BRAINE, J.; GRATIER, P.; KRAMER, C.; MOOKERJEA, B.; XILOURIS, M.; CALZETTI, D.

doi:10.1017/S1743921311022472

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BRAINE, J.
FORMATION STELLAIRE 2011

GRATIER, P.
FORMATION STELLAIRE 2011

KRAMER, C.
Instituto de RadioAstronomía Milimétrica [IRAM]

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Proceedings of the International Astronomical Union, IAU Symposium 277, Proceedings of the International Astronomical Union, IAU Symposium 277, 2011, Ouagadougou. 2011-12, vol. 277, p. 63-66

Résumé en anglais

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.< Réduire

Mots clés en anglais

stars: formation

ISM: molecules

dust

extinction

ISM: evolution

ISM: general

ISM: abundances

galaxies: evolution galaxies: formation

Local Group

infrared: ISM

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Gas and Dust in M33

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