Journal article

Galaxy populations in the 26 most massive galaxy clusters in the South Pole Telescope SPT-SZ survey

A Zenteno, JJ Mohr, S Desai, B Stalder, A Saro, JP Dietrich, M Bayliss, S Bocquet, I Chiu, AH Gonzalez, C Gangkofner, N Gupta, J Hlavacek-Larrondo, M McDonald, C Reichardt, A Rest



We present a study of the optical properties of the 26 most massive galaxy clusters within the South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) 2500 deg2 survey spanning the redshift range 0.10 < z<1.13. We measure the radial profiles, the luminosity functions (LFs), and the halo occupation numbers (HONs) using optical data of typical depthm m* + 2. The stacked radial profiles are consistent with a Navarro-Frenk-White profile of concentration 2.84+0.40-0.37 for the red sequence (RS) and 2.36+0.38-0.35 for the total population. Stacking the data in multiple redshift bins shows slight redshift evolution in the concentration when both the total population is used, and when only RS galaxies are ..

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University of Melbourne Researchers


Awarded by Transregio Program 'The Dark Universe'

Awarded by National Science Foundation

Awarded by NSF Physics Frontier Center

Awarded by Gordon and Betty Moore Foundation

Awarded by Australian Research Council

Awarded by Directorate For Geosciences

Funding Acknowledgements

We acknowledge the support by the DFG Cluster of Excellence 'Origin and Structure of the Universe', the Transregio Program TR33 'The Dark Universe' and the Ludwig-Maximilians-Universitat. The data processing has been carried out on the computing facilities of the Computational Center for Particle and Astrophysics (C2PAP), located at the Leibniz Supercomputer Center (LRZ). The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. CR acknowledges support from the Australian Research Council's Discovery Projects scheme (DP150103208). This paper includes data gathered with the Blanco 4-m telescope, located at the Cerro Tololo Inter-American Observatory in Chile, which is part of the US National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), under contract with the National Science Foundation. Other data come from the European Southern Observatory telescopes on La Silla and Paranal. We are very grateful for the efforts of the CTIO, La Silla, and Paranal support staff without whom this paper would not be possible.