XXL Survey groups and clusters in the Hyper Suprime-Cam Survey. Scaling relations between X-ray properties and weak lensing mass

Abstract

Scaling relations trace the formation and evolution of galaxy clusters. We exploited multiwavelength surveys -the XXL survey at XMM-Newton in the X-ray band, and the Hyper Suprime-Cam Subaru Strategic Program for optical weak lensing -to study an X-ray selected, complete sample of clusters and groups. The scalings of gas mass, temperature, and soft-band X-ray luminosity with the weak lensing mass show imprints of radiative cooling and AGN feedback in groups. From the multi-variate analysis, we found some evidence for steeper than self-similar slopes for gas mass (β mg|m = 1.73 ± 0.80) and luminosity (β l|m = 1.91 ± 0.94) and a nearly self-similar slope for the temperature (β t|m = 0.78 ± 0.43). Intrinsic scatters of X-ray properties appear to be positively correlated at a fixed mass (median correlation factor ρ X1X2|m ∼ 0.34) due to dynamical state and merger history of the halos. Positive correlations with the weak lensing mass (median correlation factor ρ mwlX|m ∼ 0.35) can be connected to triaxiality and orientation. Comparison of weak lensing and hydrostatic masses suggests a small role played by non-thermal pressure support (9 ± 17%).

Full-sky photon simulation of clusters and active galactic nuclei in the soft X-rays for eROSITA

“…The scaling relations obtained are close (but not equal) to the self-similar model, used in the construction of the profiles. Overall, the scaling relations obtained are in good agreement with the literature (Lovisari et al 2015;Mantz et al 2016;Schellenberger & Reiprich 2017;Adami et al 2018;Bulbul et al 2019;Lovisari et al 2020;Sereno et al 2020;Umetsu et al 2020). To obtain XMM-like temperatures and carry out these comparisons, we correct temperatures from the literature following Schellenberger et al (2015).…”

“…Top. Model scaling relation between X-ray luminosity and mass (shaded areas MDPL2 1σ, 2σ) compared to existing data sets (open symbols) (Lo15, Ma16, Sc17, Ad18, Bu18, Lo20, Se20 respectively stand for Lovisari et al 2015;Mantz et al 2016;Schellenberger & Reiprich 2017;Adami et al 2018;Bulbul et al 2019;Lovisari et al 2020;Sereno et al 2020). The cross on the topleft represent the typical uncertainty on the observed data.…”

X-ray emission from hot gas in galaxy groups and clusters in simba

“…The most massive clusters at M 500 > 10 15 M are expected to follow self similarity, but our 100h −1 Mpc volume is too small to contain such systems. Interestingly, the relation against mass computed using weak lensing has been shown to more closely follow self-similarity (Sereno et al 2020).…”

X-Ray Scaling Relations for a Representative Sample of Planck-selected Clusters Observed with XMM-Newton

“…where the values of beta.YIZ and gamma.YIZ were frozen (beta.YIZ=1.0 and gamma.YIZ=2). The LIRA software and its underlying assumptions and methods have been extensively tested with data and simulations (see, e.g., Sereno 2016or Sereno et al 2019c. Accurate sampling of the parameter posterior probability distribution is crucial.…”