-2])=7.95±0.09, and a cooling age of 2100±270 Myr. With its white dwarf companion the exoplanet host star HD 107148 A forms an evolved stellar system, which hosts at least one exoplanet. So far, only few of these evolved systems are known, which represent only about 5 % of all known exoplanet host multiple stellar systems. HD 107148 B is the second confirmed white dwarf companion of an exoplanet host star with a projected separation to its primary star of more than 1000 AU. Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC).

  20. Spectroscopic mode identification of main-sequence non-radially pulsating stars

    NASA Astrophysics Data System (ADS)

    Maisonneuve, F.; Pollard, K. R.; Cottrell, P. L.; Kilmartin, P. M.; Wright, D. J.; De Cat, P.

    2010-07-01

    We are undertaking an extensive observational campaign of a number of non-radially pulsating stars using the high-resolution HERCULES spectrograph on the 1.0-m telescope at the Mt John University Observatory. This is part of a large world-wide multi-site campaign to improve mode-identification techniques in non-radially pulsating stars, particularly for g-mode pulsators. This paper outlines our campaign and presents preliminary results for one γ Doradus star, HD 40745, and one β Cephei star, HD 61068. We have used a representative cross-correlation line-profile technique presented by Wright in 2008 to extract line profiles and these have then been analyzed using the FAMIAS package due to Zima published in 2006 to derive a spectroscopic mode identification.

  1. Nonlinear instabilities of multi-site breathers in Klein-Gordon lattices

    DOE PAGESBeta

    Cuevas-Maraver, Jesus; Kevrekidis, Panayotis G.; Pelinovsky, Dmitry E.

    2015-12-14

    Here, we explore the possibility of multi-site breather states in a nonlinear Klein–Gordon lattice to become nonlinearly unstable, even if they are found to be spectrally stable. The mechanism for this nonlinear instability is through the resonance with the wave continuum of a multiple of an internal mode eigenfrequency in the linearization of excited breather states. For the nonlinear instability, the internal mode must have its Krein signature opposite to that of the wave continuum. This mechanism is not only theoretically proposed, but also numerically corroborated through two concrete examples of the Klein–Gordon lattice with a soft (Morse) and amore » hard (Φ4) potential. Compared to the case of the nonlinear Schrödinger lattice, the Krein signature of the internal mode relative to that of the wave continuum may change depending on the period of the multi-site breather state. For the periods for which the Krein signatures of the internal mode and the wave continuum coincide, multi-site breather states are observed to be nonlinearly stable.« less

  2. Nonlinear instabilities of multi-site breathers in Klein-Gordon lattices

    SciTech Connect

    Cuevas-Maraver, Jesus; Kevrekidis, Panayotis G.; Pelinovsky, Dmitry E.

    2015-12-14

    Here, we explore the possibility of multi-site breather states in a nonlinear Klein–Gordon lattice to become nonlinearly unstable, even if they are found to be spectrally stable. The mechanism for this nonlinear instability is through the resonance with the wave continuum of a multiple of an internal mode eigenfrequency in the linearization of excited breather states. For the nonlinear instability, the internal mode must have its Krein signature opposite to that of the wave continuum. This mechanism is not only theoretically proposed, but also numerically corroborated through two concrete examples of the Klein–Gordon lattice with a soft (Morse) and a hard (Φ4) potential. Compared to the case of the nonlinear Schrödinger lattice, the Krein signature of the internal mode relative to that of the wave continuum may change depending on the period of the multi-site breather state. For the periods for which the Krein signatures of the internal mode and the wave continuum coincide, multi-site breather states are observed to be nonlinearly stable.

  3. Stellar and circumstellar activity in the Be star EW Lacertae from the 1993 multi-site campaign

    NASA Astrophysics Data System (ADS)

    Floquet, M.; Hubert, A. M.; Hirata, R.; McDavid, D.; Zorec, J.; Gies, D.; Hahula, M.; Janot-Pacheco, E.; Kambe, E.; Leister, N. V.; Štefl, S.; Tarasov, A.; Neiner, C.

    2000-10-01

    A multi-site, multi-technique campaign on the Be star EW Lac was held for about 9 days in August-September 1993. We present results of the analysis of visual, high S/N spectroscopic data (He I 6678 Å and Hα ). Search for short-term variability was carried out on He I 6678 (line profiles, radial velocity (RV), equivalent width (EW), full width at half-maximum (FWHM) on the absorption part of the line profile and on violet (V) and red (R) emission peaks) and on Hα emission line (line profiles, EW, V, R and V/R ratio). The presence of multi-periodicity is confirmed and we detected the frequencies found in 1989 by Floquet et al. (1992) during a 8-day mono-site campaign. Possible non-radial pulsation solutions for the main frequencies detected are l ~ 2-3, | m | ~ 2-3. We found evidence on the He I 6678 line of episodic matter outflows through the presence of relatively broad, variable absorption line-profile variations. At least one sharp absorption feature was also observed slowly crossing the stellar disc. It is attributed to a blob of matter temporarily orbiting the star. A brief account is given of broad-band polarimetric observations, performed over 6 nights. A correlation is found between the variation in intrinsic polarization level in the B-band and He I 6678 Å strength. Finally, we present a simple model that reproduces rather well the additional ``pseudo-photosphere" contribution in 1993 as opposed to 1989.

  4. Variations in the D/H Ratio of Extended Sight Lines from Far Ultraviolet Spectroscopic Explorer Observations

    NASA Astrophysics Data System (ADS)

    Oliveira, Cristina M.; Hébrard, Guillaume

    2006-12-01

    We use new FUSE data to determine the column densities of interstellar D I, N I, O I, Fe II, and H2 along the HD 41161 and HD 53975 sight lines. Together with N(H I) from the literature, we derive D/H, N/H, and O/H ratios. These sight lines have logN(H I)>21.00 and probe gas up to ~1300 pc, allowing us to determine the gas-phase D/H ratio in a hydrogen column density range, logN(H)>20.70, where the only five measurements available in the literature yield a weighted average of D/H=(0.86+/-0.08)×10-5. We find D/H=(2.14+0.51-0.43)×10-5 along the HD 41161 sight line. This ratio is ~3 σ higher than the weighted mean D/H ratio quoted above, while the D/H ratio for the HD 53975 line of sight, D/H=(1.02+0.23-0.20)×10-5, agrees within the 1 σ uncertainties. Our D/H measurement along the HD 41161 sight line presents the first evidence of variations of D/H at high N(H). Our result seems to indicate either that the long sight lines that, according to the deuterium depletion model, are dominated by cold undisturbed gas where deuterium would be depleted onto carbonaceous grains occur at higher N(H) than previously thought, or that the clumping of low D/H values in the literature for the long sight lines has another explanation. Both of the O/H ratios derived here, (9.12+2.15-1.83)×10-4 and (5.37+1.35-1.14)×10-4 (for HD 41161 and HD 53975, respectively), are higher than what has been found by other authors. Finally, we derive (N/H)×105=8.32+2.09-1.76 and 5.07+1.45-1.21, and (D/O)×102=2.29+0.40-0.35 and 1.91+0.51-0.43, for HD 41161 and HD 53975, respectively. In addition, the relatively high signal-to-noise ratio of the HD 41161 data allows us to place constraints on the f-values of some neutral chlorine transitions present in the FUSE bandpass for which only theoretical values are available. Based on observations made with the NASA-CNES-CSA Far Ultraviolet Spectroscopic Explorer. FUSE is operated for NASA by the Johns Hopkins University under NASA contract NAS5-32985.

  5. Spectroscopic analyses of subluminous B stars: observational constraints for the theory of stellar evolution, pulsation, and diffusion

    NASA Astrophysics Data System (ADS)

    Edelmann, Heinz

    2003-06-01

    This thesis deals with quantitative spectroscopic analyses of large samples of subluminous B stars in order to find constraints the theory of stellar evolution, pulsation, and diffusion. Subluminous B stars, also known as subdwarf B (sdB) stars, are very important in several respects: They dominate the population of faint blue stars in high galactic latitudes, and are found both in the field and in globular clusters. Therefore, sdB stars are important to understand the structure and evolution of our galaxy. From the cosmological point of view, they are candidate progenitors of supernovae of type Ia due to their membership in close binary systems. In the context of stellar astrophysics, subdwarf B stars play an important role because several of them are discovered to show non-radial pulsations, which allows to probe their interior by asteroseismology. Last but not least, sdB stars show very peculiar element abundance patterns, probably caused by diffusion processes. Subluminous B stars are generally considered to be core helium-burning stars with extremely thin hydrogen envelopes (< 0.02M) and masses around 0.5M. In the Hertzsprung-Russell diagram they populate a very narrow area which lies on a blue-ward extension of the horizontal branch (HB), the so called "Extreme Horizontal Branch" (EHB). Due to their thin hydrogen-rich envelope, they cannot sustain a hydrogen-burning shell. This means that the sdB stars cannot ascend the asymptotic giant branch after the end of the helium-core burning, but should evolve directly to the white dwarf graveyard. However, according to standard stellar evolution theory, subdwarf B stars should not exist. Their evolution is still unclear and several scenarios are under debate. For all these investigations, knowledge of the stellar parameters (effective temperature, gravity and chemical composition) is very important to verify or discard theoretical models and predictions. Numerous observing runs have been performed mostly by myself

  6. Multisite adsorption of cadmium on goethite

    SciTech Connect

    Venema, P.; Hiemstra, T.; Riemsdijk, W.H. van

    1996-11-10

    Recently a new general ion adsorption model has been developed for ion binding to mineral surfaces (Hiemstra and van Riemsdijk, 1996). The model uses the Pauling concept of charge distribution (CD) and is an extension of the multi-site complexation (MUSIC) approach. In the CD-MUSIC model the charge of an adsorbing ion that forms an inner sphere complex is distributed over its ligands, which are present in two different electrostatic planes. In this paper the authors have applied the CD-MUSIC model to the adsorption of metal cations, using an extended data set for cadmium adsorbing on goethite. The adsorption of cadmium and the cadmium-proton exchange ratio were measured as function of metal ion concentration, pH, and ionic strength. The data could be described well, taking into account the surface heterogeneity resulting from the presence of two different crystal planes (the dominant 110 face and the minor 021 face). The surface species used in the model are consistent with recent EXAFS data. In accordance with the EXAFS results, high-affinity complexes at the 021 face were used in the model.

  7. Encoded multisite two-photon microscopy

    PubMed Central

    Ducros, Mathieu; Houssen, Yannick Goulam; Bradley, Jonathan; de Sars, Vincent; Charpak, Serge

    2013-01-01

    The advent of scanning two-photon microscopy (2PM) has created a fertile new avenue for noninvasive investigation of brain activity in depth. One principal weakness of this method, however, lies with the limit of scanning speed, which makes optical interrogation of action potential-like activity in a neuronal network problematic. Encoded multisite two-photon microscopy (eMS2PM), a scanless method that allows simultaneous imaging of multiple targets in depth with high temporal resolution, addresses this drawback. eMS2PM uses a liquid crystal spatial light modulator to split a high-power femto-laser beam into multiple subbeams. To distinguish them, a digital micromirror device encodes each subbeam with a specific binary amplitude modulation sequence. Fluorescence signals from all independently targeted sites are then collected simultaneously onto a single photodetector and site-specifically decoded. We demonstrate that eMS2PM can be used to image spike-like voltage transients in cultured cells and fluorescence transients (calcium signals in neurons and red blood cells in capillaries from the cortex) in depth in vivo. These results establish eMS2PM as a unique method for simultaneous acquisition of neuronal network activity. PMID:23798397

  8. NEW RESULTS FROM THE MAGELLAN IMACS SPECTROSCOPIC Ly{alpha} SURVEY: NICMOS OBSERVATIONS OF Ly{alpha} EMITTERS AT z = 5.7

    SciTech Connect

    Henry, Alaina L.; Martin, Crystal L.; Dressler, Alan; McCarthy, Patrick; Sawicki, Marcin

    2010-08-10

    We present NICMOS J {sub 110} (rest-frame 1200-2100 A) observations of the three z = 5.7 Ly{alpha} emitters discovered in the blind multislit spectroscopic survey by Martin et al. These images confirm the presence of the two sources that were previously only seen in spectroscopic observations. The third source, which is undetected in our J {sub 110} observations, has been detected in narrowband imaging of the Cosmic Origins Survey, so our non-detection implies a rest-frame equivalent width >146 A (3{sigma}). The two J {sub 110}-detected sources have more modest rest-frame equivalent widths of 30-40 A, but all three are typical of high-redshift Ly{alpha} emitters. In addition, the J {sub 110}-detected sources have UV luminosities that are within a factor of 2 of L*{sub UV}, and sizes that appear compact (r {sub hl{approx}} 0.''15) in our NIC2 images-consistent with a redshift of 5.7. We use these UV-continuum and Ly{alpha} measurements to estimate the i {sub 775}-z {sub 850} colors of these galaxies and show that at least one and possibly all three would be missed by the i-dropout Lyman break galaxy selection. These observations help demonstrate the utility of multislit narrowband spectroscopy as a technique for finding faint emission-line galaxies.

  9. Multi-site continuous spectroscopy. 2: Spectrophotometry and energy budget of exceptional white-light flares on HR 1099 from the MUSICOS 89 campaign

    NASA Astrophysics Data System (ADS)

    Foing, B. H.; Char, S.; Ayres, T.; Catala, C.; Neff, J. E.; Zhai, D. S.; Catalano, S.; Cutispoto, G.; Jankov, S.; Rodono, M.; Simon, T.; Akan, C.; Aslanov, A.; Avellar, P.; Baudrand, J.; Beust, H.; Cao, H.; Chatzichristou, H.; Cuby, J. G.; Czarny, J.; de La Reza, R.; Dreux, M.; Felenbok, P.; Ferlet, R.; Frasca, A.; Floquet, M.; Ghosh, K.; Guo, Z.; Guerin, J.; Hao, J. X.; Houdebine, E. R.; Huang, L.; Hubert, A. M.; Hubert, H.; Huovelin, J.; Hron, J.; Ibanoglu, C.; Jiang, S.; Keskin, V.; Lagrange-Henri, A. M.; Lecontel, J. M.; Li, Q.; Mavridis, L.; Nolthenius, R.; Petrov, P.; Savanov, I.; Scherbakov, A.; Tuominen, I.; Vidal-Madjar, A.; Zhang, R.; Zhang, X.

    1994-12-01

    We report results from the December 89 multi-site continuous observing campaign (MUSICOS (MUlti-SIte COntinuous Spectroscopic) 89) dedicated to the study of surface active structures and flares on the RS CVn-type system HR 1099 (= V711 Tau). This system has been observed by up to 17 telescopes around the globe during this campaign. We obtained complete phase coverage for Doppler imaging of photospheric spots. Quasi-simultaneously, we observed the modulation of Ca II K line profile due to chromospheric plage regions. At least two exceptional white-light flares on 14 Dec. 15:00 UT and 15 Dec. 1:00 UT (the largest such optical flare episode ever reported in a RS CVn system) were detected photometrically with typical rise and decay times of 60-90 min, and with remarkable spectral dynamic signatures in H-alpha with longer decay time scale. Equivalent colors, temperature excesses and projected flare areas (0.55 and 0.89 solar disc areas) were derived for the two optical flares. We estimate the energy budget for these two events, with respective peak intensities of radiative losses of 1.65 and 14 x 1033 erg/s and integrated losses over the white-light event duration of a few hours of 8 x 1036 and 1038 ergs (in the 3100-5900 A range), indicating a total energy balance several times these values. The emission was also measured in the H-alpha and H-Beta lines during these flares with a ratio of flare optical emission over Balmer emission 3-4 times larger compared to other flares on dwarfs. More than one day after the last white-light flare, part of the flare decay phase was also measured with IUE in UV lines of low and high excitation; the extrapolated transition region EUV losses are found similar to the derived Balmer line losses. Both flares were shown to occur near the limb. We derive their physical area, and estimate their densities, column mass, and penetration depth. From Balmer line broadening and flows, we derive a kinetic energy budget comparable to the radiative

  10. Spectroscopic Investigation of the Carotenoid Deoxyperidinin: Direct Observation of the Forbidden S0 → S1 Transition.

    PubMed

    Greco, Jordan A; LaFountain, Amy M; Kinashi, Naoto; Shinada, Tetsuro; Sakaguchi, Kazuhiko; Katsumura, Shigeo; Magdaong, Nikki Cecil M; Niedzwiedzki, Dariusz M; Birge, Robert R; Frank, Harry A

    2016-03-17

    This paper presents a spectroscopic investigation of deoxyperidinin, a synthetic peridinin analogue in which the carbonyl functional group in peridinin was replaced by a nonconjugated methylene group. Steady-state and ultrafast time-resolved absorption and fluorescence spectroscopic experiments are carried out on deoxyperidinin in n-hexane and acetonitrile at room temperature and in 2-methyltetrahydrofuran at 77 K. The spectra of deoxyperidinin have higher vibronic resolution compared to those of peridinin. The higher resolution is due to a substantial reduction in both molecular conformational disorder and inhomogeneous broadening of the spectra of deoxyperidinin compared to peridinin. Features in the steady-state absorption spectrum of deoxyperidinin that are not evident in the spectrum of peridinin are unambiguously assigned to the forbidden S0 (1(1)Ag(-)) → S1 (2(1)Ag(-)) absorption transition. The characteristics of both the steady-state and time-resolved spectra are interpreted using EOM-CCSD, SAC-CI, and MNDO-PSDCI quantum computational formalisms that provided a theoretical framework for understanding the photophysical properties of the molecules. PMID:26907520

  11. Independent iPTF detection and spectroscopic follow-up observations of the Type II SN 2013am = iPTF13aaz in M65

    NASA Astrophysics Data System (ADS)

    Yaron, O.; Gal-Yam, A.; Fox, O. D.; Kelly, P.; Zheng, W.; Cenko, S. B.; Filippenko, A. V.; Silverman, J. M.; Walker, E. S.; Mazzali, P. A.; Pian, E.; Nugent, P. E.; Cao, Y.; Horesh, A.; Kasliwal, M. M.

    2013-03-01

    The iPTF (ATel #4807) announces its independent detection, spectroscopic classification, and follow-up observations of the Type II SN in the nearby galaxy M65 (d = 12.6 Mpc; NED), at RA = 11:18:56.9, Dec = +13:03:50.0 (J2000). The object was discovered on 2013-03-21.637 by M. Sugano, Kakogawa, Hyogo-ken, Japan and posted on the CBAT TOCP page, http://www.cbat.eps.harvard.edu/unconf/followups/J11185695+1303494.html , where it was designated PSN J11185695+1303494 and later renamed SN 2013am (CBET #3440).

  12. The Wasilewski sample of emission-line galaxies - Follow-up CCD imaging and spectroscopic and IRAS observations

    NASA Technical Reports Server (NTRS)

    Bothun, Gregory D.; Schmitz, Mark; Halpern, Jules P.; Lonsdale, Carol J.; Impey, Chris

    1989-01-01

    The results of an extensive imaging and spectroscopic follow-up of the objective prism-selected emission line galaxy (ELG) sample of Wasilewski (1982) are presented. Fluxes at 12, 25, 60, and 100 microns were also obtained from the coadded IRAS survey data. ELGs found by objective prism surveys are found to be generally small and underluminous galaxies which usually have higher than average optical surface brightness. The Seyfert detection rate in objective prism surveys is roughly 10 percent and the ratio of the space densities of Seyfert 2 to Seyfert 1 galaxies is significantly larger than unity. Most of the galaxies selected by objective prism surveys are star-forming, late-type spirals which often show disturbed morphology. About 25 percent of the galaxies detected by the surveys are faint, high-excitation metal-poor compact H II regions.

  13. Development of a high dynamic range spectroscopic system for observation of neutral hydrogen atom density distribution in Large Helical Device core plasma

    SciTech Connect

    Fujii, K. Atsumi, S.; Watanabe, S.; Shikama, T.; Hasuo, M.; Goto, M.; Morita, S.

    2014-02-15

    We report development of a high dynamic range spectroscopic system comprising a spectrometer with 30% throughput and a camera with a low-noise fast-readout complementary metal-oxide semiconductor sensor. The system achieves a 10{sup 6} dynamic range (∼20 bit resolution) and an instrumental function approximated by a Voigt profile with Gauss and Lorentz widths of 31 and 0.31 pm, respectively, for 656 nm light. The application of the system for line profile observations of the Balmer-α emissions from high temperature plasmas generated in the Large Helical Device is also presented. In the observed line profiles, emissions are detected in far wings more than 1.0 nm away from the line center, equivalent to neutral hydrogen atom kinetic energies above 1 keV. We evaluate atom density distributions in the core plasma by analyzing the line profiles.

  14. Optical spectroscopic observations of blazars and γ-ray blazar candidates in the Sloan digital sky survey data release nine

    SciTech Connect

    Massaro, F.; Masetti, N.; D'Abrusco, R.; Paggi, A.; Funk, S.

    2014-10-01

    We present an analysis of the optical spectra available in the Sloan Digital Sky Survey data release nine (SDSS DR9) for the blazars listed in the ROMA-BZCAT and for the γ-ray blazar candidates selected according to their IR colors. First, we adopt a statistical approach based on Monte Carlo simulations to find the optical counterparts of the blazars listed in the ROMA-BZCAT catalog. Then, we crossmatched the SDSS spectroscopic catalog with our selected samples of blazars and γ-ray blazar candidates, searching for those with optical spectra available to classify our blazar-like sources and, whenever possible, to confirm their redshifts. Our main objectives are to determine the classification of uncertain blazars listed in the ROMA-BZCAT and to discover new gamma-ray blazars. For the ROMA-BZCAT sources, we investigated a sample of 84 blazars, confirming the classification for 20 of them and obtaining 18 new redshift estimates. For the γ-ray blazars, indicated as potential counterparts of unassociated Fermi sources or with uncertain nature, we established the blazar-like nature of 8 out of the 27 sources analyzed and confirmed 14 classifications.

  15. Spectroscopic survey of Kepler stars. I. HERMES/Mercator observations of A- and F-type stars

    NASA Astrophysics Data System (ADS)

    Niemczura, E.; Murphy, S. J.; Smalley, B.; Uytterhoeven, K.; Pigulski, A.; Lehmann, H.; Bowman, D. M.; Catanzaro, G.; van Aarle, E.; Bloemen, S.; Briquet, M.; De Cat, P.; Drobek, D.; Eyer, L.; Gameiro, J. F. S.; Gorlova, N.; Kamiński, K.; Lampens, P.; Marcos-Arenal, P.; Pápics, P. I.; Vandenbussche, B.; Van Winckel, H.; Stȩślicki, M.; Fagas, M.

    2015-07-01

    The Kepler space mission provided near-continuous and high-precision photometry of about 207 000 stars, which can be used for asteroseismology. However, for successful seismic modeling it is equally important to have accurate stellar physical parameters. Therefore, supplementary ground-based data are needed. We report the results of the analysis of high-resolution spectroscopic data of A- and F-type stars from the Kepler field, which were obtained with the HERMES spectrograph on the Mercator telescope. We determined spectral types, atmospheric parameters and chemical abundances for a sample of 117 stars. Hydrogen Balmer, Fe I, and Fe II lines were used to derive effective temperatures, surface gravities, and microturbulent velocities. We determined chemical abundances and projected rotational velocities using a spectrum synthesis technique. The atmospheric parameters obtained were compared with those from the Kepler Input Catalogue (KIC), confirming that the KIC effective temperatures are underestimated for A stars. Effective temperatures calculated by spectral energy distribution fitting are in good agreement with those determined from the spectral line analysis. The analysed sample comprises stars with approximately solar chemical abundances, as well as chemically peculiar stars of the Am, Ap, and λ Boo types. The distribution of the projected rotational velocity, vsin i, is typical for A and F stars and ranges from 8 to about 280 km s-1, with a mean of 134 km s-1.

  16. A Multisite Evaluation of Reading Is Fundamental: Summary Report.

    ERIC Educational Resources Information Center

    Parker, Ronald K.; And Others

    Reading Is Fundamental (RIF) is a national program that seeks to motivate children to read. Implemented by local sponsors and aimed at disadvantaged groups, it offers participating children a wide selection of attractive paperback books about interesting people, places, and events. The multisite evaluation summarized in this report studied…

  17. A Multisite Evaluation of Reading Is Fundamental: Technical Report.

    ERIC Educational Resources Information Center

    Parker, Ronald K.; And Others

    Reading Is Fundamental (RIF) is a national program that seeks to motivate children to read. Implemented by local sponsors and aimed at disadvantaged groups, it offers participating children a wide selection of attractive paperbound books about interesting people, places, and events. The multisite evaluation discussed in this technical report…

  18. Multi-Sited Ethnography and the Field of Educational Research

    ERIC Educational Resources Information Center

    Pierides, Dean

    2010-01-01

    This paper responds to the challenge of how educational research might be practised in a contemporary world that is no longer necessarily organised by nearness and unity. Focusing on ethnography, it argues for what a multi-sited imaginary contributes to research in the field of education. By giving prominence to the notion of multi-sited…

  19. From gateway to multisite gateway in one recombination event

    Technology Transfer Automated Retrieval System (TEKTRAN)

    We created a construct, pDONR-R4-R3, to easily convert any available Gateway destination vector to a MultiSite Gateway vector in a single recombination reaction. In addition, we designed pDONR-R4-R3 so that DNA fragments already cloned upstream or downstream of the Gateway cassette in the original d...

  20. Hydrological modeling using a multi-site stochastic weather generator

    Technology Transfer Automated Retrieval System (TEKTRAN)

    Weather data is usually required at several locations over a large watershed, especially when using distributed models for hydrological simulations. In many applications, spatially correlated weather data can be provided by a multi-site stochastic weather generator which considers the spatial correl...

  1. A Multisite Cluster Randomized Field Trial of Open Court Reading

    ERIC Educational Resources Information Center

    Borman, Geoffrey D.; Dowling, N. Maritza; Schneck, Carrie

    2008-01-01

    In this article, the authors report achievement outcomes of a multisite cluster randomized field trial of Open Court Reading 2005 (OCR), a K-6 literacy curriculum published by SRA/McGraw-Hill. The participants are 49 first-grade through fifth-grade classrooms from predominantly minority and poor contexts across the nation. Blocking by grade level…

  2. Replication and Comparison of the Newly Proposed ADOS-2, Module 4 Algorithm in ASD without ID: A Multi-Site Study

    ERIC Educational Resources Information Center

    Pugliese, Cara E.; Kenworthy, Lauren; Bal, Vanessa Hus; Wallace, Gregory L.; Yerys, Benjamin E.; Maddox, Brenna B.; White, Susan W.; Popal, Haroon; Armour, Anna Chelsea; Miller, Judith; Herrington, John D.; Schultz, Robert T.; Martin, Alex; Anthony, Laura Gutermuth

    2015-01-01

    Recent updates have been proposed to the Autism Diagnostic Observation Schedule-2 Module 4 diagnostic algorithm. This new algorithm, however, has not yet been validated in an independent sample without intellectual disability (ID). This multi-site study compared the original and revised algorithms in individuals with ASD without ID. The revised…

  3. Time-Resolved Spectroscopic Observation of Deposition Processes of Ultrananocrystalline Diamond/Amorphous Carbon Composite Films by Using a Coaxial Arc Plasma Gun

    NASA Astrophysics Data System (ADS)

    Hanada, Kenji; Yoshitake, Tsuyoshi; Nishiyama, Takashi; Nagayama, Kunihito

    2010-08-01

    The deposition of ultrananocrystalline diamond (UNCD)/amorphous carbon composite films using a coaxial arc plasma gun in vacuum and, for comparison, in a 53.3 Pa hydrogen atmosphere was spectroscopically observed using a high-speed camera equipped with narrow-band-pass filters. UNCD crystallites with diameters of approximately 1.6 nm were formed even in vacuum. These extremely small crystallites imply that the formation is predominantly due to nucleation without the subsequent growth. Even in vacuum, emissions from C+ ions, C atoms, and C2 dimers lasted for approximately 100 µs, although the emission lifetimes of these species are generally 10 ns. We consider that the nucleation is due to the supersaturated environment containing excited carbon species with large number densities.

  4. A nested multisite daily rainfall stochastic generation model

    NASA Astrophysics Data System (ADS)

    Srikanthan, Ratnasingham; Pegram, Geoffrey G. S.

    2009-06-01

    SummaryThis paper describes a nested multisite daily rainfall generation model which preserves the statistics at daily, monthly and annual levels of aggregation. A multisite two-part daily model is nested in multisite monthly, then annual models. A multivariate set of fourth order Markov chains is used to model the daily occurrence of rainfall; the daily spatial correlation in the occurrence process is handled by using suitably correlated uniformly distributed variates via a Normal Scores Transform (NST) obtained from a set of matched multinormal pseudo-random variates, following Wilks [Wilks, D.S., 1998. Multisite generalisation of a daily stochastic precipitation generation model. Journal of Hydrology 210, 178-191]; we call it a hidden covariance model. A spatially correlated two parameter gamma distribution is used to obtain the rainfall depths; these values are also correlated via a specially matched hidden multinormal process. For nesting, the generated daily rainfall sequences at all the sites are aggregated to monthly rainfall values and these values are modified by a set of lag-1 autoregressive multisite monthly rainfall models. The modified monthly rainfall values are aggregated to annual rainfall and these are then modified by a lag-1 autoregressive multisite annual model. This nesting process ensures that the daily, monthly and annual means and covariances are preserved. The model was applied to a region with 30 rainfall sites, one of the five sets reported by Srikanthan [Srikanthan, R., 2005. Stochastic Generation of Daily Rainfall Data at a Number of Sites. Technical Report 05/7, CRC for Catchment Hydrology. Monash University, 66p]. A comparison of the historical and generated statistics shows that the model preserves all the important characteristics of rainfall at the daily, monthly and annual time scales, including the spatial structure. There are some outstanding features that need to be improved: depths of rainfall on isolated wet days and

  5. Photometric and Spectroscopic Analysis of Classical Novae: An Examination of Their Observational Characteristics and Greater Astronomical Impact

    NASA Astrophysics Data System (ADS)

    Helton, Lorren Andrew

    2010-12-01

    Classical novae (CNe) are violent thermonuclear explosions arising on the surface of white dwarfs in binary systems and are contributors to the chemical evolution of the interstellar medium through the production and ejection of copious amounts of metal-rich material. Observations and modeling of CNe eruptions illuminate numerous fundamental processes of astrophysical interest, including non-equilibrium thermonuclear runaway, radiative processes in dynamic nebular environments, binary star interaction, as well as dust condensation and grain growth. Here I summarize key findings from selected Galactic CNe observed as part of a 5 year, panchromatic optical/infrared observing campaign using Spitzer, Gemini, and other ground based optical facilities. In particular, I present detailed analysis of nova V1065 Centauri, including photoionization analysis of the emission lines, which enabled the derivation of abundances in the ejecta, and radiative transport modeling of the dust emission features, which allowed determination of the composition and characteristics of the dust in this system. I present analysis of three novae, V1974 Cygni, V382 Velorum, and V1494 Aquilae, observed from 4.4--15.5 years after outburst, discuss the characteristics of the nebulae at these late times, and estimate the abundances in their ejecta. In the case of V1494 Aql, I also report the first detection of neon. Finally, I present observations of three novae, DZ Crucis, V2361 Cygni, and V2362 Cygni, that exhibited unidentified infrared (UIR) features in their mid-infrared spectra, which exhibited unusual characteristics. I relate these features to other dusty novae in which features with similar characteristics were observed, and discuss possible sources for the UIR carriers. Analysis of the data obtained in the CNe monitoring campaign presented here highlights the need for synoptic observations obtained with broad wavelength coverage. Observations of V1065 Cen, which exhibited spectra rich in

  6. The galaxy's 157 micron (C 2) emission: Observations by means of a spectroscopic lunar-occultation technique

    NASA Technical Reports Server (NTRS)

    Stacey, G. J.; Smyers, S. D.; Kurtz, N. T.; Harwit, M.

    1983-01-01

    Galactic (C II) 157 micron, fine-structure emission was estimated. At a Galactic longitude of 8 deg, the peak power observed in a 7' x 7' field is approx. 5 x 10 to the -9 Watt. The method used to detect this radiation involved chopping against the cold side of the Moon.

  7. High-dispersion spectroscopic observations of Venus during 1968 and 1969 II. The carbon-dioxide band at 8689A

    NASA Technical Reports Server (NTRS)

    Schorn, R. A. J.; Woszczyk, A.; Young, L. D. G.

    1974-01-01

    Thirty well-exposed photographic plates showing the spectrum of the carbon dioxide band at 8689A in the atmosphere of Venus were obtained during 1968 and 1969. All spectra were obtained at a dispersion of 2 A/mm for Venus phase angles varying from 10 deg. to 126 deg. Rotational temperatures ranging from 236 K to 274 K were found. The average value of the rotational temperature is 246 + or - 1 K (one standard deviation); for 1967 observations, the rotational temperatures ranged from 222 to 248 K, with an average value of 238 + or - 4 K. The variation of the equivalent width of the 8689A band, with Venus phase angle, was very similar for the two sets of observations (53 plates). The temporal variations, of approximately 30 percent, were comparable with the phase variations over this limited range of phase angle.

  8. Independent positioning of microelectrodes for multisite recordings in vitro.

    PubMed

    Albus, Klaus; Sinske, Kurt; Heinemann, Uwe

    2009-01-30

    A robust and easy to handle, inexpensive multisite recording system is described which allows independent positioning of several microelectrodes with high precision axial movement of each electrode. The basic units of the system are a manually operated manipulator for left-right and up-down movement and a micrometer for positioning in the direction of the micrometer axis. The micrometer is actuated with a DC-motor operated by a stand-alone controller module allowing for remote control of the motor in either step mode or continuous mode. The multisite recording system has been proven to allow stable simultaneous recordings of single unit and population activities, extracellular ion concentrations and intracellular potentials in organotypic hippocampal slice cultures (OHSCs) of rat. PMID:18822315

  9. {sup 13}C-METHYL FORMATE: OBSERVATIONS OF A SAMPLE OF HIGH-MASS STAR-FORMING REGIONS INCLUDING ORION-KL AND SPECTROSCOPIC CHARACTERIZATION

    SciTech Connect

    Favre, Cécile; Bergin, Edwin A.; Crockett, Nathan R.; Neill, Justin L.; Carvajal, Miguel; Field, David; Jørgensen, Jes K.; Bisschop, Suzanne E.; Brouillet, Nathalie; Despois, Didier; Baudry, Alain; Kleiner, Isabelle; Margulès, Laurent; Huet, Thérèse R.; Demaison, Jean E-mail: miguel.carvajal@dfa.uhu.es

    2015-01-01

    We have surveyed a sample of massive star-forming regions located over a range of distances from the Galactic center for methyl formate, HCOOCH{sub 3}, and its isotopologues H{sup 13}COOCH{sub 3} and HCOO{sup 13}CH{sub 3}. The observations were carried out with the APEX telescope in the frequency range 283.4-287.4 GHz. Based on the APEX observations, we report tentative detections of the {sup 13}C-methyl formate isotopologue HCOO{sup 13}CH{sub 3} toward the following four massive star-forming regions: Sgr B2(N-LMH), NGC 6334 IRS 1, W51 e2, and G19.61-0.23. In addition, we have used the 1 mm ALMA science verification observations of Orion-KL and confirm the detection of the {sup 13}C-methyl formate species in Orion-KL and image its spatial distribution. Our analysis shows that the {sup 12}C/{sup 13}C isotope ratio in methyl formate toward the Orion-KL Compact Ridge and Hot Core-SW components (68.4 ± 10.1 and 71.4 ± 7.8, respectively) are, for both the {sup 13}C-methyl formate isotopologues, commensurate with the average {sup 12}C/{sup 13}C ratio of CO derived toward Orion-KL. Likewise, regarding the other sources, our results are consistent with the {sup 12}C/{sup 13}C in CO. We also report the spectroscopic characterization, which includes a complete partition function, of the complex H{sup 13}COOCH{sub 3} and HCOO{sup 13}CH{sub 3} species. New spectroscopic data for both isotopomers H{sup 13}COOCH{sub 3} and HCOO{sup 13}CH{sub 3}, presented in this study, have made it possible to measure this fundamentally important isotope ratio in a large organic molecule for the first time.

  10. Proton Adsorption onto Alumina: Extension of Multisite Complexation (MUSIC) Theory.

    PubMed

    Nagashima; Blum

    1999-09-01

    The adsorption isotherm of protons onto a commercial gamma-alumina sample was determined in aqueous nitric acid with sodium nitrate as a background electrolyte. Three discrete regions could be discerned in the log-log plots of the proton isotherm determined at the solution pH 5 to 2. The multisite complexation (MUSIC) model was modified to analyze the simultaneous adsorption of protons onto various kinds of surface species. Copyright 1999 Academic Press. PMID:10441408

  11. Optimized multisite ventricular pacing in postoperative single-ventricle patients.

    PubMed

    Havalad, Vinod; Cabreriza, Santos E; Cheung, Eva W; Aponte-Patel, Linda; Wang, Alice; Cheng, Bin; Wang, Daniel Y; Silver, Eric; Bacha, Emile A; Spotnitz, Henry M

    2014-10-01

    Ventricular dyssynchrony is associated with morbidity and mortality after palliation of a single ventricle. The authors hypothesized that resynchronization with optimized temporary multisite pacing postoperatively would be safe, feasible, and effective. Pacing was assessed in the intensive care unit within the first 24 h after surgery. Two unipolar atrial pacing leads and four bipolar ventricular pacing leads were placed at standardized sites intraoperatively. Pacing was optimized to maximize mean arterial pressure. The protocol tested 11 combinations of the 4 different ventricular lead sites, 6 atrioventricular delays (50-150 ms), and 14 intraventricular delays. Optimal pacing settings were thus determined and ultimately compared in four configurations: bipolar, unipolar, single-site atrioventricular pacing, and intrinsic rhythm. Each patient was his or her own control, and all pacing comparisons were implemented in random sequence. Single-ventricle palliation was performed for 17 children ages 0-21 years. Pacing increased mean arterial pressure (MAP) versus intrinsic rhythm, with the following configurations: bipolar multisite pacing increased MAP by 2.2 % (67.7 ± 2.4 to 69.2 ± 2.4 mmHg; p = 0.013) and unipolar multisite pacing increased MAP by 2.8 % (67.7 ± 2.4 to 69.6 ± 2.7 mmHg; p = 0.002). Atrioventricular single-site pacing increased MAP by 2.1 % (67.7 ± 2.4 to 69.1 ± 2.5 mmHg: p = 0.02, insignificant difference under Bonferroni correction). The echocardiographic fractional area change in nine patients increased significantly only with unipolar pacing (32 ± 3.1 to 36 ± 4.2 %; p = 0.02). No study-related adverse events occurred. Multisite pacing optimization is safe and feasible in the early postoperative period after single-ventricle palliation, with improvements in mean arterial pressure and fractional area shortening. Further study to evaluate clinical benefits is required. PMID:24827078

  12. Proton adsorption onto alumina: extension of multisite complexation (MUSIC) theory

    SciTech Connect

    Nagashima, K.; Blum, F.D.

    1999-09-01

    The adsorption isotherm of protons onto a commercial {gamma}-alumina sample was determined in aqueous nitric acid with sodium nitrate as a background electrolyte. Three discrete regions could be discerned in the log-log plots of the proton isotherm determined at the solution pH 5 to 2. The multisite complexation (MUSIC) model was modified to analyze the simultaneous adsorption of protons onto various kinds of surface species.

  13. NEAR-CONTEMPORANEOUS OPTICAL SPECTROSCOPIC AND INFRARED PHOTOMETRIC OBSERVATIONS OF CANDIDATE HERBIG Ae/Be STARS IN THE MAGELLANIC CLOUDS

    SciTech Connect

    Rush, Bradley W.; Bjorkman, Karen S.; Wisniewski, John P. E-mail: Karen.Bjorkman@utoledo.edu

    2011-08-15

    We present near-IR (J, H, Ks) photometry for 27 of the 28 candidate Herbig Ae/Be stars in the Small and Large Magellanic Clouds (SMC and LMC) identified via the EROS1 and EROS2 surveys as well as near-contemporaneous optical (H{alpha}) spectroscopy for 21 of these 28 candidates. Our observations extend previous efforts to determine the evolutionary status of these objects. We compare the IR brightness and colors of a subset of our sample with archival ground-based IR data and find evidence of statistically significant photometric differences for EROS LMC HAeBe candidates (ELHC) 5, 7, 12, 18, and 21 in one or more filters. In all cases, these near-IR photometric variations exhibit a gray color as compared to earlier epoch data. The {approx}1 mag IR brightening and minimal change in the H{alpha} emission strength we observe in ELHC 7 is consistent with previous claims that it is a UX Ori type HAe/Be star, which is occasionally obscured by dust clouds. We also detect a {approx}1 mag IR brightening of ELHC 12, but find little evidence of a similar large-scale change in its H{alpha} line strength, suggesting that its behavior could also be caused by a UX Ori-like event. The {approx}0.5 mag IR variability we observe for ELHC 21, which also exhibited little evidence of a change in its H{alpha} emission strength, could conceivably be caused by a major recent enhancement in the density of the inner disk region of a classical Be star. We also report the first near-IR photometry for two EROS SMC HAeBe Candidates (ESHC) stars and the first H{alpha} spectroscopy for one ELHC and five ESHC stars. Although H{alpha} emission is detected in all of these new observations, they do not exhibit a strong near-IR excess. It is therefore possible that many of these objects may be classical Be stars rather than Herbig Ae/Be stars.

  14. Chemical Reactions in Protoplanetary Disks and Possibility of Detecting H2O Snowline Using Spectroscopic Observations with ALMA

    NASA Astrophysics Data System (ADS)

    Notsu, S.; Nomura, H.; Ishimoto, D.; Walsh, C.; Honda, M.; Millar, T. J.

    2015-12-01

    We calculate chemical reactions and obtain abundance distribution of H2O gas. We confirm that the abundance of H2O is high not only in the region inside H2 O snowline near the equatorial plane but also in the hot surface layer of outer disk. We also calculate velocity profiles of H2O emission lines, and find that we can obtain the information of H2O snowline through investigating the profiles of some line transitions that have small Einstein A coefficient and large excitation energy. Some useful H2O emission lines exist at sub-millimeter wavelength and are observable with ALMA.

  15. Dynamics of allosteric action in multisite protein modification

    NASA Astrophysics Data System (ADS)

    Milotti, Edoardo; Del Fabbro, Alessio; Dalla Pellegrina, Chiara; Chignola, Roberto

    2007-06-01

    Protein functions in cells may be activated or modified by the attachment of several kinds of chemical groups. While protein phosphorylation, i.e., the attachment of a phosphoryl (PO3-) group, is the most studied form of protein modification, and is known to regulate the functions of many proteins, protein behavior can also be modified by nitrosylation, acetylation, methylation, etc. A protein can have multiple modification sites, and displays some form of transition only when enough sites are modified. In a previous paper we have modeled the generic equilibrium properties of multisite protein modification [R. Chignola, C. Dalla Pellegrina, A. Del Fabbro, E. Milotti, Physica A 371 (2006) 463] and we have shown that it can account both for sharp, robust thresholds and for information transfer between processes with widely separated timescales. Here we use the same concepts to expand that analysis starting from a dynamical description of multisite modification: we give analytical results for the basic dynamics and numerical results in an example where the modification chain is cascaded with a Michaelis-Menten step. We modify the dynamics and analyze an example with realistic phosphorylation/dephosphorylation steps, and give numerical evidence of the independence of the allosteric effect from the details of the attachment-detachment processes. We conclude that multisite protein modification is dynamically equivalent to the classic allosteric effect.

  16. A new method of observing weak extended x-ray sources with the Reuven Ramaty high-energy solar spectroscopic imager.

    PubMed

    Hannah, Iain G; Hurford, Gordon J; Hudson, Hugh S; Lin, Robert P

    2007-02-01

    We present a new method, fan-beam modulation, for observing weak extended x-ray sources with the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI). This space-based solar x-ray and gamma-ray telescope has much greater sensitivity than previous experiments in the 3-25 keV range, but is normally not well suited to detecting extended sources since their signal is not modulated by RHESSI's rotating grids. When the spacecraft is offpointed from the target source, however, the fan-beam modulation time-modulates the transmission by shadowing resulting from exploiting the finite thickness of the grids. In this article we detail how the technique is implemented and verify its consistency with sources with clear known signals that have occurred during RHESSI offpointing: microflares and the Crab Nebula. In both cases the results are consistent with previous and complementary measurements. Preliminary work indicates that this new technique allows RHESSI to observe the integrated hard x-ray spectrum of weak extended sources on the quiet Sun. PMID:17578130

  17. First spectroscopic observation of gold(i) butadiynylide: Photodetachment velocity map imaging of the AuC4H anion.

    PubMed

    Visser, Bradley R; Addicoat, Matthew A; Gascooke, Jason R; Lawrance, Warren D; Metha, Gregory F

    2016-07-28

    The velocity map imaging technique was used in the investigation of gold(i) butadiynylide, AuC4H(-), with images recorded at two excitation wavelengths. The resultant photodetachment spectra show a well defined vibrational progression in the neutral with an energy spacing of 343 ± 3 cm(-1). The adiabatic electron affinity was determined to be 1.775 ± 0.005 eV and assigned to the X(1)Σ(+)←X(2)Σ(+) transition between the anionic and neutral ground states. Franck-Condon simulations performed on density functional theory optimized geometries assisted the assignment of linear geometries to the neutral and anion and the observed vibrational progression to that of the Au-C4H stretch. PMID:27475374

  18. Compact Solar Spectroscopic Column CO2, CH4, H2O and HOD Observations: Performance Evaluation at TCCON Sites

    NASA Astrophysics Data System (ADS)

    Butterfield, Z.; Lindenmaier, R.; Dubey, M. K.; Hedelius, J.; Wunch, D.; Wennberg, P. O.; Podolske, J. R.; Iraci, L. T.; Hillyard, P. W.; Hase, F.

    2014-12-01

    Monitoring, reporting and verification (MRV) of natural sources and sinks and anthropogenic emission of carbon dioxide (CO2) and methane (CH4) are crucial to predict climate change and develop transparent accounting policies to contain climate forcing. Remote sensing technologies are beginning to monitor CO2 and CH4 from ground and space (OCO-2 and GOSAT) with solar spectroscopy enabling direct MRV. However, current ground based coverage is sparse due to the need for large and expensive high-resolution spectrometers that are part of the Total Column Carbon Observing Network (TCCON, Bruker 125HR). This limits our MRV and satellite validation abilities, both regionally and globally. There are striking monitoring gaps in Asia, South America and Africa where the CO2 emissions are growing and there is a large uncertainty in fluxes from land use change, biomass burning and rainforest vulnerability. To fill this gap we evaluate the precision, accuracy and stability of our new compact, affordable and easy to use low-resolution spectrometer (Bruker EM27SUN) by comparing it with the much larger high-resolution TCCON instruments for column CO2, CH4, H2O and HOD. Results from Four Corners, Los Alamos, Caltech and Dryden-Armstrong sites show that our EM27SUN captures the variability of the aforementioned constituents very well, but has low and high offsets for CO2 and CH4, respectively. These off-the-shelf spectrometers should dramatically expand the coverage of regional column CO2 and CH4 observations, particularly in gap regions that include the rainforest. We will present opportunities that we are exploring to help enable transparent and reliable MRV and measurement of the coupled water-carbon cycle in tropical ecosystems.

  19. Spectroscopic infrared ellipsometry

    NASA Astrophysics Data System (ADS)

    Roseler, A.

    1992-03-01

    The spectroscopic infrared ellipsometry (SIRE) by means of the combination of a photometric ellipsometer with a Fourier transform spectrometer is used to measure optical properties in the infrared. From the observed four Stokes parameters, the spectrum of the degree of polarization after the reflection at the sample is calculated and discussed.

  20. Study of diatoms/aqueous solution interface. I. Acid-base equilibria and spectroscopic observation of freshwater and marine species

    NASA Astrophysics Data System (ADS)

    Gélabert, A.; Pokrovsky, O. S.; Schott, J.; Boudou, A.; Feurtet-Mazel, A.; Mielczarski, J.; Mielczarski, E.; Mesmer-Dudons, N.; Spalla, O.

    2004-10-01

    This work reports on a concerted study of diatom-water interfaces for two marine planktonic ( Thalassiosira weissflogii= TW, Skeletonema costatum= SC) and two freshwater periphytic species ( Achnanthidium minutissimum= AMIN, Navicula minima= NMIN). Proton surface adsorption was measured at 25°C, pH of 3 to 11 and ionic strength of 0.001 to 1.0 M via potentiometric titration using a limited residence time reactor. Electrophoretic mobility of living cells and their frustules was measured as a function of pH and ionic strength. Information on the chemical composition and molecular structure of diatoms surfaces was obtained using FT-IR (in situ attenuated total reflectance) and X-ray Photoelectron Spectroscopy (XPS). The surface area of living cells and their frustules in aqueous solutions was quantified using Small Angle X-ray Scattering Spectroscopy (SAXS). These observations allowed us to identify the nature and to determine the concentration of the major surface functional groups (carboxyl, amine and silanol) responsible for the amphoteric behavior of cell surfaces in aqueous solutions. Taking into account the relative proportion of surface sites inferred from XPS and FT-IR measurements, a surface complexation model of diatom-solution interfaces was generated on the basis of surface titration results. The cell-normalized ratios of the three major surface sites {>COOH}: {>NH 3}: {>SiOH} are 1:1:0.1, 1:10:0, 1:1:0.4 and 1:1:0.3 for TW, SC, AMIN and NMIN, respectively. The total amount of proton/hydroxyl active surface sites for investigated species ranges from 1 (NMIN) to 9 (SC) mmol/g dry weight. Normalization of these site densities to the area of siliceous skeleton yields values between 0.3 (NMIN) and 0.9 mmol/m 2 (SC) which are an order of magnitude higher than corresponding values for organic-free frustules or amorphous silica. This suggests that the amphoteric properties and possibly the affinity for metal adsorption of diatom cultures are essentially

  1. Observational and laboratory studies of optical properties of black and brown carbon particles in the atmosphere using spectroscopic techniques

    NASA Astrophysics Data System (ADS)

    Nakayama, Tomoki; Matsumi, Yutaka

    2015-04-01

    Light absorption and scattering by aerosols are as an important contributor to radiation balance in the atmosphere. Black carbon (BC) is considered to be the most potent light absorbing material in the visible region of the spectrum, although light absorbing organic carbon (brown carbon or BrC) and mineral dust may also act as sources of significant absorption, especially in the ultraviolet (UV) and shorter visible wavelength regions. The optical properties of such particles depend on wavelength, particle size and shape, morphology, coating, and complex refractive index (or chemical composition), and therefore accurate in situ measurements of the wavelength dependence of the optical properties of particles are needed. Recently, cavity ring-down spectroscopy (CRDS) and photoacoustic spectroscopy (PAS) have been used for the direct measurements of extinction and absorption coefficients of particles suspended in air. We have applied these techniques to the observational studies of optical properties of BC and BrC in an urban site in Japan and to the laboratory studies of optical properties of secondary organic aerosols (SOAs) generated from a variety of biogenic and anthropogenic volatile organic compounds and those of diesel exhaust particles (DEPs). In the presentation, the basic principles of these techniques and the results obtained in our studies and in the recent literatures will be overviewed. References Guo, X. et al., Measurement of the light absorbing properties of diesel exhaust particles using a three-wavelength photoacoustic spectrometer, Atmos. Environ., 94, 428-437 (2014). Nakayama, T. et al., Measurements of aerosol optical properties in central Tokyo during summertime using cavity ring-down spectroscopy: Comparison with conventional techniques, Atmos. Environ., 44, 3034-3042 (2010). Nakayama, T. et al., Laboratory studies on optical properties of secondary organic aerosols generated during the photooxidation of toluene and the ozonolysis of alpha

  2. Unraveling the electronic structure of azolehemiporphyrazines: direct spectroscopic observation of magnetic dipole allowed nature of the lowest π-π* transition of 20π-electron porphyrinoids.

    PubMed

    Muranaka, Atsuya; Ohira, Shino; Toriumi, Naoyuki; Hirayama, Machiko; Kyotani, Fumiko; Mori, Yukie; Hashizume, Daisuke; Uchiyama, Masanobu

    2014-06-26

    Hemiporphyrazines are a large family of phthalocyanine analogues in which two isoindoline units are replaced by other rings. Here we report unambiguous identification of 20π-electron structure of triazolehemiporphyrazines (1, 2) and thiazolehemiporphyrazine (3) by means of X-ray analysis, various spectroscopic methods, and density functional theory (DFT) calculations. The hemiporphyrazines were compared in detail with dibenzotetraazaporphyrin (4), a structurally related 18π-electron molecule. X-ray analysis revealed that tetrakis(2,6-dimethylphenyloxy)triazolehemiporphyrazine (1b) adopted planar geometry in the solid state. A weak absorption band with a pronounced vibronic progression, observed for all the hemiporphyrazines, was attributed to the lowest π-π* transition with the electric-dipole-forbidden nature. In the case of intrinsically chiral vanadyl triazolehemiporphyrazine (2), a large dissymmetry (g) factor was detected for the CD signal corresponding to the lowest π-π* transition with the magnetic-dipole-allowed nature. Molecular orbital analysis and NICS calculations showed that the azolehemiporphyrazines have a 20π-electron system with a weak paratropic ring current. PMID:24866729

  3. Spectroscopic Observations of the Planets

    NASA Technical Reports Server (NTRS)

    Owen, Tobias

    1998-01-01

    During the period under review, the main effort of the research supported by this grant was concentrated on Titan, Iapetus, and two comets, Comet Hyakutake and Comet Hale-Bopp. Significant discoveries were made in each case as summarized in the report.

  4. Candidate Water Vapor Lines to Locate the H2O Snowline through High-dispersion Spectroscopic Observations. I. The Case of a T Tauri Star

    NASA Astrophysics Data System (ADS)

    Notsu, Shota; Nomura, Hideko; Ishimoto, Daiki; Walsh, Catherine; Honda, Mitsuhiko; Hirota, Tomoya; Millar, T. J.

    2016-08-01

    Inside the H2O snowline of protoplanetary disks, water evaporates from the dust-grain surface into the gas phase, whereas it is frozen out onto the dust in the cold region beyond the snowline. H2O ice enhances the solid material in the cold outer part of a disk, which promotes the formation of gas-giant planet cores. We can regard the H2O snowline as the surface that divides the regions between rocky and gaseous giant planet formation. Thus observationally measuring the location of the H2O snowline is crucial for understanding the planetesimal and planet formation processes, and the origin of water on Earth. In this paper, we find candidate water lines to locate the H2O snowline through future high-dispersion spectroscopic observations. First, we calculate the chemical composition of the disk and investigate the abundance distributions of H2O gas and ice, and the position of the H2O snowline. We confirm that the abundance of H2O gas is high not only in the hot midplane region inside the H2O snowline but also in the hot surface layer of the outer disk. Second, we calculate the H2O line profiles and identify those H2O lines that are promising for locating the H2O snowline: the identified lines are those that have small Einstein A coefficients and high upper state energies. The wavelengths of the candidate H2O lines range from mid-infrared to sub-millimeter, and they overlap with the regions accessible to the Atacama Large Millimeter/sub-millimeter Array and future mid-infrared high-dispersion spectrographs (e.g., TMT/MICHI, SPICA).

  5. Hard X-ray Spectroscopic, Microwave and H-alpha Linear Polarization Studies with Hard X-Ray Observations from HESSI

    NASA Technical Reports Server (NTRS)

    Kiplinger, Alan L.

    2005-01-01

    The Principal Investigator (P.I.) has been pursuing a three year grant under NASA's Sun-Earth Connection Guest Investigator Program in support of the Ramaty High Energy Solar Spectroscopic Imager (RHESSI). An objective of these efforts is to combine X-ray and other data on solar flares, coronal mass ejections and interplanetary particle events in order to obtain a more comprehensive recognition of signatures, and understanding of interplanetary proton events. Thus, part of these efforts are to investigate if signatures seen in hard X-rays and microwaves can lead to better predictions of interplanetary proton events that can be dangerous to astronauts and spacecraft. The original proposal was written in May, 2000 and it discusses a three-pronged approach for data comparisons with three new types of instrumentation observing at X-ray, microwave and optical wavelengths. The major impetus behind this work and the proposal is that the P.I. discovered a strong correlation between a particular type of hard X-ray signature seen in spectral evolutions and interplanetary proton events (Kiplinger, 1995). The basic signature is that hard X-ray flux peaks either exhibit spectra that soften on their decays (Le. show fewer and fewer high energy X-rays with time) or they harden during decays (i.e. high energy X-rays decay significantly slower that lower energy X-rays). This signature is called progressive hardening. Studies were conducted over an eight-year period of data from the Hard X-Ray Burst Spectrometer (HXRBS) of the Solar maximum mission. Out of the 750 well observed flares studied, 41 flares had major associated proton events. Of these, 29 events were predicted on the basis of progressive hardening for a hit rate of 71%. The 152 largest flares had a hit rate of 82%.

  6. Multi-Sited Global Ethnography and Travel: Gendered Journeys in Three Registers

    ERIC Educational Resources Information Center

    Epstein, Debbie; Fahey, Johannah; Kenway, Jane

    2013-01-01

    This paper joins a barely begun conversation about multi-sited and global ethnography in educational research; a conversation that is likely to intensify along with growing interest in the links between education, globalisation, internationalisation and transnationalism. Drawing on an ongoing multi-sited global ethnography of elite schools and…

  7. Multisite Image Data Collection and Management Using the RSNA Image Sharing Network

    PubMed Central

    Erickson, Bradley J; Fajnwaks, Patricio; Langer, Steve G; Perry, John

    2014-01-01

    The execution of a multisite trial frequently includes image collection. The Clinical Trials Processor (CTP) makes removal of protected health information highly reliable. It also provides reliable transfer of images to a central review site. Trials using central review of imaging should consider using CTP for handling image data when a multisite trial is being designed. PMID:24772205

  8. Multisite surface electromyography and complementary healing intervention: a comparative analysis.

    PubMed

    Wirth, D P; Cram, J R

    1997-01-01

    A comparative analysis was conducted on a series of three experimental studies that examined the effect of various local and nonlocal (distant) complementary healing methods on multisite surface electromyographic (sEMG) and autonomic measures. The series concentrated sEMG electrode placement on specific neuromuscular paraspinal centers (cervical [C4], thoracic [T6], and lumbar [L3]), along with the frontalis region, due to the fact that these sites corresponded to the location of individual chakra centers as delineated in ancient Eastern medical and philosophical texts. It was hypothesized that the sEMG assessment procedure had the potential to provide objective, quantifiable correlates for complementary healing treatment effects, as well as assess the energy flow through the chakras during a healing treatment. The studies were the first of their kind to incorporate randomized, double-blind, placebo-controlled protocols in order to evaluate correlative neuromuscular multisite sEMG paraspinal measures with different complementary healing treatment interventions. Although the measurement protocols were similar between experiments, the results, demonstrated by the individual studies, varied. Whereas the overall findings of the series are encouraging because they indicate a potential objective scientific correlate to complementary healing treatment intervention, the results are considered preliminary in nature and appear to be linked to either the meditational experience of the subjects or dependent on the particular healer(s) used. Additional research is needed in order to establish the multisite sEMG assessment procedure as a reliable correlative measure for complementary healing treatment effects and to determine whether a consistent replicative treatment effect can be demonstrated independent of the specific subject population or practitioner(s) used. PMID:9449057

  9. Lessons Learned From an International, Multisite Simulation Research Study.

    PubMed

    Foronda, Cynthia; Alhusen, Jeanne

    2016-01-01

    The purpose of this article is to describe the process and lessons learned in conducting an international, multisite simulation research study. Key lessons include asking site leaders to complete human subjects training early, applying for a deferral agreement for multiple sites, standardization, seeking consultation, considering differences in simulation centers, and having a back-up plan if committed team members are unable to progress. Although challenging, this process yields many rewards and raises the state of the science to improve pedagogy and student learning outcomes. PMID:26779693

  10. Effective interactions in multisite cells for adsorption in microporous materials

    NASA Astrophysics Data System (ADS)

    Demontis, Pierfranco; Pazzona, Federico G.; Suffritti, Giuseppe B.

    2009-04-01

    Local, discrete models of self-interacting multisite adsorption cells have been shown to be able to provide a coarse-grained representation of equilibrium properties of small molecules adsorbed in nanoporous materials at the mesoscopic scale. In the present work we show how the essential statistical properties of a host cell of structured sites with multiple adsorption energies and particle-particle interactions (that is the partition function, the average energy, and the average number of guests close to the windows connecting the cell to its surroundings) can be reproduced by a less-structured cell with two occupancy-dependent adsorption energy levels.

  11. Spectroscopic Observations of SN 2012fr: A Luminous, Normal Type Ia Supernova with Early High-velocity Features and a Late Velocity Plateau

    NASA Astrophysics Data System (ADS)

    Childress, M. J.; Scalzo, R. A.; Sim, S. A.; Tucker, B. E.; Yuan, F.; Schmidt, B. P.; Cenko, S. B.; Silverman, J. M.; Contreras, C.; Hsiao, E. Y.; Phillips, M.; Morrell, N.; Jha, S. W.; McCully, C.; Filippenko, A. V.; Anderson, J. P.; Benetti, S.; Bufano, F.; de Jaeger, T.; Forster, F.; Gal-Yam, A.; Le Guillou, L.; Maguire, K.; Maund, J.; Mazzali, P. A.; Pignata, G.; Smartt, S.; Spyromilio, J.; Sullivan, M.; Taddia, F.; Valenti, S.; Bayliss, D. D. R.; Bessell, M.; Blanc, G. A.; Carson, D. J.; Clubb, K. I.; de Burgh-Day, C.; Desjardins, T. D.; Fang, J. J.; Fox, O. D.; Gates, E. L.; Ho, I.-T.; Keller, S.; Kelly, P. L.; Lidman, C.; Loaring, N. S.; Mould, J. R.; Owers, M.; Ozbilgen, S.; Pei, L.; Pickering, T.; Pracy, M. B.; Rich, J. A.; Schaefer, B. E.; Scott, N.; Stritzinger, M.; Vogt, F. P. A.; Zhou, G.

    2013-06-01

    We present 65 optical spectra of the Type Ia SN 2012fr, 33 of which were obtained before maximum light. At early times, SN 2012fr shows clear evidence of a high-velocity feature (HVF) in the Si II λ6355 line that can be cleanly decoupled from the lower velocity "photospheric" component. This Si II λ6355 HVF fades by phase -5 subsequently, the photospheric component exhibits a very narrow velocity width and remains at a nearly constant velocity of ~12,000 km s-1 until at least five weeks after maximum brightness. The Ca II infrared triplet exhibits similar evidence for both a photospheric component at v ≈ 12,000 km s-1 with narrow line width and long velocity plateau, as well as an HVF beginning at v ≈ 31,000 km s-1 two weeks before maximum. SN 2012fr resides on the border between the "shallow silicon" and "core-normal" subclasses in the Branch et al. classification scheme, and on the border between normal and high-velocity Type Ia supernovae (SNe Ia) in the Wang et al. system. Though it is a clear member of the "low velocity gradient" group of SNe Ia and exhibits a very slow light-curve decline, it shows key dissimilarities with the overluminous SN 1991T or SN 1999aa subclasses of SNe Ia. SN 2012fr represents a well-observed SN Ia at the luminous end of the normal SN Ia distribution and a key transitional event between nominal spectroscopic subclasses of SNe Ia.

  12. Multisite multivariate modeling of daily precipitation and temperature in the Canadian Prairie Provinces using generalized linear models

    NASA Astrophysics Data System (ADS)

    Asong, Zilefac E.; Khaliq, M. N.; Wheater, H. S.

    2016-02-01

    Based on the Generalized Linear Model (GLM) framework, a multisite stochastic modelling approach is developed using daily observations of precipitation and minimum and maximum temperatures from 120 sites located across the Canadian Prairie Provinces: Alberta, Saskatchewan and Manitoba. Temperature is modeled using a two-stage normal-heteroscedastic model by fitting mean and variance components separately. Likewise, precipitation occurrence and conditional precipitation intensity processes are modeled separately. The relationship between precipitation and temperature is accounted for by using transformations of precipitation as covariates to predict temperature fields. Large scale atmospheric covariates from the National Center for Environmental Prediction Reanalysis-I, teleconnection indices, geographical site attributes, and observed precipitation and temperature records are used to calibrate these models for the 1971-2000 period. Validation of the developed models is performed on both pre- and post-calibration period data. Results of the study indicate that the developed models are able to capture spatiotemporal characteristics of observed precipitation and temperature fields, such as inter-site and inter-variable correlation structure, and systematic regional variations present in observed sequences. A number of simulated weather statistics ranging from seasonal means to characteristics of temperature and precipitation extremes and some of the commonly used climate indices are also found to be in close agreement with those derived from observed data. This GLM-based modelling approach will be developed further for multisite statistical downscaling of Global Climate Model outputs to explore climate variability and change in this region of Canada.

  13. A queueing approach to multi-site enzyme kinetics

    PubMed Central

    Hochendoner, Philip; Ogle, Curtis; Mather, William H.

    2014-01-01

    Multi-site enzymes, defined as where multiple substrate molecules can bind simultaneously to the same enzyme molecule, play a key role in a number of biological networks, with the Escherichia coli protease ClpXP a well-studied example. These enzymes can form a low latency ‘waiting line’ of substrate to the enzyme's catalytic core, such that the enzyme molecule can continue to collect substrate even when the catalytic core is occupied. To understand multi-site enzyme kinetics, we study a discrete stochastic model that includes a single catalytic core fed by a fixed number of substrate binding sites. A natural queueing systems analogy is found to provide substantial insight into the dynamics of the model. From this, we derive exact results for the probability distribution of the enzyme configuration and for the distribution of substrate departure times in the case of identical but distinguishable classes of substrate molecules. Comments are also provided for the case when different classes of substrate molecules are not processed identically. PMID:24904740

  14. Spectroscopic Binary Stars

    NASA Astrophysics Data System (ADS)

    Batten, A.; Murdin, P.

    2000-11-01

    Historically, spectroscopic binary stars were binary systems whose nature was discovered by the changing DOPPLER EFFECT or shift of the spectral lines of one or both of the component stars. The observed Doppler shift is a combination of that produced by the constant RADIAL VELOCITY (i.e. line-of-sight velocity) of the center of mass of the whole system, and the variable shift resulting from the o...

  15. The s-process in low-metallicity stars - II. Interpretation of high-resolution spectroscopic observations with asymptotic giant branch models

    NASA Astrophysics Data System (ADS)

    Bisterzo, S.; Gallino, R.; Straniero, O.; Cristallo, S.; Käppeler, F.

    2011-11-01

    High-resolution spectroscopic observations of 100 metal-poor carbon and s-rich stars (CEMP-s) collected from the literature are compared with the theoretical nucleosynthesis models of the asymptotic giant branch (AGB) presented in Paper I (MAGBini= 1.3, 1.4, 1.5, 2 M⊙, - 3.6 ≲ [ Fe/H ] ≲- 1.5). The s-process enhancement detected in these objects is associated with binary systems: the more massive companion evolved faster through the thermally pulsing AGB phase (TP-AGB), synthesizing s-elements in the inner He intershell, which are partly dredged up to the surface during the third dredge-up (TDU) episode. The secondary observed low-mass companion became CEMP-s by the mass transfer of C- and s-rich material from the primary AGB. We analyse the light elements C, N, O, Na and Mg, as well as the two s-process indicators, [hs/ls] (where ls = is the the light-s peak at N = 50 and hs = the heavy-s peak at N = 82) and [Pb/hs]. We distinguish between CEMP-s with high s-process enhancement, [hs/Fe] >rsim 1.5 (CEMP-sII), and mild s-process enhanced stars, [hs/Fe] < 1.5 (CEMP-sI). To interpret the observations, a range of s-process efficiencies at any given metallicity is necessary. This is confirmed by the high spread observed in [Pb/hs] (˜2 dex). A degeneration of solutions is found with some exceptions: most main-sequence CEMP-sII stars with low [Na/Fe] can only be interpreted with MAGBini= 1.3-1.4 M⊙. Giants having suffered the first dredge-up (FDU) need a dilution >rsim1 dex (dil is defined as the mass of the convective envelope of the observed star, Mobs★, over the material transferred from the AGB to the companion, MtransAGB). Then AGB models with higher AGB initial masses (MAGBini= 1.5-2 M⊙) are adopted to interpret CEMP-sII giants. In general, solutions with AGB models in the mass range MAGBini= 1.3-2 M⊙ and different dilution factors are found for CEMP-sI stars. About half of the CEMP-s stars with europium measurements show a high r

  16. Deciphering the Interplay among Multisite Phosphorylation, Interaction Dynamics, and Conformational Transitions in a Tripartite Protein System

    PubMed Central

    2016-01-01

    Multisite phosphorylation is a common pathway to regulate protein function, activity, and interaction pattern in vivo, but routine biochemical analysis is often insufficient to identify the number and order of individual phosphorylation reactions and their mechanistic impact on the protein behavior. Here, we integrate complementary mass spectrometry (MS)-based approaches to characterize a multisite phosphorylation-regulated protein system comprising Polo-like kinase 1 (Plk1) and its coactivators Aurora kinase A (Aur-A) and Bora, the interplay of which is essential for mitotic entry after DNA damage-induced cell cycle arrest. Native MS and cross-linking–MS revealed that Aur-A/Bora-mediated Plk1 activation is accompanied by the formation of Aur-A/Bora and Plk1/Bora heterodimers. We found that the Aur-A/Bora interaction is independent of the Bora phosphorylation state, whereas the Plk1/Bora interaction is dependent on extensive Bora multisite phosphorylation. Bottom-up and top-down proteomics analyses showed that Bora multisite phosphorylation proceeds via a well-ordered sequence of site-specific phosphorylation reactions, whereby we could reveal the involvement of up to 16 phosphorylated Bora residues. Ion mobility spectrometry–MS demonstrated that this multisite phosphorylation primes a substantial structural rearrangement of Bora, explaining the interdependence between extensive Bora multisite phosphorylation and Plk1/Bora complex formation. These results represent a first benchmark of our multipronged MS strategy, highlighting its potential to elucidate the mechanistic and structural implications of multisite protein phosphorylation. PMID:27504491

  17. High-resolution spectroscopic observations of binary stars and yellow stragglers in three open clusters: NGC 2360, NGC 3680, and NGC 5822

    SciTech Connect

    Sales Silva, J. V.; Peña Suárez, V. J.; Katime Santrich, O. J.; Pereira, C. B.; Drake, N. A.; Roig, F. E-mail: jearim@on.br E-mail: claudio@on.br E-mail: froig@on.br

    2014-11-01

    Binary stars in open clusters are very useful targets in constraining the nucleosynthesis process. The luminosities of the stars are known because the distances of the clusters are also known, so chemical peculiarities can be linked directly to the evolutionary status of a star. In addition, binary stars offer the opportunity to verify a relationship between them and the straggler population in both globular and open clusters. We carried out a detailed spectroscopic analysis to derive the atmospheric parameters for 16 red giants in binary systems and the chemical composition of 11 of them in the open clusters NGC 2360, NGC 3680, and NGC 5822. We obtained abundances of C, N, O, Na, Mg, Al, Ca, Si, Ti, Ni, Cr, Y, Zr, La, Ce, and Nd. The atmospheric parameters of the studied stars and their chemical abundances were determined using high-resolution optical spectroscopy. We employ the local thermodynamic equilibrium model atmospheres of Kurucz and the spectral analysis code MOOG. The abundances of the light elements were derived using the spectral synthesis technique. We found that the stars NGC 2360-92 and 96, NGC 3680-34, and NGC 5822-4 and 312 are yellow straggler stars. We show that the spectra of NGC 5822-4 and 312 present evidence of contamination by an A-type star as a secondary star. For the other yellow stragglers, evidence of contamination is given by the broad wings of the Hα. Detection of yellow straggler stars is important because the observed number can be compared with the number predicted by simulations of binary stellar evolution in open clusters. We also found that the other binary stars are not s-process enriched, which may suggest that in these binaries the secondary star is probably a faint main-sequence object. The lack of any s-process enrichment is very useful in setting constraints for the number of white dwarfs in the open cluster, a subject that is related to the birthrate of these kinds of stars in open clusters and also to the age of a

  18. Multi-site identification of a distributed hydrological nitrogen model using Bayesian uncertainty analysis

    NASA Astrophysics Data System (ADS)

    Jiang, Sanyuan; Jomaa, Seifeddine; Büttner, Olaf; Meon, Günter; Rode, Michael

    2015-10-01

    For capturing spatial variations of runoff and nutrient fluxes attributed to catchment heterogeneity, multi-site hydrological water quality monitoring strategies are increasingly put into practice. This study aimed to investigate the impacts of spatially distributed streamflow and streamwater Inorganic Nitrogen (IN) concentration observations on the identification of a continuous time, spatially semi-distributed and process-based hydrological water quality model HYPE (HYdrological Predictions for the Environment). A Bayesian inference based approach DREAM(ZS) (DiffeRential Evolution Adaptive Metrololis algorithm) was combined with HYPE to implement model optimisation and uncertainty analysis on streamflow and streamwater IN concentration simulations at a nested meso scale catchment in central Germany. To this end, a 10-year period (1994-1999 for calibration and 1999-2004 for validation) was utilised. We compared the parameters' posterior distributions, modelling performance using the best estimated parameter set and 95% prediction confidence intervals at catchment outlet for the calibration period that were derived from single-site calibration (SSC) and multi-site calibration (MSC) modes. For SSC, streamflow and streamwater IN concentration observations at only the catchment outlet were used. While, for MSC, streamflow and streamwater IN concentration observations from both catchment outlet and two internal sites were considered. Results showed that the uncertainty intervals of hydrological water quality parameters' posterior distributions estimated from MSC, were narrower than those obtained from SSC. In addition, it was found that the MSC outperformed SSC on streamwater IN concentration simulations at internal sites for both calibration and validation periods, while the influence on streamflow modelling performance was small. This can be explained by the "nested" nature of the catchment and high correlation between discharge observations from different sites

  19. In-Situ Measurements of HCN and CH3CN in the Pacific Troposphere: Sources, Sinks, and Comparisons with Spectroscopic Observations

    NASA Technical Reports Server (NTRS)

    Singh, Hanwant B.; Salas, L.; Herlth, D.; Czech, E.; Viezee, W.; Li, Q.; Jacob, D. J.; Blake, D.; Sachse, G.; Harward, C. N.; Hipskind, R. Stephen (Technical Monitor)

    2002-01-01

    We report the first in-situ measurements of hydrogen cyanide (HCN) and acetonitrile (CH3CN) from the Pacific troposphere (0-12 km) obtained during the NASA/Trace-P mission (Feb.-April, 2001). Mean HCN and CH3CN mixing ratios of 243 (+/-118) ppt and 149 (+/-56) ppt respectively, were measured. The in-situ observations correspond to a total HCN column of 4.4-4.9 x 10(exp 15) molec. cm(exp -2) and a CH3CN column of 2.8-3.0 x 10(exp 15) molec. cm(exp -2). This HCN column is in good agreement with available spectroscopic observations. The atmospheric concentrations of HCN and CH3CN were greatly influenced by outflow of pollution from Asia. There is a linear relationship between the mixing ratios of HCN and CH3CN, and in turn these are well correlated with tracers of biomass combustion (e.g. CH3Cl, CO). Relative enhancements with respect to known tracers of biomass combustion within selected plumes in the free troposphere, and pollution episodes in the boundary layer allow an estimation of a global biomass burning source of 0.8+/-0.4 Tg (N)/y for HCN and 0.4+/-0.1 Tg (N)/y for CH3CN. In comparison, emissions from automobiles and industry are quite small (<0.05 Tg (N)/y). The vertical structure of HCN and CH3CN indicated reduced mixing ratios in the MBL (Marine Boundary Layer). Using, a simple box model, the observed gradients across the top of the MBL are used to derive an oceanic flux of 6.7 x 10(exp -15) g (N) cm(exp -2)/s for HCN and 4.8 x 10(exp -15) g (N) cm(exp -2)/s for CH3CN. An air-sea exchange model is used to conclude that this flux can be maintained if the oceans are under-saturated in HCN and CH3CN by 23% and 17%, respectively. It is inferred that oceanic loss is a dominant sink for these nitrites, and they deposit some 1.3 Tg (N) of nitrogen annually to the oceans. Assuming reaction with OH radicals and loss to the oceans as the major removal processes, a mean atmospheric residence time of 4.7 months for HCN and 5.1 months for CH3CN is calculated. A global

  20. Spectroscopic pulsational frequency identification and mode determination of γ Doradus star HD 12901

    NASA Astrophysics Data System (ADS)

    Brunsden, E.; Pollard, K. R.; Cottrell, P. L.; Wright, D. J.; De Cat, P.

    2012-12-01

    Using multisite spectroscopic data collected from three sites, the frequencies and pulsational modes of the γ Doradus star HD 12901 were identified. A total of six frequencies in the range 1-2 d-1 were observed, their identifications supported by multiple line-profile measurement techniques and previously published photometry. Five frequencies were of sufficient signal-to-noise ratio for mode identification, and all five displayed similar three-bump standard deviation profiles which were fitted well with (l,m) = (1,1) modes. These fits had reduced χ2 values of less than 18. We propose that this star is an excellent candidate to test models of non-radially pulsating γ Doradus stars as a result of the presence of multiple (1,1) modes. This paper includes data taken at the Mount John University Observatory of the University of Canterbury (New Zealand), the McDonald Observatory of the University of Texas at Austin (Texas, USA) and the European Southern Observatory at La Silla (Chile).

  1. Spectroscopic parallaxes of MAP region stars from UBVRI, DDO, and uvbyH-beta photometry. [Multichannel Astrometric Photometer for astronomical observation

    NASA Technical Reports Server (NTRS)

    Persinger, Tim; Castelaz, Michael W.

    1990-01-01

    This paper presents the results of spectral type and luminosity classification of reference stars in the Allegheny Observatory MAP parallax program, using broadband and intermediate-band photometry. In addition to the use of UBVRI and DDO photometric systems, the uvbyH-beta photometric system was included for classification of blue (B - V less than 0.6) reference stars. The stellar classifications made from the photometry are used to determine spectroscopic parallaxes. The spectroscopic parallaxes are used in turn to adjust the relative parallaxes measured with the MAP to absolute parallaxes. A new method for dereddening stars using more than one photometric system is presented. In the process of dereddening, visual extinctions, spectral types, and luminosity classes are determined, as well as a measure of the goodness of fit. The measure of goodness of fit quantifies confidence in the stellar classifications. It is found that the spectral types are reliable to within 2.5 spectral subclasses.

  2. Multisite Pacing for Cardiac Resynchronization Therapy: Promise and Pitfalls.

    PubMed

    Antoniadis, Antonios P; Behar, Jonathan M; Claridge, Simon; Jackson, Tom; Sohal, Manav; Rinaldi, Christopher Aldo

    2016-07-01

    Cardiac resynchronization therapy (CRT) reduces the morbidity and mortality of patients with symptomatic heart failure and intraventricular conduction delay. However, its clinical outcomes are non-uniform and up to one third of treated patients are subsequently classified as non-responders. Multisite pacing (MSP), i.e. stimulating the myocardium from multiple locations, has emerged as a potential therapeutic option in patients requiring CRT. The rationale for MSP is based on the hypothesis that increasing the pacing locations in the left ventricle results in a more physiologic and coordinated myocardial systole. MSP can be achieved by additional leads in the right or left ventricle but this can lead to high battery drain and more frequent generator replacements. Multipolar left ventricular leads can deliver pacing at multiple sites, and therefore, a single lead can be used for MSP. However, the optimal programming settings and the outcomes of this approach remain yet to be determined. PMID:27216844

  3. Four-dimensional multi-site two-photon excitation

    NASA Astrophysics Data System (ADS)

    Daria, Vincent R.; Stricker, Christian; Bowman, Richard; Bachor, Hans-A.; Redman, Stephen

    2010-02-01

    We use the holographic method to project an arbitrary array of diffraction-limited focal spots suitable for multi-site twophoton excitation. The spot array can be projected arbitrarily within a three-dimensional (3D) volume, while the fourth dimension in time is attributed to high temporal resolution via high-speed non-iterative calculation of the hologram using a video graphics accelerator board. We show that the spots have sufficient energy and spatiotemporal photon density for localized two-photon excitation at individual spots in the array. The significance of this work points to 3D microscopy, non-linear micro-fabrication, volume holographic optical storage and biomedical instrumentation. In neuroscience, timecritical release of neurotransmitters at multiple sites within complex dendritic trees of neurons can lead to insights on the mechanisms of information processing in the brain.

  4. Power estimation for non-standardized multisite studies.

    PubMed

    Keshavan, Anisha; Paul, Friedemann; Beyer, Mona K; Zhu, Alyssa H; Papinutto, Nico; Shinohara, Russell T; Stern, William; Amann, Michael; Bakshi, Rohit; Bischof, Antje; Carriero, Alessandro; Comabella, Manuel; Crane, Jason C; D'Alfonso, Sandra; Demaerel, Philippe; Dubois, Benedicte; Filippi, Massimo; Fleischer, Vinzenz; Fontaine, Bertrand; Gaetano, Laura; Goris, An; Graetz, Christiane; Gröger, Adriane; Groppa, Sergiu; Hafler, David A; Harbo, Hanne F; Hemmer, Bernhard; Jordan, Kesshi; Kappos, Ludwig; Kirkish, Gina; Llufriu, Sara; Magon, Stefano; Martinelli-Boneschi, Filippo; McCauley, Jacob L; Montalban, Xavier; Mühlau, Mark; Pelletier, Daniel; Pattany, Pradip M; Pericak-Vance, Margaret; Cournu-Rebeix, Isabelle; Rocca, Maria A; Rovira, Alex; Schlaeger, Regina; Saiz, Albert; Sprenger, Till; Stecco, Alessandro; Uitdehaag, Bernard M J; Villoslada, Pablo; Wattjes, Mike P; Weiner, Howard; Wuerfel, Jens; Zimmer, Claus; Zipp, Frauke; Hauser, Stephen L; Oksenberg, Jorge R; Henry, Roland G

    2016-07-01

    A concern for researchers planning multisite studies is that scanner and T1-weighted sequence-related biases on regional volumes could overshadow true effects, especially for studies with a heterogeneous set of scanners and sequences. Current approaches attempt to harmonize data by standardizing hardware, pulse sequences, and protocols, or by calibrating across sites using phantom-based corrections to ensure the same raw image intensities. We propose to avoid harmonization and phantom-based correction entirely. We hypothesized that the bias of estimated regional volumes is scaled between sites due to the contrast and gradient distortion differences between scanners and sequences. Given this assumption, we provide a new statistical framework and derive a power equation to define inclusion criteria for a set of sites based on the variability of their scaling factors. We estimated the scaling factors of 20 scanners with heterogeneous hardware and sequence parameters by scanning a single set of 12 subjects at sites across the United States and Europe. Regional volumes and their scaling factors were estimated for each site using Freesurfer's segmentation algorithm and ordinary least squares, respectively. The scaling factors were validated by comparing the theoretical and simulated power curves, performing a leave-one-out calibration of regional volumes, and evaluating the absolute agreement of all regional volumes between sites before and after calibration. Using our derived power equation, we were able to define the conditions under which harmonization is not necessary to achieve 80% power. This approach can inform choice of processing pipelines and outcome metrics for multisite studies based on scaling factor variability across sites, enabling collaboration between clinical and research institutions. PMID:27039700

  5. Efficient Calculations with Multisite Local Orbitals in a Large-Scale DFT Code CONQUEST.

    PubMed

    Nakata, Ayako; Bowler, David R; Miyazaki, Tsuyoshi

    2014-11-11

    Multisite local orbitals, which are formed from linear combinations of pseudoatomic orbitals from a target atom and its neighbor atoms, have been introduced in the large-scale density functional theory calculation code CONQUEST. Multisite local orbitals correspond to local molecular orbitals so that the number of required local orbitals can be minimal. The multisite support functions are determined by using the localized filter diagonalization (LFD) method [ Phys. Rev. B 2009 , 80 , 205104 ]. Two new methods, the double cutoff method and the smoothing method, are introduced to the LFD method to improve efficiency and stability. The Hamiltonian and overlap matrices with multisite local orbitals are constructed by efficient sparse-matrix multiplications in CONQUEST. The investigation of the calculated energetic and geometrical properties and band structures of bulk Si, Al, and DNA systems demonstrate the accuracy and the computational efficiency of the present method. The representability of both occupied and unoccupied band structures with the present method has been also confirmed. PMID:26584368

  6. Spectroscopically Unlocking Exoplanet Characteristics

    NASA Astrophysics Data System (ADS)

    Lewis, Nikole

    2016-05-01

    Spectroscopy plays a critical role in a number of areas of exoplanet research. The first exoplanets were detected by precisely measuring Doppler shifts in high resolution (R ~ 100,000) stellar spectra, a technique that has become known as the Radial Velocity (RV) method. The RV method provides critical constraints on exoplanet masses, but is currently limited to some degree by robust line shape predictions. Beyond the RV method, spectroscopy plays a critical role in the characterization of exoplanets beyond their mass and radius. The Hubble Space Telescope has spectroscopically observed the atmospheres of exoplanets that transit their host stars as seen from Earth giving us key insights into atmospheric abundances of key atomic and molecular species as well as cloud optical properties. Similar spectroscopic characterization of exoplanet atmospheres will be carried out at higher resolution (R ~ 100-3000) and with broader wavelength coverage with the James Webb Space Telescope. Future missions such as WFIRST that seek to the pave the way toward the detection and characterization of potentially habitable planets will have the capability of directly measuring the spectra of exoplanet atmospheres and potentially surfaces. Our ability to plan for and interpret spectra from exoplanets relies heavily on the fidelity of the spectroscopic databases available and would greatly benefit from further laboratory and theoretical work aimed at optical properties of atomic, molecular, and cloud/haze species in the pressure and temperature regimes relevant to exoplanet atmospheres.

  7. The value and potential of multisited ethnography for science education research: a review of Jrène Rahm's Science in the Making at the Margin

    NASA Astrophysics Data System (ADS)

    Beeman-Cadwallader, Nicole

    2012-03-01

    Rahm sought to illuminate how children and youth make meaning of science in three out-of-school time programs, and the identity work that is done through the trajectory of their youth toward their young adulthood. Through using multisited ethnography, she asserts that we can learn more about what the youth say about their science learning and science literacy development in these programs. She has revealed through her rich data the potential value of multisited ethnography for science education research. A similar theme of insider/outsider status to science emerged in each of the three sites. The nature of the data collected in Rahm's multisited ethnography allowed for the unveiling of the similarities in this theme, but also made evident the nuanced ways that this theme presented itself differently across the three sites. The additional potential came through in the varied data Rahm could have delved into and did not. A unique characteristic of ethnographic research, that is not necessarily present in other research methods, is that a wide array of varied data is collected. An analysis of documents, images, and observational field notes, which go beyond interview data, may provide deeper understandings previously untouched in science education.

  8. Increased free-water in the substantia nigra of Parkinson’s disease: a single-site and multi-site study

    PubMed Central

    Ofori, E.; Pasternak, O.; Planetta, P.J.; Burciu, R.; Snyder, A.; Febo, M.; Golde, T.E.; Okun, M.S.; Vaillancourt, D.E.

    2014-01-01

    Measures from diffusion magnetic resonance imaging reflect changes in the substantia nigra of Parkinson’s disease. It is the case, however, that partial volume effects from free-water can bias diffusion measurements. The bi-tensor diffusion model was introduced to quantify the contribution of free-water and eliminates its bias on estimations of tissue microstructure. Here, we test the hypothesis that free-water is elevated in the substantia nigra for Parkinson’s disease compared with controls. This hypothesis was tested between large cohorts of Parkinson’s disease and control participants in a single-site study, and validated against a multi-site study using multiple scanners. The fractional volume of free-water was increased in the posterior region of the substantia nigra in Parkinson’s disease compared with controls in both the single-site and multi-site studies. We did not observe changes in either cohort for free-water corrected fractional anisotropy or free-water corrected mean diffusivity. Our findings provide new evidence that the free-water index reflects alteration of the substantia nigra in Parkinson’s disease, and this was evidenced across both single-site and multi-site cohorts. PMID:25467638

  9. High-Accuracy Quartic Force Field Calculations for the Spectroscopic Constants and Vibrational Frequencies of 1(exp 1)A' l-C3H(-): A Possible Link to Lines Observed in the Horsehead Nebula PDR

    NASA Technical Reports Server (NTRS)

    Fortenberry, Ryan C.; Huang, Xinchuan; Crawford, T. Daniel; Lee, Timothy J.

    2013-01-01

    It has been shown that rotational lines observed in the Horsehead nebula photon-dominated-region (PDR) are probably not caused by l-C3H+, as was originally suggested. In the search for viable alternative candidate carriers, quartic force fields are employed here to provide highly accurate rotational constants, as well as fundamental vibrational frequencies, for another candidate carrier: 1 (sup 1)A' C3H(-). The ab initio computed spectroscopic constants provided in this work are, compared to those necessary to define the observed lines, as accurate as the computed spectroscopic constants for many of the known interstellar anions. Additionally, the computed D-eff for C3H(-) is three times closer to the D deduced from the observed Horsehead nebula lines relative to l-C3H(+). As a result, 1 (sup 1)A' C3H(-). is a more viable candidate for these observed rotational transitions and would be the seventh confirmed interstellar anion detected within the past decade and the first C(sub n)H(-) molecular anion with an odd n.

  10. A modular class of multisite monthly rainfall generators for water resource management and impact studies

    NASA Astrophysics Data System (ADS)

    Serinaldi, Francesco; Kilsby, Chris G.

    2012-09-01

    SummaryThis study introduces a class of stochastic multisite monthly rainfall generators devised for application in water resources management problems, such as the sensitivity analysis of droughts and extreme rainfall scenarios under external climatic and non-climatic forcing mechanisms. The modelling framework relies on three elements: (1) a classical deseasonalisation scheme based on log-transformed observations, (2) the nonparametric bootstrap resampling approach and (3) parametric Generalized Additive Models for Location, Scale and Shape (GAMLSS). As the bootstrap and GAMLSS modules are alternative techniques for simulating each month, the free choice between them makes the structure of the model modular and flexible, so that it can be easily adapted to different climatic conditions, and can be customized based on the specific water resource problem. The model was set up and calibrated to simulate monthly rainfall from six locations in England and Wales to produce a suitable input for drought analysis. The results of the case study point out that the model can capture several characteristics of the rainfall series. In particular, it enables the simulation of low and high rainfall scenarios more extreme than those observed as well as the reproduction of the distribution of the annual accumulated rainfall, and of the relationship between the rainfall and circulation indices such as North Atlantic Oscillation (NAO) and Sea Surface Temperature (SST), thus making the framework well-suited for sensitivity analysis under alternative climate scenarios and additional forcing variables.

  11. A DVD Spectroscope: A Simple, High-Resolution Classroom Spectroscope

    ERIC Educational Resources Information Center

    Wakabayashi, Fumitaka; Hamada, Kiyohito

    2006-01-01

    Digital versatile disks (DVDs) have successfully made up an inexpensive but high-resolution spectroscope suitable for classroom experiments that can easily be made with common material and gives clear and fine spectra of various light sources and colored material. The observed spectra can be photographed with a digital camera, and such images can…

  12. Four-dimensional multi-site photolysis of caged neurotransmitters

    PubMed Central

    Go, Mary Ann; To, Minh-Son; Stricker, Christian; Redman, Stephen; Bachor, Hans-A.; Stuart, Greg J.; Daria, Vincent R.

    2013-01-01

    Neurons receive thousands of synaptic inputs that are distributed in space and time. The systematic study of how neurons process these inputs requires a technique to stimulate multiple yet highly targeted points of interest along the neuron's dendritic tree. Three-dimensional multi-focal patterns produced via holographic projection combined with two-photon photolysis of caged compounds can provide for highly localized release of neurotransmitters within each diffraction-limited focus, and in this way emulate simultaneous synaptic inputs to the neuron. However, this technique so far cannot achieve time-dependent stimulation patterns due to fundamental limitations of the hologram-encoding device and other factors that affect the consistency of controlled synaptic stimulation. Here, we report an advanced technique that enables the design and application of arbitrary spatio-temporal photostimulation patterns that resemble physiological synaptic inputs. By combining holographic projection with a programmable high-speed light-switching array, we have overcome temporal limitations with holographic projection, allowing us to mimic distributed activation of synaptic inputs leading to action potential generation. Our experiments uniquely demonstrate multi-site two-photon glutamate uncaging in three dimensions with submillisecond temporal resolution. Implementing this approach opens up new prospects for studying neuronal synaptic integration in four dimensions. PMID:24348330

  13. Complementary Therapies for Children Undergoing Stem Cell Transplant: Report of A Multisite Trial

    PubMed Central

    Phipps, Sean; Barrera, Maru; Vannatta, Kathryn; Xiong, Xiaoping; Doyle, John J; Alderfer, Melissa A.

    2010-01-01

    Background Children undergoing stem cell transplant (SCT) experience high levels of somatic distress and mood disturbance. This trial evaluated the efficacy of complementary therapies (massage, humor therapy, relaxation/imagery) for reducing distress associated with pediatric SCT. Methods Across 4 sites, 178 pediatric patients scheduled to undergo SCT were randomized to a child-targeted intervention involving massage and humor therapy (HPI-C), the identical child intervention plus a parent intervention involving massage and relaxation/imagery (HPI-CP) or standard care (SC). Randomization was stratified by site, age, and type of transplant. The interventions began at admission and continued through SCT week +3. Primary outcomes included patient and parent reports of somatic distress and mood disturbance obtained weekly from admission through week +6 using the BASES scales. Secondary outcomes included length of hospitalization, time to engraftment, and usage of narcotic analgesic and antiemetic medications. Results A mixed model approach was used to assess longitudinal trends of patient and parent-report outcomes and test differences between groups on these measures. Significant changes across time were observed on all patient and parent-report outcomes. However, no significant differences between treatment arms were found on the primary outcomes. Similarly, no signficant between group differences were noted on any of the medical variables as secondary outcomes. Conclusions Results of this multi-site trial failed to document significant benefits of complementary interventions in the pediatric SCT setting. PMID:20626016

  14. Multisite, multimodal neuroimaging of chronic urological pelvic pain: Methodology of the MAPP Research Network.

    PubMed

    Alger, Jeffry R; Ellingson, Benjamin M; Ashe-McNalley, Cody; Woodworth, Davis C; Labus, Jennifer S; Farmer, Melissa; Huang, Lejian; Apkarian, A Vania; Johnson, Kevin A; Mackey, Sean C; Ness, Timothy J; Deutsch, Georg; Harris, Richard E; Clauw, Daniel J; Glover, Gary H; Parrish, Todd B; Hollander, Jan den; Kusek, John W; Mullins, Chris; Mayer, Emeran A

    2016-01-01

    The Multidisciplinary Approach to the Study of Chronic Pelvic Pain (MAPP) Research Network is an ongoing multi-center collaborative research group established to conduct integrated studies in participants with urologic chronic pelvic pain syndrome (UCPPS). The goal of these investigations is to provide new insights into the etiology, natural history, clinical, demographic and behavioral characteristics, search for new and evaluate candidate biomarkers, systematically test for contributions of infectious agents to symptoms, and conduct animal studies to understand underlying mechanisms for UCPPS. Study participants were enrolled in a one-year observational study and evaluated through a multisite, collaborative neuroimaging study to evaluate the association between UCPPS and brain structure and function. 3D T1-weighted structural images, resting-state fMRI, and high angular resolution diffusion MRI were acquired in five participating MAPP Network sites using 8 separate MRI hardware and software configurations. We describe the neuroimaging methods and procedures used to scan participants, the challenges encountered in obtaining data from multiple sites with different equipment/software, and our efforts to minimize site-to-site variation. PMID:27408791

  15. Gattini: a multisite campaign for the measurement of sky brightness in Antarctica

    NASA Astrophysics Data System (ADS)

    Moore, Anna; Allen, Graham; Aristidi, Eric; Ashley, Michael; Bedding, Tim; Beichman, Chas; Briguglio, Runa; Busso, Maurizio; Candidi, Maurizio; Ciardi, David; Cui, Xiangqun; Cutispoto, Giuseppe; Distefano, Elisa; Espy, Patrick; Everett, Jon; Feng, Longlong; Hu, Jingyao; Jiang, Zhaoji; Kenyon, Suzanne; Kulesa, Craig; Lawrence, Jon; Le Roux, Brice; Leslie, Tim; Li, Yuangshen; Luong-Van, Daniel; Phillips, Andre; Qin, Weijian; Ragazzoni, Roberto; Riddle, Reed; Sabbatini, Lucia; Salinari, Piero; Saunders, Will; Shang, Zhaohui; Stello, Dennis; Storey, John; Sun, Bo; Suntzeff, Nicolas; Taylor, Melinda; Tosti, Gino; Tothill, Nick; Travouillon, Tony; Van Belle, Gerard; Von Braun, Kaspar; Wang, Lifan; Yan, Jun; Yang, Huigen; Yuan, Xiangyan; Zhu, Zhenxi; Zhou, Xu

    2008-07-01

    We present the Gattini project: a multisite campaign to measure the optical sky properties above the two high altitude Antarctic astronomical sites of Dome C and Dome A. The Gattini-DomeC project, part of the IRAIT site testing campaign and ongoing since January 2006, consists of two cameras for the measurement of optical sky brightness, large area cloud cover and auroral detection above the DomeC site, home of the French-Italian Concordia station. The cameras are transit in nature and are virtually identical except for the nature of the lenses. The cameras have operated successfully throughout the past two Antarctic winter seasons and here we present the first results obtained from the returned 2006 dataset. The Gattini-DomeA project will place a similar site testing facility at the highest point on the Antarctic plateau, Dome A, with observations commencing in 2008. The project forms a small part of a much larger venture coordinated by the Polar Research Institute of China as part of the International Polar Year whereby an automated site testing facility called PLATO will be traversed into the DomeA site. The status of this exciting and ambitious project with regards to the Gattini-DomeA cameras will be presented.

  16. Coping Skills Among Adolescent Suicide Attempters: Results of a Multisite Study

    PubMed Central

    Mirkovic, Bojan; Labelle, Réal; Guilé, Jean-Marc; Belloncle, Vincent; Bodeau, Nicolas; Knafo, Alexandra; Condat, Agnès; Bapt-Cazalets, Nathalie; Marguet, Christophe; Breton, Jean-Jacques; Cohen, David; Gérardin, Priscille

    2015-01-01

    Objectives: A multisite study was undertaken to advance our understanding of how coping skills, depression, and suicidal ideation are related among adolescents who attempt suicide. Two hypotheses were postulated: productive coping and nonproductive coping would be associated, respectively, with lower and higher depression scores when age, sex, and stressful life events (SLEs) were controlled; and productive coping and nonproductive coping would be associated, respectively, with the presence and absence of suicidal ideation when age, sex, and SLEs were controlled. Methods: Participants were 167 adolescents (13 to 17 years of age) hospitalized for attempting suicide in 5 pediatric departments across France. Four instruments were administered: the Kiddie Schedule for Affective Disorders and Schizophrenia—Present and Lifetime Version, the Adolescent Coping Scale, the Life Events Questionnaire, and the Columbia-Suicide Severity Rating Scale. Descriptive analyses and univariate and multiple regression models were completed. Results: Both hypotheses were confirmed. Focus on the positive emerged as a significant variable in both models; depression emerged as a significant variable in the suicidal ideation model. The only sex difference observed was that girls made greater use of wishful thinking and seek social support. Conclusions: These findings suggest that coping skills are important mechanisms through which depression and suicidal ideation are maintained after attempting suicide. In intervening with adolescents who have attempted suicide, it may be useful to emphasize cognitive work geared to looking on the bright side, positive thinking, and fighting depression. PMID:25886670

  17. Spectroscopic survey of LAMOST

    NASA Astrophysics Data System (ADS)

    Zhao, Yongheng

    2014-07-01

    LAMOST is a special reflecting Schmidt telescope. LAMOST breaks through the bottleneck of the large scale spectroscopic survey observation with both large aperture (effective aperture of 3.6 - 4.9m) and wide field of view (5 degrees). It is an innovative active reflecting Schmidt configuration achieved by changing mirror surface continuously to achieve a series different reflecting Schmidt system in different moments. By using the parallel controllable fiber positioning technique, the focal surface of 1.75 meters in diameter accommodates 4000 optical fibers. Also, LAMOST has 16 spectrographs with 32 CCD cameras. LAMOST is the telescope of the highest spectrum acquiring rate. As a national large scientific project, LAMOST project was proposed formally in 1996. The construction was started in 2001 and completed in 2008. After commission period, LAMOST pilot survey was started in October 2011 and spectroscopic survey began in September 2012. From October 2011 to June 2013, LAMOST has obtained more than 2 million spectra of celestial objects. There are 1.7 million spectra of stars, in which the stellar parameters (effective temperature, surface gravity, metalicitiy and radial velocity) of more than 1 million stars was obtained. In the first period of spectroscopic survey of LAMOST, 5 million of stellar spectra will be obtained and will make substantial contribution to the study of the stellar astrophysics and the structure of the Galaxy, such as the spheroid substructure of the Galaxy, the galactic gravitational potential and the distribution of the dark matter in the Galaxy, the extremely metal poor stars and hypervelocity stars, the 3D extinction in the Galaxy, the structure of thin and thick disks of the Galaxy, and so on.

  18. How Institutional and University Counselor Policies Effectively Respond to Victims of Cyber Violent Acts: A Multisite Case Study

    ERIC Educational Resources Information Center

    Richards, Gretchen M.

    2012-01-01

    This multisite case study examined how institutional and university counselor policies effectively respond to cyber violent acts. Stake's (2006) multisite case study methodology was used to identify seven themes from current literature. Two sites with four participants were selected. The participants included two counseling directors and the…

  19. Spectroscopic survey of LAMOST

    NASA Astrophysics Data System (ADS)

    Zhao, Yongheng

    2015-08-01

    LAMOST is a special reflecting Schmidt telescope. LAMOST breaks through the bottleneck of the large scale spectroscopic survey observation with both large aperture (effective aperture of 3.6 - 4.9m) and wide field of view (5 degrees). It is an innovative active reflecting Schmidt configuration achieved by changing mirror surface continuously to achieve a series different reflecting Schmidt system in different moments. By using the parallel controllable fiber positioning technique, the focal surface of 1.75 meters in diameter accommodates 4000 optical fibers. Also, LAMOST has 16 spectrographs with 32 CCD cameras. LAMOST is the telescope of the highest spectrum acquiring rate.In the spectroscopic survey of LAMOST from October 2011 to June 2014, LAMOST has obtained more than 4.13 million spectra of celestial objects. There are 3.27 million spectra of stars, in which the stellar parameters of 2.16 million stars were obtained.In the five-year regular survey upto 2017, LAMOST will obtaine 5 million stellar spectra, which would make substantial contribution to the study of the stellar astrophysics and the structure of the Galaxy, such as the spheroid substructure of the Galaxy, the galactic gravitational potential and the distribution of the dark matter in the Galaxy, the extremely metal poor stars and hypervelocity stars, the 3D extinction in the Galaxy, the structure of thin and thick disks of the Galaxy, and so on.

  20. Middle-Eastern plant communities tolerate 9 years of drought in a multi-site climate manipulation experiment

    PubMed Central

    Tielbörger, Katja; Bilton, Mark C.; Metz, Johannes; Kigel, Jaime; Holzapfel, Claus; Lebrija-Trejos, Edwin; Konsens, Irit; Parag, Hadas A.; Sternberg, Marcelo

    2014-01-01

    For evaluating climate change impacts on biodiversity, extensive experiments are urgently needed to complement popular non-mechanistic models which map future ecosystem properties onto their current climatic niche. Here, we experimentally test the main prediction of these models by means of a novel multi-site approach. We implement rainfall manipulations—irrigation and drought—to dryland plant communities situated along a steep climatic gradient in a global biodiversity hotspot containing many wild progenitors of crops. Despite the large extent of our study, spanning nine plant generations and many species, very few differences between treatments were observed in the vegetation response variables: biomass, species composition, species richness and density. The lack of a clear drought effect challenges studies classifying dryland ecosystems as most vulnerable to global change. We attribute this resistance to the tremendous temporal and spatial heterogeneity under which the plants have evolved, concluding that this should be accounted for when predicting future biodiversity change. PMID:25283495

  1. HIGH-ACCURACY QUARTIC FORCE FIELD CALCULATIONS FOR THE SPECTROSCOPIC CONSTANTS AND VIBRATIONAL FREQUENCIES OF 1{sup 1} A' l-C{sub 3}H{sup -}: A POSSIBLE LINK TO LINES OBSERVED IN THE HORSEHEAD NEBULA PHOTODISSOCIATION REGION

    SciTech Connect

    Fortenberry, Ryan C.; Lee, Timothy J.; Huang, Xinchuan; Crawford, T. Daniel

    2013-07-20

    It has been shown that rotational lines observed in the Horsehead nebula photodissociation region (PDR) are probably not caused by l-C{sub 3}H{sup +}, as was originally suggested. In the search for viable alternative candidate carriers, quartic force fields are employed here to provide highly accurate rotational constants, as well as fundamental vibrational frequencies, for another candidate carrier: 1 {sup 1} A' C{sub 3}H{sup -}. The ab initio computed spectroscopic constants provided in this work are, compared to those necessary to define the observed lines, as accurate as the computed spectroscopic constants for many of the known interstellar anions. Additionally, the computed D{sub eff} for C{sub 3}H{sup -} is three times closer to the D deduced from the observed Horsehead nebula lines relative to l-C{sub 3}H{sup +}. As a result, 1 {sup 1} A' C{sub 3}H{sup -} is a more viable candidate for these observed rotational transitions. It has been previously proposed that at least C{sub 6}H{sup -} may be present in the Horsehead nebular PDR formed by way of radiative attachment through its dipole-bound excited state. C{sub 3}H{sup -} could form in a similar way through its dipole-bound state, but its valence excited state increases the number of relaxation pathways possible to reach the ground electronic state. In turn, the rate of formation for C{sub 3}H{sup -} could be greater than the rate of its destruction. C{sub 3}H{sup -} would be the seventh confirmed interstellar anion detected within the past decade and the first C{sub n}H{sup -} molecular anion with an odd n.

  2. High-accuracy Quartic Force Field Calculations for the Spectroscopic Constants and Vibrational Frequencies of 11 A' l-C3H-: A Possible Link to Lines Observed in the Horsehead Nebula Photodissociation Region

    NASA Astrophysics Data System (ADS)

    Fortenberry, Ryan C.; Huang, Xinchuan; Crawford, T. Daniel; Lee, Timothy J.

    2013-07-01

    It has been shown that rotational lines observed in the Horsehead nebula photodissociation region (PDR) are probably not caused by l-C3H+, as was originally suggested. In the search for viable alternative candidate carriers, quartic force fields are employed here to provide highly accurate rotational constants, as well as fundamental vibrational frequencies, for another candidate carrier: 1 1 A' C3H-. The ab initio computed spectroscopic constants provided in this work are, compared to those necessary to define the observed lines, as accurate as the computed spectroscopic constants for many of the known interstellar anions. Additionally, the computed D eff for C3H- is three times closer to the D deduced from the observed Horsehead nebula lines relative to l-C3H+. As a result, 1 1 A' C3H- is a more viable candidate for these observed rotational transitions. It has been previously proposed that at least C6H- may be present in the Horsehead nebular PDR formed by way of radiative attachment through its dipole-bound excited state. C3H- could form in a similar way through its dipole-bound state, but its valence excited state increases the number of relaxation pathways possible to reach the ground electronic state. In turn, the rate of formation for C3H- could be greater than the rate of its destruction. C3H- would be the seventh confirmed interstellar anion detected within the past decade and the first C n H- molecular anion with an odd n.

  3. THE BOLOCAM GALACTIC PLANE SURVEY. X. A COMPLETE SPECTROSCOPIC CATALOG OF DENSE MOLECULAR GAS OBSERVED TOWARD 1.1 mm DUST CONTINUUM SOURCES WITH 7.°5 ≤ l ≤ 194°

    SciTech Connect

    Shirley, Yancy L.; Svoboda, Brian; Ellsworth-Bowers, Timothy P.; Schlingman, Wayne M.; Ginsburg, Adam; Battersby, Cara; Stringfellow, Guy; Glenn, Jason; Bally, John; Rosolowsky, Erik; Gerner, Thomas; Mairs, Steven; Dunham, Miranda K.

    2013-11-01

    The Bolocam Galactic Plane Survey (BGPS) is a 1.1 mm continuum survey of dense clumps of dust throughout the Galaxy covering 170 deg{sup 2}. We present spectroscopic observations using the Heinrich Hertz Submillimeter Telescope of the dense gas tracers, HCO{sup +} and N{sub 2}H{sup +} 3-2, for all 6194 sources in the BGPS v1.0.1 catalog between 7.°5 ≤ l ≤ 194°. This is the largest targeted spectroscopic survey of dense molecular gas in the Milky Way to date. We find unique velocities for 3126 (50.5%) of the BGPS v1.0.1 sources observed. Strong N{sub 2}H{sup +} 3-2 emission (T {sub mb} > 0.5 K) without HCO{sup +} 3-2 emission does not occur in this catalog. We characterize the properties of the dense molecular gas emission toward the entire sample. HCO{sup +} is very sub-thermally populated and the 3-2 transitions are optically thick toward most BGPS clumps. The median observed line width is 3.3 km s{sup –1} consistent with supersonic turbulence within BGPS clumps. We find strong correlations between dense molecular gas integrated intensities and 1.1 mm peak flux and the gas kinetic temperature derived from previously published NH{sub 3} observations. These intensity correlations are driven by the sensitivity of the 3-2 transitions to excitation conditions rather than by variations in molecular column density or abundance. We identify a subset of 113 sources with stronger N{sub 2}H{sup +} than HCO{sup +} integrated intensity, but we find no correlations between the N{sub 2}H{sup +}/HCO{sup +} ratio and 1.1 mm continuum flux density, gas kinetic temperature, or line width. Self-absorbed profiles are rare (1.3%)

  4. Ethics Review for a Multi-Site Project Involving Tribal Nations in the Northern Plains.

    PubMed

    Angal, Jyoti; Petersen, Julie M; Tobacco, Deborah; Elliott, Amy J

    2016-04-01

    Increasingly, Tribal Nations are forming ethics review panels, which function separately from institutional review boards (IRBs). The emergence of strong community representation coincides with a widespread effort supported by the U.S. Department of Health & Human Services and other federal agencies to establish a single IRB for all multi-site research. This article underscores the value of a tribal ethics review board and describes the tribal oversight for the Safe Passage Study-a multi-site, community-based project in the Northern Plains. Our experience demonstrates the benefits of tribal ethics review and makes a strong argument for including tribal oversight in future regulatory guidance for multi-site, community-based research. PMID:26928897

  5. Patterns of multisite pain and associations with risk factors

    PubMed Central

    Coggon, David; Ntani, Georgia; Palmer, Keith T.; Felli, Vanda E.; Harari, Raul; Barrero, Lope H.; Felknor, Sarah A.; Gimeno, David; Cattrell, Anna; Vargas-Prada, Sergio; Bonzini, Matteo; Solidaki, Eleni; Merisalu, Eda; Habib, Rima R.; Sadeghian, Farideh; Masood Kadir, M.; Warnakulasuriya, Sudath S.P.; Matsudaira, Ko; Nyantumbu, Busisiwe; Sim, Malcolm R.; Harcombe, Helen; Cox, Ken; Marziale, Maria H.; Sarquis, Leila M.; Harari, Florencia; Freire, Rocio; Harari, Natalia; Monroy, Magda V.; Quintana, Leonardo A.; Rojas, Marianela; Salazar Vega, Eduardo J.; Harris, E. Clare; Serra, Consol; Martinez, J. Miguel; Delclos, George; Benavides, Fernando G.; Carugno, Michele; Ferrario, Marco M.; Pesatori, Angela C.; Chatzi, Leda; Bitsios, Panos; Kogevinas, Manolis; Oha, Kristel; Sirk, Tuuli; Sadeghian, Ali; Peiris-John, Roshini J.; Sathiakumar, Nalini; Wickremasinghe, A. Rajitha; Yoshimura, Noriko; Kelsall, Helen L.; Hoe, Victor C.W; Urquhart, Donna M.; Derrett, Sarah; McBride, David; Herbison, Peter; Gray, Andrew

    2013-01-01

    To explore definitions for multisite pain, and compare associations with risk factors for different patterns of musculoskeletal pain, we analysed cross-sectional data from the Cultural and Psychosocial Influences on Disability (CUPID) study. The study sample comprised 12,410 adults aged 20–59 years from 47 occupational groups in 18 countries. A standardised questionnaire was used to collect information about pain in the past month at each of 10 anatomical sites, and about potential risk factors. Associations with pain outcomes were assessed by Poisson regression, and characterised by prevalence rate ratios (PRRs). Extensive pain, affecting 6–10 anatomical sites, was reported much more frequently than would be expected if the occurrence of pain at each site were independent (674 participants vs 41.9 expected). In comparison with pain involving only 1–3 sites, it showed much stronger associations (relative to no pain) with risk factors such as female sex (PRR 1.6 vs 1.1), older age (PRR 2.6 vs 1.1), somatising tendency (PRR 4.6 vs 1.3), and exposure to multiple physically stressing occupational activities (PRR 5.0 vs 1.4). After adjustment for number of sites with pain, these risk factors showed no additional association with a distribution of pain that was widespread according to the frequently used American College of Rheumatology criteria. Our analysis supports the classification of pain at multiple anatomical sites simply by the number of sites affected, and suggests that extensive pain differs importantly in its associations with risk factors from pain that is limited to only a small number of anatomical sites. PMID:23727463

  6. Spectroscopic Classifications of Optical Transients with SOAR

    NASA Astrophysics Data System (ADS)

    Hounsell, R. A.; Miller, J. A.; Pan, Y.-C.; Foley, R. J.; Jha, S. W.; Rest, A.; Scolnic, D.; Smith, K. W.; Wright, D.; Smartt, S. J.; Huber, M.; Chambers, K. C.; Flewelling, H.; Willman, M.; Primak, N.; Schultz, A.; Gibson, B.; Magnier, E.; Waters, C.; Tonry, J.; Wainscoat, R. J.

    2016-06-01

    We report the following classifications of optical transients from spectroscopic observations with the Goodman spectrograph on the SOAR 4-m telescope. Targets were supplied by the Pan-STARRS Survey for Transients (PSST).

  7. Implementation and validation of a Wilks-type multi-site daily precipitation generator over a typical Alpine river catchment

    NASA Astrophysics Data System (ADS)

    Keller, D. E.; Fischer, A. M.; Frei, C.; Liniger, M. A.; Appenzeller, C.; Knutti, R.

    2015-05-01

    Many climate impact assessments require high-resolution precipitation time series that have a spatio-temporal correlation structure consistent with observations, for simulating either current or future climate conditions. In this respect, weather generators (WGs) designed and calibrated for multiple sites are an appealing statistical downscaling technique to stochastically simulate multiple realisations of possible future time series consistent with the local precipitation characteristics and their expected future changes. In this study, we present the implementation and validation of a multi-site daily precipitation generator re-built after the methodology described in Wilks (1998). The generator consists of several Richardson-type WGs run with spatially correlated random number streams. This study aims at investigating the capabilities, the added value and the limitations of the precipitation generator for a typical Alpine river catchment in the Swiss Alpine region under current climate. The calibrated multi-site WG is skilful at individual sites in representing the annual cycle of the precipitation statistics, such as mean wet day frequency and intensity as well as monthly precipitation sums. It reproduces realistically the multi-day statistics such as the frequencies of dry and wet spell lengths and precipitation sums over consecutive wet days. Substantial added value is demonstrated in simulating daily areal precipitation sums in comparison to multiple WGs that lack the spatial dependency in the stochastic process. Limitations are seen in reproducing daily and multi-day extreme precipitation sums, observed variability from year to year and in reproducing long dry spell lengths. Given the performance of the presented generator, we conclude that it is a useful tool to generate precipitation series consistent with the mean climatic aspects and likely helpful to be used as a downscaling technique for climate change scenarios.

  8. Medication Errors in the Home: A Multisite Study of Children With Cancer

    PubMed Central

    Roblin, Douglas W.; Weingart, Saul N.; Houlahan, Kathleen E.; Degar, Barbara; Billett, Amy; Keuker, Christopher; Biggins, Colleen; Li, Justin; Wasilewski, Karen; Mazor, Kathleen M.

    2013-01-01

    OBJECTIVE: As home medication use increases, medications previously managed by nurses are now managed by patients and their families. Our objective was to describe the types of errors occurring in the home medication management of children with cancer. METHODS: In a prospective observational study at 3 pediatric oncology clinics in the northeastern and southeastern United States, patients undergoing chemotherapy and their parents were recruited from November 2007 through April 2011. We reviewed medical records and checked prescription doses. A trained nurse visited the home, reviewed medication bottles, and observed administration. Two physicians independently made judgments regarding whether an error occurred and its severity. Overall rates of errors were weighted to account for clustering within sites. RESULTS: We reviewed 963 medications and observed 242 medication administrations in the homes of 92 patients. We found 72 medication errors. Four errors led to significant patient injury. An additional 40 errors had potential for injury: 2 were life-threatening, 13 were serious, and 25 were significant. Error rates varied between study sites (40–121 errors per 100 patients); the weighted overall rate was 70.2 errors per 100 patients (95% confidence interval [CI]: 58.9–81.6). The weighted rate of errors with injury was 3.6 (95% CI: 1.7–5.5) per 100 patients and with potential to injure the patient was 36.3 (95% CI: 29.3–43.3) per 100 patients. Nonchemotherapy medications were more often involved in an error than chemotherapy. CONCLUSIONS: Medication errors were common in this multisite study of outpatient pediatric cancer care. Rates of preventable medication-related injuries in this outpatient population were comparable or higher than those found in studies of hospitalized patients. PMID:23629608

  9. The Ionization of the Local Interstellar Medium as Revealed by Far Ultraviolet Spectroscopic Explorer Observations of N, O, and AR toward White Dwarf Stars

    NASA Astrophysics Data System (ADS)

    Jenkins, E. B.; Oegerle, W. R.; Gry, C.; Vallerga, J.; Sembach, K. R.; Shelton, R. L.; Ferlet, R.; Vidal-Madjar, A.; York, D. G.; Linsky, J. L.; Roth, K. C.; Dupree, A. K.; Edelstein, J.

    2000-07-01

    Far Ultraviolet Spectroscopic Explorer spectra of the white dwarf stars G191-B2B, GD 394, WD 2211-495, and WD 2331-475 cover the absorption features out of the ground electronic states of N I, N II, N III, O I, and Ar I in the far-ultraviolet, providing new insights on the origin of the partial ionization of the local interstellar medium (LISM) and, for the case of G191-B2B, the interstellar cloud that immediately surrounds the solar system. Toward these targets the interstellar abundances of Ar I, and sometimes N I, are significantly below their cosmic abundances relative to H I. In the diffuse interstellar medium, these elements are not likely to be depleted onto dust grains. Generally, we expect that Ar should be more strongly ionized than H (and also O and N, whose ionizations are coupled to that of H via charge-exchange reactions) because the cross section for the photoionization of Ar I is very high. Our finding that Ar I/H I is low may help to explain the surprisingly high ionization of He in the LISM found by other investigators. Our result favors the interpretation that the ionization of the local medium is maintained by a strong extreme-ultraviolet flux from nearby stars and hot gases, rather than an incomplete recovery from a past, more highly ionized condition. Based on data obtained for the Guaranteed Time Team by the NASA-CNES-CSA FUSE mission operated by Johns Hopkins University. Financial support to US participants has been provided by NASA contract NAS5-32985.

  10. Scattered light in the echelle modes of the Goddard High Resolution Spectrograph aboard the Hubble Space Telescope. II - Analysis of in-flight spectroscopic observations

    NASA Technical Reports Server (NTRS)

    Cardelli, Jason A.; Ebbets, Dennis C.; Savage, Blair D.

    1993-01-01

    We report on an analysis of observations made with the GHRS aboard the HST for the purpose of calibrating the effects of scattered light. The data were obtained during the first 2 years of flight operations as part of the Science Verification, Science Assessment Observations, and Guaranteed Time Observations programs. Both the general level of background light near the spectra and the filling-in of the cores of saturated interstellar absorption lines have been determined as functions of grating, order, wavelength, and aperture. The behavior is in accordance with our detailed analysis of prelaunch laboratory data and validates both the observing procedures and the data reduction developed on the basis of that experience. We present and discuss the use of a background (scattered light) removal algorithm designed to produce net spectra properly corrected for the effects of grating scattered light. The coefficients of the scattered light removal algorithm have been determined, and recommended numerical values are presented.