Journal article

Cluster mass calibration at high redshift: HST weak lensing analysis of 13 distant galaxy clusters from the South Pole Telescope Sunyaev-Zel'dovich Survey

T Schrabback, D Applegate, JP Dietrich, H Hoekstra, S Bocquet, AH Gonzalez, A von der Linden, M McDonald, CB Morrison, SF Raihan, SW Allen, M Bayliss, BA Benson, LE Bleem, I Chiu, S Desai, RJ Foley, T de Haan, FW High, S Hilbert Show all



We present an HST/Advanced Camera for Surveys (ACS) weak gravitational lensing analysis of 13 massive high-redshift (zmedian = 0.88) galaxy clusters discovered in the South Pole Telescope (SPT) Sunyaev-Zel'dovich Survey. This study is part of a larger campaign that aims to robustly calibrate mass-observable scaling relations over a wide range in redshift to enable improved cosmological constraints from the SPT cluster sample. We introduce new strategies to ensure that systematics in the lensing analysis do not degrade constraints on cluster scaling relations significantly. First, we efficiently remove cluster members from the source sample by selecting very blue galaxies in V - I colour. Our..

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University of Melbourne Researchers


Awarded by German Federal Ministry of Economics and Technology (BMWi) through DLR

Awarded by NSF

Awarded by SAO

Awarded by Kavli Institute for Cosmological Physics at the University of Chicago

Awarded by NWO VIDI

Awarded by ERC

Awarded by U.S. Department of Energy

Awarded by Transregio program 'The Dark Universe'

Awarded by European DUEL Research-Training Network

Awarded by Deutsche Forschungsgemeinschaft

Awarded by DFG

Awarded by Fermi Research Alliance, LLC

Awarded by Australian Research Council's Discovery Projects scheme

Awarded by SPT follow-up GO programmes

Awarded by GO programmes

Awarded by 3D-HST Treasury Program

Awarded by UVUDF Project

Awarded by NASA

Awarded by La Silla Paranal Observatory

Awarded by Science and Technology Facilities Council

Awarded by Office of Polar Programs (OPP)

Funding Acknowledgements

This work is based on observations made with the NASA/ESA HST, using imaging data from the SPT follow-up GO programmes 12246 (PI: C. Stubbs) and 12477 (PI: F. W. High), as well as archival data from GO programmes 9425, 9500, 9583, 10134, 12064, 12440 and 12757, obtained via the data archive at the Space Telescope Science Institute, and catalogues based on observations taken by the 3D-HST Treasury Program (GO 12177 and 12328) and the UVUDF Project (GO 12534, also based on data from GO programmes 9978, 10086, 11563, 12498). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. It is also based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programmes 086.A-0741, 088.A-0796, 088.A-0889, 089.A-0824. The scientific results reported in this article are based in part on observations made by the Chandra X-ray Observatory (ObsIDs 9332, 9333, 9334, 9335, 9336, 9345, 10851, 10864, 11738, 11739, 11741, 11742, 11748, 11799, 11859, 11864, 11870, 11997, 12001, 12002, 12014, 12091, 12180, 12189, 12258, 12264, 13116, 13117, 14017, 14018, 14022, 14023, 14349, 14350, 14351, 14437, 15572, 15574, 15579, 15582, 15588, 15589, 18241).r TS, DA and SFR acknowledge support from the German Federal Ministry of Economics and Technology (BMWi) provided through DLR under projects 50 OR 1210, 50 OR 1308, 50 OR 1407 and 50 OR 1610. TS also acknowledges support from NSF through grant AST-0444059-001 and SAO through grant GO0-11147A. This work was supported in part by the Kavli Institute for Cosmological Physics at the University of Chicago through grant NSF PHY-1125897 and an endowment from the Kavli Foundation and its founder Fred Kavli. HH acknowledges support from NWO VIDI grant number 639.042.814 and ERC FP7 grant 279396. Work at Argonne National Laboratorywas supported under U.S. Department of Energy contract DE-AC02-06CH11357. The Munich group acknowledges the support by the DFG Cluster of Excellence 'Origin and Structure of the Universe' and the Transregio program TR33 'The Dark Universe'. RJF is supported in part by fellowships from the Alfred P. Sloan Foundation and the David and Lucile Packard Foundation. TdH is supported by a Miller Research Fellowship. PS acknowledges support by the European DUEL Research-Training Network (MRTN-CT-2006-036133) and by the Deutsche Forschungsgemeinschaft under the project SCHN 342/7-1. CBM acknowledges the support of the DFG under Emmy Noether grant Hi 1495/2-1. BAB is supported by the Fermi Research Alliance, LLC under Contract No. De-AC02-07CH11359 with the United States Department of Energy. CLR acknowledges support from the Australian Research Council's Discovery Projects scheme (DP150103208). The Dark Cosmology Centre is funded by the Danish National Research Foundation.