Journal article

Exploring the contamination of the DES-Y1 cluster sample with SPT-SZ selected clusters

S Grandis, JJ Mohr, M Costanzi, A Saro, S Bocquet, M Klein, M Aguena, S Allam, J Annis, B Ansarinejad, D Bacon, E Bertin, L Bleem, D Brooks, DL Burke, A Carnero Rosel, M Carrasco Kind, J Carretero, FJ Castander, A Choi Show all



We perform a cross validation of the cluster catalogue selected by the red-sequence Matched-filter Probabilistic Percolation algorithm (redMaPPer) in Dark Energy Survey year 1 (DES-Y1) data by matching it with the Sunyaev-Zel'dovich effect (SZE) selected cluster catalogue from the South Pole Telescope SPT-SZ survey. Of the 1005 redMaPPer selected clusters with measured richness $\hat{\lambda }\gt 40$ in the joint footprint, 207 are confirmed by SPT-SZ. Using the mass information from the SZE signal, we calibrate the richness-mass relation using a Bayesian cluster population model. We find a mass trend λ ∝ MB consistent with a linear relation (B ∼1), no significant redshift evolution ..

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Awarded by ERC-StG 'ClustersXCosmo'

Awarded by FARE-MIUR grant 'ClustersXEuclid'

Awarded by National Science Foundation

Awarded by NSF Physics Frontier Center

Awarded by Gordon and Betty Moore Foundation

Awarded by US NSF

Awarded by MINECO

Awarded by European Research Council under the European Union

Awarded by U.S. Department of Energy, Office of Science, Office of High Energy Physics

Funding Acknowledgements

We acknowledge financial support from the MPG Faculty Fellowship program, the DFG Cluster of Excellence 'Origin and Structure of the Universe', the new DFG cluster 'Origins' and the LudwigMaximilians-Universit at Munich. AS is supported by the ERC-StG 'ClustersXCosmo' grant agreement 716762, by the FARE-MIUR grant `ClustersXEuclid' R165SBKTMA, and by the INFN INDARK grant Numerical computations in this work relied on the PYTHON packages NUMPY (Travis 2006) and SCIPY (Jones et al. 2001). The plots were produced using the package matplotlib (Hunter 2007).Posterior samples have been drawn from the likelihood functions and the priors using emcee (Foreman-Mackey et al. 2013). This work was performed in the context of the South-Pole Telescope scientific program. SPT is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation and the Gordon and Betty Moore Foundation grant GBMF 947 to the University of Chicago. This work is also supported by the U.S. Department of Energy. AAS acknowledges support by US NSF AST-1814719.This paper has gone through internal review by the DES collaboration. 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 UrbanaChampaign, 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, Fundacao Carlos Chagas Filho de Amparoa Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ci`encies de l'Espai (IEEC/CSIC), the Institut de F ' isica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium.Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171.The DES participants from Spanish institutions are partially supported by MINECO under grants AYA201571825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Depa rtment of Energy, Office of Science, Office of High Energy Physics.