%0 Generic %1 Popesso2011 %A Popesso, P. %A Biviano, A. %A Rodighiero, G. %A Baronchelli, I. %A Salvato, M. %A Saintonge, A. %A Finoguenov, A. %A Magnelli, B. %A Gruppioni, C. %A Pozzi, F. %A Lutz, D. %A Elbaz, D. %A Altieri, B. %A Andreani, P. %A Aussel, H. %A Berta, S. %A Capak, P. %A Cava, A. %A Cimatti, A. %A Coia, D. %A Daddi, E. %A Dannerbauer, H. %A Dickinson, M. %A Dasyra, K. %A Fadda, D. %A Schreiber, N. Förster %A Genzel, R. %A Hwang, H. S. %A Kartaltepe, J. %A Ilbert, O. %A Floch, E. Le %A Leiton, R. %A Magdis, G. %A Nordon, R. %A Patel, S. %A Poglitsch, A. %A Riguccini, L. %A Portal, M. Sanchez %A Shao, L. %A Tacconi, L. %A Tomczak, A. %A Tran, K. %A Valtchanov, I. %D 2011 %K evolution sfr specific %T The evolution of the star formation activity per halo mass up to redshift ~ 1.6 as seen by Herschel %U http://arxiv.org/abs/1110.2946 %X Star formation in massive galaxies is quenched at some point during hierarchical mass assembly. To understand where and when the quenching processes takes place, we study the evolution of the total star formation rate per unit total halo mass (\Sigma(SFR/M)) in three different mass scales: low mass halos (field galaxies), groups, and clusters, up to a redshift ~1.6. We use deep far-infrared PACS data at 100 and 160 um to accurately estimate the total star formation rate of the Luminous Infrared Galaxy population of 9 clusters with mass ~10^15 M_ødot, and 9 groups/poor clusters with mass ~ 5 x 10^13 M_ødot. Estimates of the field \Sigma(SFR/M) are derived from the literature, by dividing the star formation rate density by the mean comoving matter density of the universe. The field \Sigma(SFR/M) increases with redshift up to z~1 and it is constant thereafter. The evolution of the \Sigma(SFR/M)-z relation in galaxy systems is much faster than in the field. Up to redshift z~0.2, the field has a higher \Sigma(SFR/M) than galaxy groups and galaxy clusters. At higher redshifts, galaxy groups and the field have similar \Sigma(SFR/M), while massive clusters have significantly lower \Sigma(SFR/M) than both groups and the field. There is a hint of a reversal of the SFR activity vs. environment at z~1.6, where the group \Sigma(SFR/M) lies above the field \Sigma(SFR/M)-z relation. We discuss possible interpretations of our results in terms of the processes of downsizing, and star-formation quenching.

@misc{Popesso2011, abstract = { Star formation in massive galaxies is quenched at some point during hierarchical mass assembly. To understand where and when the quenching processes takes place, we study the evolution of the total star formation rate per unit total halo mass (\Sigma(SFR/M)) in three different mass scales: low mass halos (field galaxies), groups, and clusters, up to a redshift ~1.6. We use deep far-infrared PACS data at 100 and 160 um to accurately estimate the total star formation rate of the Luminous Infrared Galaxy population of 9 clusters with mass ~10^{15} M_{\odot}, and 9 groups/poor clusters with mass ~ 5 x 10^{13} M_{\odot}. Estimates of the field \Sigma(SFR/M) are derived from the literature, by dividing the star formation rate density by the mean comoving matter density of the universe. The field \Sigma(SFR/M) increases with redshift up to z~1 and it is constant thereafter. The evolution of the \Sigma(SFR/M)-z relation in galaxy systems is much faster than in the field. Up to redshift z~0.2, the field has a higher \Sigma(SFR/M) than galaxy groups and galaxy clusters. At higher redshifts, galaxy groups and the field have similar \Sigma(SFR/M), while massive clusters have significantly lower \Sigma(SFR/M) than both groups and the field. There is a hint of a reversal of the SFR activity vs. environment at z~1.6, where the group \Sigma(SFR/M) lies above the field \Sigma(SFR/M)-z relation. We discuss possible interpretations of our results in terms of the processes of downsizing, and star-formation quenching. }, added-at = {2011-10-14T17:56:51.000+0200}, author = {Popesso, P. and Biviano, A. and Rodighiero, G. and Baronchelli, I. and Salvato, M. and Saintonge, A. and Finoguenov, A. and Magnelli, B. and Gruppioni, C. and Pozzi, F. and Lutz, D. and Elbaz, D. and Altieri, B. and Andreani, P. and Aussel, H. and Berta, S. and Capak, P. and Cava, A. and Cimatti, A. and Coia, D. and Daddi, E. and Dannerbauer, H. and Dickinson, M. and Dasyra, K. and Fadda, D. and Schreiber, N. Förster and Genzel, R. and Hwang, H. S. and Kartaltepe, J. and Ilbert, O. and Floch, E. Le and Leiton, R. and Magdis, G. and Nordon, R. and Patel, S. and Poglitsch, A. and Riguccini, L. and Portal, M. Sanchez and Shao, L. and Tacconi, L. and Tomczak, A. and Tran, K. and Valtchanov, I.}, biburl = {https://www.bibsonomy.org/bibtex/26ad920e475b5741dbc6519e6b0c12b8b/miki}, description = {[1110.2946] The evolution of the star formation activity per halo mass up to redshift ~ 1.6 as seen by Herschel}, interhash = {2e493567e78401867f5836d76bf26b61}, intrahash = {6ad920e475b5741dbc6519e6b0c12b8b}, keywords = {evolution sfr specific}, note = {cite arxiv:1110.2946 Comment: 8 pages, 3 figures, accepted for publication on A&A}, timestamp = {2011-10-14T17:56:51.000+0200}, title = {The evolution of the star formation activity per halo mass up to redshift ~ 1.6 as seen by Herschel}, url = {http://arxiv.org/abs/1110.2946}, year = 2011 }