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26 April 2024
 
  » arxiv » 1304.4593

 Article overview



Far-IR Emission From Dust-Obscured Galaxies
J.A. Calanog ; J. Wardlow ; Hai Fu ; A. Cooray ; R.J. Assef ; J. Bock ; C.M. Casey ; A. Conley ; D. Farrah ; E. Ibar ; J. Kartaltepe ; G. Magdis ; L. Marchetti ; S.J. Oliver ; I. Perez-Fournon ; D. Riechers ; D. Rigopoulou ; I.G. Roseboom ; B. Schulz ; Douglas Scott ; M. Symeonidis ; M. Vaccari ; M. Viero ; M. Zemcov ;
Date 16 Apr 2013
AbstractDust-obscured galaxies (DOGs) are a UV-faint, IR-bright galaxy population that reside at z~2 and are believed to be in a phase of dusty star-forming and AGN activity. We present far-IR observations of a complete sample of DOGs in the 2 deg^2 of COSMOS. The 3077 DOGs have <z>=1.9+/-0.3 and are selected from 24 um and r+ observations using a color cut of r+ - [24] >= 7.5 (AB mag) and S24 >= 100 uJy. Based on the mid-IR SEDs, 47% are star-formation dominated and 10% are AGN-dominated. We use SPIRE far-IR photometry from HerMES to calculate the IR luminosity and characteristic dust temperature for the 1572 (51%) DOGs that are detected at 250 um (>=3sigma). For the remaining 1505 (49%) that are undetected, we perform a median stacking analysis to probe fainter luminosities. Detected and undetected DOGs have average IR luminosities of (2.8+/-0.4) x 10^12 L_Sun and (0.77+/-0.08) x 10^12L_Sun, and dust temperatures of 34+/-7 K and 31+/-3 K, respectively. Using far-IR observations, DOGs contribute 30% to the 24 um-selected galaxies’ IR luminosity. If the IR luminosity is extrapolated using the 24 um flux density alone, it is overestimated by a factor of 2 on average. DOGs contribute 10-30% to the total star formation rate density of the Universe at z=1.5-2.5, dominated by 250{mu}m detected and bump DOGs, compared to around 40% for all 24 um galaxies above our flux limit. DOGs have a large scatter about the star-formation main sequence and their specific star-formation rates show that the observed phase of star-formation could be responsible for their observed stellar mass at z~2.
Source arXiv, 1304.4593
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