Palmese, A, Annis, J, Burgad, J, Farahi, A, Soares-Santos, M, Welch, B, Pereira, MDS, Lin, H, Bhargava, S, Hollowood, DL, Wilkinson, R, Giles, P, Jeltema, T, Romer, AK, Evrard, AE, Hilton, M, Cervantes, CV, Bermeo, A, Mayers, J, DeRose, J et al, Gruen, D, Hartley, WG, Lahav, O, Leistedt, B, McClintock, T, Rozo, E, Rykoff, ES, Varga, TN, Wechsler, RH, Zhang, Y, Avila, S, Brooks, D, Buckley-Geer, E, Burke, DL, Rosell, AC, Kind, MC, Carretero, J, Castander, FJ, Collins, CA, da Costa, LN, Desai, S, De Vicente, J, Diehl, HT, Dietrich, JP, Doel, P, Flaugher, B, Fosalba, P, Frieman, J, Garcia-Bellido, J, Gerdes, DW, Gruendl, RA, Gschwend, J, Gutierrez, G, Honscheid, K, James, DJ, Krause, E, Kuehn, K, Kuropatkin, N, Liddle, A, Lima, M, Maia, MAG, Mann, RG, Marshall, JL, Menanteau, F, Miquel, R, Ogando, RLC, Plazas, AA, Roodman, A, Rooney, P, Sahlen, M, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Sobreira, F, Stott, J, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Tucker, DL, Viana, PTP, Vikram, V and Walker, AR (2020) Stellar mass as a galaxy cluster mass proxy: application to the Dark Energy Survey redMaPPer clusters. Monthly Notices of the Royal Astronomical Society, 493 (4). pp. 4591-4606. ISSN 0035-8711

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Abstract

We introduce a galaxy cluster mass observable, μ⋆, based on the stellar masses of cluster members, and we present results for the Dark Energy Survey (DES) Year 1 (Y1) observations. Stellar masses are computed using a Bayesian model averaging method, and are validated for DES data using simulations and COSMOS data. We show that μ⋆ works as a promising mass proxy by comparing our predictions to X-ray measurements. We measure the X-ray temperature–μ⋆ relation for a total of 129 clusters matched between the wide-field DES Y1 redMaPPer catalogue and Chandra and XMM archival observations, spanning the redshift range 0.1 < z < 0.7. For a scaling relation that is linear in logarithmic space, we find a slope of α = 0.488 ± 0.043 and a scatter in the X-ray temperature at fixed μ⋆ of σlnTX|μ⋆=0.266+0.019−0.020 for the joint sample. By using the halo mass scaling relations of the X-ray temperature from the Weighing the Giants program, we further derive the μ⋆-conditioned scatter in mass, finding σlnM|μ⋆=0.26+0.15−0.10⁠. These results are competitive with well-established cluster mass proxies used for cosmological analyses, showing that μ⋆ can be used as a reliable and physically motivated mass proxy to derive cosmological constraints.

Item Type:	Article
Additional Information:	This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2020 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Uncontrolled Keywords:	0201 Astronomical and Space Sciences
Subjects:	Q Science > QB Astronomy Q Science > QC Physics
Divisions:	Astrophysics Research Institute
Publisher:	Oxford University Press
Related URLs:	Author
Date Deposited:	02 Feb 2021 11:30
Last Modified:	04 Sep 2021 06:01
DOI or ID number:	10.1093/mnras/staa526
URI:	https://researchonline.ljmu.ac.uk/id/eprint/14383

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