Relating dust, gas and the rate of star formation in M31

Details Relating dust, gas and the rate of star formation in M31 Relating dust, gas and the rate of star formation in M31

2010-04-24

arxiv.org/abs/1004.4306v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

22 pages accepted for publication in A&A

Scientific paper

We derive distributions of dust temperature and dust opacity across M31 at 45" resolution using the Spitzer data. With the opacity map and a standard dust model we de-redden the Ha emission yielding the first de-reddened Ha map of M31. We compare the emissions from dust, Ha, HI and H2 by means of radial distributions, pixel-to-pixel correlations and wavelet cross-correlations. The dust temperature steeply decreases from 30K near the center to 15K at large radii. The mean dust optical depth at the Ha wavelength along the line of sight is about 0.7. The radial decrease of the dust-to-gas ratio is similar to that of the oxygen abundance. On scales<2kpc, cold dust emission is best correlated with that of neutral gas and warm dust emission with that of ionized gas. Ha emission is slightly better correlated with emission at 70um than at 24um. In the area 6kpc

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