Polycyclic Aromatic Hydrocarbon Contribution to the Infrared Output Energy of the Universe at z ≃ 2

By G. Lagache, H. Dole, J. Puget, P. Pérez-González, É. Le Floc'h, G. Rieke, C. Papovich, E. Egami, A. Alonso-Herrero, C. Engelbracht and 3 more. 2004

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We present an updated phenomenological galaxy evolution model to fit the Spitzer 24, 70, and 160 μm number counts, as well as all the previous mid- and far-infrared observations. Only a minor change of the comoving luminosity density distribution in the previous model (Lagache, Dole, & Puget), combined with a slight modification of the starburst template spectra mainly between 12 and 30 μm, are required to fit all the data available. We show that the peak in the Spitzer Multiband Imaging Photometer 24 μm counts is dominated by galaxies with redshift between 1 and 2, with a nonnegligible contribution from the z ≥ 2 galaxies (∼30% at S = 0.2 mJy). The very close agreement between the model and number counts at 15 and 24 μm strikingly implies that (1) the polycyclic aromatic hydrocarbon features remain prominent in the redshift band 0.5-2.5 and (2) the IR energy output has to be dominated by ∼3 × 1011 L⊙ to ∼3 × 1012 L⊙ galaxies from redshift 0.5 to 2.5. Combining Spitzer with Infrared Space Observatory deep cosmological surveys gives for the first time an unbiased view of the infrared universe from z = 0 to 2.5.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b24dcd30a47805e23d829e8d7a63d9171dc0ac38

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In Astronomy and Astrophysics

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Citations in the corpus

• Analysis of galaxy spectral energy distributions from far-UV to far-IR with CIGALE: studying a SINGS test sample (2009, methodology): “2002, Lagache et al. 2003, 2004).”
• The Cosmic Infrared Background Resolved by Spitzer. Contributions of Mid-Infrared Galaxies to the Far-Infrared Background. (2006, methodology): “The Lagache et al. (2004) model predicts a CIB at 240 µm of 0.98 MJy/sr, which is in very good agreement with the estimate from combined measurements discussed above.”
• Modeling the evolution of infrared galaxies: a parametric backward evolution model (2010, methodology): “The backward evolution models (like Lagache et al. 2004; Franceschini et al. 2010; Rowan-Robinson 2009; Valiante et al. 2009) use an evolution the luminosity function (LF) of the galaxies to reproduce empirically the galaxy counts, and other constraints.”
• Deep Spitzer 24 μm COSMOS Imaging. I. The Evolution of Luminous Dusty Galaxies—Confronting the Models (2009, methodology): “Finally, Lagache et al. (2004) assume a population of luminous starbursts characterized by luminosity-dependent SEDs as well as a population of quiescent cold galaxies evolving independently from the star-forming sources.”
• 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).”
• Toward an Understanding of the Rapid Decline of the Cosmic Star Formation Rate (2005, background): “There is a total range of a factor of 2 difference between the conversions that would be predicted by various templates for galaxies in the appropriate luminosity range of 1011 L (Devriendt et al. 1999; Dale et al. 2001; Chary & Elbaz 2001; Lagache et al. 2003, 2004).”
• The Mid-Infrared Spectrum of Star-forming Galaxies: Global Properties of Polycyclic Aromatic Hydrocarbon Emission (2006, background): “The importance of quantifying not just the average shape of the mid-infrared spectrum of star-forming galaxies, but the range of variation in that shape, is well illustrated by the source count models of Lagache et al. (2004).”
• Evolution of the dusty infrared luminosity function from z = 0 to z = 2.3 using observations from Spitzer (2011, background): “…1012L⊙ < LIR) in the evolution of the star-formation rate (SFR) history of the Universe is now well established up toz ∼ 1 (Chary & Elbaz 2001; Franceschini et al. 2001; Xu et al. 2001; Elbaz et al. 2002; Metcalfe et al. 2003; Lagache et al. 2004; Le Floc’h et al. 2005; Magnelli et al. 2009).”
• Fitting the integrated spectral energy distributions of galaxies (2010, background): “Well known examples of templates include those of Chary and Elbaz (2001), Dale and Helou (2002), Lagache et al. (2004), and, more recently, Rieke et al. (2009).”
• A semi-empirical simulation of the extragalactic radio continuum sky for next generation radio telescopes (2008, background): “More complex models of the evolution of star-forming galaxies have been put forward to interpret mid- and far-infraredobservations (e.g. Franceshini et al. 2001; Lagache et al. 2004).”
• Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelength Spitzer observations up to z ~ 2.5 (2009, unknown): “The ISO results have been further extended in redshift, to z > 1, by theSpitzer Space Telescope (Papovich et al. 2004; Marleau et al. 2004; Dole et al. 2004, Lagache et al. 2004), operating between 3.6 and 160µm with improved sensitivity and spatial resolution compared to previous IR observatories.”
• Building the cosmic infrared background brick by brick with Herschel/PEP. ⋆ (2011, background): “These models do not implement fundamental physical information but simply attempt to describe the evolution of galaxy populations (e.g. Lagache et al. 2004; Franceschiniet al. 2010; Rowan-Robinson 2009; Le Borgne et al. 2009; Valiante et al. 2009; Béthermin et al. 2010c; Marsden et al. 2010;…”
• Dusty Star Forming Galaxies at High Redshift (2014, background): “At redshifts z ∼ 1–2, the observed 24 µm band could be dominated by emission features generated by heavier dust grains, in particular Polycyclic Aromatic Hydrocarbons (PAHs; Lagache et al., 2004) which are associated with star-forming regions (see more in Section 5.7).”
• HerMES: SPIRE galaxy number counts at 250, 350, and 500 μm (2010, methodology): “We compare the number counts with eight models, one pre-Spitzer (Xu et al. 2003), two based on the ISO, SCUBA and Spitzer first results (Lagache et al. 2004; Negrello et al. 2007) and 5 being more constrained by deep Spitzer, SCUBA, AzTEC, and recent BLAST observations (Le Borgne et al. 2009;…”
• The Infrared Luminosity Function of Galaxies at Redshifts z = 1 and z ~ 2 in the GOODS Fields (2007, methodology): “Also, IR-galaxy models which assume such similarity in the SEDs can fit the 24, 70 and 160 µm number counts simultaneously (Lagache et al. 2004).”
• DUSTY INFRARED GALAXIES: Sources of the Cosmic Infrared Background (2005, methodology): “(2004) In this paper, we make extensive use of the Lagache et al. (2004) phenomenological model to illustrate our points.”
• 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): “Our simulation is based on Béthermin et al. (2011) model, which is a parametric model based on the Lagache et al. (2004) spectral energy distribution (SED) library (two populations: normal and starburst galaxies).”