Interstellar H I and H2 in the Magellanic Clouds: An Expanded Sample Based on UV Absorption-Line Data

Details Interstellar H I and H2 in the Magellanic Clouds: An Expanded Sample Based on UV Absorption-Line Data Interstellar H I and H2 in the Magellanic Clouds: An Expanded Sample Based on UV Absorption-Line Data

Nov 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010mwac.meet..p15w&link_type=abstract

"Midwest Astrochemistry Meeting 2010, held 5-6 November at the University of Illinois at Urbana-Champaign. http://midwest.astroc

Astronomy and Astrophysics

Astronomy

Scientific paper

We have determined column densities of H I and/or H2 for sight lines in the Magellanic Clouds from archival HST and FUSE spectra of H I Lyman-α and H2 Lyman-band absorption. Together with (some) similar data from the literature, we now have absorption-based N(H I) and/or N(H2) for about 250 Magellanic Clouds sight lines - enabling more extensive, direct, and accurate determinations of molecular fractions, dust-to-gas ratios, and elemental depletions. The N(H I) estimated from 21 cm emission (for the same sight lines) can be lower by factors of 2-3 in the LMC - suggestive of small-scale structure within the 21 cm beam(s) and/or some saturation in the emission. Both E(B-V)/N(H I) and E(B-V)/N(Htot) are smaller than in our Galaxy, by factors of 2.7-3.4 in the LMC and 4.3-4.9 in the SMC - similar to the differences in metallicity. The E(B-V)/N(N2) ratio is more similar in the three galaxies, however. These data may be used to test models of the atomic-to-molecular transition at low metallicities and predictions of N(H2) based on comparisons of 21 cm emission and the IR emission from dust.

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