The dynamical state of galaxy groups and their luminosity content

Authors

  • Héctor J. Martínez,

    Corresponding author
    1. Instituto de Astronomía Teórica y Experimental, IATE, CONICET, Laprida 854, X5000BGR Córdoba, Argentina
    2. Observatorio Astronómico, Universidad Nacional de Córdoba, Laprida 854, X5000BGR Córdoba, Argentina
      E-mail: julian@oac.uncor.edu
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  • Ariel Zandivarez

    1. Instituto de Astronomía Teórica y Experimental, IATE, CONICET, Laprida 854, X5000BGR Córdoba, Argentina
    2. Observatorio Astronómico, Universidad Nacional de Córdoba, Laprida 854, X5000BGR Córdoba, Argentina
    3. Instituto de Astronomía, Geofísica e Ciencias Atmosfericas, IAG, USP, Rua do Matão 1226, 05508-090 São Paulo, Brazil
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E-mail: julian@oac.uncor.edu

ABSTRACT

We analyse the dependence of the luminosity function (LF) of galaxies in groups on group dynamical state. We use the Gaussianity of the velocity distribution of galaxy members as a measurement of the dynamical equilibrium of groups identified in the Sloan Digital Sky Survey Data Release 7 by Zandivarez & Martínez. We apply the Anderson–Darling goodness-of-fit test to distinguish between groups according to whether they have Gaussian or non-Gaussian velocity distributions, i.e. whether they are relaxed or not. For these two subsamples, we compute the 0.1r-band LF as a function of group virial mass and group total luminosity. For massive groups, inline image, we find statistically significant differences between the LF of the two subsamples: the LFs of groups that have Gaussian velocity distributions have a brighter characteristic absolute magnitude (∼0.3 mag) and a steeper faint-end slope (∼0.25). We detect a similar effect when comparing the LF of bright [inline image] Gaussian and non-Gaussian groups. Our results indicate that, for massive/luminous groups, the dynamical state of the system is directly related to the luminosity of its galaxy members.

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