The Star Formation Rate Function of the Local Universe
D. Christopher Martin, Mark Seibert, Veronique Buat, Jorge Inglesias-Paramo, Tom A. Barlow, Luciana Bianchi, Yong-Ik Byun, Jose Donas, Karl Forster, Peter G. Friedman, Timothy M. Heckman, Patrick N. Jelinsky, Young-Wook Lee, Barry F. Madore, Roger F. Malina, Bruno Milliard, Patrick F. Morrissey, Susan G. Neff, R. Michael Rich, David Schiminovich, Oswald H. W. Siegmund, Todd Small, Alex S. Szalay, Barry Y. Welsh, Ted K. Wyder
Abstract
We have derived the bivariate luminosity function for the far ultraviolet (1530Angstroms) and far infrared (60 microns). We used matched GALEX and IRAS data, and redshifts from NED and PSC-z. We have derived a total star formation luminosity function phi(Ltot), with Ltot = LFUV+LFIR. Using these, we determined the cosmic ``star formation rate'' function and density for the local universe. The total SFR function is fit very well by a log-normal distribution over five decades of luminosity. We find that the bivariate luminosity function phi(LFUV,LFIR) shows a bimodal behavior, with LFIR tracking LFUV for LTOT< 1010 Lsun, and LFUV saturating at 1010 Lsun, while LTOT LFIR for higher luminosities. We also calculate the SFR density and compare it to other measurements.
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