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We investigate the LF in the very relaxed cluster Abell 496. Our analysis isbased on deep images obtained at CFHT with MegaPrime/MegaCam in four bands(ugri) covering a 1x1 deg2 region, which is centered on the cluster Abell 496and extends to near its virial radius. The LFs are estimated by statisticallysubtracting a reference field taken as the mean of the 4 Deep fields of theCFHTLS survey. Background contamination is minimized by cutting out galaxiesredder than the observed Red Sequence in the g-i versus i colour-magnitudediagram. In Abell 496, the global LFs show a faint-end slope alpha=-1.55+/-0.06and vary little with observing band. Without colour cuts, the LFs are muchnoisier but not significantly steeper. The faint-end slopes show astatistically significant steepening from alpha=-1.4+/-0.1 in the centralregion (extending to half a virial radius) to -1.8+/-0.1 in the Southernenvelope of the cluster. Cosmic variance and uncertain star-galaxy separationare our main limiting factors in measuring the faint-end of the LFs. Thelarge-scale environment of Abell 496, probed with the fairly complete 6dFGScatalogue, shows a statistically significant 36 Mpc long filament at PA=137deg, but we do not find an enhanced LF along this axis. Our LFs do not displaythe large number of dwarf galaxies (alpha ~ -2) inferred by several authors,whose analyses may suffer from field contamination caused by inexistent orinadequate colour cuts. Alternatively, different clusters may have differentfaint-end slopes, but this is hard to reconcile with the wide range of slopesfound for given clusters and for wide sets of clusters.

The galaxy luminosity function of the Abell 496 cluster and its spatial variations