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Issue A&A
Volume 445, Number 1, January I 2006
Page(s) 51 - 58
Section Cosmology (including clusters of galaxies)
DOI http://dx.doi.org/10.1051/0004-6361:20053277



A&A 445, 51-58 (2006)
DOI: 10.1051/0004-6361:20053277

The faint-end of the galaxy luminosity function in groups

R. E. González1, M. Lares2, D. G. Lambas2 and C. Valotto2

1  Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile
    e-mail: regonzar@astro.puc.cl
2  Grupo de Investigaciones en Astronomía Teórica y Experimental (IATE), Observatorio Astronómico de Córdoba, UNC, and Consejo Nacional de Investigaciones Científicas y Tecnológicas. (CONICET), Argentina

(Received 20 April 2005 / Accepted 8 September 2005)

Abstract
We compute the galaxy luminosity function in spectroscopically selected nearby groups and clusters. Our sample comprises 728 systems extracted from the third release of the Sloan Digital Sky Survey in the redshift range 0.03 < z < 0.06 with virial mass range $10^{11}~M_\odot < M_{\rm vir} < 2\times 10^{14}~M_\odot$. To compute the galaxy luminosity function, we apply a statistical background subtraction method following usually adopted techniques. In the r band, the composite galaxy luminosity function shows a slope $\alpha=-1.3$ in the bright-end, and an upturn of the slope in the faint-end, $M_r\ga -18+5\log~(h)$, to slopes $-1.9<\alpha<-1.6$. We find that this feature is present also in the i,g and z bands, and for all explored group subsamples, irrespective of the group mass, number of members, integrated color or the presence of a hot intra-cluster gas associated to X-ray emission.


Key words: methods: statistical -- galaxies: clusters: general -- galaxies: luminosity function, mass function

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© ESO 2005


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