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

L. Salvati, A. Saro, S. Bocquet, M. Costanzi, B. Ansarinejad, B. A. Benson, L. E. Bleem, M. S. Calzadilla, J. E. Carlstrom, C. L. Chang, R. Chown, A. T. Crites, T. De Haan, M. A. Dobbs, W. B. Everett, B. Floyd, S. Grandis, E. M. George, N. W. Halverson, G. P. HolderW. L. Holzapfel, J. D. Hrubes, A. T. Lee, D. Luong-Van, M. McDonald, J. J. McMahon, S. S. Meyer, M. Millea, L. M. Mocanu, J. J. Mohr, T. Natoli, Y. Omori, S. Padin, C. Pryke, C. L. Reichardt, J. E. Ruhl, F. Ruppin, K. K. Schaffer, T. Schrabback, E. Shirokoff, Z. Staniszewski, A. A. Stark, J. D. Vieira, R. Williamson

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Abstract

We provide the first combined cosmological analysis of the 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 νΛ CDM scenario, focusing on the mass slope and mass bias of Planck scaling relations, we find αSZ=1.49-0.10+0.07 and 1-bSZ=0.69-0.14+0.07, respectively. The results for the mass slope show a ∼4 σ 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, ωm=0.37-0.06+0.02. 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 M 500. We estimate the ratio between the published Planck M SZ masses and our derived masses M 500, as a "measured mass bias,"1-bM. We analyze the mass, redshift, and detection noise dependence of 1-bM, 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.

Original languageEnglish (US)
Article number7ab4
JournalAstrophysical Journal
Volume934
Issue number2
DOIs
StatePublished - Aug 1 2022

Bibliographical note

Funding Information:
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. ; Taffoni et al. ); 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.

Funding Information:
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).

Funding Information:
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.

Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.

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