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Molecular properties of (U)LIRGs: CO, HCN, HNC and HCO+

Published online by Cambridge University Press:  01 March 2007

A. F. Loenen ,
W. A. Baan  and
M. Spaans
A. F. Loenen
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, The Netherlands email: loenen@astro.rug.nl, spaans@astro.rug.nl ASTRON, P.O. Box 2, 7990 AA Dwingeloo, The Netherlands email: baan@astron.nl
W. A. Baan
Affiliation:
ASTRON, P.O. Box 2, 7990 AA Dwingeloo, The Netherlands email: baan@astron.nl
M. Spaans
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, The Netherlands email: loenen@astro.rug.nl, spaans@astro.rug.nl
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Abstract

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The observed molecular properties of a sample of FIR-luminous and OH megamaser (OH-MM) galaxies have been investigated. The ratio of high and low-density tracer lines is found to be determined by the progression of the star formation in the system. The HCO+/HCN and HCO+/HNC line ratios are good proxies for the density of the gas, and PDR and XDR sources can be distinguished using the HNC/HCN line ratio. The properties of the OH-MM sources in the sample can be explained by PDR chemistry in gas with densities higher than 105.5cm−3, confirming the classical OH-MM model of IR pumped amplification with (variable) low gains.

Keywords

galaxies: nucleigalaxies: ISMgalaxies: activegalaxies: starburstISM: moleculesISM: evolutionradio lines: ISM

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