Samir Salim (Indiana) -- Intrinsic Form of the Galaxy

Knowing the exact form of the galaxy SFR distribution function (i.e., the SFR function) is essential for the precise measurements of the global SFR density and its evolution, and for comparisons with models of galaxy evolution. However, the SFR function when measured as the luminosity function in the UV, emission lines (H alpha, OII) and sometimes the IR is usually fit with a Schechter function, which we show is inadequate for describing its intrinsic functional form. Instead, using mock samples and empirical SFR-stellar mass relations we find that the true dust-corrected SFR function has a much shallower bright-end tail than the exponential decline of the Schechter function. Such non-Schechter form is best seen in the far-IR LF. The seemingly Schechter-like behavior of the UV and emission line LFs is not intrinsic, as it is for the optical and near-IR LFs, but stems from either not correcting for dust or using average corrections.