The eROSITA Final Equatorial-Depth Survey (eFEDS): X-ray Observable-to-Mass-and-Redshift Relations of Galaxy Clusters and Groups with Weak-Lensing Mass Calibration from the Hyper Suprime-Cam Subaru Strategic Program Survey

I-Non Chiu; Vittorio Ghirardini; Ang Liu; Sebastian Grandis; Esra Bulbul; Y. Emre Bahar; Johan Comparat; Sebastian Bocquet; Nicolas Clerc; Matthias Klein; Teng Liu; Xiangchong Li; Hironao Miyatake; Joseph Mohr; Masamune Oguri; Nobuhiro Okabe; Florian Pacaud; Miriam E. Ramos-Ceja; Thomas H. Reiprich; Tim Schrabback; Keiichi Umetsu

doi:10.1051/0004-6361/202141755

paper

The eROSITA Final Equatorial-Depth Survey (eFEDS): X-ray Observable-to-Mass-and-Redshift Relations of Galaxy Clusters and Groups with Weak-Lensing Mass Calibration from the Hyper Suprime-Cam Subaru Strategic Program Survey

arXiv:2107.05652 · doi:10.1051/0004-6361/202141755

Abstract

We present the first weak-lensing mass calibration and X-ray scaling relations of galaxy clusters and groups selected in the $e R O S I T A$ Final Equatorial Depth Survey (eFEDS) observed by Spectrum Roentgen Gamma/ $e R O S I T A$ over a contiguous footprint with an area of $\approx 140$ deg $^{2}$ , using the three-year (S19A) weak-lensing data from the Hyper Suprime-Cam (HSC) Subaru Strategic Program survey. In this work, a sample of $434$ optically confirmed galaxy clusters (and groups) at redshift $0.01 ≲ z ≲ 1.3$ with a median of $0.35$ is studied, of which $313$ systems are uniformly covered by the HSC survey to enable the extraction of the weak-lensing shear observable. In a Bayesian population modelling, we perform a blind analysis for the weak-lensing mass calibration by simultaneously modelling the observed count rate $η$ and the shear profile $g$ of individual clusters through the count rate-to-mass-and-redshift ( $η$ -- $M_{500}$ -- $z$ ) and weak-lensing mass-to-mass-and-redshift ( $M_{WL}$ -- $M_{500}$ -- $z$ ) relations, respectively, while accounting for the bias in these observables using simulation-based calibrations. As a result, the count rate-inferred and lensing-calibrated cluster mass is obtained from the joint modelling of the scaling relations, as the ensemble mass spanning a range of $1 0^{13} h^{- 1} M_{⊙} ≲ M_{500} ≲ 1 0^{15} h^{- 1} M_{⊙}$ with a median of $\approx 1 0^{14} h^{- 1} M_{⊙}$ for the eFEDS sample. With the mass calibration, we further model the X-ray observable-to-mass-and-redshift relations, including the rest-frame soft-band and bolometric luminosity ( $L_{X}$ and $L_{b}$ ), the emission-weighted temperature $T_{X}$ , the mass of intra-cluster medium $M_{g}$ , and the mass proxy $Y_{X}$ , which is the product of $T_{X}$ and $M_{g}$ . (abridged)

arXiv commentAccepted for publication in A&A. Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission

The eROSITA Final Equatorial-Depth Survey (eFEDS): X-ray Observable-to-Mass-and-Redshift Relations of Galaxy Clusters and Groups with Weak-Lensing Mass Calibration from the Hyper Suprime-Cam Subaru Strategic Program Survey

Abstract

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