Biology – Quantitative Biology – Populations and Evolution
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.8001p&link_type=abstract
2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #80.01; Bulletin of the American Astronomical Society, V
Biology
Quantitative Biology
Populations and Evolution
Scientific paper
The luminosity function (LF) is a powerful tool for studying galaxy populations and evolution. We present the LF of the radio sources from the VLA-COSMOS catalog. The sensitivity limit of VLA-COSMOS only 0.04 mJy allows us to probe the fainter, presumably star-forming galaxies often undetected by large area surveys. The accompanying COSMOS optical catalog, which provides photometric redshifts and galaxy spectral types, allows us to estimate the luminosities of a large sample (2,647) of radio sources and to compare their radio properties with galaxy type. We examine a very broad range of luminosities, 18 < logP < 25.5, where P is the total 1.4 GHz luminosity in W/Hz/sr. We have photometric redshifts up to z = 2.97 and spectroscopic redshifts up to 1.87. The COSMOS radio LF is consistent with the 2dFGRS radio LF, and shows contributions from both AGN and star-forming spirals. The available spectroscopic redshifts are mostly for sources selected for their likely AGN activity (X-ray and radio emission), but our LF derived using them is consistent with that of the photometric sample given a higher fraction of active galaxies rather than spirals. The 1/Vmax method we use to calculate the LF is known to show bias for clustered fields, so we also measure the correlation function to measure this effect. Though not as strongly clustered as early type galaxies, the amplitude of the VLA-COSMOS correlation function is higher than that of the NVSS and FIRST sources. This result is consistent with those of the optical clustering in the COSMOS field. We have studied the effects of the radio spectral index (the K-correction) on the LF as well, and investigate the possible evolution of the population. We are examining methods to distinguish between the star-forming galaxies and the AGN to track their evolution separately.
Bondi Marco
Ciliegi Paolo
Paglione Timothy
Salvador K.
Schinnerer Eva
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