Mass calibration of DES Year-3 clusters via SPT-3G CMB cluster lensing

Creators: Ansarinejad, B.; Raghunathan, S.; Abbott, T. M. C.; Ade, P. A. R.; Aguena, M.; Alves, O.; Anderson, A. J.; Andrade-Oliveira, F.; Archipley, M.; Balkenhol, L.; Benabed, K.; Bender, A. N.; Benson, B. A.; Bertin, E.; Bianchini, F.; Bleem, L. E.; Bocquet, S.; Bouchet, F. R.; Brooks, D.; Bryant, L.; Burke, D. L.; Camphuis, E.; Carlstrom, J. E.; Carnero Rosell, A.; Carretero, J.; Castander, F. J.; Cecil, T. W.; Chang, C. L.; Chaubal, P.; Chichura, P. M.; Chou, T.-L.; Coerver, A.; Costanzi, M.; Crawford, T. M.; Cukierman, A.; da Costa, L. N.; Daley, C.; Davis, T. M.; de Haan, T.; Desai, S.; De Vicente, J.; Dibert, K. R.; Dobbs, M. A.; Doel, P.; Doussot, A.; Doux, C.; Dutcher, D.; Everett, W.; Feng, C.; Ferguson, K. R.; Ferrero, I.; Fichman, K.; Foster, A.; Frieman, J.; Galli, S.; Gambrel, A. E.; García-Bellido, J.; Gardner, R. W.; Gaztanaga, E.; Ge, F.; Giannini, G.; Goeckner-Wald, N.; Grandis, S.; Gruendl, R. A.; Gualtieri, R.; Guidi, F.; Guns, S.; Gutierrez, G.; Halverson, N. W.; Hinton, S. R.; Hivon, E.; Holder, G. P.; Hollowood, D. L.; Holzapfel, W. L.; Honscheid, K.; Hood, J. C.; Huang, N.; James, D. J.; Kéruzoré, F.; Knox, L.; Korman, M.; Kuo, C.-L.; Lee, A. T.; Lee, S.; Levy, K.; Lowitz, A. E.; Lu, C.; Maniyar, A.; Marshall, J. L.; Mena-Fernández, J.; Menanteau, F.; Miquel, R.; Millea, M.; Mohr, J. J.; Montgomery, J.; Nakato, Y.; Natoli, T.; Noble, G. I.; Novosad, V.; Ogando, R. L. C.; Omori, Y.; Padin, S.; Palmese, A.; Pan, Z.; Paschos, P.; Pereira, M. E. S.; Pieres, A.; Plazas Malagón, A. A.; Prabhu, K.; Quan, W.; Rahlin, A.; Rahimi, M.; Reichardt, C. L.; Reil, K.; Romer, A. K.; Rouble, M.; Ruhl, J. E.; Sanchez, E.; Sanchez Cid, D.; Schiappucci, E.; Sevilla-Noarbe, I.; Smecher, G.; Smith, M.; Sobrin, J. A.; Stark, A. A.; Stephen, J.; Suchyta, E.; Suzuki, A.; Swanson, M. E. C.; Tandoi, C.; Tarle, G.; Thompson, K. L.; Thorne, B.; Trendafilova, C.; Tucker, C.; Umilta, C.; Vieira, J.D.; Wang, G.; Weaverdyck, N.; Whitehorn, N.; Wiseman, P.; Wu, W. L. K.; Yefremenko, V.; Young, M.R.; Zebrowski, J. A.; DES Collaboration

Abstract

We measure the stacked lensing signal in the direction of galaxy clusters in the Dark Energy Survey Year 3 (DES Y3) redMaPPer sample, using cosmic microwave background (CMB) temperature data from SPT-3G, the third-generation CMB camera on the South Pole Telescope (SPT). Here, we estimate the lensing signal using temperature maps constructed from the initial 2 years of data from the SPT-3G 'Main' survey, covering 1500 deg² of the Southern sky. We then use this lensing signal as a proxy for the mean cluster mass of the DES sample. The thermal Sunyaev-Zel'dovich (tSZ) signal, which can contaminate the lensing signal if not addressed, is isolated and removed from the data before obtaining the mass measurement. In this work, we employ three versions of the redMaPPer catalogue: a Flux-Limited sample containing 8865 clusters, a Volume-Limited sample with 5391 clusters, and a Volume&Redshift-Limited sample with 4450 clusters. For the three samples, we detect the CMB lensing signal at a significance of 12.4σ, 10.5σ and 10.2σ and find the mean cluster masses to be M_200m = 1.66±0.13 [stat.]± 0.03 [sys.], 1.97±0.18 [stat.]± 0.05 [sys.], and 2.11±0.20 [stat.]± 0.05 [sys.]×10¹⁴ M_⊙, respectively. This is a factor of ∼ 2 improvement relative to the precision of measurements with previous generations of SPT surveys and the most constraining cluster mass measurements using CMB cluster lensing to date. Overall, we find no significant tensions between our results and masses given by redMaPPer mass-richness scaling relations of previous works, which were calibrated using CMB cluster lensing, optical weak lensing, and velocity dispersion measurements from various combinations of DES, SDSS and Planck data. We then divide our sample into 3 redshift and 3 richness bins, finding no significant discrepancies with optical weak-lensing calibrated masses in these bins. We forecast a 5.7% constraint on the mean cluster mass of the DES Y3 sample with the complete SPT-3G surveys when using both temperature and polarization data and including an additional ∼ 1400 deg² of observations from the 'Extended' SPT-3G survey.

Copyright and License

© 2024 The Author(s). Published by IOP Publishing Ltd on behalf of Sissa Medialab. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.

Acknowledgement

We thank the anonymous referee for their review of the paper and useful comments.

The Melbourne team acknowledges support from the Australian Research Council’s Discovery Projects scheme (DP200101068).

SR acknowledges support from the Center for AstroPhysical Surveys (CAPS) at the National Center for Supercomputing Applications (NCSA), University of Illinois Urbana-Champaign.

The South Pole Telescope program is supported by the National Science Foundation (NSF) through award OPP-1852617. Partial support is also provided by the Kavli Institute of Cosmological Physics at the University of Chicago.

This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 101001897).

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 Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF’s NOIRLab, 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 at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed 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 MICINN under grants ESP2017-89838, PGC2018- 094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, 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 Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).

This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

Argonne National Laboratory’s work was supported by the U.S. Department of Energy, Office of High Energy Physics, under Contract No. DE- AC02-06CH11357.

Software References

We acknowledge the use of http://astromap.icrar.org/ for producing figure 1. Some of the results in this paper have been derived using the healpy [79] and HEALPix [80] packages. The analysis of this work also made use of Python3 [81] and packages including scipy [82], numpy [83], astropy [84] and pandas [85].

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