The Rest-Frame Optical Luminosity Function of Cluster Galaxies at z<0.8 and the Assembly of the Cluster Red Sequence
Gregory Rudnick, Anja von der Linden, Roser Pello, Alfonso Aragon-Salamanca, Danilo Marchesini, Douglas Clowe, Gabriella De Lucia, Claire Halliday, Pascale Jabl… 展开作者
Gregory Rudnick, Anja von der Linden, Roser Pello, Alfonso Aragon-Salamanca, Danilo Marchesini, Douglas Clowe, Gabriella De Lucia, Claire Halliday, Pascale Jablonka, Bo Milvang-Jensen, Bianca Poggianti, Roberto Saglia, Luc Simard, Simon White, Dennis Zaritsky
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Accepted for publication in the Astrophysical Journal. 36 pages, 16 figures, 10 tables
We present the rest-frame optical luminosity function (LF) of red sequence galaxies in 16 clusters at 0.4<z<0.8 drawn from the ESO Distant Cluster Survey (EDisCS). We compare our clusters to an analogous sample from the Sloan Digital Sky Survey (SDSS) and match the EDisCS clusters to their most likely descendants. We measure all LFs down to M M* + (2.5 - 3.5). At z<0.8, the bright end of the LF is consistent with passive evolution but there is a significant build-up of the faint end of the red sequence towards lower redshift. There is a weak dependence of the LF on cluster velocity dispersion for EDisCS but no such dependence for the SDSS clusters. We find tentative evidence that red sequence galaxies brighter than a threshold magnitude are already in place, and that this threshold evolves to fainter magnitudes toward lower redshifts. We compare the EDisCS LFs with the LF of co-eval red sequence galaxies in the field and find that the bright end of the LFs agree. However, relative to the number of bright red galaxies, the field has more faint red galaxies than clusters at 0.6<z<0.8 but fewer at 0.4<z<0.6, implying differential evolution. We compare the total light in the EDisCS cluster red sequences to the total red sequence light in our SDSS cluster sample. Clusters at 0.4<z<0.8 must increase their luminosity on the red sequence (and therefore stellar mass in red galaxies) by a factor of 1-3 by z=0. The necessary processes that add mass to the red sequence in clusters predict local clusters that are over-luminous as compared to those observed in the SDSS. The predicted cluster luminosities can be reconciled with observed local cluster luminosities by combining multiple previously known effects.
Constraints on the assembly and dynamics of galaxies. II. Properties of kiloparsec-scale clumps in rest-frame optical emission of z ~ 2 star-forming galaxies
Halo assembly bias in the early Universe: a clustering probe of the origin of the Little Red Dots
Peking University（北京大学）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学科维理天文与天体物理研究所）；Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院科维理天体物理与空间研究）
