Herschel PEP: The star-formation rates of 1.5<z<2.5 massive galaxies

R. Nordon; D. Lutz; L. Shao; B. Magnelli; S. Berta; B. Altieri; P. Andreani; H. Aussel; A. Bongiovanni; A. Cava; J. Cepa; A. Cimatti; E. Daddi; H. Dominguez; D. Elbaz; N. M. Forster Schreiber; R. Genzel; A. Grazian; G. Magdis; R. Maiolino; A. M. Perez Garcia; A. Poglitsch; P. Popesso; F. Pozzi; L. Riguccini; G. Rodighiero; A. Saintonge; M. Sanchez-Portal; P. Santini; E. Sturm; L. Tacconi; I. Valtchanov; M. Wetzstein; E. Wieprecht

doi:10.1051/0004-6361/201014621

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arXiv · 1005.1074

Herschel PEP: The star-formation rates of 1.5<z<2.5 massive galaxies

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Abstract

The star formation rate (SFR) is a key parameter in the study of galaxy evolution. The accuracy of SFR measurements at z~2 has been questioned following a disagreement between observations and theoretical models. The latter predict SFRs at this redshift that are typically a factor 4 or more lower than the measurements. We present star-formation rates based on calorimetric measurements of the far-infrared (FIR) luminosities for massive 1.5 12.2 L_sun. The SFGs and AGNs tend to exhibit the same 24 micron excess. The UV SFRs are in closer agreement with the FIR-based SFRs. Using a Calzetti UV extinction correction results in a mean excess of up to 0.3 dex and a scatter of 0.35 dex from the FIR SFRs. The previous UV SFRs are thus confirmed and the mean excess, while narrowing the gap, is insufficient to explain the discrepancy between the observed SFRs and simulation predictions.

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R. Nordon, D. Lutz, L. Shao, B. Magnelli, S. Berta, B. Altieri, P. Andreani, H. Aussel, A. Bongiovanni, A. Cava, J. Cepa, A. Cimatti, E. Daddi, H. Dominguez, D. Elbaz, N. M. Forster Schreiber, R. Genzel, A. Grazian, G. Magdis, R. Maiolino, A. M. Perez Garcia, A. Poglitsch, P. Popesso, F. Pozzi, L. Riguccini, G. Rodighiero, A. Saintonge, M. Sanchez-Portal, P. Santini, E. Sturm, L. Tacconi, I. Valtchanov, M. Wetzstein, E. Wieprecht. 2010-05-06. Herschel PEP: The star-formation rates of 1.5<z<2.5 massive galaxies. https://doi.org/10.1051/0004-6361/201014621

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