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Title:
Luminosity functions for galaxies and quasars in the Spitzer Wide-area Infrared Extragalactic Legacy Survey
Authors:
Babbedge, T. S. R.; Rowan-Robinson, M.; Vaccari, M.; Surace, J. A.; Lonsdale, C. J.; Clements, D. L.; Fang, F.; Farrah, D.; Franceschini, A.; Gonzalez-Solares, E.; Hatziminaoglou, E.; Lacey, C. G.; Oliver, S.; Onyett, N.; Pérez-Fournon, I.; Polletta, M.; Pozzi, F.; Rodighiero, G.; Shupe, D. L.; Siana, B.; Smith, H. E.
Affiliation:
AA(Astrophysics Group, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2BW), AB(Astrophysics Group, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2BW), AC(Astrophysics Group, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2BW), AD(Spitzer Science Center, MS 220-6, California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA 91125, USA), AE(Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology, JPL, Pasadena, CA 91125, USA; Center for Astrophysics & Space Sciences, University of California San Diego, La Jolla, CA 92093-0424, USA), AF(Astrophysics Group, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2BW), AG(Spitzer Science Center, MS 220-6, California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA 91125, USA), AH(Department of Astronomy, Cornell University, Space Sciences Building, Ithaca, NY 14853, USA), AI(Dipartimento di Astronomia, Universita di Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy), AJ(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA), AK(Institute de Astrofisica de Canarias, C/Via Lactea s/n, E-38200 La Laguna, Spain), AL(Institute for Computational Cosmology, University of Durham, South Road, Durham DH1 3LE), AM(Astronomy Centre, Department of Physics & Astronomy, University of Sussex, Brighton BN1 9QH), AN(Astronomy Centre, Department of Physics & Astronomy, University of Sussex, Brighton BN1 9QH), AO(Institute de Astrofisica de Canarias, C/Via Lactea s/n, E-38200 La Laguna, Spain), AP(Center for Astrophysics & Space Sciences, University of California San Diego, La Jolla, CA 92093-0424, USA), AQ(Dipartimento di Astronomia, Universit di Bologna, viale Berti Pichat 6, I-40127 Bologna, Italy), AR(Dipartimento di Astronomia, Universita di Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy), AS(Spitzer Science Center, MS 220-6, California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA 91125, USA), AT(Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology, JPL, Pasadena, CA 91125, USA), AU(Center for Astrophysics & Space Sciences, University of California San Diego, La Jolla, CA 92093-0424, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 370, Issue 3, pp. 1159-1180. (MNRAS Homepage)
Publication Date:
08/2006
Origin:
MNRAS
MNRAS Keywords:
galaxies: evolution: galaxies: photometry: quasars: general: cosmology: observations
Abstract Copyright:
(c) 2006 The Authors. Journal compilation © 2006 RAS
DOI:
10.1111/j.1365-2966.2006.10547.x
Bibliographic Code:
2006MNRAS.370.1159B

Abstract

We construct rest-frame luminosity functions (LFs) at 3.6, 4.5, 5.8, 8 and 24 μm over the redshift range 0 < z < 2 for galaxies and 0 < z < 4 for optical quasi-stellar objects (QSOs), using optical and infrared (IR) data from the Spitzer Wide-area Infrared Extragalactic (SWIRE) Survey. The 3.6- and 4.5-μm galaxy LFs show evidence for moderate positive luminosity evolution up to z ~ 1.5, consistent with the passive ageing of evolved stellar populations. Their comoving luminosity density was found to evolve passively, gradually increasing out to z ~ 0.5-1 but flattening, or even declining, at higher redshift. Conversely, the 24-μm galaxy LF, which is more sensitive to obscured star formation and/or active galactic nuclei (AGN) activity, undergoes strong positive evolution, with the derived IR energy density and star formation rate (SFR) density ~ (1 + z)γ with γ = 4.5+0.7-0.6 and the majority of this evolution occurring since z ~ 1. Optical QSOs, however, show positive luminosity evolution in all bands, out to the highest redshifts (3 < z < 4). Modelling as L* ~ (1 + z)γ gave γ = 1.3+0.1-0.1 at 3.6μm,γ = 1.0+0.1-0.1 at 4.5μm and stronger evolution at the longer wavelengths (5.8, 8 and 24μm), of γ ~ 3. Comparison of the galaxy LFs to predictions from a semi-analytic model based on cold dark matter (CDM) indicates that an initial mass function (IMF) skewed towards higher mass star formation in bursts compared to locally be preferred. As a result, the currently inferred massive SFRs in distant submm sources may require substantial downwards revision.
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