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Title:
Molecular Hydrogen in the Far Ultraviolet Spectroscopic Explorer Translucent Lines of Sight: The Full Sample
Authors:
Rachford, Brian L.; Snow, Theodore P.; Destree, Joshua D.; Ross, Teresa L.; Ferlet, Roger; Friedman, Scott D.; Gry, Cecile; Jenkins, Edward B.; Morton, Donald C.; Savage, Blair D.; Shull, J. Michael; Sonnentrucker, Paule; Tumlinson, Jason; Vidal-Madjar, Alfred; Welty, Daniel E.; York, Donald G.
Affiliation:
AA(Department of Physics, Embry-Riddle Aeronautical University, 3700 Willow Creek Road, Prescott, AZ 86301, USA ), AB(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309-0389, USA ), AC(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309-0389, USA ), AD(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309-0389, USA ), AE(Institut d'Astrophysique de Paris, UMR7095 CNRS, Universite Pierre & Marie Curie, 98 bis Boulevard Arago, 75014 Paris, France ), AF(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA ), AG(Laboratoire d'Astrophysique de Marseille, CNRS, 38 rue Frederic Joliot-Curie, 13388 Marseille Cedex 13, France ), AH(Princeton University Observatory, Peyton Hall, Princeton, NJ 08544, USA ), AI(Herzberg Institute of Astrophysics, National Research Council, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada ), AJ(Department of Astronomy, University of Wisconsin, 475 North Charter Street, Madison, WI 53706, USA ), AK(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309-0389, USA ), AL(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA ), AM(Yale Center for Astronomy and Astrophysics, Department of Physics, P.O. Box 208121, New Haven, CT 06520, USA ), AN(Institut d'Astrophysique de Paris, UMR7095 CNRS, Universite Pierre & Marie Curie, 98 bis Boulevard Arago, 75014 Paris, France ), AO(Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA ), AP(Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA ; Enrico Fermi Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA)
Publication:
The Astrophysical Journal Supplement, Volume 180, Issue 1, pp. 125-137 (2009). (ApJS Homepage)
Publication Date:
01/2009
Origin:
IOP
ApJ Keywords:
ISM: abundances, ISM: clouds, ISM: lines and bands, ISM: molecules, ultraviolet: ISM
DOI:
10.1088/0067-0049/180/1/125
Bibliographic Code:
2009ApJS..180..125R

Abstract

We report total abundances and related parameters for the full sample of the Far Ultraviolet Spectroscopic Explorer survey of molecular hydrogen in 38 translucent lines of sight. New results are presented for the "second half" of the survey involving 15 lines of sight to supplement data for the first 23 lines of sight already published. We assess the correlations between molecular hydrogen and various extinction parameters in the full sample, which covers a broader range of conditions than the initial sample. In particular, we are now able to confirm that many, but not all, lines of sight with shallow far-UV extinction curves and large values of the total-to-selective extinction ratio, RV = AV /E(B - V)—characteristic of larger than average dust grains—are associated with particularly low hydrogen molecular fractions (f_H_2). In the lines of sight with large RV , there is in fact a wide range in molecular fractions, despite the expectation that the larger grains should lead to less H2 formation. However, we see specific evidence that the molecular fractions in this sub-sample are inversely related to the estimated strength of the UV radiation field and thus the latter factor is more important in this regime. We have provided an update to previous values of the gas-to-dust ratio, N(Htot)/E(B - V), based on direct measurements of N(H2) and N(H I). Although our value is nearly identical to that found with Copernicus data, it extends the relationship by a factor of 2 in reddening. Finally, as the new lines of sight generally show low-to-moderate molecular fractions, we still find little evidence for single monolithic "translucent clouds" with f_H_2 \sim 1.
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