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    Mass variance from archival X-ray properties of Dark Energy Survey Year-1 galaxy clusters

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    Author
    Farahi, A
    Chen, X
    Evrard, A E
    Hollowood, D L
    Wilkinson, R
    Bhargava, S
    Giles, P
    Romer, A K
    Jeltema, T
    Hilton, M
    Bermeo, A
    Mayers, J
    Vergara Cervantes, C
    Rozo, E
    Rykoff, E S
    Collins, C
    Costanzi, M
    Everett, S
    Liddle, A R
    Mann, R G
    Mantz, A
    Rooney, P
    Sahlen, M
    Stott, J
    Viana, P T P
    Zhang, Y
    Annis, J
    Avila, S
    Brooks, D
    Buckley-Geer, E
    Burke, D L
    Carnero Rosell, A
    Carrasco Kind, M
    Carretero, J
    Castander, F J
    da Costa, L N
    De Vicente, J
    Desai, S
    Diehl, H T
    Dietrich, J P
    Doel, P
    Flaugher, B
    Fosalba, P
    Frieman, J
    García-Bellido, J
    Gaztanaga, E
    Gerdes, D W
    Gruen, D
    Gruendl, R A
    Gschwend, J
    Gutierrez, G
    Honscheid, K
    James, D J
    Krause, E
    Kuehn, K
    Kuropatkin, N
    Lima, M
    Maia, M A G
    Marshall, J L
    Melchior, P
    Menanteau, F
    Miquel, R
    Ogando, R L C
    Plazas, A A
    Sanchez, E
    Scarpine, V
    Schubnell, M
    Serrano, S
    Sevilla-Noarbe, I
    Smith, M
    Sobreira, F
    Suchyta, E
    Swanson, M E C
    Tarle, G
    Thomas, D
    Tucker, D L
    Vikram, V
    Walker, A R
    Weller, J
    Show allShow less
    Affiliation
    Univ Arizona, Dept Phys
    Univ Arizona, Steward Observ, Dept Astron
    Issue Date
    2019-09-26
    Keywords
    galaxies: clusters: general
    X-rays: galaxies: clusters
    
    Metadata
    Show full item record
    Publisher
    OXFORD UNIV PRESS
    Citation
    Farahi, A., Chen, X., Evrard, A. E., Hollowood, D. L., Wilkinson, R., Bhargava, S., ... & Bermeo, A. (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), 3341-3354.
    Journal
    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
    Rights
    Copyright © 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model).
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    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, T-X, with optical richness, lambda(RM), 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 T-X measurements are > 50 per cent complete for clusters with lambda(RM) > 130. Regression analysis on the two samples produces consistent posterior scaling parameters, from which we derive a combined constraint on the residual scatter, sigma(ln) (T) (vertical bar) (lambda) = 0.275 +/- 0.019. Joined with constraints for T-X 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, sigma(ln) (M) (vertical bar) (lambda) = 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 T-X-mass relation and the covariance of T-X and lambda(RM) at fixed mass, dominate the systematic error. The 95 per cent confidence region from joint sample analysis is relatively broad, sigma(ln) (M) (vertical bar) (lambda) is an element of [0.14, 0.55], or a factor 10 in variance.
    ISSN
    0035-8711
    DOI
    10.1093/mnras/stz2689
    Version
    Final published version
    Sponsors
    McWilliams Postdoctoral Fellowship; NASANational Aeronautics & Space Administration (NASA) [CXC17800360]; US Department of EnergyUnited States Department of Energy (DOE); US National Science FoundationNational Science Foundation (NSF); Ministry of Science and Education of SpainMinistry of Education and Science, Spain; Science and Technology Facilities Council of the United KingdomScience & Technology Facilities Council (STFC); Higher Education Funding Council for EnglandHigher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State UniversityOhio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e ProjetosCiencia Tecnologia e Inovacao (FINEP); Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e TecnologicoNational Council for Scientific and Technological Development (CNPq); Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche ForschungsgemeinschaftGerman Research Foundation (DFG); Argonne National LaboratoryUnited States Department of Energy (DOE)University of Chicago; University of California at Santa Cruz; University of CambridgeUniversity of Cambridge; Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; University of ChicagoUniversity of Chicago; University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) ZurichETH Zurich; Fermi National Accelerator LaboratoryUnited States Department of Energy (DOE)University of Chicago; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National LaboratoryUnited States Department of Energy (DOE); Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe; University of MichiganUniversity of Michigan System; National Optical Astronomy ObservatoryNational Science Foundation (NSF)NSF - Directorate for Mathematical & Physical Sciences (MPS); University of Nottingham; Ohio State UniversityOhio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford UniversityStanford University; University of Sussex; Texas AM University; OzDES Membership Consortium; National Science FoundationNational Science Foundation (NSF) [AST-1138766, AST-1536171]; MINECO [AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, MDM-2015-0509]; ERDF funds from the European Union; Generalitat de CatalunyaGeneralitat de Catalunya; European Research Council under the European Union including ERC [240672, 291329, 306478]; Brazilian Instituto Nacional de Cienciae Tecnologia (INCT) e-Universe (CNPq)National Council for Scientific and Technological Development (CNPq) [465376/2014-2]; U.S. Department of Energy, Office of Science, Office of High Energy PhysicsUnited States Department of Energy (DOE) [DE-AC02-07CH11359]; [DE-SC0010107]; [DE-SC0013541]
    ae974a485f413a2113503eed53cd6c53
    10.1093/mnras/stz2689
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