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Title:
A New FUSE Survey of Interstellar HD
Authors:
Snow, Theodore P.; Ross, Teresa L.; Destree, Joshua D.; Drosback, Meredith M.; Jensen, Adam G.; Rachford, Brian L.; Sonnentrucker, Paule; Ferlet, Roger
Affiliation:
AA(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado at Boulder, Campus Box 389, Boulder, CO 80309-0391 ; ; .), AB(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado at Boulder, Campus Box 389, Boulder, CO 80309-0391 ; ; .), AC(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado at Boulder, Campus Box 389, Boulder, CO 80309-0391 ; ; .), AD(Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904; .), AE(NASA Postdoctoral Program Fellow, Goddard Space Flight Center, Code 665, NASA/GSFC, Greenbelt, MD 20771; .), AF(Department of Physics, Embry-Riddle Aeronautical University, 3700 Willow Creek Road, Prescott, AZ 86301; .), AG(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218; .), AH(Institut d'Astrophysique de Paris, UMR7095 CNRS, Universite Pierre & Marie Curie, 98bis Boulevard Arago, 75014 Paris, France; .)
Publication:
The Astrophysical Journal, Volume 688, Issue 2, pp. 1124-1136. (ApJ Homepage)
Publication Date:
12/2008
Origin:
UCP
ApJ Keywords:
ISM: Abundances
DOI:
10.1086/592288
Bibliographic Code:
2008ApJ...688.1124S

Abstract

We have used archival FUSE data to complete a survey of interstellar HD in 41 lines of sight with a wide range of extinctions. This follow-up to an earlier survey was made to further assess the utility of HD as a cosmological probe; to analyze the HD formation process; and to see what trends with other interstellar properties were present in the data. We employed the curve-of-growth method, supported by line profile fitting, to derive accurate column densities of HD. We find that the N(HD)/2N(H2) ratio is substantially lower than the atomic D/H ratio and conclude that the molecular ratio has no bearing on cosmology, because local processes are responsible for the formation of HD. Based on correlations with E(B-V), H2, CO, and iron depletion, we find that HD is formed in the densest portion of the clouds; the slope of the logN(HD)/logN(H2) correlation is greater than 1.0, caused by the destruction rate of HD declining more slowly than that of H2; and, as a sidelight, that the depletions are density dependent.
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