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|Title:||The evolution of the cluster optical galaxy luminosity function between z = 0.4 and 0.9 in the DAFT/FADA survey||Authors:||Martinet, Nicolas
Ulmer, Melville P.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||575||First Page:||A116||Abstract:||Context. There is some disagreement about the abundance of faint galaxies in high-redshift clusters, with contradictory results in the literature arising from studies of the optical galaxy luminosity function (GLF) for small cluster samples. <BR /> Aims: We compute GLFs for one of the largest medium-to-high-redshift (0.4 ≤ z < 0.9) cluster samples to date in order to probe the abundance of faint galaxies in clusters. We also study how the GLF depends on cluster redshift, mass, and substructure and compare the GLFs of clusters with those of the field. We separately investigate the GLFs of blue and red-sequence (RS) galaxies to understand the evolution of different cluster populations. <BR /> Methods: We calculated the GLFs for 31 clusters taken from the DAFT/FADA survey in the B,V,R, and I rest-frame bands. We used photometric redshifts computed from BVRIZJ images to constrain galaxy cluster membership. We carried out a detailed estimate of the completeness of our data. We distinguished the red-sequence and blue galaxies using a V - I versus I colour-magnitude diagram. We studied the evolution of these two populations with redshift. We fitted Schechter functions to our stacked GLFs to determine average cluster characteristics. <BR /> Results: We find that the shapes of our GLFs are similar for the B,V,R, and I bands with a drop at the red GLF faint ends that is more pronounced at high redshift: α<SUB>red</SUB> ~ -0.5 at 0.40 ≤ z < 0.65 and α<SUB>red</SUB> > 0.1 at 0.65 ≤ z < 0.90. The blue GLFs have a steeper faint end (α<SUB>blue</SUB> ~ -1.6) than the red GLFs, which appears to be independent of redshift. For the full cluster sample, blue and red GLFs meet at M<SUB>V</SUB> = -20, M<SUB>R</SUB> = -20.5, and M<SUB>I</SUB> = -20.3. A study of how galaxy types evolve with redshift shows that late-type galaxies appear to become early types between z ~ 0.9 and today. Finally, the faint ends of the red GLFs of more massive clusters appear to be richer than less massive clusters, which is more typical of the lower redshift behaviour. <BR /> Conclusions: Our results indicate that these clusters form at redshifts higher than z = 0.9 from galaxy structures that already have an established red sequence. Late-type galaxies then appear to evolve into early types, enriching the red sequence between this redshift and today. This effect is consistent with the evolution of the faint-end slope of the red sequence and the galaxy type evolution that we find. Finally, faint galaxies accreted from the field environment at all redshifts might have replaced the blue late-type galaxies that converted into early types, explaining the lack of evolution in the faint-end slopes of the blue GLFs. Appendix is available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201423796/olm">http://www.aanda.org||Acknowledgments:||We thank Greg Rudnick for useful discussions. We also thank Eric Jullo, Marceau Limousin, Dennis Zaritsky for comments on earlier versions of this paper. We are grateful to the referee for interesting comments. F.D. acknowledges long-term financial support from CNES. I.M. acknowledges financial support from the Spanish grant AYA2010-15169 and from the Junta de Andalucia through TIC-114 and the Excellence Project P08-TIC-03531. Based on observations made with the FORS2 multi-object spectrograph mounted on the Antu VLT telescope at ESO-Paranal Observatory (programme 085.A-0016, 089A-0666, 191.A-0268; PI: C. Adami). Also based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Also based on observations obtained at the WIYN telescope (KNPO). The WIYN Observatory is a joint facility of the University of Wisconsin-Madison, Indiana University, Yale University, and the National Optical Astronomy Observatory. Kitt Peak National Observatory, National Optical Astronomy Observatory. It is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. Also based on observations obtained at the MDM observatory (2.4 m telescope). MDM consortium partners are Columbia University Department of Astronomy and Astrophysics, Dartmouth College Department of Physics and Astronomy, University of Michigan Astronomy Department, The Ohio State University Astronomy Department, and the Ohio University Dept. of Physics and Astronomy. Also based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia, e Inovação (MCTI) da República Federativa do Brasil, the US National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). Also based on observations obtained at the Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, under contract with the National Science Foundation. Also based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma. Also based on archive data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. Finally, this research has made use of the VizieR catalogue access tool at the CDS, Strasbourg, France.||URI:||http://hdl.handle.net/20.500.12386/23619||URL:||https://www.aanda.org/articles/aa/abs/2015/03/aa23796-14/aa23796-14.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201423796||Bibcode ADS:||2015A&A...575A.116M||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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