Julian A. Mayers, J. De Vicente, Flavia Sobreira, John P. Stott, W. G. Hartley, J. Carretero, N. Kuropatkin, R. D. Wilkinson, M. Carrasco Kind, Joshua A. Frieman, J. P. Dietrich, S. Desai, David J. Brooks, B. Welch, J. Burgad, A. K. Romer, Marcelle Soares-Santos, Robert G. Mann, J. DeRose, David J. James, Pablo Fosalba, V. Scarpine, Andrew R. Liddle, G. Gutierrez, Salcedo Romero de Ávila, F. J. Castander, Pedro T. P. Viana, E. Suchyta, A. A. Plazas, C. Vergara Cervantes, I. Sevilla-Noarbe, Marcos Lima, August E. Evrard, Antonella Palmese, T. McClintock, T. N. Varga, P. Rooney, M. A. G. Maia, L. N. da Costa, Matt Hilton, E. J. Sanchez, B. Flaugher, Daniel Thomas, E. Buckley-Geer, Douglas L. Tucker, Kyler Kuehn, Paul Giles, Martin Sahlén, Chris A. Collins, Daniel Gruen, Michael Schubnell, Vinu Vikram, M. da Silva Pereira, Tesla E. Jeltema, D. L. Hollowood, S. Serrano, Juan Garcia-Bellido, D. W. Gerdes, Eduardo Rozo, Ramon Miquel, Han Lin, A. Bermeo, Peter Doel, D. L. Burke, H. T. Diehl, R. L. C. Ogando, Robert A. Gruendl, J. Gschwend, Elisabeth Krause, Ofer Lahav, Yanxi Zhang, Arya Farahi, A. Roodman, M. E. C. Swanson, J. Annis, Felipe Menanteau, Boris Leistedt, Sunayana Bhargava, Gregory Tarle, Jennifer L. Marshall, K. Honscheid, Risa H. Wechsler, Eli S. Rykoff, A. Carnero Rosell, A. R. Walker, 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), and German Research Foundation
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., 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.