[29.12] The $H_2$ spectrum as a probe of physical conditions in photoionized clouds.

AAS 202nd Meeting, May 2003
Session 29 Molecular Clouds and the ISM
Poster, Tuesday, May 27, 2003, 10:00am-6:30pm, West Exhbit Hall

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[29.12] The H₂ spectrum as a probe of physical conditions in photoionized clouds.

G. Shaw, G. Ferland (University of Kentucky)

We describe a complete model of the H₂ molecule that we have implemented in the spectra simulation code Cloudy. The H₂ molecule has 1893 levels which produce tens of thousands of lines. We consider all physical processes, including heating, cooling, molecule formation, and grain physics, simultaneously and self consistently. Effects of cosmic rays and the x-ray continuum are included as well. This allows the full UV – IR spectrum, including emission from atoms, ions, and molecules, to be predicted after the gas density and ionizing continuum are specified. We present diagnostic diagrams show H₂ line ratios as a function of these parameters, and apply these to IR observations of condensations within cooling flows of galaxy clusters.

The author(s) of this abstract have provided an email address for comments about the abstract: gshaw@pa.uky.edu

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[29.12] The H2 spectrum as a probe of physical conditions in photoionized clouds.

[29.12] The H₂ spectrum as a probe of physical conditions in photoionized clouds.