Farahi, A, Chen, X, Evrard, AE, Hollowood, DL, Wilkinson, R, Bhargava, S, Giles, P, Romer, AK, Jeltema, T, Hilton, M, Bermeo, A, Mayers, J, Cervantes, CV, Rozo, E, Rykoff, ES, Collins, CA, Costanzi, M, Everett, S, Liddle, AR, Mann, RG et al, Mantz, A, Rooney, P, Sahlen, M, Stott, J, Viana, PTP, Zhang, Y, Annis, J, Avila, S, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Kind, MC, Carretero, J, Castander, FJ, da Costa, LN, De Vicente, J, Desai, S, Diehl, HT, Dietrich, JP, Doel, P, Flaugher, B, Fosalba, P, Frieman, J, Garcia-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Honscheid, K, James, DJ, Krause, E, Kuehn, K, Kuropatkin, N, Lima, M, Maia, MAG, Marshall, JL, Melchior, P, Menanteau, F, Miquel, R, Ogando, RLC, Plazas, AA, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Smith, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Tucker, DL, Vikram, V, Walker, AR and Weller, J (2019) Mass variance from archival X-ray properties of Dark Energy Survey Year-1 galaxy clusters. Monthly Notices of the Royal Astronomical Society, 490 (3). pp. 3341-3354. ISSN 0035-8711

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Abstract

Using archival X-ray observations and a lognormal population model, we estimate constraints on the intrinsic scatter in halo mass at fixed optical richness for a galaxy cluster sample identified in Dark Energy Survey Year-One (DES-Y1) data with the redMaPPer algorithm. We examine the scaling behaviour of X-ray temperatures, TX, with optical richness, λRM, for clusters in the redshift range 0.2 < z < 0.7. X-ray temperatures are obtained from Chandra and XMM observations for 58 and 110 redMaPPer systems, respectively. Despite non-uniform sky coverage, the TX measurements are >50 per cent complete for clusters with λRM > 130. Regression analysis on the two samples produces consistent posterior scaling parameters, from which we derive a combined constraint on the residual scatter, σlnT|λ=0.275±0.019⁠. Joined with constraints for TX scaling with halo mass from the Weighing the Giants program and richness–temperature covariance estimates from the LoCuSS sample, we derive the richness-conditioned scatter in mass, σlnM|λ=0.30±0.04(stat)±0.09(sys)⁠, at an optical richness of approximately 100. Uncertainties in external parameters, particularly the slope and variance of the TX–mass relation and the covariance of TX and λRM at fixed mass, dominate the systematic error. The 95 per cent confidence region from joint sample analysis is relatively broad, σlnM|λ∈[0.14,0.55]⁠, or a factor 10 in variance.

Item Type:	Article
Additional Information:	This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2019 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:	03 Mar 2020 10:04
Last Modified:	04 Sep 2021 07:48
DOI or ID number:	10.1093/mnras/stz2689
URI:	https://researchonline.ljmu.ac.uk/id/eprint/12365

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