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Title:
Molecular Cloud Structure in the Magellanic Clouds: CO-to-H2 Conversion Factor
Authors:
Pak, S.; Jaffe, D. T.
Journal:
New Views of the Magellanic Clouds, IAU Symposium #190, Edited by Y.-H. Chu, N. Suntzeff, J. Hesser, & D. Bohlender. ISBN: 1-58381-021-8, p.114
Publication Date:
00/1999
Origin:
AUTHOR
Bibliographic Code:
1999IAUS..190..114P

Abstract

The chemical structure of neutral clouds in low metallicity environments is examined with particular emphasis on the H to H2 and C+ to CO transitions. We observed near-IR H2 (1,0) S(1), (2,1) S(1), and (5,3) O(3) lines and the 12CO J=1->0 line from 30 Doradus and N159/N160 in the Large Magellanic Cloud and from DEM S 16, DEM S 37, and LI-SMC 36 in the Small Magellanic Cloud. We find that the H2 emission is UV-excited and that (weak) CO emission always exists (in our surveyed regions) toward positions where H2 and [CII] emission have been detected. Using a PDR code and a radiative transfer code, we simulate the emission of line radiation from spherical clouds and from large planar clouds. Because the [CII] emission and H2 emission arise on the surface of the cloud and the lines are optically thin, these lines are not affected by changes in the relative sizes of the neutral cloud and the CO bearing core, while the optically thick CO emission can be strongly affected. The sizes of clouds are estimated by measuring the deviation of CO emission strength from that predicted by a planar cloud model of a given size. The average cloud column density and therefore size increases as the metallicity decreases. Our result agrees with the photoionization regulated star formation theory by McKee (1989). Based on our model, we also suggest that the CO-to-H2 conversion factor increases as the metallicity decreases.
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