Umetsu, KeiichiKeiichiUmetsuSereno, MauroMauroSerenoLieu, MaggieMaggieLieuMiyatake, HironaoHironaoMiyatakeMedezinski, ElinorElinorMedezinskiNishizawa, Atsushi J.Atsushi J.NishizawaGiles, PaulPaulGilesGASTALDELLO, FABIOFABIOGASTALDELLOMcCarthy, Ian G.Ian G.McCarthyKilbinger, MartinMartinKilbingerBirkinshaw, MarkMarkBirkinshawETTORI, STEFANOSTEFANOETTORIOkabe, NobuhiroNobuhiroOkabeChiu, I. -NonI. -NonChiuCoupon, JeanJeanCouponEckert, DominiqueDominiqueEckertFujita, YutakaYutakaFujitaHiguchi, YuichiYuichiHiguchiKoulouridis, EliasEliasKoulouridisMaughan, BenBenMaughanMiyazaki, SatoshiSatoshiMiyazakiOguri, MasamuneMasamuneOguriPacaud, FlorianFlorianPacaudPierre, MargueriteMargueritePierreRapetti, DavidDavidRapettiSmith, Graham P.Graham P.Smith2021-11-232021-11-2320200004-637Xhttp://hdl.handle.net/20.500.12386/31128We present a weak-lensing analysis of X-ray galaxy groups and clusters selected from the XMM-XXL survey using the first-year data from the Hyper Suprime-Cam (HSC) Subaru Strategic Program. Our joint weak-lensing and X-ray analysis focuses on 136 spectroscopically confirmed X-ray-selected systems at 0.031 ≤ z ≤ 1.033 detected in the 25 deg<SUP>2</SUP> XXL-N region, which largely overlaps with the HSC-XMM field. With high-quality HSC weak-lensing data, we characterize the mass distributions of individual clusters and establish the concentration-mass (c-M) relation for the XXL sample, by accounting for selection bias and statistical effects and marginalizing over the remaining mass calibration uncertainty. We find the mass-trend parameter of the c-M relation to be $\beta =-0.07\pm 0.28$ and the normalization to be ${c}_{200}=4.8\pm 1.0\,(\mathrm{stat})\pm 0.8\,(\mathrm{syst})$ at ${M}_{200}={10}^{14}\,{h}^{-1}\,{M}_{\odot }$ and z = 0.3. We find no statistical evidence for redshift evolution. Our weak-lensing results are in excellent agreement with dark-matter-only c-M relations calibrated for recent ΛCDM cosmologies. The level of intrinsic scatter in c<SUB>200</SUB> is constrained as $\sigma (\mathrm{ln}{c}_{200})\lt 24 \% $ ( $99.7 \% $ CL), which is smaller than predicted for the full population of ΛCDM halos. This is likely caused in part by the X-ray selection bias in terms of the cool-core or relaxation state. We determine the temperature-mass (T<SUB>X</SUB>-M<SUB>500</SUB>) relation for a subset of 105 XXL clusters that have both measured HSC lensing masses and X-ray temperatures. The resulting T<SUB>X</SUB>-M<SUB>500</SUB> relation is consistent with the self-similar prediction. Our T<SUB>X</SUB>-M<SUB>500</SUB> relation agrees with the XXL DR1 results at group scales but has a slightly steeper mass trend, implying a smaller mass scale in the cluster regime. The overall offset in the T<SUB>X</SUB>-M<SUB>500</SUB> relation is at the ∼1.5σ level, corresponding to a mean mass offset of $34 \% \pm 20 \% $ . We also provide bias-corrected, weak-lensing-calibrated M<SUB>200</SUB> and M<SUB>500</SUB> mass estimates of individual XXL clusters based on their measured X-ray temperatures.STAMPAenArticle10.3847/1538-4357/ab6bcahttps://iopscience.iop.org/article/10.3847/1538-4357/ab6bca2020ApJ...890..148UFIS/05 - ASTRONOMIA E ASTROFISICAERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_9 Clusters of galaxies and large scale structures