Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelength Spitzer observations up to z ~ 2.5

By G. Rodighiero, Mattia Vaccari, A. Franceschini, L. Tresse, O. Fèvre, V. Brun, C. Mancini, I. Matute, A. Cimatti, L. Marchetti and 18 more. 2009

145 citations recorded by the source corpus.

Context. Studies of the infrared (IR) emission of cosmic sources have proven essential to constraining the evolutionary history of cosmic star formation and the gravitational accretion of nuclear black holes, because many of these events occur inside heavily dust-extinguished environments. Aims. The Spitzer Space Telescope has provided a large amount of data to constrain the nature and cosmological evolution of infrared source populations. In the present paper we exploit a large homogeneous dataset to derive a self-consistent picture of IR emission based on the time-dependent λ_(eff) = 24, 15, 12, and 8 μm monochromatic and bolometric IR luminosity functions (LF) over the full 0 < z < 2.5 redshift range. Methods. Our present analysis is based on a combination of data from deep Spitzer surveys of the VIMOS VLT Deep Survey (VVDS-SWIRE) and GOODS fields. To our limiting flux of S_(24) = 400 μJy, our sample derived from VVDS-SWIRE includes 1494 sources, and 666 and 904 sources brighter than S_(24) = 80 μJy are catalogued in GOODS-S and GOODS-N, respectively, for a total area of ~0.9 square degrees. Apart from a few galaxies, we obtain reliable optical identifications and redshifts for all these sources, providing a rich and robust dataset for our luminosity function determination. The final combined reliable sample includes 3029 sources, the fraction with photometric redshifts being 72% over all redshifts and almost all galaxies at z > 1.5. Based on the multiwavelength information available in these areas, we constrain the LFs at 8, 12, 15, and 24 μm. We also infer the total IR luminosities from our best-fit model of the observed SEDs of each source, and use this to derive the bolometric (8–1000 μm) LF and comoving volume emissivity to z ~ 2.5. Results. In the redshift interval 0 1. The mean redshift of the peak in the source number density shifts with luminosity: the brightest IR galaxies appear to form stars at earlier cosmic times (z > 1.5), while star formation in the less luminous galaxies continues until more recent epochs (z ~ 1 for L_(IR) < 10^(11)_☉), in overall agreement with similar analyses in the literature. Conclusions. Our results are indicative of a rapid increase in the galaxy IR comoving volume emissivity up to z ~ 1 and a constant average emissivity at z > 1. We also appear to measure a difference in the evolutionary rate of the source number densities as a function of luminosity, which is consistent with the downsizing evolutionary patterns reported for other samples of cosmic sources.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

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Citations in the corpus

• GeV OBSERVATIONS OF STAR-FORMING GALAXIES WITH THE FERMI LARGE AREA TELESCOPE (2012, methodology): “TheX-band luminosity distribution is drawn from the total IR luminosity function of Rodighiero et al. (2010) at redshiftz = 0, with a minimum IR luminosity of 108L⊙.”
• The LABOCA survey of the Extended Chandra Deep Field-South: clustering of submillimetre galaxies (2011, background): “This evolution may explain why the most powerful starbursts at low redshift (ULIRGs) have lower typical SFRs than z ∼ 2 SMGs (e.g. Le Floc’h et al. 2005; Rodighiero et al. 2010).”
• The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z ≃ 4 (2013, methodology): “…z∼1 (Elbaz et al. 2007) and up to z∼2 (Daddi et al. 2007, Rodighiero et al. 2011) and z∼3 (Magdis et al. 2010), with normalisation scaling as ∼(1+z)2.8 out to z∼2, as shown by Sargent et al. (2012) (see also Elbaz et al. 2007, Rodighiero et al. 2010b, Pannella et al. 2009, Karim et al. 2011).”
• THE CONTRIBUTION OF STARBURSTS AND NORMAL GALAXIES TO INFRARED LUMINOSITY FUNCTIONS AT z < 2 (2012, background): “We compare our prediction with measurements of the z > 0 IR LFs of Le Floc’h et al. (2005) and Rodighiero et al. (2010), both based on Spitzer/MIPS 24µm photometry.”
• THE STAR FORMATION HISTORY OF MASS-SELECTED GALAXIES IN THE COSMOS FIELD (2010, methodology): “Most recently, based on first Herschel/PACS far-infrared data, even the opposite effect, the so-called SSFR-upsizing at z & 1.5, has been proposed (Rodighiero et al. 2010a).16 More measurements are needed to understand the relation of SFR and stellar mass and its evolution with redshift.”
• Star-forming galaxies as the origin of diffuse high-energy backgrounds: gamma-ray and neutrino connections, and implications for starburst history (2014, methodology): “Up to now, the total emissivity of IR galaxies at high redshifts had been poorly known because of the scarcity of Spitzer galaxies at z > 2, the large spectral extrapolations to derive the total IR luminosity from the mid-IR, and the incomplete information on the redshift distribution of mid-IR sour”
• REGULARITY UNDERLYING COMPLEXITY: A REDSHIFT-INDEPENDENT DESCRIPTION OF THE CONTINUOUS VARIATION OF GALAXY-SCALE MOLECULAR GAS PROPERTIES IN THE MASS-STAR FORMATION RATE PLANE (2013, unknown): “…Peng et al. 2010, Leitner 2012, Behroozi et al. 2013) and that the strong decline of the cosmic SFR density since z∼ 2 (e.g., Reddy & Steidel 2009, Rodighiero et al. 2010, Karim et al. 2011, Magnelli et al. 2011, Cucciati et al. 2012; and references therein) reflects the uniform SFR evolution…”
• What drives the growth of black holes (2011, background): “However, powerful starbursts are rare in the local Universe, compared to higher redshift where they dominate the star formation density (e.g., Le Floc’h et al., 2005; Rodighiero et al., 2010b).”
• A POPULATION OF MASSIVE, LUMINOUS GALAXIES HOSTING HEAVILY DUST-OBSCURED GAMMA-RAY BURSTS: IMPLICATIONS FOR THE USE OF GRBs AS TRACERS OF COSMIC STAR FORMATION (2013, background): “…galaxies (ULIRGs and SMGs), with the remaining fraction about evenly distributed between moderately luminous galaxies (LIRGs and luminous LBGs) and lower-luminosity systems (Reddy et al. 2008; Reddy & Steidel 2009; Rodighiero et al. 2010; Murphy et al. 2011; Magnelli et al. 2011).”
• The LABOCA survey of the Extended Chandra Deep Field South: A photometric redshift survey of submillimetre galaxies (2010, background): “…strong evolution in the FIR luminosity function: the z = 2–3 SMGs are more luminous and have higher space densities than the z = 1–2 SMGs, which in turn are more luminous than the z < 0.3 24-µm-selected galaxies from Rodighiero et al. (2010) (see also the Herschel sample of Vaccari et al. 2010).”
• The BAHAMAS project: Calibrated hydrodynamical simulations for large-scale structure cosmology (2016, background): “For comparison, we show a range of recent measurements which use different SFR tracers, including Rodighiero et al. (2010) (IR), Karim et al. (2011) (radio), Cucciati et al. (2012) (UV), Bouwens et al. (2012) (UV), and Burgarella et al. (2013) (IR+UV).”
• A CORRELATION BETWEEN STAR FORMATION RATE AND AVERAGE BLACK HOLE ACCRETION IN STAR-FORMING GALAXIES (2013, methodology): “We generated IR luminosities for the galaxies in the mock catalog based on the IRLF from Rodighiero et al. (2010).”
• Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation (2013, background): “Our derived star formation history nicely agrees with the infrared measurements of the dustobscured star-formation rate density of Rodighiero et al. (2010) A30, page 19 of 39 and Magnelli et al. (2011), up to z ∼ 2.”
• Modeling the evolution of infrared galaxies: a parametric backward evolution model (2010, methodology): “We also agree well with higher redshift measurements of Rodighiero et al. (2010) and Pascale et al. (2009, see Fig.”
• Herschel PEP/HerMES: the redshift evolution (0 ≤ z ≤ 4) of dust attenuation and of the total (UV+IR) star formation rate density (2013, background): “The plateau up to z ∼ 2.5 is seen by Rodighiero et al.(2010) and Magnelli et al.(2011) while the decrease of ρS FR at z ≥ 2 The conversion from IRX to AFUV from Burgarella et al.(2005) is valid at log10 (LFIR/LFUV )>-1.2: AFUV = -0.028 [log10 LFIR/LFUV ] 3 + 0.392 [log10 LFIR/LFUV ] 2 + 1.094…”
• Panchromatic spectral energy distributions of Herschel sources (2013, methodology): “For reference, the MS locus defined by stacking 4.5µm selected galaxies (Rodighiero et al. 2010a) is shown by dashed lines (obtained by interpolating between Rodighiero’s redshift bins), andthe levels of MS+0.6 and+1.0 dex are marked with dotted lines.”
• The extragalactic background light and the gamma-ray opacity of the universe (2012, methodology): “However, the recent deep surveys with the Spitzer and Herschel satellites show strong evolution in number counts, compared to predictions made with no evolution models (Lagache et al., 2005; Rodighiero et al., 2010).”
• THE LESSER ROLE OF STARBURSTS IN STAR FORMATION AT z = 2 (2011, methodology): “IR luminosities (hence SFRs) are derived from PACS fluxes using a set of empirical templates of local objects (Polletta et al. 2007; Gruppioni et al. 2010) as described in Rodighiero et al. (2010a).”