Stellar mass as a galaxy cluster mass proxy: Application to the Dark Energy Survey redMaPPer clusters
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 a...
| Autores: | , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2020 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/237333 |
| Acceso en línea: | http://hdl.handle.net/10261/237333 |
| Access Level: | acceso abierto |
| Palabra clave: | Cosmology: observations Galaxies: clusters: general Galaxies: evolution Galaxies: haloesSurveys |
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| dc.title.none.fl_str_mv |
Stellar mass as a galaxy cluster mass proxy: Application to the Dark Energy Survey redMaPPer clusters |
| title |
Stellar mass as a galaxy cluster mass proxy: Application to the Dark Energy Survey redMaPPer clusters |
| spellingShingle |
Stellar mass as a galaxy cluster mass proxy: Application to the Dark Energy Survey redMaPPer clusters Palmese, A. Cosmology: observations Galaxies: clusters: general Galaxies: evolution Galaxies: haloesSurveys |
| title_short |
Stellar mass as a galaxy cluster mass proxy: Application to the Dark Energy Survey redMaPPer clusters |
| title_full |
Stellar mass as a galaxy cluster mass proxy: Application to the Dark Energy Survey redMaPPer clusters |
| title_fullStr |
Stellar mass as a galaxy cluster mass proxy: Application to the Dark Energy Survey redMaPPer clusters |
| title_full_unstemmed |
Stellar mass as a galaxy cluster mass proxy: Application to the Dark Energy Survey redMaPPer clusters |
| title_sort |
Stellar mass as a galaxy cluster mass proxy: Application to the Dark Energy Survey redMaPPer clusters |
| dc.creator.none.fl_str_mv |
Palmese, A. Castander, Francisco J. Fosalba, Pablo Serrano, Santiago Viana, Pedro Walker, Alistair R. DES Collaboration |
| author |
Palmese, A. |
| author_facet |
Palmese, A. Castander, Francisco J. Fosalba, Pablo Serrano, Santiago Viana, Pedro Walker, Alistair R. DES Collaboration |
| author_role |
author |
| author2 |
Castander, Francisco J. Fosalba, Pablo Serrano, Santiago Viana, Pedro Walker, Alistair R. DES Collaboration |
| author2_role |
author author author author author author |
| dc.contributor.none.fl_str_mv |
Department of Energy (US) National Science Foundation (US) Ministerio de Ciencia, Innovación y Universidades (España) Science and Technology Facilities Council (UK) University of Illinois Kavli Institute for Theoretical Physics University of Chicago The Ohio State University Texas A&M University Financiadora de Estudos e Projetos (Brasil) Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil) Ministério da Ciência, Tecnologia e Inovação (Brasil) German Research Foundation Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72] |
| dc.subject.none.fl_str_mv |
Cosmology: observations Galaxies: clusters: general Galaxies: evolution Galaxies: haloesSurveys |
| topic |
Cosmology: observations Galaxies: clusters: general Galaxies: evolution Galaxies: haloesSurveys |
| description |
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 σ|μ* = 0.266 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 σM|μ* = 0.26. 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. |
| publishDate |
2020 |
| dc.date.none.fl_str_mv |
2020 2021 2021 2021 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article http://purl.org/coar/resource_type/c_6501 Publisher's version info:eu-repo/semantics/publishedVersion |
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article |
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publishedVersion |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/10261/237333 |
| url |
http://hdl.handle.net/10261/237333 |
| dc.language.none.fl_str_mv |
Inglés |
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Inglés |
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info:eu-repo/semantics/openAccess |
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openAccess |
| dc.publisher.none.fl_str_mv |
Royal Astronomical Society |
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Royal Astronomical Society |
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reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC instname:Consejo Superior de Investigaciones Científicas (CSIC) |
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Consejo Superior de Investigaciones Científicas (CSIC) |
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DIGITAL.CSIC. Repositorio Institucional del CSIC |
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DIGITAL.CSIC. Repositorio Institucional del CSIC |
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1869417241045368832 |
| spelling |
Stellar mass as a galaxy cluster mass proxy: Application to the Dark Energy Survey redMaPPer clustersPalmese, A.Castander, Francisco J.Fosalba, PabloSerrano, SantiagoViana, PedroWalker, Alistair R.DES CollaborationCosmology: observationsGalaxies: clusters: generalGalaxies: evolutionGalaxies: haloesSurveysWe 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 σ|μ* = 0.266 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 σM|μ* = 0.26. 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.AP acknowledges the UCL PhD studentship and the URA Visiting scholar award. AF is supported by a McWilliams Postdoctoral Fellowship. OL acknowledges support from a European Research Council Advanced Grant FP7/291329. SB acknowledges support from the UK Science and Technology Facilities Council via Research Training Grant ST/N504452/1. TOPCAT (Taylor 2005) has been extensively used in this work. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The DES data management system is supported by the National Science Foundation under Grant Number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478.Royal Astronomical SocietyDepartment of Energy (US)National Science Foundation (US)Ministerio de Ciencia, Innovación y Universidades (España)Science and Technology Facilities Council (UK)University of IllinoisKavli Institute for Theoretical PhysicsUniversity of ChicagoThe Ohio State UniversityTexas A&M UniversityFinanciadora de Estudos e Projetos (Brasil)Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de JaneiroConselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil)Ministério da Ciência, Tecnologia e Inovação (Brasil)German Research FoundationConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2021202120202021info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/237333reponame:DIGITAL.CSIC. 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