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Improving Cosmological Constraints from Galaxy Cluster Number Counts with CMB-cluster-lensing Data: Results from the SPT-SZ Survey and Forecasts for the Future

Chaubal, P. S. and Reichardt, C. L. and Gupta, N. and Ansarinejad, B. and Aylor, K. and Balkenhol, L. and Baxter, E. J. and Bianchini, F. and Benson, B. A. and Bleem, L. E. and Bocquet, S. and Carlstrom, J. E. and Chang, C. L. and Crawford, T. M. and Crites, A. T. and de Haan, T. and Dobbs, M. A. and Everett, W. B. and Floyd, B. and George, E. M. and Halverson, N. W. and Holzapfel, W. L. and Hrubes, J. D. and Knox, L. and Lee, A. T. and Luong-Van, D. and McMahon, J. J. and Meyer, S. S. and Mocanu, L. M. and Mohr, J. J. and Natoli, T. and Padin, S. and Pryke, C. and Ruhl, J. E. and Ruppin, F. and Salvati, L. and Saro, A. and Schaffer, K. K. and Shirokoff, E. and Staniszewski, Z.K. and Stark, A. A. and Vieira, J. D. and Williamson, R. (2022) Improving Cosmological Constraints from Galaxy Cluster Number Counts with CMB-cluster-lensing Data: Results from the SPT-SZ Survey and Forecasts for the Future. Astrophysical Journal, 931 (2). Art. No. 139. ISSN 0004-637X. doi:10.3847/1538-4357/ac6a55. https://resolver.caltech.edu/CaltechAUTHORS:20220606-736249000

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Abstract

We show the improvement to cosmological constraints from galaxy cluster surveys with the addition of cosmic microwave background (CMB)-cluster lensing data. We explore the cosmological implications of adding mass information from the 3.1σ detection of gravitational lensing of the CMB by galaxy clusters to the Sunyaev–Zel'dovich (SZ) selected galaxy cluster sample from the 2500 deg² SPT-SZ survey and targeted optical and X-ray follow-up data. In the ΛCDM model, the combination of the cluster sample with the Planck power spectrum measurements prefers σ₈(Ωₘ/0.3)^(0.5} = 0.831 ± 0.020. Adding the cluster data reduces the uncertainty on this quantity by a factor of 1.4, which is unchanged whether the 3.1σ CMB-cluster lensing measurement is included or not. We then forecast the impact of CMB-cluster lensing measurements with future cluster catalogs. Adding CMB-cluster lensing measurements to the SZ cluster catalog of the ongoing SPT-3G survey is expected to improve the expected constraint on the dark energy equation of state w by a factor of 1.3 to σ(w) = 0.19. We find the largest improvements from CMB-cluster lensing measurements to be for σ₈, where adding CMB-cluster lensing data to the cluster number counts reduces the expected uncertainty on σ₈ by respective factors of 2.4 and 3.6 for SPT-3G and CMB-S4.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/ac6a55DOIArticle
https://arxiv.org/abs/2111.07491arXivDiscussion Paper
ORCID:
AuthorORCID
Reichardt, C. L.0000-0003-2226-9169
Gupta, N.0000-0001-7652-9451
Balkenhol, L.0000-0001-6899-1873
Baxter, E. J.0000-0002-6836-3196
Bianchini, F.0000-0003-4847-3483
Benson, B. A.0000-0002-5108-6823
Bleem, L. E.0000-0001-7665-5079
Bocquet, S.0000-0002-4900-805X
Carlstrom, J. E.0000-0002-2044-7665
Chang, C. L.0000-0002-6311-0448
Crawford, T. M.0000-0001-9000-5013
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
Holzapfel, W. L.0000-0002-5744-6439
Lee, A. T.0000-0002-8428-8050
McMahon, J. J.0000-0002-7245-4541
Meyer, S. S.0000-0003-3315-4332
Mocanu, L. M.0000-0002-2416-2552
Mohr, J. J.0000-0002-6875-2087
Ruhl, J. E.0000-0001-5875-4751
Ruppin, F.0000-0002-0955-8954
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 November 14; revised 2022 April 20; accepted 2022 April 24; published 2022 June 3. The South Pole Telescope program is supported by the National Science Foundation (NSF) through award OPP-1852617. Argonne National Laboratory's work was supported by the U.S. Department of Energy, Office of High Energy Physics, under contract DE-AC02-06CH11357. We also acknowledge support from the Argonne Center for Nanoscale Materials. The Melbourne group acknowledges support from the Australian Research Council's Discovery Projects scheme (DP200101068). A.A.S. acknowledges support by U.S. National Science Foundation grant AST-1814719. A.S. is supported by the FARE-MIUR grant "ClustersXEuclid" R165SBKTMA, INFN InDark, and by the ERC-StG "ClustersXCosmo" grant agreement 716762. The data analysis pipeline also uses the scientific Python stack (Jones et al. 2001; Hunter 2007; van der Walt et al. 2011). We acknowledge the use of the Spartan, a high performance computing facility at the University of Melbourne (Lafayette et al. 2016).
Funders:
Funding AgencyGrant Number
NSFOPP-1852617
Department of Energy (DOE)DE-AC02- 06CH11357
Australian Research CouncilDP200101068
NSFAST-1814719
Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)R165SBKTMA
Istituto Nazionale di Fisica Nucleare (INFN)UNSPECIFIED
European Research Council (ERC)716762
Subject Keywords:Cosmology; Sigma8
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: Cosmology (343); Sigma8 (1455)
DOI:10.3847/1538-4357/ac6a55
Record Number:CaltechAUTHORS:20220606-736249000
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220606-736249000
Official Citation:P. S. Chaubal et al 2022 ApJ 931 139
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:115042
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:07 Jun 2022 14:40
Last Modified:07 Jun 2022 14:40

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