The evolution of the star formation activity per halo mass up to redshift ∼1.6 as seen by Herschel

P. Popesso, A. Biviano, G. Rodighiero, I. Baronchelli, M. Salvato, A. Saintonge, A. Finoguenov, B. Magnelli, C. Gruppioni, F. Pozzi, D. Lutz, D. Elbaz, B. Altieri, P. Andreani, H. Aussel, S. Berta, P. Capak, A. Cava, A. Cimatti, D. CoiaE. Daddi, H. Dannerbauer, M. Dickinson, K. Dasyra, D. Fadda, N. Förster Schreiber, R. Genzel, H. S. Hwang, J. Kartaltepe, O. Ilbert, E. Le Floch, R. Leiton, G. Magdis, R. Nordon, S. Patel, A. Poglitsch, L. Riguccini, M. Sanchez Portal, L. Shao, L. Tacconi, A. Tomczak, K. Tran, I. Valtchanov

Research output: Contribution to journalArticlepeer-review

60 Scopus citations


Aims. 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 (Σ(SFR)/M) in three different mass scales: low mass halos (field galaxies), groups, and clusters, up to a redshift z ≈ 1.6. Methods. We use deep far-infrared PACS data at 100 and 160 μm to accurately estimate the total star formation rate of the luminous infrared galaxy population of 9 clusters with mass ∼1015 M, and 9 groups/poor clusters with mass ∼5 × 1013 M. Estimates of the field Σ(SFR)/M are derived from the literature, by dividing the star formation rate density by the mean comoving matter density of the universe. Results. The field Σ(SFR)/M increases with redshift up to z ∼ 1 and it is constant thereafter. The evolution of the Σ(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 Σ(SFR)/M than galaxy groups and galaxy clusters. At higher redshifts, galaxy groups and the field have similar Σ(SFR)/M, while massive clusters have significantly lower Σ(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 Σ(SFR)/M lies above the field Σ(SFR)/M-z relation. We discuss possible interpretations of our results in terms of the processes of downsizing, and star-formation quenching.

Original languageEnglish (US)
Article numberA58
JournalAstronomy and Astrophysics
StatePublished - 2012

Bibliographical note

Funding Information:
PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, 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 (Italy), and CICYT/MCYT (Spain). We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information about the COSMOS survey is available at . This research has made use of NASA’s Astrophysics Data System, of NED, which is operated by JPL/Caltech, under contract with NASA, and of SDSS, which has been funded by the Sloan Foundation, NSF, the US Department of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council of England. The SDSS is managed by the participating institutions ( ).


  • galaxies: clusters: general
  • galaxies: evolution
  • galaxies: high-redshift


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