The Anatomy of Star Formation in NGC 300

Details The Anatomy of Star Formation in NGC 300 The Anatomy of Star Formation in NGC 300

2004-08-13

arxiv.org/abs/astro-ph/0408248v1

Astrophys.J.Suppl.154:253,2004

Astronomy and Astrophysics

Astrophysics

to appear in the ApJS Spitzer special issue (September 2004)

Scientific paper

10.1086/422640

The Spitzer Space Telescope was used to study the mid-infrared to far-infrared properties of NGC 300, and to compare dust emission to Halpha to elucidate the heating of the ISM and the star formation cycle at scales < 100 pc. The new data allow us to discern clear differences in the spatial distribution of 8 micron dust emission with respect to 24 micron dust and to HII regions traced by the Halpha light. The 8 micron emission highlights the rims of HII regions, and the 24 micron emission is more strongly peaked in star forming regions than at 8 microns. We confirm the existence and approximate amplitude of interstellar dust emission at 4.5 microns, detected statistically in Infrared Space Observatory (ISO) data, and conclude it arises in star forming regions. When averaging over regions larger than ~ 1 kpc, the ratio of Halpha to Aromatic Feature emission in NGC 300 is consistent with the values observed in disks of spiral galaxies. The mid-to-far-infrared spectral energy distribution of dust emission is generally consistent with pre-Spitzer models.

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