Journal article
Galaxy Clusters Selected via the Sunyaev-Zel'dovich Effect in the SPTpol 100-square-degree Survey
N Huang, LE Bleem, B Stalder, PAR Ade, SW Allen, AJ Anderson, JE Austermann, JS Avva, JA Beall, AN Bender, BA Benson, F Bianchini, S Bocquet, M Brodwin, JE Carlstrom, CL Chang, HC Chiang, R Citron, C Corbett Moran, TM Crawford Show all
The Astronomical Journal | American Astronomical Society | Published : 2020
Abstract
We present a catalog of galaxy cluster candidates detected in 100 square degrees surveyed with the SPTpol receiver on the South Pole Telescope. The catalog contains 89 candidates detected with a signal-to-noise ratio greater than 4.6. The candidates are selected using the Sunyaev–Zel'dovich effect at 95 and 150 GHz. Using both space- and ground-based optical and infrared telescopes, we have confirmed 81 candidates as galaxy clusters. We use these follow-up images and archival images to estimate photometric redshifts for 66 galaxy clusters and spectroscopic observations to obtain redshifts for 13 systems. An additional two galaxy clusters are confirmed using the overdensity of near-infrared g..
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Awarded by National Science Foundation
Awarded by NSF Physics Frontier Center
Awarded by Gordon and Betty Moore Foundation
Awarded by U.S. Department of Energy
Awarded by National Science Foundation Graduate Research Fellowship
Awarded by Argonne, a U.S. Department of Energy Office of Science Laboratory
Awarded by Fermi Research Alliance LLC
Awarded by NSF
Awarded by National Aeronautics and Space Administration (NASA)
Awarded by ERC-StG "ClustersXCosmo"
Awarded by FARE-MIUR grant "ClustersXEuclid"
Awarded by Australian Research Council
Funding Acknowledgements
This work was performed in the context of the South Pole Telescope scientific program. SPT is supported by the National Science Foundation through grants PLR-1248097 and 1852617. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, and the Kavli Foundation and the Gordon and Betty Moore Foundation grant GBMF 947 to the University of Chicago. This work is also supported by the U.S. Department of Energy. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE 1752814. Argonne National Laboratory's work was supported by the U.S. Department of Energy, Office of High Energy Physics. Argonne, a U.S. Department of Energy Office of Science Laboratory, is operated by UChicago Argonne LLC under contract no. DE-AC02-06CH11357. We also acknowledge support from the Argonne Center for Nanoscale Materials. B.B. is supported by the Fermi Research Alliance LLC under contract No. De-AC02-07CH11359 with the U.S. Department of Energy. The CU Boulder group acknowledges support from NSF AST-0956135. The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, and the Fonds de Recherche du Quebec Nature et Technologies. The UCLA authors acknowledge support from NSF AST-1716965 and CSSI-1835865. The Stanford/SLAC group acknowledges support from the U.S. Department of Energy under contract number DE-AC0276SF00515, and from the National Aeronautics and Space Administration (NASA) under grant No. NNX15AE12G, issued through the ROSES 2014 Astrophysics Data Analysis Program. A.S. is supported by the ERC-StG "ClustersXCosmo" grant agreement 71676, and by the FARE-MIUR grant "ClustersXEuclid" R165SBKTMA. The Melbourne group acknowledges support from the Australian Research Council's Discovery Projects scheme (DP150103208). PISCO observations are supported by NSF AST-1814719.