Hostname: page-component-cd9895bd7-hc48f Total loading time: 0 Render date: 2024-12-25T04:51:22.739Z Has data issue: false hasContentIssue false
  • English
  • Français

Gas and Dust in M33

Published online by Cambridge University Press:  05 December 2011

J. Braine ,
P. Gratier ,
C. Kramer ,
B. Mookerjea ,
M. Xilouris  and
D. Calzetti
J. Braine
Affiliation:
Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU, 33271 Floirac, France
P. Gratier
Affiliation:
Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU, 33271 Floirac, France
C. Kramer
Affiliation:
Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU, 33271 Floirac, France
B. Mookerjea
Affiliation:
Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU, 33271 Floirac, France
M. Xilouris
Affiliation:
Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU, 33271 Floirac, France
D. Calzetti
Affiliation:
Laboratoire d'Astrophysique de Bordeaux, Université de Bordeaux, OASU, CNRS/INSU, 33271 Floirac, France
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present results from the Herschel and IRAM projects to map M33 in the dust continuum and main emission lines, particularly C[II] and CO. The temperature of the cool dust decreases with distance from the center of M33 from ~25K to ~13K. The CO emission generally follows the dust temperature and the overall dust emission. However, about 1/6 of the molecular clouds are not associated with massive stars, such that about 1/6th the lifetime of an entity identifiable as a molecular cloud is in a pre-star formation state. These clouds are less CO-bright than those with massive stars. The largest sample of molecular clouds currently available for an external galaxy shows that the cloud CO luminosity function, usually viewed as the cloud H2 mass, steepens with radius such that smaller clouds are more numerous in the outer parts. The observations of the C[II] line with Herschel indicate that the C[II] emission traces on-going star formation rather than the neutral gas. This identification will be tested via velocity-resolved Herschel/HIFI C[II] spectra in the near future.

Keywords

stars: formationISM: moleculesdust – extinctionISM: evolutionISM: generalISM: abundancesgalaxies: evolution galaxies: formationLocal Groupinfrared: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S277: Tracing the Ancestry of Galaxies (on the land of our ancestors) , December 2010 , pp. 63 - 66
Copyright
Copyright © International Astronomical Union 2011

References

Boquien, M., et al. 2010, A&A, 518, L70Google Scholar
Braine, J., et al. 2010, A&A, 518, L69Google Scholar
Gardan, E., et al. 2007, A&A, 473, 91Google Scholar
Gratier, P., et al. 2010, A&A, 522, A3Google Scholar
Gratier, P., et al. 2010, A&A, 512, A68Google Scholar
Heiles, C. 1994, ApJ, 436, 720CrossRefGoogle Scholar
Kramer, C., et al. 2010, A&A, 518, L67Google Scholar
Verley, S., et al. 2010, A&A, 518, L68Google Scholar