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Combining Planck and SPT Cluster Catalogs: Cosmological Analysis and Impact on the Planck Scaling Relation Calibration

Salvati, L. and Saro, A. and Bocquet, S. and Costanzi, M. and Ansarinejad, B and Benson, B. A. and Bleem, L. E. and Calzadilla, M. S. and Carlstrom, J. E. and Chang, C. L. and Chown, R. and Crites, A. T. and de Haan, T. and Dobbs, M. A. and Everett, W. B. and Floyd, B. and Grandis, S. and George, E. M. and Halverson, N. W. and Holder, G. P. and Holzapfel, W. L. and Hrubes, J. D. and Lee, A. T. and Luong-Van, D. and McDonald, M. and McMahon, J. J. and Meyer, S. S. and Millea, M. and Mocanu, L. M. and Mohr, J. J. and Natoli, T. and Omori, Y. and Padin, S. and Pryke, C. and Reichardt, C. L. and Ruhl, J. E. and Ruppin, F. and Schaffer, K. K. and Schrabback, T. and Shirokoff, E. and Staniszewski, Z. and Stark, A. A. and Vieira, J. D. and Williamson, R. (2022) Combining Planck and SPT Cluster Catalogs: Cosmological Analysis and Impact on the Planck Scaling Relation Calibration. Astrophysical Journal, 934 (2). Art. No. 129. ISSN 0004-637X. doi:10.3847/1538-4357/ac7ab4. https://resolver.caltech.edu/CaltechAUTHORS:20220802-730099000

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Abstract

We provide the first combined cosmological analysis of South Pole Telescope (SPT) and Planck cluster catalogs. The aim is to provide an independent calibration for Planck scaling relations, exploiting the cosmological constraining power of the SPT-SZ cluster catalog and its dedicated weak lensing (WL) and X-ray follow-up observations. We build a new version of the Planck cluster likelihood. In the νΛCDM scenario, focusing on the mass slope and mass bias of Planck scaling relations, we find α_(SZ) = 1.49^(+0.07)_(−0.10) and (1−b)_(SZ) = 0.69^(+0.07)_(−0.14) respectively. The results for the mass slope show a ∼4σ departure from the self-similar evolution, α_(SZ) ∼1.8. This shift is mainly driven by the matter density value preferred by SPT data, Ω_m = 0.30 ± 0.03, lower than the one obtained by Planck data alone, Ω_m = 0.37^(+0.02)_(−0.06). The mass bias constraints are consistent both with outcomes of hydrodynamical simulations and external WL calibrations, (1−b) ∼ 0.8, and with results required by the Planck cosmic microwave background cosmology, (1−b) ∼ 0.6. From this analysis, we obtain a new catalog of Planck cluster masses M₅₀₀. We estimate the relation between the published Planck derived M_(SZ) masses and our derived masses, as a "measured mass bias," (1-b)_M. We analyze the mass, redshift, and detection noise dependence of (1-b)_M, finding an increasing trend toward high redshift and low mass. These results mimic the effect of departure from self-similarity in cluster evolution, showing different dependencies for the low-mass, high-mass, low-z, and high-z regimes.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/ac7ab4DOIArticle
https://arxiv.org/abs/2112.03606arXivDiscussion Paper
http://pole.uchicago.edu/public/data/sptplanck_clusterRelated ItemCatalogs
ORCID:
AuthorORCID
Saro, A.0000-0002-9288-862X
Bocquet, S.0000-0002-4900-805X
Costanzi, M.0000-0001-8158-1449
Benson, B. A.0000-0002-5108-6823
Bleem, L. E.0000-0001-7665-5079
Calzadilla, M. S.0000-0002-2238-2105
Carlstrom, J. E.0000-0002-2044-7665
Chang, C. L.0000-0002-6311-0448
Chown, R.0000-0001-8241-7704
de Haan, T.0000-0001-5105-9473
Dobbs, M. A.0000-0001-7166-6422
Everett, W. B.0000-0002-5370-6651
Floyd, B.0000-0003-4175-571X
George, E. M.0000-0001-7874-0445
Halverson, N. W.0000-0003-2606-9340
Holder, G. P.0000-0002-0463-6394
Lee, A. T.0000-0003-3106-3218
McDonald, M.0000-0001-5226-8349
Meyer, S. S.0000-0003-3315-4332
Mocanu, L. M.0000-0002-2416-2552
Mohr, J. J.0000-0002-6875-2087
Reichardt, C. L.0000-0003-2226-9169
Ruppin, F.0000-0002-0955-8954
Schrabback, T.0000-0002-6987-7834
Shirokoff, E.0000-0002-2757-1423
Stark, A. A.0000-0002-2718-9996
Vieira, J. D.0000-0001-7192-3871
Williamson, R.0000-0002-6945-2975
Additional Information:© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 December 7; revised 2022 May 9; accepted 2022 June 14; published 2022 August 1. The authors thank the anonymous referee for the useful comments they provided to improve the presentation and discussion of the analysis. L.S. and M.C. are supported by ERC-StG "ClustersXCosmo" grant agreement 716762. A.S. is supported by the ERC-StG ClustersXCosmo' grant agreement 716762 and by the FARE-MIUR grant ClustersXEuclid' R165SBKTMA and INFN InDark Grant. T.S. acknowledges support from the German Federal Ministry for Economic Affairs und Energy (BMWi) provided through DLR under projects 50OR2002 and 50OR2106, as well as support provided by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under grant 415537506. The Melbourne group acknowledges support from the Australian Research Council's Discovery Projects scheme (DP200101068). This research made use of computation facilities of CINECA, within the projects INA17_C5B32, INA20_C6B51, INA21_C8B43, and at the Observatory of Trieste (Bertocco et al. 2020; Taffoni et al. 2020); observations obtained with Planck (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada; the SZ-Cluster Database (http://szcluster-db.ias.u-psud.fr) operated by the Integrated Data and Operation Centre (IDOC) at the Institut d'Astrophysique Spatiale (IAS) under contract with CNES and CNRS. The South Pole Telescope program is supported by the National Science Foundation (NSF) through grants PLR-1248097 and OPP-1852617. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation through grant GBMF #947 to the University of Chicago. Argonne National Laboratory's work was supported by the US Department of Energy, Office of Science, Office of High Energy Physics, under contract DE-AC02-06CH11357. Facilities: Magellan: Clay (Megacam), Hubble Space Telescope, Chandra, Gemini:South (GMOS), Magellan: Clay (PISCO).
Funders:
Funding AgencyGrant Number
European Research Council (ERC)716762
Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)R165SBKTMA
Istituto Nazionale di Fisica Nucleare (INFN)UNSPECIFIED
Bundesministerium für Wirtschaft und Technologie (BMWi)50OR2002
Bundesministerium für Wirtschaft und Technologie (BMWi)50OR2106
Deutsche Forschungsgemeinschaft (DFG)415537506
Australian Research CouncilDP200101068
ESA Member StatesUNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
NSFPLR-1248097
NSFOPP-1852617
NSFPHY-1125897
Kavli FoundationUNSPECIFIED
Gordon and Betty Moore FoundationGBMF947
Department of Energy (DOE)DE-AC02-06CH11357
Subject Keywords:Cosmology; Large-scale structure of the universe; Galaxy cluster counts
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: Cosmology (343); Large-scale structure of the universe (902); Galaxy cluster counts (583)
DOI:10.3847/1538-4357/ac7ab4
Record Number:CaltechAUTHORS:20220802-730099000
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220802-730099000
Official Citation:L. Salvati et al 2022 ApJ 934 129
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:116039
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:02 Aug 2022 16:45
Last Modified:02 Aug 2022 16:45

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