Μ⋆ masses: weak-lensing calibration of the Dark Energy Survey Year 1 redMaPPer clusters using stellar masses. Issue 4 (7th September 2020)

• Record Type: Journal Article
• Authors: Pereira, M E S; Palmese, A; Varga, T N; McClintock, T; Soares-Santos, M; Burgad, J; Annis, J; Farahi, A; Lin, H; Choi, A; DeRose, J; Esteves, J; Gatti, M; Gruen, D; Hartley, W G; Hoyle, B; Jeltema, T; MacCrann, N; Roodman, A; Sánchez, C; Shin, T; von der Linden, A; Zuntz, J; Abbott, T M C; Aguena, M; Avila, S; Bertin, E; Bhargava, S; Bridle, S L; Brooks, D; Burke, D L; Carnero Rosell, A; Carrasco Kind, M; Carretero, J; Costanzi, M; da Costa, L N; Desai, S; Diehl, H T; Dietrich, J P; Doel, P; Estrada, J; Everett, S; Flaugher, B; Fosalba, P; Frieman, J; García-Bellido, J; Gaztanaga, E; Gerdes, D W; Gruendl, R A; Gschwend, J; Gutierrez, G; Hinton, S R; Hollowood, D L; Honscheid, K; James, D J; Kuehn, K; Kuropatkin, N; Lahav, O; Lima, M; Maia, M A G; March, M; Marshall, J L; Melchior, P; Menanteau, F; Miquel, R; Ogando, R L C; Paz-Chinchón, F; Plazas, A A; Romer, A K; Sanchez, E; Scarpine, V; Schubnell, M; Serrano, S; Sevilla-Noarbe, I; Smith, M; Suchyta, E; Swanson, M E C; Tarle, G; Wechsler, R H; Weller, J; Zhang, Y;
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 498:Issue 4(2020)
• Page Start: 5450
• Page End: 5467
• Publication Date: 2020-09-07
• Subjects: gravitational lensing: weak -- galaxies: clusters: general -- cosmology: observations; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa2687
• Languages: English
• ISSNs: 0035-8711

Abstract

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 ${\sim} 5.5 \times 10^{13} \, \mathrm{M}_{\odot }$, 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 $\langle M_{200c} | \mu _{\star }, z \rangle = M_0 (\mu _{\star }/5.16\times 10^{12} \, \mathrm{M_{\odot }})^{F_{\mu _{\star }}} ((1+z)/1.35)^{G_z}$ . We find $M_0= (1.14 \pm 0.07) \times 10^{14} \, \mathrm{M_{\odot }}$ with $F_{\mu _{\star }}= 0.76 \pm 0.06$ 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.