Galaxy luminosity functions in WINGS clusters
Aims. Using V band photometry of the WINGS survey, we derive galaxy luminosity functions (LF) in nearby clusters. This sample is complete down to MV =−15.15, and it is homogeneous, thus allowing the study of an unbiased sample of clusters with different characteristics. Methods. We constructed the photometric LF for 72 out of the original 76 WINGS clusters, excluding only those without a velocity dispersion estimate. For each cluster we obtained the LF for galaxies in a region of radius=0.5× r200, and fitted them with single and double Schechter’s functions. We also derive the composite LF for the entire sample, and those pertaining to different morphological classes. Finally we derive the spectroscopic cumulative LF for 2009 galaxies that are cluster members. Results. The double Schechter fit parameters are neither correlated w ith the cluster velocity dispersion, nor with the X‐ray lumi nosity. Our median values of the Schechter’s fit slope are, on average , in agreement with measurements of nearby clusters, but are less steep that those derived from large surveys, such as the SDSS. Early‐type galaxies outnumber late‐types at all magnitudes, but both early and late types contribute equally to the faint end of the LF. F inally, the spectroscopic LF is in excellent agreement with the ones derived for A2199, A85 and Virgo, and with the photometric one at the bright magnitudes (where both are available). Conclusions. There is a large spread in the LF of different clusters. However, this spread is not caused by correl ation of the LF shape with cluster characteristics such as X‐ray luminosity or velocity dispersions. The faint end is flatter than what previo usly derived (α f =−1.7) at odds with what predicted from numerical simulations.