The star formation rate distribution function of the local Universe

摘要: We present total infrared (IR) and ultraviolet (UV) luminosity functions derived from large representative samples of galaxies at z ~ 0, selected IR UV wavelengths the Imperial IRAS Faint Source Catalogue redshift data base (IIFSCz) catalogue, GALEX All-Sky Imaging Survey (AIS), respectively. augment these with deep Spitzer imaging in 11 Mpc Local Volume Legacy (LVL) Survey, allowing us to extend lower luminosities (~10^6 L_⊙), providing good constraints on slope function extreme faint end for first time. Using conventional star formation prescriptions, we generate our rate (SFR) distribution local Universe. find that it has a Schechter form, faint-end constant value (to limits data) α=−1.51 ± 0.08 'characteristic' SFR ψ^* is 9.2 M_⊙ yr^(−1). also show volume density; then use this calculate density 0 0.025 0.0016 yr^(−1) Mpc^(−3), which ~20 per cent occurring starbursts. Decomposing by luminosity, can be seen 9 1 due LIRGs, 0.7 0.2 ULIRGs. By comparing emission sample, fraction dust-obscured environments, examine dusty formation: very shallow highly extincted end, may attributable line-of-sight orientation effects as well internal extinction.