SIMBAD references

Using deep VLT/ISAAC near-infrared imaging data, we derive the K_s-band luminosity function (LF) of the z=1.237 massive X-ray luminous cluster of galaxies RDCS J1252-2927{RDCS J1252.9-2927}. Photometric redshifts, derived from deep multi-wavelength BVRIzJK_s data, and calibrated using a large subset of galaxies with spectroscopic redshifts, are used to separate the cluster galaxy population from the foreground and background field galaxy population. This allows for a simultaneous determination of the characteristic magnitude K^*_s and faint end slope α of the LF without having to make an uncertain statistical background subtraction. The derived LF is well represented by the Schechter function with K_s^*=18.54^+0.45_–0.55 and α=-0.64^+0.27_–0.25. The shape of the bright end of the derived LF is similar to that measured at similar restframe wavelengths (in the z-band) in local clusters, but the characteristic magnitude is brighter by ΔM_z^*=-1.40^+0.49_–0.58mag. The derived α is similar to the value derived in the K_s-band in the z=1 cluster of galaxies MG2016+112 but is shallower (at the 2.2σ level) than the value measured at similar restframe wavelength (in the z-band) in clusters in the local universe. The brightening of the characteristic magnitude and lack of evolution in the shape of the bright end of the LF suggests that the massive cluster ellipticals that dominate the bright end of the LF were already in place at z=1.237, while the flattening of the faint end slope suggest that clusters at z∼1 contains relatively smaller fractions of low mass galaxies than clusters in the local universe. The results presented in this paper are a challenge for semi analytical hierarchical models of galaxy formation which predict the characteristic magnitude to grow fainter and the faint end slope to steepen with redshift as the massive galaxies break up into their progenitors. The observed evolution is consistent with a scenario in which clusters are composed of a population of massive galaxies which formed at high redshift (z≫1) and subsequently evolved passively, and a population of lower mass galaxies which are gradually accreted from the field, primarily at lower redshift (z<1).