2010/01/08 by Tomotsugu Goto, Toshinobu Takagi, T. Takagi +36 · 4 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Cosmic infrared background #Cosmic microwave background #Extrapolation #Galaxies: Formation, Evolution, Phenomena #Galaxy #Gamma-ray bursts and supernovae #Hubble Deep Field #Infrared #Luminosity #Luminosity function #Luminous infrared galaxy #Optics #Physics #Redshift #Star formation #astro-ph.CO
paper · pdf · doi:10.1051/0004-6361/200913182
Accepted for publication in A&A AKARI special issue
arxiv created 2010/01/08 · openalex publication_date 2010/02/08 · arxiv updated 2015/05/14 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
<i>Aims. <i/>Dust-obscured star-formation increases with increasing intensity and increasing redshift. We aim to reveal the cosmic star-formation history obscured by dust using deep infrared observation with AKARI.<i>Methods. <i/>We constructed restframe 8 <i>μ<i/>m, 12 <i>μ<i/>m, and total infrared (TIR) luminosity functions (LFs) at 0.15 <i><<i/> <i>z<i/> <i><<i/> 2.2 using 4128 infrared sources in the AKARI NEP-deep field. A continuous filter coverage in the mid-IR wavelength (2.4, 3.2, 4.1, 7, 9, 11, 15, 18, and 24 <i>μ<i/>m) by the AKARI satellite allowed us to estimate restframe 8 <i>μ<i/>m and 12 <i>μ<i/>m luminosities without using a large extrapolation based on an SED fit, which was the largest uncertainty in previous work.<i>Results. <i/>We find that all 8 <i>μ<i/>m (0.38 <i><<i/> <i>z<i/> <i><<i/> 2.2), 12 <i>μ<i/>m (0.15 <i><<i/> <i>z<i/> <i><<i/> 1.16), and TIR LFs (0.2 <i><<i/> <i>z<i/> <i><<i/>1.6) show continuous and strong evolution toward higher redshift. Our direct estimate of 8 <i>μ<i/>m LFs is useful since previous work often had to use a large extrapolation from the <i>Spitzer<i/> 24 <i>μ<i/>m to 8 <i>μ<i/>m, where SED modeling is more difficult because of the PAH emissions. In terms of cosmic infrared luminosity density (<i>Ω<i/><sub>IR<sub/>), which was obtained by integrating analytic fits to the LFs, we find good agreement with previous work at <i>z<1.2<i/>. We find the <i>Ω<i/><sub>IR<sub/> evolves as (1 + <i>z<i/>). When we separate contributions to <i>Ω<i/><sub>IR<sub/> by LIRGs and ULIRGs, we found more IR luminous sources are increasingly more important at higher redshift. We find that the ULIRG (LIRG) contribution increases by a factor of 10 (1.8) from <i>z<i/> = 0.35 to <i>z<i/> = 1.4.