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Gas and Dust in M33

  • J. Braine (a1), P. Gratier (a1), C. Kramer (a1), B. Mookerjea (a1), M. Xilouris (a1) and D. Calzetti (a1)...

Abstract

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.

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References

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Boquien, M., et al. 2010, A&A, 518, L70
Braine, J., et al. 2010, A&A, 518, L69
Gardan, E., et al. 2007, A&A, 473, 91
Gratier, P., et al. 2010, A&A, 522, A3
Gratier, P., et al. 2010, A&A, 512, A68
Heiles, C. 1994, ApJ, 436, 720
Kramer, C., et al. 2010, A&A, 518, L67
Verley, S., et al. 2010, A&A, 518, L68
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Keywords

Gas and Dust in M33

  • J. Braine (a1), P. Gratier (a1), C. Kramer (a1), B. Mookerjea (a1), M. Xilouris (a1) and D. Calzetti (a1)...

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