Volume 528, April 2011
|Number of page(s)||18|
|Published online||23 February 2011|
Evolution of the dusty infrared luminosity function from z = 0 to z = 2.3 using observations from Spitzer⋆,⋆⋆
Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, IRFU/Service
d’Astrophysique, Bât. 709, CEA-Saclay,
2 Max Planck Institut für extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany
3 Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA
4 National Optical Astronomy Observatory, Tucson, AZ 85719, USA
5 UPMC Univ Paris 06, UMR7095, Institut d’Astrophysique de Paris, 75014 Paris, France
6 CNRS, UMR7095, Institut d’Astrophysique de Paris, 75014 Paris, France
7 National Radio Astronomy Observatory, PO Box 2, Green Bank, WV 24944, USA
8 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA
Received: 22 December 2009
Accepted: 11 January 2011
Aims. We derive the evolution of the infrared luminosity function (LF) over the last 4/5ths of cosmic time using deep 24 and 70 μm imaging of the GOODS North and South fields.
Methods. We use an extraction technique based on prior source positions at shorter wavelengths to build the 24 and 70 μm source catalogs. The majority (93%) of the sources have a spectroscopic (39%) or a photometric redshift (54%) and, in our redshift range of interest (i.e., 1.3 < z < 2.3) s20% of the sources have a spectroscopic redshift. To extend our study to lower 70 μm luminosities we perform a stacking analysis and we characterize the observed L24/(1 + z) vs. L70/(1 + z) correlation. Using spectral energy distribution (SED) templates which best fit this correlation, we derive the infrared luminosity of individual sources from their 24 and 70 μm luminosities. We then compute the infrared LF at zs1.55 ± 0.25 and zs2.05 ± 0.25.
Results. We observe the break in the infrared LF up to zs2.3. The redshift evolution of the infrared LF from z = 1.3 to z = 2.3 is consistent with a luminosity evolution proportional to (1 + z)1.0 ± 0.9 combined with a density evolution proportional to (1 + z)−1.1 ± 1.5. At zs2, luminous infrared galaxies (LIRGs: 1011L⊙ < LIR < 1012 L⊙) are still the main contributors to the total comoving infrared luminosity density of the Universe. At zs2, LIRGs and ultra-luminous infrared galaxies (ULIRGs: 1012L⊙ < LIR) account for s49% and s17% respectively of the total comoving infrared luminosity density of the Universe. Combined with previous results using the same strategy for galaxies at z < 1.3 and assuming a constant conversion between the infrared luminosity and star-formation rate (SFR) of a galaxy, we study the evolution of the SFR density of the Universe from z = 0 to z = 2.3. We find that the SFR density of the Universe strongly increased with redshift from z = 0 to z = 1.3, but is nearly constant at higher redshift out to z = 2.3. As part of the online material accompanying this article, we present source catalogs at 24 μm and 70 μm for both the GOODS-North and -South fields.
Key words: Galaxy: evolution / infrared: galaxies / galaxies: starburst / cosmology: observations
Appendices are only available in electronic form at http://www.aanda.org
Full Tables B1–B4 are only available in electronic form at CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/528/A35
© ESO, 2011
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