Too dense to go through: The importance of low-mass clusters for satellite quenching

Pallero, Diego; Gómez, Facundo A.; Padilla, Nelson D.; Bahé, Yannick M.; Vega-Martínez, Cristian A.; Torres-Flores, S.

doi:10.48550/arxiv.2012.08593

Cited by 8 publications

(12 citation statements)

References 52 publications

(67 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Finally, we note that simulations are also increasingly demonstrating the importance of groups for the evolution of cluster satellites: around 50% of all z = 0 satellites in massive clusters of the TNG300 simulation were quenched in a group before being accreted onto their final host (Donnari et al, 2021); Pallero et al (2020) came to a similar conclusion with the Hydrangea/C-EAGLE simulations. Similarly, Jung et al (2018) found that almost half of all M 10 9 M galaxies accreted onto clusters as (group) satellites are already gas poor at the time of cluster infall, compared to only 6% of central galaxies.…”

Section: Satellite Galaxies In Groupsmentioning

confidence: 53%

Simulating Groups and the IntraGroup Medium: The Surprisingly Complex and Rich Middle Ground between Clusters and Galaxies

et al. 2021

View full text Add to dashboard Cite

Galaxy groups are more than an intermediate scale between clusters and halos hosting individual galaxies, they are crucial laboratories capable of testing a range of astrophysics from how galaxies form and evolve to large scale structure (LSS) statistics for cosmology. Cosmological hydrodynamic simulations of groups on various scales offer an unparalleled testing ground for astrophysical theories. Widely used cosmological simulations with ∼(100 Mpc)3 volumes contain statistical samples of groups that provide important tests of galaxy evolution influenced by environmental processes. Larger volumes capable of reproducing LSS while following the redistribution of baryons by cooling and feedback are the essential tools necessary to constrain cosmological parameters. Higher resolution simulations can currently model satellite interactions, the processing of cool (T≈104−5 K) multi-phase gas, and non-thermal physics including turbulence, magnetic fields and cosmic ray transport. We review simulation results regarding the gas and stellar contents of groups, cooling flows and the relation to the central galaxy, the formation and processing of multi-phase gas, satellite interactions with the intragroup medium, and the impact of groups for cosmological parameter estimation. Cosmological simulations provide evolutionarily consistent predictions of these observationally difficult-to-define objects, and have untapped potential to accurately model their gaseous, stellar and dark matter distributions.

show abstract

Section: Satellite Galaxies In Groupsmentioning

confidence: 53%

Simulating Groups and the IntraGroup Medium: The Surprisingly Complex and Rich Middle Ground between Clusters and Galaxies

et al. 2021

View full text Add to dashboard Cite

show abstract

“…The different perturbing mechanisms affecting galaxies in high density environments act on different timescales for the gas removal, and thus have different effects on the star formation activity of the perturbed objects. The typical timescale for RPS to be efficient has been derived using semi-analytical models and full or zoomed-in hydrodynamic cosmological simulations of rich clusters of galaxies (Abadi et al 1999;Balogh et al 2000;Quilis et al 2000;Mori & Burkert 2000;Schulz & Struck 2001;Marcolini et al 2003;Tonnesen et al 2007;Roediger & Brüggen 2007;Marasco et al 2016;Trayford et al 2016;Lotz et al 2019;Pallero et al 2020) or tuned simulations of selected objects with multifrequency data consistently indicating that they are undergoing a stripping event (Vollmer 2003;Vollmer & Huchtmeier 2003;Vollmer et al 2004Vollmer et al , 2005bVollmer et al , 2006Vollmer et al , 2008aVollmer et al ,b, 2009Vollmer et al , 2012Vollmer et al , 2021Boselli et al 2021). 3-D hydrodynamic simulations suggest that a large fraction of the total gas reservoir (Abadi et al 1999;Quilis et al 2000;Schulz & Struck 2001;Tonnesen et al 2007;Roediger & Brüggen 2007;Lotz et al 2019) can be efficiently stripped on relatively short timescales compared to the typical crossing time within a cluster (∼ 2 Gyr; see however Bahé & McCarthy (2015)).…”

Section: Timescales For Stripping and Quenchingmentioning

confidence: 99%

Ram Pressure Stripping in High-Density Environments

Boselli,

Fossati,

Sun

2021

Preprint

View full text Add to dashboard Cite

Galaxies living in rich environments are suffering different perturbations able to drastically affect their evolution. Among these, ram pressure stripping, i.e. the pressure exerted by the hot and dense intracluster medium (ICM) on galaxies moving at high velocity within the cluster gravitational potential well, is a key process able to remove their interstellar medium (ISM) and quench their activity of star formation. This review is aimed at describing this physical mechanism in different environments, from rich clusters of galaxies to loose and compact groups. We summarise the effects of this perturbing process on the baryonic components of galaxies, from the different gas phases (cold atomic and molecular, ionised, hot) to magnetic fields and cosmic rays, and describe their induced effects on the different stellar populations, with a particular attention to its role in the quenching episode generally observed in high density environments. We also discuss on the possible fate of the stripped material once removed from the perturbed galaxies and mixed with the ICM, and we try to estimate its contribution to the pollution of the surrounding environment. Finally, combining the results of local and high redshift observations with the prediction of tuned models and simulations, we try to quantify the importance of this process on the evolution of galaxies of different mass, from dwarfs to giants, in various environments and at different epochs.

show abstract

“…Groups are an important regime for studies of environmental quenching since the majority of galaxies in the local Universe reside in galaxy groups, and previous works have shown that star formation quenching in groups prior to accretion onto galaxy clusters (known as 'pre-processing') may account for a substantial portion of the cluster red sequence (e.g. Fujita 2004;McGee et al 2009;von der Linden et al 2010;Haines et al 2015;Roberts & Parker 2017;Pallero et al 2020). There are ∼10 times more galaxies in groups than clusters at low-z (e.g.…”

Section: Prospects For Automated Selection Of Lotss Jellyfish Galaxiesmentioning

confidence: 99%

LoTSS jellyfish galaxies: I. Radio tails in low redshift clusters

Roberts,

van Weeren,

McGee

et al. 2021

Preprint

View full text Add to dashboard Cite

Context. The cluster environment has a strong impact on galaxy star formation, as seen by the fact that clusters host proportionally more red, passive galaxies relative to the field. Ram pressure stripping may drive this environmental quenching by directly stripping cold gas from galactic disks. In some cases, ram pressure stripping gives rise to 'jellyfish galaxies', observed with clear 'tentacles' of stripped gas extending beyond the optical extent of the galaxy. Aims. In this paper we present a large sample of jellyfish galaxies in low redshift clusters (z < 0.05), identified through 120-168 MHz radio continuum from the LOFAR Two-metre Sky Survey (LoTSS). Methods. From a parent sample of 29 X-ray-detected SDSS galaxy clusters and their spectroscopic members, we visually identify 95 star-forming, LoTSS jellyfish galaxies with 144 MHz radio tails. Star formation rates (SFRs) and stellar masses are obtained for all galaxies from SED fits. For each jellyfish galaxy we determine the tail orientation with respect to the cluster centre and quantify the prominence of the radio tails with the 144 MHz shape asymmetry. Results. After carefully accounting for redshift-dependent selection effects, we find that the frequency of jellyfish galaxies is relatively constant from cluster to cluster. LoTSS jellyfish galaxies are preferentially found at small clustercentric radius and large velocity offsets within their host clusters and have radio tails that are oriented away from the cluster centre. These galaxies also show enhanced star formation, relative to both 'normal' cluster galaxies and isolated field galaxies, but generally fall within the scatter of the L 144MHz − SFR relation. Conclusions. The properties of the LoTSS jellyfish galaxies identified in this work are fully consistent with expectations from ram pressure stripping. This large sample of jellyfish galaxies will be valuable for further constraining ram pressure stripping and star formation quenching in nearby galaxy clusters. We show that LOFAR is a powerful instrument for identifying ram pressure stripped galaxies across extremely wide fields. Moving forward we will push the search for jellyfish galaxies beyond this initial cluster sample, including a comprehensive survey of the galaxy group regime.

show abstract

Too dense to go through: The importance of low-mass clusters for satellite quenching

Cited by 8 publications

References 52 publications

Simulating Groups and the IntraGroup Medium: The Surprisingly Complex and Rich Middle Ground between Clusters and Galaxies

Simulating Groups and the IntraGroup Medium: The Surprisingly Complex and Rich Middle Ground between Clusters and Galaxies

Ram Pressure Stripping in High-Density Environments

LoTSS jellyfish galaxies: I. Radio tails in low redshift clusters

Contact Info

Product

Resources

About