Molecular line intensities as measures of cloud masses - II. Conversion factors for specific galaxy types

Details Molecular line intensities as measures of cloud masses - II. Conversion factors for specific galaxy types Molecular line intensities as measures of cloud masses - II. Conversion factors for specific galaxy types

2007-04-19

arxiv.org/abs/0704.2603v1

Mon.Not.Roy.Astron.Soc.378:983-994,2007

Astronomy and Astrophysics

Astrophysics

14 pages, 11 figures, accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2007.11830.x

We present theoretically-established values of the CO-to-H2 and C-to-H2 conversion factors that may be used to estimate the gas masses of external galaxies. We consider four distinct galaxy types, represented by M51, NGC 6946, M82 and SMC N27. The physical parameters that best represent the conditions within the molecular clouds in each of the galaxy types are estimated using a chi^2 analysis of several observed atomic fine structure and CO rotational lines. This analysis is explored over a wide range of density, radiation field, extinction, and other relevant parameters. Using these estimated physical conditions in methods that we have previously established, CO-to-H2 conversion factors are then computed for CO transitions up to J=9-8. For the conventional CO(1-0) transition, the computed conversion factor varies significantly below and above the canonical value for the Milky Way in the four galaxy types considered. Since atomic carbon emission is now frequently used as a probe of external galaxies, we also present, for the first time, the C-to-H2 conversion factor for this emission in the four galaxy types considered.

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