Infrared luminosity functions of AKARI Sloan Digital Sky Survey galaxies

By cross-correlating the AKARI all-sky survey in six infrared (IR) bands (9, 18, 65, 90, 140 and 160 mu m) with the Sloan Digital Sky Survey (SDSS) galaxies, we identified 2357 IR galaxies with a spectroscopic redshift. This is not just one of the largest samples of local IR galaxies, but AKARI provides crucial far-IR (FIR) bands for accurately measuring the galaxy spectral energy distribution (SED) across the peak of the dust emission at > 100 mu m. By fitting modern IR SED models to the AKARI photometry, we measured the total infrared luminosity (LIR) of individual galaxies. Using this L-IR, we constructed the luminosity functions (LF) of IR galaxies at a median redshift of z = 0.031. The LF agrees well with that at z = 0.0082 (the Revised Bright Galaxy Sample), showing smooth and continuous evolution towards higher redshift LFs measured in the AKARI North Ecliptic Pole (NEP) deep field. By integrating the IR LF weighted by LIR, we measured the local cosmic IR luminosity density of Omega(IR) = (3.8(-1.2)(+5.8)) x 10(8) L-circle dot Mpc(-3). We separate galaxies into active galactic nuclei (AGN), star-forming galaxies (SFG) and composite by using the [N-II]/H alpha versus [O III]/H beta line ratios. The fraction of AGN shows a continuous increase with increasing LIR from 25 to 90 per cent at 9 < log L-IR < 12.5. The SFRH alpha and L[ O III] show good correlations with LIR for SFG and AGN, respectively. The self-absorption-corrected H alpha/H beta ratio shows a weak increase with LIR with a substantial scatter. When we separate IR LFs into contributions from AGN and SFG, the AGN contribution becomes dominant at LIR > 10(11) L-circle dot, coinciding with the break of both the SFG and AGN IR LFs. At LIR = 10(11) L-circle dot, SFG dominates IR LFs. Only 1.1 +/- 0.1 per cent of Omega(IR) is produced by luminous infrared galaxies (LIR > 10(11) L-circle dot), and only 0.03 +/- 0.01 per cent by ultraluminous infrared galaxies (L-IR > 10(12) L-circle dot) in the local Universe. Compared with high-redshift results from the AKARI NEP deep survey, we observed a strong evolution of Omega(SFG)(IR) proportional to (1 + z)(4.1 +/- 0.4) and Omega(AGN)(IR) proportional to (1 + z)(4.1 +/- 0.5). Our results show that all of our measured quantities (IR LFs, L*, Omega(AGN)(IR), Omega(SFG)(IR)) show smooth and steady increase from lower redshift (the Revised Bright Galaxy Sample) to higher redshift (the AKARI NEP deep survey).