A UNIFIED EMPIRICAL MODEL FOR INFRARED GALAXY COUNTS BASED ON THE OBSERVED PHYSICAL EVOLUTION OF DISTANT GALAXIES

By M. B'ethermin, E. Daddi, G. Magdis, M. Sargent, Y. Hezaveh, D. Elbaz, D. Le Borgne, James Mullaney, M. Pannella, V. Buat and 3 more. 2012

173 citations recorded by the source corpus.

We reproduce the mid-infrared to radio galaxy counts with a new empirical model based on our current understanding of the evolution of main-sequence (MS) and starburst (SB) galaxies. We rely on a simple spectral energy distribution (SED) library based on Herschel observations: a single SED for the MS and another one for SB, getting warmer with redshift. Our model is able to reproduce recent measurements of galaxy counts performed with Herschel, including counts per redshift slice. This agreement demonstrates the power of our 2-Star-Formation Modes (2SFM) decomposition in describing the statistical properties of infrared sources and their evolution with cosmic time. We discuss the relative contribution of MS and SB galaxies to the number counts at various wavelengths and flux densities. We also show that MS galaxies are responsible for a bump in the 1.4 GHz radio counts around 50 μJy. Material of the model (predictions, SED library, mock catalogs, etc.) is available online.

View Paper: https://www.semanticscholar.org/paper/025b71affa1ac8a1bde61f331c77b82887d4e254

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1. P. Hopkins
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5. R. Dav'e
6. D. M. Alexander
7. E. Daddi
8. Volker Springel

Citations in the corpus

• Submillimetre galaxies in a hierarchical universe: number counts, redshift distribution, and implications for the IMF (2012, unknown): “…models (e.g. Pearson & RowanRobinson 1996; Blain et al. 1999b; Devriendt & Guiderdoni 2000; Lagache, Dole & Puget 2003; Negrello et al. 2007; Béthermin et al. 2012), semi-analytic models (SAMs; e.g. Guiderdoni et al. 1998; Blain et al. 1999a; Granato et al. 2000, 2004; Kaviani, Haehnelt &…”
• THE EVOLVING INTERSTELLAR MEDIUM OF STAR-FORMING GALAXIES SINCE z = 2 AS PROBED BY THEIR INFRARED SPECTRAL ENERGY DISTRIBUTIONS (2012, methodology): “• 250, 350 and 500µm: We use the GOODSHerschel SPIRE (Elbaz et al. 2011) data and the mean of pixels centred on sources as in Béthermin et al. (2012a).”
• ALMA REDSHIFTS OF MILLIMETER-SELECTED GALAXIES FROM THE SPT SURVEY: THE REDSHIFT DISTRIBUTION OF DUSTY STAR-FORMING GALAXIES (2013, background): “Béthermin et al. (2012) present an empirical model starting from the observed FIR number counts split into “main-sequence” and starburst mode star-forming galaxies.”
• Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation (2013, methodology): “(56) We assume the shot-noise levels given by the sum of the values quoted in Tables 6 and 7, from Béthermin et al. (2012a) and Tucci et al. (2011), respectively, and we assume flat priors around them with width given by their 1σ error.”
• Planck 2015 results. XI. CMB power spectra, likelihoods, and robustness of parameters (2015, methodology): “For dusty galaxies we use the Béthermin et al. (2012) model, as in Planck Collaboration XXX (2014). The model is in good agreement with the number counts measured with te Spitzer Space Telescope and the Herschel Space Observatory.”
• Herschel PEP/HerMES: the redshift evolution (0 ≤ z ≤ 4) of dust attenuation and of the total (UV+IR) star formation rate density (2013, methodology): “At z = 3− 4, the decrease observed in the SFRD is not unexpected: most high redshift studies clearly suggest such a trend through rest-frame UV observations (Hopkins & Beacom(2006), Bouwens et al.(2011)) and predicted by Béthermin et al.(2012a).”
• GOODS-HERSCHEL: STAR FORMATION, DUST ATTENUATION, AND THE FIR–RADIO CORRELATION ON THE MAIN SEQUENCE OF STAR-FORMING GALAXIES UP TO z ≃ 4 (2014, methodology): “…are deemed more accurate than methods based on bolometric correction extrapolation of singleIR band measurements because they use the more extended photometric information that can also account for the slight evolution in redshift of the median IR SED (Magdis et al. 2012; Béthermin et al. 2012a).”
• The star formation main sequence and stellar mass assembly of galaxies in the Illustris simulation (2014, methodology): “This minor contribution of starbursts to the total SFR density is consistent with semi-empirical models for infrared galaxy number counts (Béthermin et al. 2012) and luminosity functions (Hopkins et al. 2010).”
• The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z ≃ 4 (2013, result): “Our results have been compared to the SFR densities (converted to ρIR using the Kennicutt 1998 relation) for on- and off-MS sources based on the Sargent et al. (2012) model recently derived by Bethermin et al. (2012).”
• The evolution of the dust temperatures of galaxies in the SFR–M∗ plane up to z ~ 2 (2013, methodology): “…in the SFR−M∗ plane is also important to test the accuracy of FIR spectral energy distribution (SED) libraries routinely used to infer total infrared luminosities from monochromatic observations, or used in backward evolutionary models (see e.g., Valiante et al. 2009; Béthermin et al. 2012a).”
• Clustering of intermediate redshift quasars using the final SDSS III-BOSS sample (2015, background): “2010; Behroozi, Conroy & Wechsler 2010; Béthermin et al. 2012; Viero et al. 2013b), providing further circumstantial evidence for a link.”
• The deepest Herschel-PACS far-infrared survey: number counts and infrared luminosity functions from combined PEP/GOODS-H observations (2013, background): “…from backwards or forwards evolutionary models (Lagache et al. 2004; Rowan-Robinson 2009; Valiante et al. 2009; Le Borgne et al. 2009; Franceschini et al. 2010; Gruppioni et al. 2010; Lacey et al. 2010; Marsden et al. 2011; Rahmati & van der Werf 2011; Niemi et al. 2012; Béthermin et al. 2012).”
• Cosmological parameters derived from the final Planck data release (PR4) (2023, methodology): “…a flat Poisson-like power spectrum for each component and use a power law to describe the spectral energy distribution (SED) for the radio sources as a rad ν ∝ ν − β s (Tucci et al. 2011), while we use a IR ν = ν β IR B ν ( T ) (Béthermin et al. 2012) for infrared dusty star-forming galaxies.”
• ISM MASSES AND THE STAR FORMATION LAW AT Z = 1 TO 6: ALMA OBSERVATIONS OF DUST CONTINUUM IN 145 GALAXIES IN THE COSMOS SURVEY FIELD (2015, background): “In recent years, there have been numerous works specifying the MS evolution (Noeske et al. 2007; Rodighiero et al. 2011; Béthermin et al. 2012; Speagle et al. 2014; Lee et al. 2015; Schreiber et al. 2015).”