The Three Hundred project: the gas disruption of infalling objects in cluster environments

Abstract

We analyse the gas content evolution of infalling haloes in cluster environments from The Three Hundred project, a collection of 324 numerically modelled galaxy clusters. The haloes in our sample were selected within 5R200 of the main cluster halo at $z$ = 0 and have total halo mass M200 ≥ 1011h−1M⊙. We track their main progenitors and study their gas evolution since their crossing into the infall region, which we define as 1–4R200. Studying the radial trends of our populations using both the full phase-space information and a line-of-sight projection, we confirm the Arthur et al. (2019) result and identify a characteristic radius around 1.7R200 in 3D and at R200 in projection at which infalling haloes lose nearly all of the gas prior their infall. Splitting the trends by subhalo status,we show that subhaloes residing in group-mass and low-mass host haloes in the infall region follow similar radial gas-loss trends as their hosts, whereas subhaloes of cluster-mass host haloes are stripped of their gas much further out. Our results show that infalling objects suffer significant gaseous disruption that correlates with time-since-infall, cluster-centric distance, and host mass, and that the gaseous disruption they experience is a combination of subhalo pre-processing and object gas depletion at a radius that behaves like an accretion shock.

The Three Hundred Project: The stellar angular momentum evolution of cluster galaxies

“…Smith et al 2016;Łokas 2020) have shown that infalling and orbiting haloes within galaxy clusters are disrupted by a series of processes which dominate in such environments, such as ram-pressure stripping (e.g. Bahé & McCarthy 2015;Arthur et al 2019;Mostoghiu et al 2021), mergers (e.g. Behroozi et al 2014;Lagos et al 2018a), or tidal torques (e.g.…”

“…outside the central aperture) and thus they are prone to suffer from mass loss from processes that strip the halo at its outskirts. The gas component, on the other hand, is mostly gone regardless of their mass, as gas is affected by an entirely different set of processes as they fall into the central halo, that is to say ram-pressure stripping (Arthur et al 2019;Mostoghiu et al 2021). In studying the radial distribution of the gas inside infalling haloes (not shown here), we find that haloes that never reached the denser regions of the cluster halo are still considerably stripped of their gas component, which is in agreement with Power et al (2020), Arthur et al (2019), and Mostoghiu et al (2021).…”

“…However, galaxies and their haloes also feel the influence of the environment. Haloes falling towards and eventually orbiting within galaxy clusters are disrupted by a series of processes predominant in the cluster environment, for example, including the following: ram-pressure stripping (Gunn & Gott 1972;Abadi et al 1999;Bahé & McCarthy 2015;Arthur et al 2019;Mostoghiu et al 2021) that removes the gas in haloes and quenches the star formation of galaxies; galaxy harassment (Moore et al 1996(Moore et al , 1998Smith et al 2010Smith et al , 2015, mergers (Dressler 1980;Hashimoto & Oemler 2000;Behroozi et al 2014), tidal torques (Fujita 1998;Balogh et al 2000;Park et al 2007), and interactions in general (Knebe et al 2006;Recchi 2014) that can disrupt the haloes' components; and dynamical friction (Valtonen et al 1990;Jiang & Binney 2000;Fujii et al 2006;van den Bosch 2017;Miller et al 2020) which slows down infalling haloes and, over time, causes them to fall to the centre of the cluster. While the stars residing deep inside the potential well of the halo are shielded from tidal effects, they might nevertheless feel and react to the change of their own halo caused by the aforementioned processes.…”

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].…”

Significant Molecular Gas Deficiencies in Star-forming Cluster Galaxies at $z\sim1.4$

“…On the other hand, the use of stacking to probe below detection limits suggests the existence of a population of cluster galaxies with low gas fractions and short depletion timescales (Betti et al 2019;Zavala et al 2019). Theoretically, evidence from cosmological simulations is mounting that gas loss should start at large radii, with significant depletion of the gas reservoir by or at first passage of the cluster center (Oman & Hudson 2016;Zinger et al 2018;Arthur et al 2019;Mostoghiu et al 2021;Oman et al 2021).…”