Dissecting the Star Formation Within Late-Type Galaxies

Computer Science

Scientific paper

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Scientific paper

The past decade has brought the discovery and characterization of star-forming galaxies in the distant universe, detected through signatures of their rest-frame UV emission. One question about these galaxies is whether the UV continuum is a complete and unbiased picture of the star formation activity. Late-type galaxies are the best local analog candidates to the star formation occuring in galaxies in the distant universe. While samples reaching ~1000 galaxies at high redshift have been constructed, local samples are comparatively small. Early Spitzer observations have generated several large, general surveys the IR properties of nearby galaxies, but these survey inadequately sample the wide range of UV/Halpha/IR properties of late-type galaxies, so it is difficult to assess any trends---or to identify which kinds of local galaxies are the best analogs to the distant ones. In fact, late-type galaxies show so little self-similarity, that large samples of them are needed to span the full, multi-dimensional parameter space of those galaxy properties. We propose to fill-in this gap by obtaining IRAC and MIPS 3-24um images of a large sample of late-type galaxies (T>7) that all have UV (and many have Halpha) imaging already publicly-available in the HST archive. The result will be a wide and varied sample spanning many magnitudes of galaxy luminosity, star formation rate, stellar ages, metallicities, and merger activity. We will trace out the star formation activity in a variety of environments, and combine this with high-resolution HST imaging in order to dissect the processes occuring within those regions. The loss of HST's STIS, CTE degradation of WFPC-2, and uncertainity over WFC-3 all mean that our proposed sample is the complete list of galaxies with high spatial resolution UV images from HST. Our proposal will generate a generally useful Great Observatories dataset on star formation in late-type galaxies.

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