Volume 493, Number 2, January II 2009
|Page(s)||453 - 466|
|Published online||27 October 2008|
Star formation in M 33: multiwavelength signatures across the disk
Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy e-mail: [simon;edvige;giova]@arcetri.astro.it
2 INAF - Istituto di Radioastronomia-Sezione Firenze, Largo E. Fermi 5, 50125 Firenze, Italy e-mail: email@example.com
Accepted: 27 September 2008
Aims. We use different tracers, such as Hα, ultraviolet (UV), and infrared (IR) emissions at various wavelengths, to study the dust and star formation (SF) conditions throughout the disk of M 33.
Methods. We derive the radial distribution of dust, of the old and young stellar population using Spitzer and GALEX data, complemented by ground-based optical data and available surveys of atomic and molecular gas. We separate the contribution of discrete sources to the IR brightness from the diffuse emission.
Results. At 8 and 24 μm, discrete sources account for 40% of the IR emission in the innermost 3 kpc, and for 20% further out. We find that stochastic emission from very small grains in the diffuse interstellar medium accounts for only ~10% of the diffuse 24 μm emission, and that dusty circumstellar shells of unresolved, evolved AGB stars (carbon stars) are a viable alternative. The 8 μm profile suggests that PAH emission declines faster with radius than the dust continuum. In annular regions 0.24 kpc wide, we find a mean extinction value for the stellar continuum mag with a weak dependence on radius, consistent with the shallow metallicity gradient observed. Dust opacity derived from the 160 μm emission decreases instead by a factor of 10 from the center to edge of the star forming disk.
Conclusions. Using extinction corrected UV and Hα maps we find the global SF rate in M 33 over the last 100 Myr to be yr-1. Far-IR and total-IR luminosities can trace SF even though a high conversion factor is required to recover the effective rate. If carbon stars are powering the diffuse 24 μm emission in M 33, this can trace star formation 1 Gyr ago and provide a more complete view of the SF history of the galaxy. Today the SF rate declines radially with a scale length of ~2 kpc, longer than for the old stellar population, suggesting an inside-out growth of the disk.
Key words: galaxies: individual: M 33 / galaxies: ISM / galaxies: Local Group / galaxies: spiral
© ESO, 2009
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