HSC-XXL : Baryon budget of the 136 XXL Groups and Clusters

Abstract

We present our determination of the baryon budget for an X-ray-selected XXL sample of 136 galaxy groups and clusters spanning nearly two orders of magnitude in mass (M 500 ∼ 10 13 − 10 15 M ) and the redshift range 0 < ∼ z < ∼ 1. Our joint analysis is based on the combination of HSC-SSP weak-lensing mass measurements, XXL X-ray gas mass measurements, and HSC and SDSS multiband photometry. We carry out a Bayesian analysis of multivariate mass-scaling relations of gas mass, galaxy stellar mass, stellar mass of brightest cluster galaxies (BCGs), and soft-band X-ray luminosity, by taking into account the intrinsic covariance between cluster properties, selection effect, weak-lensing mass calibration, and observational error covariance matrix. The mass-dependent slope of the gas mass-total mass (M 500 ) relation is found to be 1.29 +0.16 −0.10 , which is steeper than the self-similar prediction of unity, whereas the slope of the stellar mass-total mass relation is shallower than unity, 0.85 +0.12 −0.09 . The BCG stellar mass weakly depends on cluster mass with a slope of 0.49 +0.11 −0.10 . The baryon, gas mass, and stellar mass fractions as a function of M 500 agree with the results from numerical simulations and previous observations. We successfully constrain the full intrinsic covariance of the baryonic contents. The BCG stellar mass shows the larger intrinsic scatter at a given halo total mass, followed in order by stellar mass and gas mass. We find a significant positive intrinsic correlation coefficient between total (and satellite) stellar mass and BCG stellar mass and no evidence for intrinsic correlation between gas mass and stellar mass. All the baryonic components show no redshift evolution.

\textsc{The Three Hundred} project: The \textsc{Gizmo-Simba} run

“…The right-hand panel of Figure 1 shows the stellar mass fractions versus 𝑀 500 . Here, G -X and G -S show very similar results, and IllustrisTNG (Pillepich et al 2018) shows a similar slope but a slightly higher amplitude that is in better agreement with the observations from Akino et al (2021). In contrast, FABLE shows higher stellar fractions at group scales (𝑀 500 < 10 14 M ), and thus a slope that matches better with the individual observations shown.…”

“…The fitting function from Lovisari et al (2015) is the flattest among observations, and agrees well with G -X results. Meanwhile, Dietrich et al ( 2019) and Akino et al (2021) are in better agreement with G -S at 𝑀 500 > 10 14 M ; measurements to even lower masses are as yet highly uncertain. The downturn for 𝑀 500 < 10 14 𝑀 * in G -S owes to the high jet velocity which blows gas particles well outside of these low-mass halos' virial radius (Sorini et al 2021).…”

“…Note that other works, such as Lin & Mohr (2004); Gonzalez et al (2007); Andersson et al (2011); Budzynski et al (2014) and also the recent works Lim et al (2020); Chen et al (2022) (estimating gas fractions with SZ signal instead of X-ray) that also examined clusters at 𝑧 ∼ 0.1 to investigate similar fractions, are not included in this comparison due to different reasons, such as no 𝑀 500 or 𝑀 * being available, or that the sample is dominated by 𝑧 0 clusters. However, it has been suggested that there is almost no redshift evolution in both gas and stellar fractions within 𝑧 ∼ 1 (see more discussion below), so we include the best fitting results from the recent work of Akino et al (2021) out to modest redshifts using weak-lensing masses (Umetsu et al 2020) for the 136 XXL clusters in the HSC-SSP survey, shown as the grey shaded band.…”

Do blue galaxy-clusters have hot intracluster gas?

“…The CAMIRA clusters exhibited a positive correlation. The linear regression method (Akino et al 2021) resulted in the best-fit power-law model of E(z) −1 (LX /10 43 ergs −1 ) = 10 a (M500E(z)/10 14 M ) b , a = 0.05 +0.17…”

“…The CAMIRA clusters exhibited a positive correlation. The linear regression method(Akino et al 2021) resulted in the best-fit power-law model of E(z) −1 (LX /10 43 ergs −1 ) = 10 a (M500E(z)/10 14 M ) b , a = 0.05 +0.17−0.19 and b = 1.40 +0.45 −0.44 . In contrast, the upper bounds on the average luminosity and mass were obtained for the blue clusters, and the data points of the two subsamples overlapped with each other.…”