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The relation between star formation, morphology, and local density in high-redshift clusters and groups

Poggianti, Bianca M. and Desai, Vandana and Finn, Rose and Bamford, Steven and De Lucia, Gabriella and Varela, Jesus and Aragón-Salamanca, Alfonso and Halliday, Claire and Noll, Stefan and Saglia, Roberto and Zaritsky, Dennis and Best, Philip and Clowe, Douglas and Milvang-Jensen, Bo and Jablonka, Pascale and Pelló, Roser and Rudnick, Gregory and Simard, Luc and von der Linden, Anja and White, Simon (2008) The relation between star formation, morphology, and local density in high-redshift clusters and groups. Astrophysical Journal, 684 (2). pp. 888-904. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20090526-140442640

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Abstract

We investigate how the [O II] properties and the morphologies of galaxies in clusters and groups at z = 0.4–0.8 depend on projected local galaxy density, and compare with the field at similar redshifts and clusters at low z. In both nearby and distant clusters, higher density regions contain proportionally fewer star-forming galaxies, and the average [O II] equivalent width of star-forming galaxies is independent of local density. However, in distant clusters the average current star formation rate (SFR) in star-forming galaxies seems to peak at densities ~15-40 galaxies Mpc^−2. At odds with low-z results, at high z the relation between star-forming fraction and local density varies from high- to low-mass clusters. Overall, our results suggest that at high z the current star formation (SF) activity in star-forming galaxies does not depend strongly on global or local environment, though the possible SFR peak seems at odds with this conclusion. We find that the cluster SFR normalized by cluster mass anticorrelates with mass and correlates with the star-forming fraction. These trends can be understood given (1) that the average star-forming galaxy forms about 1⊙M yr^−1 (uncorrected for dust) in all clusters; (2) that the total number of galaxies scales with cluster mass; and (3) the dependence of star-forming fraction on cluster mass. We present the morphology-density (MD) relation for our z = 0.4 − 0.8 clusters, and uncover that the decline of the spiral fraction with density is entirely driven by galaxies of type Sc or later. For galaxies of a given Hubble type, we see no evidence that SF properties depend on local environment. In contrast with recent findings at low z, in our distant clusters the SF-density relation and the MD relation are equivalent, suggesting that neither of the two is more fundamental than the other.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/589936DOIArticle
http://www.iop.org/EJ/abstract/0004-637X/684/2/888/PublisherArticle
ORCID:
AuthorORCID
Poggianti, Bianca M.0000-0001-8751-8360
Desai, Vandana0000-0002-1340-0543
Zaritsky, Dennis0000-0002-5177-727X
Rudnick, Gregory0000-0001-5851-1856
Additional Information:© 2008 The American Astronomical Society. Received 2008 March 20; accepted 2008 May 7. We would like to thank the referee, Arjen van der Wel, for the constructive and careful report that helped us improving the paper. B. M. P. thanks the Alexander von Humboldt Foundation and the Max Planck Instituut fur Extraterrestrische Physik in Garching for a very pleasant and productive stay during which the work presented in this paper was carried out. The Dark Cosmology Centre is funded by the Danish National Research Foundation. B. M. P. acknowledges financial support from the FIRB scheme of the Italian Ministry of Education, University and Research (RBAU018Y7E) and from the INAFY National Institute for Astrophysics through its PRIN-INAF2006 scheme. Facilities: VLT(FORS2), HST(ACS). Based on observations collected at the European Sputhern Observatory, Chile, as part of large program 166.A-0162 (the ESO Distant Cluster Survey) and with the NASA/ESA Hubble Space Telescope with proposal 9476. Print publication: Issue 2 (2008 September 10).
Funders:
Funding AgencyGrant Number
Danish National Research FoundationUNSPECIFIED
Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)RBAU018Y7E
Istituto Nazionale di Astrofisica (INAF)PRIN-INAF2006
Subject Keywords:galaxies: clusters: general; galaxies: evolution; galaxies: stellar content
Issue or Number:2
Record Number:CaltechAUTHORS:20090526-140442640
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20090526-140442640
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:14303
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:27 May 2009 18:18
Last Modified:03 Oct 2019 00:48

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