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

DES Collaboration, 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. RoodmanC. Sánchez, T. 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

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

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-μ-z scaling relation given by M200c, z = M0/5.16 × 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
Publication statusPublished - 1 Nov 2020

Keywords

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

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