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The Atacama Cosmology Telescope: Detection of the pairwise kinematic Sunyaev-Zel’dovich effect with SDSS DR15 galaxies

Calafut, V. and Gallardo, P. A. and Vavagiakis, E. M. and Amodeo, S. and Aiola, S. and Austermann, J. E. and Battaglia, N. and Battistelli, E. S. and Beall, J. A. and Bean, R. and Bond, J. R. and Calabrese, E. and Choi, S. K. and Cothard, N. F. and Devlin, M. J. and Duell, C. J. and Duff, S. M. and Duivenvoorden, A. J. and Dunkley, J. and Dunner, R. and Ferraro, S. and Guan, Y. and Hill, J. C. and Hilton, G. C. and Hilton, M. and Hložek, R. and Huber, Z. B. and Hubmayr, J. and Huffenberger, K. M. and Hughes, J. P. and Koopman, B. J. and Kosowsky, A. and Li, Y. and Lokken, M. and Madhavacheril, M. and McMahon, J. and Moodley, K. and Naess, S. and Nati, F. and Newburgh, L. B. and Niemack, M. D. and Page, L. A. and Partridge, B. and Schaan, E. and Schillaci, A. and Sifón, C. and Spergel, D. N. and Staggs, S. T. and Ullom, J. N. and Vale, L. R. and Van Engelen, A. and Van Lanen, J. and Wollack, E. J. and Xu, Z. (2021) The Atacama Cosmology Telescope: Detection of the pairwise kinematic Sunyaev-Zel’dovich effect with SDSS DR15 galaxies. Physical Review D, 104 (4). Art. No. 043502. ISSN 2470-0010. doi:10.1103/PhysRevD.104.043502.

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We present a 5.4σ detection of the pairwise kinematic Sunyaev-Zeldovich (kSZ) effect using Atacama Cosmology Telescope (ACT) and Planck CMB observations in combination with Luminous Red Galaxy samples from the Sloan Digital Sky Survey (SDSS) DR15 catalog. Results are obtained using three ACT CMB maps: co-added 150 and 98 GHz maps, combining observations from 2008–2018 (ACT DR5), which overlap with SDSS DR15 over 3,700 sq. deg., and a component-separated map using night-time only observations from 2014–2015 (ACT DR4), overlapping with SDSS DR15 over 2,089 sq. deg. Comparisons of the results from these three maps provide consistency checks in relation to potential frequency-dependent foreground contamination. A total of 343,647 galaxies are used as tracers to identify and locate galaxy groups and clusters from which the kSZ signal is extracted using aperture photometry. We consider the impact of various aperture photometry assumptions and covariance estimation methods on the signal extraction. Theoretical predictions of the pairwise velocities are used to obtain best-fit, mass-averaged, optical depth estimates for each of five luminosity-selected tracer samples. A comparison of the kSZ-derived optical depth measurements obtained here to those derived from the thermal SZ effect for the same sample is presented in a companion paper.

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Schillaci, A.0000-0002-0512-1042
Additional Information:© 2021 American Physical Society. (Received 4 February 2021; accepted 27 May 2021; published 6 August 2021) V. C. and R. B. acknowledge support from DOE Grant No. DE-SC0011838, NASA ATP Grant No. 80NSSC18K0695, NASA ROSES Grant No. 12-EUCLID12-0004 and funding related to the Roman High Latitude Survey Science Investigation Team. E. M. V. acknowledges support from the NSF Graduate Research Fellowship Program under Grant No. DGE-1650441. N. B. acknowledges support from NSF Grant No. AST-1910021, NASA ATP Grant No. 80NSSC18K0695 and from the Research and Technology Development fund at the Jet Propulsion Laboratory through the project entitled “Mapping the Baryonic Majority.” E. C. acknowledges support from the STFC Ernest Rutherford Fellowship ST/M004856/2 and STFC Consolidated Grant ST/S00033X/1, and from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation program (Grant Agreement No. 849169). S. K. C. acknowledges support from NSF Grant AST-2001866. J. D. is supported through NSF Grant No. AST-1814971. R. D. thanks CONICYT for grant BASAL CATA AFB-170002. R. H. acknowledges funding from the CIFAR Azrieli Global Scholars program and the Alfred P. Sloan Foundation. J. P. H. acknowledges funding for SZ cluster studies from NSF Grant No. AST-1615657. K. M. acknowledges support from the National Research Foundation of South Africa. M. D. N. acknowledges support from NSF CAREER Grant 1454881. C. S. acknowledges support from the Agencia Nacional de Investigación y Desarrollo (ANID) through FONDECYT Iniciación Grant No. 11191125. Z. X. is supported by the Gordon and Betty Moore Foundation. This work was supported by the U.S. National Science Foundation through Grants No. AST-0408698, No. AST-0965625 and No. AST-1440226 for the ACT project, as well as Grants No. PHY-0355328, No. PHY-0855887 and No. PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astronómico Atacama in northern Chile under the auspices of the Comisión Nacional de Investigación Científica y Tecnológica de Chile (CONICYT). Canadian co-authors acknowledge support from the Natural Sciences and Engineering Research Council of Canada. The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High Performance Computing at the University of Utah. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, Center for Astrophysics—Harvard & Smithsonian, the Chilean Participation Group, the French Participation Group, Instituto de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, the Korean Participation Group, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatário Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.
Funding AgencyGrant Number
Department of EnergyDE-SC0011838
NSF Graduate Research FellowshipDGE-1650441
JPL Research and Technology Development FundUNSPECIFIED
Science and Technology Facilities Council (STFC)ST/M004856/2
Science and Technology Facilities Council (STFC)ST/S00033X/1
European Research Council (ERC)849169
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
National Research Foundation (South Africa)UNSPECIFIED
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)11191125
Gordon and Betty Moore FoundationUNSPECIFIED
Princeton UniversityUNSPECIFIED
University of PennsylvaniaUNSPECIFIED
Canada Foundation for InnovationUNSPECIFIED
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)UNSPECIFIED
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
David Dunlap FamilyUNSPECIFIED
University of TorontoUNSPECIFIED
Participating InstitutionsUNSPECIFIED
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ID Code:110618
Deposited By: George Porter
Deposited On:31 Aug 2021 14:24
Last Modified:31 Aug 2021 14:24

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