Publication: A multiwavelength consensus on the main sequence of star-forming galaxies at z similar to 2
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2014-09-01
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Wiley
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We compare various star formation rate (SFR) indicators for star-forming galaxies at 1.4 < z < 2.5 in the COSMOS field. The main focus is on the SFRs from the far-IR (PACS-Herschel data) with those from the ultraviolet, for galaxies selected according to the BzK criterion. FIR-selected samples lead to a vastly different slope of the SFR-stellar mass (M-*) relation, compared to that of the dominant main-sequence population as measured from the UV, since the FIR selection picks predominantly only a minority of outliers. However, there is overall agreement between the main sequences derived with the two SFR indicators, when stacking on the PACS maps the BzK-selected galaxies. The resulting logarithmic slope of the SFR-M-* relation is similar to 0.8-0.9, in agreement with that derived from the dust-corrected UV luminosity. Exploiting deeper 24 mu m Spitzer data, we have characterized a subsample of galaxies with reddening and SFRs poorly constrained, as they are very faint in the B band. The combination of Herschel with Spitzer data has allowed us to largely break the age/reddening degeneracy for these intriguing sources, by distinguishing whether a galaxy is very red in B-z because of being heavily dust reddened, or whether because star formation has been (or is being) quenched. Finally, we have compared our SFR(UV) to the SFRs derived by stacking the radio data and to those derived from the H alpha luminosity of a sample of star-forming galaxies at 1.4 < z < 1.7. The two sets of SFRs are broadly consistent as they are with the SFRs derived from the UV and by stacking the corresponding PACS data in various mass bins.
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This article has been accepted for publication in Monthly notices of the Royal Astronomical Society. © 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. ArtÃculo firmado por 21 autores. GR, IB and AF acknowledge support from the University of Padova from ASI (Herschel Science Contract I/005/07/0). AR acknowledges funding support from an INAF-PRIN-2010 grant. ED acknowledges funding support from the ERC-StG grants UPGAL 240039 and ANR-08-JCJC-0008. GC acknowledges support from the grant PRIN-INAF 2011 'Black hole growth and AGN feedback through the cosmic time'. AC acknowledges support from the MIUR PRIN 2010-2011 'The dark Universe and the cosmic evolution of baryons: from current surveys to Euclid'. This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan.PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain).
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