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The evolution of galaxy star formation activity in massive haloes

Popesso, P. and Biviano, A. and Finoguenov, A. and Wilman, D. and Salvato, M. and Magnelli, B. and Gruppioni, C. and Pozzi, F. and Rodighiero, G. and Ziparo, F. and Berta, S. and Elbaz, D. and Dickinson, M. and Lutz, D. and Altieri, B. and Aussel, H. and Cimatti, A. and Fadda, D. and Ilbert, O. and Le Floc'h, E. and Nordon, R. and Poglitsch, A. and Xu, C. K. (2015) The evolution of galaxy star formation activity in massive haloes. Astronomy and Astrophysics, 574 . Art. No. A105. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20150326-143759028

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Abstract

Context. There is now a large consensus that the current epoch of the cosmic star formation history (CSFH) is dominated by low mass galaxies while the most active phase, between redshifts 1 and 2, is dominated by more massive galaxies, which evolve more quickly. Aims. Massive galaxies tend to inhabit very massive haloes, such as galaxy groups and clusters. We aim to understand whether the observed “galaxy downsizing” could be interpreted as a “halo downsizing”, whereas the most massive haloes, and their galaxy populations, evolve more rapidly than the haloes with lower mass. Methods. We studied the contribution to the CSFH of galaxies inhabiting group-sized haloes. This is done through the study of the evolution of the infra-red (IR) luminosity function of group galaxies from redshift 0 to redshift ~1.6. We used a sample of 39 X-ray-selected groups in the Extended Chandra Deep Field South (ECDFS), the Chandra Deep Field North (CDFN), and the COSMOS field, where the deepest available mid- and far-IR surveys have been conducted with Spitzer MIPS and with the Photodetector Array Camera and Spectrometer (PACS) on board the Herschel satellite. Results. Groups at low redshift lack the brightest, rarest, and most star forming IR-emitting galaxies observed in the field. Their IR-emitting galaxies contribute ≤10% of the comoving volume density of the whole IR galaxy population in the local Universe. At redshift ≳1, the most IR-luminous galaxies (LIRGs and ULIRGs) are mainly located in groups, and this is consistent with a reversal of the star formation rate (SFR) vs. density anti-correlation observed in the nearby Universe. At these redshifts, group galaxies contribute 60–80% of the CSFH, i.e. much more than at lower redshifts. Below z ~ 1, the comoving number and SFR densities of IR-emitting galaxies in groups decline significantly faster than those of all IR-emitting galaxies. Conclusions. Our results are consistent with a “halo downsizing” scenario and highlight the significant role of “environment” quenching in shaping the CSFH.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201424711DOIArticle
http://www.aanda.org/articles/aa/abs/2015/02/aa24711-14/aa24711-14.htmlPublisherArticle
http://arxiv.org/abs/1407.8214arXivDiscussion Paper
ORCID:
AuthorORCID
Salvato, M.0000-0001-7116-9303
Gruppioni, C.0000-0002-5836-4056
Berta, S.0000-0002-0320-1532
Elbaz, D.0000-0002-7631-647X
Dickinson, M.0000-0001-5414-5131
Lutz, D.0000-0003-0291-9582
Aussel, H.0000-0002-1371-5705
Fadda, D.0000-0002-3698-7076
Ilbert, O.0000-0002-7303-4397
Xu, C. K.0000-0002-1588-6700
Additional Information:© 2015 ESO. Article published by EDP Sciences. Received 30 July 2014. Accepted 13 October 2014. Published online 03 February 2015. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The authors aknowledge G. Zamorani for the very useful comments on the early draft. 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 http://www.astro.caltech.edu/~cosmos. This research 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 (http://www.sdss.org/collaboration/credits.html).
Funders:
Funding AgencyGrant Number
Bundesministerium für Verkehr, Innovation und Technologie (BMVIT) UNSPECIFIED
ESA-PRODEX (Belgium)UNSPECIFIED
Commissariat à l’Energie Atomique (CEA)UNSPECIFIED
Deutsches Zentrum für Luft- und Raumfahrt (DLR)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)UNSPECIFIED
Comisión Interministerial de Ciencia y Tecnología (CICYT)UNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
NSFUNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
NASAUNSPECIFIED
Japanese MonbukagakushoUNSPECIFIED
Max Planck SocietyUNSPECIFIED
Higher Education Funding Council of EnglandUNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Ministerio de Ciencia Y Tecnologia (MCYT)UNSPECIFIED
Subject Keywords:galaxies: evolution, galaxies: clusters: general, galaxies: luminosity function, mass function, galaxies: groups: general
Record Number:CaltechAUTHORS:20150326-143759028
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20150326-143759028
Official Citation:The evolution of galaxy star formation activity in massive haloes P. Popesso, A. Biviano, A. Finoguenov, D. Wilman, M. Salvato, B. Magnelli, C. Gruppioni, F. Pozzi, G. Rodighiero, F. Ziparo, S. Berta, D. Elbaz, M. Dickinson, D. Lutz, B. Altieri, H. Aussel, A. Cimatti, D. Fadda, O. Ilbert, E. Le Floch, R. Nordon, A. Poglitsch and C. K. Xu A&A 574 A105 (2015) DOI: http://dx.doi.org/10.1051/0004-6361/201424711
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:56148
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:26 Mar 2015 23:09
Last Modified:03 Oct 2019 08:11

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