Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20913301e&link_type=abstract
2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #133.01; Bulletin of the American Astronomical Society,
Astronomy and Astrophysics
Astronomy
Scientific paper
The earliest phases of star formation, from prestellar cores to Class I protostars, are best observed at far-infrared to millimeter wavelengths. Here we analyze large-scale Bolocam 1.1 mm surveys of Perseus (7.5 sq. deg.), Ophiuchus (10.8 sq. deg.), and Serpens (1.5 sq. deg.) in combination with Spitzer IRAC and MIPS maps from the c2d Legacy Program. The Bolocam 30" resolution observations trace optically thin dust emission, which is a measure of the total mass in dense cores. Combining the millimeter data with Spitzer infrared data allows us to separate starless cores from those with internal luminosity sources (protostellar cores). From a comparison of the properties of the starless and protostellar core populations in each cloud, we infer how formation of a central protostar alters core properties. The starless core sample reveals pre-collapse initial conditions, and enables a comparison of the prestellar core mass function to the stellar initial mass function. From Spitzer IRAC and MIPS photometry together with Bolocam flux densities, we calculate bolometric temperatures and luminosities for the coldest protostellar sources in each cloud, and compare to protostellar evolutionary models. Different protostellar classification methods are considered, and our classifications are used to estimate lifetimes for the prestellar and Class 0 phases. We discuss how these results further our understanding of the processes controlling star formation on molecular cloud scales.
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