Gone after one orbit: How cluster environments quench galaxies

Lotz, Marcel; Remus, Rhea-Silvia; Dolag, K.; Biviano, A.; Burkert, Andreas

doi:10.1093/mnras/stz2070

Cited by 97 publications

(141 citation statements)

References 96 publications

Supporting

Mentioning

113

Contrasting

Unclassified

Order By: Relevance

“…When the range of (log) pericenters is wide, the velocity anisotropy at a given radius r is dominated by the orbits with pericenters much smaller than r, which are near radial at r. But in the limit of a unique pericenter, the velocity anisotropy of spirals would be fully tangential (i.e., circular) at r = r peri , rapidly increasing with radius to the radial values caused by infall (if the apocenters were all equal, one would return to circular at r = r apo ). This rapid transition in the velocity anisotropy profile is seen in recent hydrodynamical simulations (Lotz et al 2019). But, as illustrated in Fig.…”

Section: Isotropizationsupporting

confidence: 68%

Structural and dynamical modeling of WINGS clusters

Mamon

Cava

Biviano

et al. 2019

A&A

View full text Add to dashboard Cite

The orbital shapes of galaxies of different classes are a probe of their formation and evolution. The Bayesian MAMPOSSt mass-orbit modeling algorithm is used to jointly fit the distribution of elliptical, spiral-irregular, and lenticular galaxies in projected phase space, on three pseudo-clusters (built by stacking the clusters after re-normalizing their positions and velocities) of 54 regular clusters from the Wide-field Nearby Galaxy-clusters Survey (WINGS), with at least 30 member velocities. Our pseudo-clusters (i.e., stacks) contain nearly 5000 galaxies with available velocities and morphological types. Thirty runs of MAMPOSSt with different priors are presented. The highest MAMPOSSt likelihoods are obtained for generalized Navarro-Frenk-White (NFW) models with steeper inner slope, free-index Einasto models, and double NFW models for the cluster and the brightest cluster galaxy. However, there is no strong Bayesian evidence for a steeper profile than the NFW model. The mass concentration matches the predictions from cosmological simulations. Ellipticals usually best trace the mass distribution while S0s are close. Spiral galaxies show increasingly elongated orbits at increasing radii, as do S0s on two stacks, and ellipticals on one stack. The inner orbits of all three types in the three stacks are consistent with isotropy. Spiral galaxies should transform rapidly into early-types given their much larger extent in clusters. Elongated outer orbits are expected for the spirals, a consequence of their recent radial infall into the cluster. The less elongated orbits we find for early-types could be related to the longer time spent by these galaxies in the cluster. We demonstrate that two-body relaxation is too slow to explain the inner isotropy of the early types, which suggests that inner isotropy is the consequence of violent relaxation during major cluster mergers or dynamical friction and tidal braking acting on subclusters. We propose that the inner isotropy of the short-lived spirals is a selection effect of spirals passing only once through pericenter before being transformed into early-type morphologies.

show abstract

Section: Isotropizationsupporting

confidence: 68%

Structural and dynamical modeling of WINGS clusters

Mamon

Cava

Biviano

et al. 2019

A&A

View full text Add to dashboard Cite

show abstract

“…Their main finding showed that radial gas fractions decrease with decreasing cluster-centric distance, and contamination from backsplash and pre-processed galaxies (which will also increase with decreasing cluster-centric distance) brings the distribution down. This is in disagreement with Lotz et al (2019) and Arthur et al (2019), who find that the instantaneous gas fraction does decline radially, but the gas in (sub)haloes is lost on first passage, rather than contamination being the cause for the radial decline. In fact, in Arthur et al (2019), it was postulated that the majority of gas in infalling objects is stripped by some sort of accretion shock at 1.5-2R 200 , where R 200 is the radius of the halo at 200 times the critical density of the universe at that redshift.…”

contrasting

confidence: 75%

“…Our results show that, at similar radii, half of the gas of the infalling objects is already gone. As we do not make a distinction between relaxed and unrelaxed galaxy clusters, we expect that the contamination by these populations does not alter our trends by a substantial amount and therefore we conclude that most fractional gas-loss from infalling objects is lost on first infall (see Lotz et al 2019) at a characteristic radius.…”

Section: How Gas-loss Since Infall Relates To Cluster-centric Distancementioning

confidence: 80%

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

Mostoghiu

Arthur

Pearce

et al. 2021

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

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.

show abstract

“…Moreover, recent studies indicate that galaxies are systematically more quenched in cosmic filaments around clusters, than their counterparts from other isotropic directions (see for example, Martínez et al 2016;Salerno et al 2019;Sarron et al 2019). In fact, Lotz et al (2019) found that star-forming galaxies are in majority quenched during their first orbit around clusters in Magneticum simulation. Two main possible scenarios can potentially explain a stronger quenching of galaxies in comic filaments at cluster peripheries: either passive galaxies fall more rapidly inside galaxy clusters, since they are located closer to filament spin (Laigle et al 2018;Kraljic et al 2018); or the quenching efficiency is stronger in filaments around clusters due to a larger probability to merge, and to be accreted by small galaxy groups.…”

Section: The Dependency On Galaxy Activity (In Case 1 and 2)mentioning

confidence: 99%

Probing the azimuthal environment of galaxies around clusters

Gouin

Aghanim

Bonjean

et al. 2020

A&A

View full text Add to dashboard Cite

Galaxy clusters are connected at their peripheries to the large scale structures by cosmic filaments that funnel accreting material. These filamentary structures are studied to investigate both environment-driven galaxy evolution and structure formation and evolution. In the present work, we probe in a statistical manner the azimuthal distribution of galaxies around clusters as a function of the cluster-centric distance, the cluster richness, and the galaxy activity (star-forming or passive). We perform a harmonic decomposition in large photometric galaxy catalogue around 6400 SDSS clusters with masses M > 10 14 solar masses, in the redshift range of 0.1 < z < 0.3. The same analysis is performed on the mock galaxy catalogue from the light-cone of Magneticum hydrodynamical simulation. We use the multipole analysis to quantify asymmetries in the 2-D galaxy distribution. In the inner cluster regions at R < 2R500, we confirm that the galaxy distribution traces an ellipsoidal shape, which is more pronounced for richest clusters. In the clusters' outskirts (R = [2 − 8]R500), filamentary patterns are detected in harmonic space with a mean angular scale mmean = 4.2 ± 0.1. Massive clusters seem to have a larger number of connected filaments than low massive ones. We also find that passive galaxies appear to better trace the filamentary structures around clusters, even if the contribution of SF ones tend to increase with the cluster-centric distance, suggesting a gradient of galaxy activity in filaments around clusters.

show abstract

Gone after one orbit: How cluster environments quench galaxies

Cited by 97 publications

References 96 publications

Structural and dynamical modeling of WINGS clusters

Structural and dynamical modeling of WINGS clusters

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

Probing the azimuthal environment of galaxies around clusters

Contact Info

Product

Resources

About