The SPTpol Extended Cluster Survey

Creators: Bleem, L. E.; Bocquet, S.; Stalder, B.; Gladders, M. D.; Ade, P. A. R.; Allen, S. W.; Anderson, A. J.; Annis, J.; Ashby, M. L. N.; Austermann, J. E.; Avila, S.; Avva, J. S.; Bayliss, M.; Beall, J. A.; Bechtol, K.; Bender, A. N.; Benson, B. A.; Bertin, E.; Bianchini, F.; Blake, C.; Brodwin, M.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Carlstrom, J. E.; Rosell, A. Carnero; Carrasco Kind, M.; Carretero, J.; Chang, C. L.; Chiang, H. C.; Citron, R.; Moran, C. Corbett; Costanzi, M.; Crawford, T. M.; Crites, A. T.; da Costa, L. N.; de Haan, T.; De Vicente, J.; Desai, S.; Diehl, H. T.; Dietrich, J. P.; Dobbs, M. A.; Eifler, T. F.; Everett, W.; Flaugher, B.; Floyd, B.; Frieman, J.; Gallicchio, J.; García-Bellido, J.; George, E. M.; Gerdes, D. W.; Gilbert, A.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Gupta, N.; Gutierrez, G.; Halverson, N. W.; Harrington, N.; Henning, J. W.; Heymans, C.; Holder, G. P.; Hollowood, D. L.; Holzapfel, W. L.; Honscheid, K.; Hrubes, J. D.; Huang, N.; Hubmayr, J.; Irwin, K. D.; James, D. J.; Jeltema, T.; Joudaki, S.; Khullar, G.; Klein, M.; Knox, L.; Kuropatkin, N.; Lee, A. T.; Li, D.; Lidman, C.; Lowitz, A.; MacCrann, N.; Mahler, G.; Maia, M. A. G.; Marshall, J. L.; McDonald, M.; McMahon, J. J.; Melchior, P.; Menanteau, F.; Meyer, S. S.; Miquel, R.; Mocanu, L. M.; Mohr, J. J.; Montgomery, J.; Nadolski, A.; Natoli, T.; Nibarger, J. P.; Noble, G.; Novosad, V.; Padin, S.; Palmese, A.; Parkinson, D.; Patil, S.; Paz-Chinchón, F.; Plazas, A. A.; Pryke, C.; Ramachandra, N. S.; Reichardt, C. L.; Remolina González, J. D.; Romer, A. K.; Roodman, A.; Ruhl, J. E.; Rykoff, E. S.; Saliwanchik, B. R.; Sanchez, E.; Saro, A.; Sayre, J. T.; Schaffer, K. K.; Schrabback, T.; Serrano, S.; Sharon, K.; Sievers, C.; Smecher, G.; Smith, M.; Soares-Santos, M.; Stark, A. A.; Story, K. T.; Suchyta, E.; Tarle, G.; Tucker, C.; Vanderlinde, K.; Veach, T.; Vieira, J. D.; Wang, G.; Weller, J.; Whitehorn, N.; Wu, W. L. K.; Yefremenko, V.; Zhang, Y.

Abstract

We describe the observations and resultant galaxy cluster catalog from the 2770 deg² SPTpol Extended Cluster Survey (SPT-ECS). Clusters are identified via the Sunyaev–Zel'dovich (SZ) effect and confirmed with a combination of archival and targeted follow-up data, making particular use of data from the Dark Energy Survey (DES). With incomplete follow-up we have confirmed as clusters 244 of 266 candidates at a detection significance ξ ≥ 5 and an additional 204 systems at 4 < ξ < 5. The confirmed sample has a median mass of M_(500c) ∼ 4.4×10¹⁴ M⊙ h⁻¹₇₀ and a median redshift of z = 0.49, and we have identified 44 strong gravitational lenses in the sample thus far. Radio data are used to characterize contamination to the SZ signal; the median contamination for confirmed clusters is predicted to be ~1% of the SZ signal at the ξ > 4 threshold, and <4% of clusters have a predicted contamination >10% of their measured SZ flux. We associate SZ-selected clusters, from both SPT-ECS and the SPT-SZ survey, with clusters from the DES redMaPPer sample, and we find an offset distribution between the SZ center and central galaxy in general agreement with previous work, though with a larger fraction of clusters with significant offsets. Adopting a fixed Planck-like cosmology, we measure the optical richness–SZ mass (λ−M) relation and find it to be 28% shallower than that from a weak-lensing analysis of the DES data—a difference significant at the 4σ level—with the relations intersecting at λ = 60. The SPT-ECS cluster sample will be particularly useful for studying the evolution of massive clusters and, in combination with DES lensing observations and the SPT-SZ cluster sample, will be an important component of future cosmological analyses.

Additional Information

© 2020 The American Astronomical Society. Received 2019 October 14; revised 2019 December 3; accepted 2019 December 12; published 2020 March 5. This work was performed in the context of the South Pole Telescope scientific program. SPT is supported by the National Science Foundation through grant PLR-1248097. 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, 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. PISCO observations are supported by NSF AST-1814719. Work at Argonne National Lab is supported by UChicago Argonne LLC, operator of Argonne National Laboratory (Argonne). Argonne, a U.S. Department of Energy Office of Science Laboratory, is operated under contract No. DE-AC02-06CH11357. We also acknowledge support from the Argonne Center for Nanoscale Materials. M.G. and L.B. acknowledge partial support from HST-GO-15307.001. 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 No. DE-AC02-76SF00515. A.S. is supported by the ERC-StG "ClustersXCosmo" grant agreement 716762 and by the FARE-MIUR grant "ClustersXEuclid" R165SBKTMA. C.H. acknowledges support from the Max Planck Society and the Alexander von Humboldt Foundation, in the framework of the Max Planck-Humboldt Research Award endowed by the Federal Ministry of Education and Research, in addition to support from the European Research Council under grant No. 647112. S.J. acknowledges support from the Beecroft Trust and ERC 693024. T.S. acknowledges support from the German Federal Ministry of Economics and Technology (BMWi) provided through DLR under projects 50 OR 1610 and 50 OR 1803, as well as support from the Deutsche Forschungsgemeinschaft, DFG, under project SCHR 1400/3-1. The Melbourne authors acknowledge support from the Australian Research Council's Discovery Projects scheme (DP150103208). The 2dFLenS survey is based on data acquired through the Australian Astronomical Observatory, under program A/2014B/008. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at The Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l'Espai (IEEC/CSIC), the Institut de Física d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC, under contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a nonexclusive, paid-up, irrevocable, worldwide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. Facilities: Blanco (DECAM) - , Hubble Space Telescope (WFC3) - , Magellan:Baade (FourStar) - , Magellan:Clay (PISCO - , LDSS3C) - , NSF/US Department of Energy 10 m South Pole Telescope (SPTpol) - , Spitzer (IRAC) - , AAT(2dF+AAOmega). -

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