What is L*?: Anatomy of the Galaxy Luminosity Function

Details What is L*?: Anatomy of the Galaxy Luminosity Function What is L*?: Anatomy of the Galaxy Luminosity Function

2005-04-27

arxiv.org/abs/astro-ph/0504580v2

Astrophys.J. 627 (2005) L89-L92

Astronomy and Astrophysics

Astrophysics

4 pages, 5 figures, updated figure 2b and the related discussion to correct for difference in Hubble constant between data and

Scientific paper

10.1086/432259

Using the empirical relations between the central galaxy luminosity and the halo mass, and between the total galaxy luminosity in a halo and the halo mass, we construct the galaxy luminosity function (LF). To the luminosity of the central galaxy in a halo of a given mass we assign log-normal scatter with a mean calibrated against the observations. In halos where the total galaxy luminosity exceeds that of the central galaxy, satellite galaxies are distributed as a power-law in luminosity. Combined with the halo mass function, this description reproduces the observed characteristics of the galaxy LF, including a shape consistent with the Schechter function. When all galaxies are included, regardless of the environment or the Hubble type, the Schechter L* is the luminosity scale above which the central galaxy luminosity-halo mass relation flattens; L* corresponds to ~10^{13}Msun on the halo mass scale. In surveys where central galaxies in massive clusters are neglected, either by design or because of the cosmic variance, L* is simply the mean luminosity of central galaxies in halos at the upper end of the selected mass range. The smooth, exponential decay of the Schechter function toward high luminosities reflects the intrinsic scatter in the central galaxy luminosity-halo mass relation. In addition to the LF, the model successfully reproduces the observed dependence of galaxy clustering bias on luminosity.

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