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Title: $$\mu_{\star}$$ Masses: Weak Lensing Calibration of the Dark Energy Survey Year 1 redMaPPer Clusters using Stellar Masses

Abstract

We present the weak lensing mass calibration of the stellar mass based $$\mu_{\star}$$ 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 $$\mu_{\star}$$ at high redshifts, $z>0.33$. In a blinded analysis, we use $$\sim 6,000$$ clusters split into 12 subsets spanning the ranges $$0.1 \leqslant z<0.65$$ and $$\mu_{\star}$$ up to $$\sim 5.5 \times 10^{13} M_{\odot}$$, 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 NFW halo profile, halo triaxiality and projection effects. We use the inferred masses to estimate the joint mass--$$\mu_{\star}$$--$z$ 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 $$G_z= -1.14 \pm 0.37$$. We discuss the use of $$\mu_{\star}$$ as a complementary mass proxy to the well-studied richness $$\lambda$$ for: $i)$ exploring the regimes of low $z$, $$\lambda<20$$ and high $$\lambda$$, $$z \sim 1$$; $ii)$ testing systematics such as projection effects for applications in cluster cosmology.

Authors:
Publication Date:
Research Org.:
SLAC National Accelerator Lab., Menlo Park, CA (United States); Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
Sponsoring Org.:
USDOE Office of Science (SC), High Energy Physics (HEP)
Contributing Org.:
DES
OSTI Identifier:
1637627
Report Number(s):
arXiv:2006.10162; FERMILAB-PUB-20-250-A-AD-AE-SCD
oai:inspirehep.net:1801946
DOE Contract Number:  
AC02-07CH11359
Resource Type:
Journal Article
Journal Name:
TBD
Additional Journal Information:
Journal Name: TBD
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS

Citation Formats

Pereira, M. E.S., and et al. $\mu_{\star}$ Masses: Weak Lensing Calibration of the Dark Energy Survey Year 1 redMaPPer Clusters using Stellar Masses. United States: N. p., 2020. Web.
Pereira, M. E.S., & et al. $\mu_{\star}$ Masses: Weak Lensing Calibration of the Dark Energy Survey Year 1 redMaPPer Clusters using Stellar Masses. United States.
Pereira, M. E.S., and et al. Wed . "$\mu_{\star}$ Masses: Weak Lensing Calibration of the Dark Energy Survey Year 1 redMaPPer Clusters using Stellar Masses". United States. https://www.osti.gov/servlets/purl/1637627.
@article{osti_1637627,
title = {$\mu_{\star}$ Masses: Weak Lensing Calibration of the Dark Energy Survey Year 1 redMaPPer Clusters using Stellar Masses},
author = {Pereira, M. E.S. and et al.},
abstractNote = {We present the weak lensing mass calibration of the stellar mass based $\mu_{\star}$ 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 $\mu_{\star}$ at high redshifts, $z>0.33$. In a blinded analysis, we use $\sim 6,000$ clusters split into 12 subsets spanning the ranges $0.1 \leqslant z<0.65$ and $\mu_{\star}$ up to $\sim 5.5 \times 10^{13} M_{\odot}$, 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 NFW halo profile, halo triaxiality and projection effects. We use the inferred masses to estimate the joint mass--$\mu_{\star}$--$z$ 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 $G_z= -1.14 \pm 0.37$. We discuss the use of $\mu_{\star}$ as a complementary mass proxy to the well-studied richness $\lambda$ for: $i)$ exploring the regimes of low $z$, $\lambda<20$ and high $\lambda$, $z \sim 1$; $ii)$ testing systematics such as projection effects for applications in cluster cosmology.},
doi = {},
journal = {TBD},
number = ,
volume = ,
place = {United States},
year = {2020},
month = {6}
}