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The luminosity function of the NoSOCS galaxy cluster sample

De Filippis, E. and Paolillo, M. and Longo, G. and La Barbera, F. and de Carvalho, R. R. and Gal, R. (2011) The luminosity function of the NoSOCS galaxy cluster sample. Monthly Notices of the Royal Astronomical Society, 414 (3). pp. 2771-2784. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20110812-140026356

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Abstract

We present the analysis of the luminosity function of a large sample of galaxy clusters from the Northern Sky Optical Cluster Survey, using latest data from the Sloan Digital Sky Survey. Our global luminosity function (down to M_r ≾ -16) does not show the presence of an 'upturn' at faint magnitudes, while we do observe a strong dependence of its shape on both the richness and the clustercentric radius, with a brightening of M^* and an increase in the dwarf-to-giant galaxy ratio with the richness, indicating that more massive systems are more efficient in creating/retaining a population of dwarf satellites. This is observed within both physical (0.5R_(200)) and fixed (0.5 Mpc) apertures, suggesting that the trend is either due to a global effect, operating at all scales, or due to a local one but operating on even smaller scales. We further observe a decrease in the relative number of dwarf galaxies towards the cluster centre; this is most probably due to tidal collisions or the collisional disruption of the dwarfs since merging processes are inhibited by the high velocity dispersions in cluster cores and, furthermore, we do not observe a strong dependence of the bright end on the environment. We find an indication that the dwarf-to-giant ratio decreases with increasing redshift, within 0.07 ≤z < 0.2. We also measure a trend for the stronger suppression of faint galaxies (below M^*+ 2) with increasing redshift in poor systems, with respect to more massive ones, indicating that the evolutionary stage of less-massive galaxies depends more critically on the environment. Finally, we point out that the luminosity function is far from universal; hence, the uncertainties introduced by the different methods used to build a composite function may partially explain the variety of faint-end slopes reported in the literature, as well as, in some cases, the presence of a faint-end upturn.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1111/j.1365-2966.2011.18596.xDOIArticle
http://onlinelibrary.wiley.com/doi/10.1111/j.1365-2966.2011.18596.x/abstractPublisherArticle
ORCID:
AuthorORCID
de Carvalho, R. R.0000-0002-1283-3363
Additional Information:© 2011 The Authors. Monthly Notices of the Royal Astronomical Society © 2011 RAS. Accepted 2011 February 23. Received 2011 February 3; in original form 2010 September 14. Article first published online: 15 Apr 2011. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/. The authors thank Eric Feigelson and Yogesh Babu for their useful suggestions about the statistical treatment of the data.
Funders:
Funding AgencyGrant Number
Alfred P. Sloan FoundationUNSPECIFIED
NSFUNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
NASAUNSPECIFIED
Japanese MonbukagakushoUNSPECIFIED
Max Planck SocietyUNSPECIFIED
Higher Education Funding Council for EnglandUNSPECIFIED
Subject Keywords:galaxies: clusters: general; galaxies: evolution; galaxies: luminosity function, mass function; galaxies: statistics; large-scale structure of Universe
Issue or Number:3
Record Number:CaltechAUTHORS:20110812-140026356
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20110812-140026356
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:24835
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:12 Aug 2011 21:48
Last Modified:03 Oct 2019 03:00

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