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The irradiated ISM of ULIRGs

Published online by Cambridge University Press:  01 March 2007

M. Spaans ,
R. Meijerink ,
F. P. Israel ,
A. F. Loenen  and
W. A. Baan
M. Spaans
Affiliation:
Kapteyn Astronomical Institute, P.O. Box 800, 9700 AV Groningen, The Netherlands email: spaans@astro.rug.nl
R. Meijerink
Affiliation:
Astronomy Department, Berkeley, CA 94720, United States
F. P. Israel
Affiliation:
Leiden Observatory, P.O. Box 9513, 2300 RA Leiden, The Netherlands
A. F. Loenen
Affiliation:
Kapteyn Astronomical Institute, P.O. Box 800, 9700 AV Groningen, The Netherlands email: spaans@astro.rug.nl ASTRON, P.O. Box 2, 7990 AA Dwingeloo, The Netherlands
W. A. Baan
Affiliation:
ASTRON, P.O. Box 2, 7990 AA Dwingeloo, The Netherlands
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Abstract

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The nuclei of ULIRGs harbor massive young stars, an accreting central black hole, or both. Results are presented for molecular gas that is exposed to X-rays (1–100 keV, XDRs) and far-ultraviolet radiation (6–13.6 eV, PDRs). Attention is paid to species like HCO+, HCN, HNC, OH, H2O and CO. Line ratios of HCN/HCO+ and HNC/HCN discriminate between PDRs and XDRs. Very high J (>10) CO lines, observable with HIFI/Herschel, discriminate very well between XDRs and PDRs. In XDRs, it is easy to produce large abundances of warm (T > 100 k) H2O and OH. In PDRs, only OH is produced similarly well.

Keywords

ISM: moleculesgalaxies: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S242: Astrophysical Masers and their Environments , March 2007 , pp. 452 - 456
Copyright
Copyright © International Astronomical Union 2008

References

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