The Three Hundred Project: dissecting the fundamental plane of galaxy clusters up to $z=1$

Abstract

We carry out a systematic study of the recently discovered fundamental plane of galaxy clusters (CFP) using a sample of ∼ 250 simulated clusters from T T H project, focusing on the stability of the plane against different temperature definitions and its dependence on the dynamical relaxation state of clusters. The CFP is characterised in the form of 𝑇 ∝ 𝑀 𝛼 s 𝑟 𝛽 s , defined with the gas temperature (𝑇) and the characteristic halo scale radius and mass (𝑟 s and 𝑀 s ) assuming an NFW halo description. We explore two definitions of weighted temperatures, namely mass-weighted and spectroscopic-like temperatures, in three radial ranges: [0.1, 1.0]𝑟 200 , [0.15, 1.0]𝑟 500 , and [50, 500]ℎ −1 kpc. We find that T T H project clusters at 𝑧 = 0 lie on a thin plane whose parameters (𝛼, 𝛽) and dispersion (0.015-0.030 dex) depend on the gas temperature definition. The CFP for mass-weighted temperatures is closer to the virial equilibrium expectation (𝛼 = 1, 𝛽 = −1) with a smaller dispersion. When gas temperatures are measured inside 500ℎ −1 kpc, which is close to the median value of 𝑟 s , the resulting CFP deviates the most from the virial expectation and shifts towards the similarity solution for a secondary infall model (𝛼 = 1.5, 𝛽 = −2). Independently of the temperature definition, we find that clusters at 𝑧 = 1 form a CFP similar to the virial expectation. At all epochs, the CFP remains well defined throughout the evolution of the cluster population. The CFP of relaxed clusters is always close to the virial expectation, with a milder evolution than for the unrelaxed case. We find that only systems formed over the last 4 Gyr have a CFP that is closer to the self-similar solution. All these findings are compatible with the CFP obtained for a CLASH subsample excluding the hottest clusters with 𝑇 X > 12 keV.

A test of galaxy cluster fundamental plane for the X-COP sample

“…where r s is the scale radius for which the logarithm of the slope of the density is equal to -2; and ρ s is the characteristic density which change from halo to halo [27,29] and is given by:…”

“…Recently, the FP was comprehensively tested using a sample of about 250 simulated clusters [29] (G21, hereafter) from the Three Hundred project sample [38]. For their analysis, G21 used two different definitions for the temperature: mass-weighted and spectroscopic temperatures.…”

“…G21 also re-analyzed only the relaxed cluster sample in F18 (consisting of 13 objects), and found that the fundamental plane is compatible with both the virial as well as the self-similar solution. More details about the findings in G21 can be found in [29].…”

The THREEHUNDRED project: the effect of baryon processes at galaxy cluster scale

“…Furthermore, the cluster backsplash galaxies [19,20] and shock radius [21] have also been well addressed. The advanced baryon models in hydrodynamic simulations allow us to perform a detailed investigation on the cluster properties, such as profiles [22,23], substructure and its baryonic content [24][25][26][27], dynamical state and morphology [28,29], cluster (non-)thermalization [30,31], the fundamental plane [32], and the cluster mass biases [33, for hydrostatic-equilibrium assumption], [34, for sigma-mass relation] and [35, for weaklensing]. Lastly, comparing to the void/field region runs in this project allows us to study the effect of environment [36]; including the self-interacting dark matter run allow us to constrain the dark matter cross-section [37]; It further help us to examine the chameleon gravity [38].…”

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

“…the galaxy clusters (Kuchner et al 2021a;Kotecha et al 2021), cluster backsplash galaxies (Haggar et al 2020;Knebe et al 2020), and the virial shock radius (Baxter et al 2021;Anbajagane et al 2021). The advanced input physics in the hydrodynamic simulations allow us to perform a detailed investigation on the cluster properties, such as cluster profiles (Mostoghiu et al 2019;Li et al 2020), substructure and its baryonic content (Arthur et al 2019;Haggar et al 2021;Mostoghiu et al 2021b,a), dynamical state and morphology (Capalbo et al 2021;De Luca et al 2021;Capalbo et al 2022;Zhang et al 2021), ICM (non-)thermalization (Sayers et al 2021;Sereno et al 2021), the fundamental plane (Díaz-García et al 2021), the effects of mergers on the BCG properties (Contreras-Santos et al 2022) and the hydrostatic equilibrium mass bias (Ansarifard et al 2020;Li et al 2021;Gianfagna et al 2022). Lastly, comparing to the void/field region runs in this project allows us to study the effect of environment (Wang et al 2018); a self-interacting dark matter run that allows constraints on the dark matter cross-section (Vega-Ferrero et al 2021); and even to examine chameleon gravity (Tamosiunas et al 2021).…”