Modeling the evolution of infrared galaxies: a parametric backward evolution model

By M. B'ethermin, H. Dole, G. Lagache, D. L. Borgne, A. P'enin. 2010

135 citations recorded by the source corpus.

Aims. We attempt to model the infrared galaxy evolution in as simple a way as possible and reproduce statistical properties such as the number counts between 15 μm and 1.1 mm, the luminosity functions, and the redshift distributions. We then use the fitted model to interpret observations from Spitzer, AKARI, BLAST, LABOCA, AzTEC, SPT, and Herschel, and make predictions for Planck and future experiments such as CCAT or SPICA. Methods. This model uses an evolution in density and luminosity of the luminosity function parametrized by broken power-laws with two breaks at redshift ∼0.9 and 2, and contains the two populations of the Lagache model: normal and starburst galaxies. We also take into account the effect of the strong lensing of high-redshift sub-millimeter galaxies. This effect is significant in the sub-mm and mm range near 50 mJy. It has 13 free parameters and eight additional calibration parameters. We fit the parameters to the IRAS, Spitzer, Herschel ,a ndAzTEC measurements with a Monte Carlo Markov chain. Results. The model adjusted to deep counts at key wavelengths reproduces the counts from mid-infrared to millimeter wavelengths, as well as the mid-infrared luminosity functions. We discuss the contribution to both the cosmic infrared background (CIB) and the infrared luminosity density of the different populations. We also estimate the effect of the lensing on the number counts, and discuss the discovery by the South Pole Telescope (SPT) of a very bright population lying at high redshift. We predict the contribution of the lensed sources to the Planck number counts, the confusion level for future missions using a P(D) formalism, and the Universe opacity to TeV photons caused by the CIB. Material of the model (software, tables and predictions) is available online � .

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/13c3c341b3761864a35bcca4039b18efd8ef04eb

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Citations in the corpus

HerMES: CANDIDATE GRAVITATIONALLY LENSED GALAXIES AND LENSING STATISTICS AT SUBMILLIMETER WAVELENGTHS (2012, methodology): “We note that if we use the redshift distribution from the Valiante et al. (2009) model instead for the Béthermin et al. (2011) model, the difference in the predicted number counts, mean magnification and lensed fractions is within the 68% confidence limits of our results.”
The pre-launch Planck Sky Model: a model of sky emission at submillimetre to centimetre wavelengths (2012, methodology): “Much improved models, successfully reproducing the recent data, are now available both for the epoch-dependent luminosity function (hence for the source counts; e.g. Béthermin et al. 2011; Lapi et al. 2011) and for the clustering properties (e.g. Xia et al. 2012; Pénin et al. 2012).”
THE CONTRIBUTION OF STARBURSTS AND NORMAL GALAXIES TO INFRARED LUMINOSITY FUNCTIONS AT z < 2 (2012, background): “The evolving shape of IR LFs hence implicitly contains information on the relative importance of the two modes of SF in the past (e.g., Franceschini et al. 2001, Béthermin et al. 2011).”
The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z ≃ 4 (2013, background): “The results of these works (especially those of Bethermin et al. 2011, showing a decrease of Φ? at z>1 and a flatter trend on the evolution of L? at z>2), are close to ours, though with the source counts only it was not possible to constrain the evolution of IR sources at z>2.”
Evolution of the dust emission of massive galaxies up to z=4 and constraints on their dominant mode of star formation (2014, methodology): “This effect has been discussed in detail by several authors (e.g., Bavouzet 2008; Béthermin et al. 2010b, 2012b; Kurczynski & Gawiser 2010; Bourne et al. 2012; Viero et al. 2013).”
GOODS-HERSCHEL AND CANDELS: THE MORPHOLOGIES OF ULTRALUMINOUS INFRARED GALAXIES AT z ∼ 2 (2011, background): “…with Spitzer and now Herschel have shown that while rare locally, (U)LIRGs were once much more common and even dominated the cosmic star formation rate at z > 1 (e.g., Floc’h et al. 2005; Caputi et al. 2007; Magnelli et al. 2009; Magnelli et al. 2011; Béthermin et al. 2011; Murphy et al. 2011).”
HerMES: deep number counts at 250 μm, 350 μm and 500 μm in the COSMOS and GOODS-N fields and the build-up of the cosmic infrared background (2012, methodology): “In large fields, this effect is not negligible, and the clustering of the sources must be taken into account (Béthermin et al. 2010a).”
Dusty Star Forming Galaxies at High Redshift (2014, methodology): “Another phenomenological approach described in Béthermin et al. (2011), working backwards from constrained luminosity functions to redshift distributions and number counts predicts a peak at very low redshifts with a secondary peak10 at z ∼ 2.”
Panchromatic spectral energy distributions of Herschel sources (2013, background): “…the statistical properties of galaxy populations, for example while interpreting and modeling observed number counts (e.g. Berta et al. 2011, 2010; Béthermin et al. 2011; Franceschini et al. 2010) or assessing luminosity functions at different wavelengths (e.g. Gruppioni et al. 2013, 2010;…”
A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH TWO YEARS OF SOUTH POLE TELESCOPE OBSERVATIONS (2011, methodology): “We test the impact of the flux cut with the modeled source counts of Béthermin et al. (2011) and Negrello et al. (2007), and find the two models predict a difference in the Poisson power of 4% or 16% respectively.”