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Analysis of CO and temperature distributions in simulatedmolecular clouds

Published online by Cambridge University Press:  25 November 2011

M. Röllig ,
R. Simon ,
V. Ossenkopf ,
J. Stutzki ,
F. Molina ,
S. Glover  and
C. Federrath
F. Molina
Affiliation:
Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle-Str. 2, 69120, Germany
S. Glover
Affiliation:
Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle-Str. 2, 69120, Germany
C. Federrath
Affiliation:
École Normale Supérieure de Lyon, Centre de Recherche Astrophysique, 46 allée d’Italie, 69364, France
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Abstract

We have analyzed the distributions of CO and temperature in a large suite of simulatedmolecular clouds, in order to help us understand how to interpret CO line emission fromreal molecular clouds. We find that most of the CO is located at densities over103cm-3 where the temperature is roughly 10–20 K independently ofthe mean density, metallicity and UV field strength. Although, most of the volume is inwarmer and thinner regions where CO abundance is small. On that account, CO observationsalone give a misleading view of the physical conditions in the clouds.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 52: Conditions and Impact of Star Formation , 2011 , pp. 289 - 290
Copyright
© EAS, EDP Sciences 2011

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References

Glover, S.C.O., Federrath, C., Mac Low, M.-M., & Klessen, R.S., 2010, MNRAS, 404, 2
Glover, S.C.O., & Mac Low, M.-M., 2010, MNRAS, in press [arXiv:1003.1340]