μ* masses: Weak-lensing calibration of the dark energy survey year 1 redMaPPer clusters using stellar masses

M. E.S. Pereira, A. Palmese, T. N. Varga, T. McClintock, M. Soares-Santos, J. Burgad, J. Annis, A. Farahi, H. Lin, A. Choi, J. DeRose, J. Esteves, M. Gatti, D. Gruen, W. G. Hartley, B. Hoyle, T. Jeltema, N. MacCrann, A. Roodman, C. SánchezT. Shin, A. von der Linden, J. Zuntz, T. M.C. Abbott, M. Aguena, S. Avila, E. Bertin, S. Bhargava, S. L. Bridle, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, S. Desai, H. T. Diehl, J. P. Dietrich, P. Doel, J. Estrada, S. Everett, B. Flaugher, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, R. A. Gruendl, J. Gschwend, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, N. Kuropatkin, O. Lahav, M. Lima, M. A.G. Maia, M. March, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, R. L.C. Ogando, F. Paz-Chinchón, A. A. Plazas, A. K. Romer, E. Sanchez, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, M. Smith, E. Suchyta, M. E.C. Swanson, G. Tarle, R. H. Wechsler, J. Weller, Y. Zhang

Research output: Contribution to journalArticlepeer-review

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Abstract

We present the weak-lensing mass calibration of the stellar-mass-based μ mass proxy for redMaPPer galaxy clusters in the Dark Energy Survey Year 1. For the first time, we are able to perform a calibration of μ at high redshifts, z > 0.33. In a blinded analysis, we use ∼6000 clusters split into 12 subsets spanning the ranges 0.1 ≤ z < 0.65 and μ up to ∼5.5 × 1013 M, and infer the average masses of these subsets through modelling of their stacked weak-lensing signal. In our model, we account for the following sources of systematic uncertainty: shear measurement and photometric redshift errors, miscentring, cluster-member contamination of the source sample, deviations from the Navarro-Frenk-White halo profile, halo triaxiality, and projection effects. We use the inferred masses to estimate the joint mass-μz scaling relation given by M200c|μ, z = M0(μ5.16 × 1012 M) ((1 + z)/1.35)Gz. We find M0 = (1.14 ± 0.07) × 1014 M with Fμ= 0.76 ± 0.06 and Gz = −1.14 ± 0.37. We discuss the use of μ as a complementary mass proxy to the well-studied richness λ for: (i) exploring the regimes of low z, λ < 20 and high λ, z ∼ 1; and (ii) testing systematics such as projection effects for applications in cluster cosmology.

Original languageEnglish
Pages (from-to)5450-5467
Number of pages18
JournalMonthly Notices of the Royal Astronomical Society
Volume498
Issue number4
DOIs
StatePublished - Nov 1 2020

Funding

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 AYA2015-71825, ESP2015-66861, FPA2015-68048, 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 programme 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 Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).

Keywords

  • Cosmology: observations
  • Galaxies: clusters: general
  • Gravitational lensing: weak

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