Volume 557, September 2013
|Number of page(s)||22|
|Section||Cosmology (including clusters of galaxies)|
|Published online||02 September 2013|
The redshift evolution of the distribution of star formation among dark matter halos as seen in the infrared⋆
Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu – CNRS – Université Paris
pt courrier 131,
2 Computational Cosmology, Department of Physics, University of Durham, South Road, Durham, DH1 3LE, UK
3 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
4 California Institute of Technology, MC249-17, Pasadena, CA 91125, USA
5 Institut d’Astrophysique Spatiale, CNRS (UMR 8617), Université Paris-Sud 11, Bâtiment 121, 91405 Orsay, France
Accepted: 8 June 2013
Recent studies have revealed a strong correlation between the star formation rate (SFR) and stellar mass of the majority of star-forming galaxies, the so-called star-forming main sequence. An empirical modeling approach (the 2-SFM framework) that distinguishes between the main sequence and rarer starburst galaxies is capable of reproducing most statistical properties of infrared galaxies, such as number counts, luminosity functions, and redshift distributions. In this paper, we extend this approach by establishing a connection between stellar mass and halo mass with the technique of abundance matching. Based on a few simple assumptions and a physically motivated formalism, our model successfully predicts the (cross-)power spectra of the cosmic infrared background (CIB), the cross-correlation between CIB and cosmic microwave background (CMB) lensing, and the correlation functions of bright, resolved infrared galaxies measured by Herschel, Planck, ACT, and SPT. We use this model to infer the redshift distribution of CIB-anisotropies and of the CIB × CMB lensing signal, as well as the level of correlation between CIB-anisotropies at different wavelengths. We study the link between dark matter halos and star-forming galaxies in the framework of our model. We predict that more than 90% of cosmic star formation activity occurs in halos with masses between 1011.5 and 1013.5 M⊙. If taking subsequent mass growth of halos into account, this implies that the majority of stars were initially (at z > 3) formed in the progenitors of clusters (Mh(z = 0) > 1013.5 M⊙), then in groups (1012.5 < Mh(z = 0) < 1013.5 M⊙) at 0.5 < z < 3, and finally in Milky-Way-like halos (1011.5 < Mh(z = 0) < 1012.5 M⊙) at z < 0.5. At all redshifts, the dominant contribution to the SFR density stems from halos of mass ~1012 M⊙, in which the instantaneous star formation efficiency – defined here as the ratio between SFR and baryonic accretion rate – is maximal (~70%). The strong redshift-evolution of SFR in the galaxies that dominate the CIB is thus plausibly driven by increased accretion from the cosmic web onto halos of this characteristic mass scale. Material (effective spectral energy distributions, differential emissivities of halos, relations between Mh and SFR) associated to this model is available at http://irfu.cea.fr/Sap/Phocea/Page/index.php?id=537.
Key words: galaxies: star formation / galaxies: halos / galaxies: statistics / diffuse radiation / dark matter / submillimeter: galaxies
The effective SEDs are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/557/A66
© ESO, 2013
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