Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· On-line Data
· References in the article
· Citations to the Article (67) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (6)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Deuterium Abundance toward G191-B2B: Results from the FUSE Mission
Authors:
Lemoine, M.; Vidal-Madjar, A.; Hébrard, G.; Désert, J.-M.; Ferlet, R.; Lecavelier des Étangs, A.; Howk, J. C.; André, M.; Blair, W. P.; Friedman, S. D.; Kruk, J. W.; Lacour, S.; Moos, H. W.; Sembach, K.; Chayer, P.; Jenkins, E. B.; Koester, D.; Linsky, J. L.; Wood, B. E.; Oegerle, W. R.; Sonneborn, G.; York, D. G.
Affiliation:
AA(Institut d'Astrophysique de Paris, CNRS, 98 bis Boulevard Arago, F-75014 Paris, France.), AB(Institut d'Astrophysique de Paris, CNRS, 98 bis Boulevard Arago, F-75014 Paris, France.), AC(Institut d'Astrophysique de Paris, CNRS, 98 bis Boulevard Arago, F-75014 Paris, France.), AD(Institut d'Astrophysique de Paris, CNRS, 98 bis Boulevard Arago, F-75014 Paris, France.), AE(Institut d'Astrophysique de Paris, CNRS, 98 bis Boulevard Arago, F-75014 Paris, France.), AF(Institut d'Astrophysique de Paris, CNRS, 98 bis Boulevard Arago, F-75014 Paris, France.), AG(Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218.), AH(Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218.), AI(Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218.), AJ(Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218.), AK(Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218.), AL(Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218.), AM(Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218.), AN(Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218.), AO(Department of Physics and Astronomy, University of Victoria, P.O. Box 3055, Victoria, BC V8W 3P6, Canada.), AP(Princeton University Observatory, Princeton, NJ 08544.), AQ(Institut für Theoretische Physik und Astrophysik, Universität Kiel, D-24098 Kiel, Germany.), AR(JILA, University of Colorado and NIST, Boulder, CO 80309-0440.), AS(JILA, University of Colorado and NIST, Boulder, CO 80309-0440.), AT(Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Code 681, Greenbelt, MD 20771.), AU(Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Code 681, Greenbelt, MD 20771.), AV(Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637.)
Publication:
The Astrophysical Journal Supplement Series, Volume 140, Issue 1, pp. 67-80. (ApJS Homepage)
Publication Date:
05/2002
Origin:
UCP
ApJ Keywords:
ISM: Abundances, ISM: Clouds, Stars: Individual: Alphanumeric: G191-B2B, Ultraviolet: ISM
DOI:
10.1086/339128
Bibliographic Code:
2002ApJS..140...67L

Abstract

High-resolution spectra of the hot white dwarf G191-B2B, covering the wavelength region 905-1187 Å, were obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE). These data were used in conjunction with existing high-resolution Hubble Space Telescope Space Telescope Imaging Spectrograph (STIS) observations to evaluate the total H I, D I, O I, and N I column densities along the line of sight. Previous determinations of N(D I) based upon GHRS and STIS observations were controversial as a result of the saturated strength of the D I Lyα line. In the present analysis the column density of D I has been measured using only the unsaturated Lyβ and Lyγ lines observed by FUSE. A careful inspection of possible systematic uncertainties tied to the modeling of the stellar continuum or to the uncertainties in the FUSE instrumental characteristics has been performed. The column densities derived are logN(DI)=13.40+/-0.07, logN(OI)=14.86+/-0.07, and logN(NI)=13.87+/-0.07, quoted with 2 σ uncertainties. The measurement of the H I column density by profile fitting of the Lyα line has been found to be uncertain. If additional weak, hot interstellar components are added to the three detected clouds along the line of sight, the H I column density can be reduced quite significantly, even though the signal-to-noise ratio and spectral resolution at Lyα are excellent. The new estimate of N(H I) toward G191-B2B reads logN(HI)=18.18+/-0.18 (2 σ), so that the average D/H ratio on the line of sight is D/H=(1.66+0.9-0.6)×10-5 (2 σ). This work is based on data obtained for the Guaranteed Time Team by the NASA-CNES-CSA FUSE mission operated by Johns Hopkins University.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints