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Galaxy Clusters Selected via the Sunyaev–Zel'dovich Effect in the SPTpol 100-square-degree Survey

Huang, N. and Moran, C. Corbett and Crites, A. T. and Padin, S. (2020) Galaxy Clusters Selected via the Sunyaev–Zel'dovich Effect in the SPTpol 100-square-degree Survey. Astronomical Journal, 159 (3). Art. No. 110. ISSN 1538-3881. https://resolver.caltech.edu/CaltechAUTHORS:20200219-102007519

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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 galaxies only and are presented without redshifts. We find that 15 candidates (18% of the total sample) are at redshift z ≥ 1.0, with a maximum confirmed redshift of z_(max) = 1.38±0.10. We expect this catalog to contain every galaxy cluster with M_(500c) > 2.6×10¹⁴M⊙h⁻¹₇₀ and z > 0.25 in the survey area. The mass threshold is approximately constant above z = 0.25, and the complete catalog has a median mass of approximately M_(500c) > 2.7×10¹⁴M⊙h⁻¹₇₀. Compared to previous SPT works, the increased depth of the millimeter-wave data (11.2 and 6.5 μK-arcmin at 95 and 150 GHz, respectively) makes it possible to find more galaxy clusters at high redshift and lower mass.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-3881/ab6a96DOIArticle
https://arxiv.org/abs/1907.09621arXivDiscussion Paper
ORCID:
AuthorORCID
Moran, C. Corbett0000-0003-2088-7465
Additional Information:© 2020 The American Astronomical Society. Received 2019 July 23; revised 2020 January 7; accepted 2020 January 10; published 2020 February 17. 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 Québec 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-AC02-76SF00515, 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. Facilities: NSF/US Department of Energy 10 m South Pole Telescope (SPT):SPTpol - , Magellan:Clay (PISCO - , LDSS3) - , Spitzer (IRAC). -
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funders:
Funding AgencyGrant Number
NSFPLR-1248097
NSFPLR-1852617
NSFPHY-0114422
Kavli FoundationUNSPECIFIED
Gordon and Betty Moore FoundationGBMF 947
Department of Energy (DOE)DE-AC02-06CH11357
NSF Graduate Research FellowshipDGE-1752814
Department of Energy (DOE)DE-AC02-07CH11359
NSFAST-0956135
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Fonds de recherche du Québec - Nature et technologies (FRQNT)UNSPECIFIED
NSFAST-1716965
NSFCSSI-1835865
Department of Energy (DOE)DE-AC02-76SF00515
NASANNX15AE12G
European Research Council (ERC)71676
Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)R165SBKTMA
Australian Research CouncilDP150103208
NSFAST-1814719
Subject Keywords:Galaxy clusters; Observational cosmology; Large-scale structure of the universe
Issue or Number:3
Classification Code:Unified Astronomy Thesaurus concepts: Galaxy clusters (584); Observational cosmology (1146); Large-scale structure of the universe (902)
Record Number:CaltechAUTHORS:20200219-102007519
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200219-102007519
Official Citation:N. Huang et al 2020 AJ 159 110
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:101373
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:19 Feb 2020 18:40
Last Modified:06 Mar 2020 20:47

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