Modelling infrared galaxy evolution using a phenomenological approach

By G. Lagache, H. Dole, J. Puget. 2002

238 citations recorded by the source corpus.

To characterize the cosmological evolution of the sources contributing to the infrared extragalactic background, we have developed a phenomenological model that constrains in a simple way the evolution of the galaxy luminosity function with redshift, and fits all the existing source counts and redshift distributions, cosmic infrared background intensity and fluctuation observations, from the mid-infrared to the submillimetre range. The model is based on template spectra of starburst and normal galaxies, and on the local infrared luminosity function. Although the cosmic infrared background can be modelled with very different luminosity functions as long as the radiation production with redshift is the right one, the number counts and the anisotropies of the unresolved background imply that the luminosity function must change dramatically with redshift, with a rapid evolution of the high-luminosity sources (L > 3 × 10 11 L� ) from z = 0t oz = 1, which then stay rather constant up to redshift z = 5. The derived evolution of the infrared luminosity function may be linked to a bimodal star formation process: one associated with the quiescent and passive phase of the galaxy evolution, and one associated with the starburst phase, triggered by merging and interactions. The latter dominates the infrared and submillimetre output energy of the Universe. The model is intended as a convenient tool to plan further observations, as illustrated through predictions for Herschel, Planck and ALMA observations. Our model predictions for given wavelengths, together with some useful routines, are available for general use.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ca036073441263c041b2e6fc48974935ca460c0e

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Citations in the corpus

The Infrared Luminosity Function of Galaxies at Redshifts z = 1 and z ~ 2 in the GOODS Fields (2007, methodology): “Most of them rely on calibrations made using nearby galaxies in IRAS or ISO catalogues (e.g. Chary & Elbaz 2001; Elbaz et al. 2002; Takeuchi et al. 2005) or on the use of semi-empirical SEDs (e.g. Dale & Helou 2002; Lagache et al. 2003, 2004; Dale et al. 2005).”
A Significant Population of Very Luminous Dust-Obscured Galaxies at Redshift z ~ 2 (2008, background): “…most extreme IRAS sources, constraints on the redshift evolution out to z ∼ 1 (largely due to ISO; e.g., Franceschini et al. 2001; Chary & Elbaz 2001; Lagache et al. 2003), small samples of galaxies discovered at sub-millimeter wavelengths (e.g., Smail et al. 2002; Blain et al. 2002; Chapman et…”
A simple model to interpret the ultraviolet, optical and infrared emission from galaxies (2008, background): “They have proved useful to characterise the infrared emission from observed galaxies and to investigate the origin of the cosmic infrared background (e.g. Franceschini et al. 2001; Chary & Elbaz 2001; Elbaz et al. 2002; Lagache et al. 2003, 2004; Dale et al. 2005; Marcillac et al. 2006).”
Building the cosmic infrared background brick by brick with Herschel/PEP. ⋆ (2011, background): “Adopting the Lagache et al. (2003) definition of beam (i.e., Ω = 1.14 × θ2FWHM ), and allowing a probabilityP = 10% that sources are tightly blended and thus cannot be extracted, Dole et al. (2003) derived a SDC limit of 16.7 beams/source.”
The Herschel Multi-tiered Extragalactic Survey: HerMES (2012, methodology): “This resolution corresponds to the scale of features in the luminosity density surface from the Lagache et al. (2003) model, for example.”
Evolution of the dusty infrared luminosity function from z = 0 to z = 2.3 using observations from Spitzer (2011, methodology): “Based on these correlations SED libraries have been developed and extensively used to estimate the total infrared luminosity of galaxies (e.g., Chary & Elbaz 2001; Lagache et al. 2003; Dale & Helou 2002, hereafter CE01, LDP, and DH2 respectively).”
PAH and Mid-Infrared Luminosities as Measures of Star Formation Rate in Spitzer First Look Survey Galaxies (2005, result): “To estimate the uncertainty of the SED template, we compared it with those of 20 other SINGS normal galaxies, M82, and the models of normal and starburst galaxies by Lagache et al. (2003).”
HerMES: CANDIDATE GRAVITATIONALLY LENSED GALAXIES AND LENSING STATISTICS AT SUBMILLIMETER WAVELENGTHS (2012, background): “These sources form a separate population from traditional SMGs, which are dusty, star-bursting spheroidals, primarily at z > 0.5 (Lagache et al. 2003; Negrello et al. 2007).”
DUSTY INFRARED GALAXIES: Sources of the Cosmic Infrared Background (2005, methodology): “Predicting unbiased confusion (for instance Condon 1974; Franceschini et al. 1989; Helou & Beichman 1990; Dole et al. 2003; Lagache et al. 2003; Takeuchi et al.”
GOODS-HERSCHEL AND CANDELS: THE MORPHOLOGIES OF ULTRALUMINOUS INFRARED GALAXIES AT z ∼ 2 (2011, methodology): “…MIR-FIR SED (using the MIPS 24µm, 70µm [where available], PACS 100µm and 160µm photometry) with several different template libraries (Chary & Elbaz 2001; Dale & Helou 2002; Lagache et al. 2003; Siebenmorgen & Krügel 2007) using the SED fitting code Le Phare30 written by S. Arnouts and O. Ilbert.”
The extragalactic background light and the gamma-ray opacity of the universe (2012, background): “…number of the different type galaxies: quiescent star forming galaxies, starbursts, AGNs, and ellipticals with redshift (Rowan-Robinson, 2001, 2009; Lagache et al., 2003; Domı́nguez et al., 2011), or by simply evolving the relative number of ultraluminous infrared galaxies (ULIRGs), characterized…”