Quenching Low-mass Satellite Galaxies: Evidence for a Threshold ICM Density

Roberts, Ian; Parker, Laura C.; Brown, Toby; Joshi, Gandhali D.; Hlavacek-Larrondo, J.; Wadsley, James

doi:10.3847/1538-4357/ab04f7

Cited by 60 publications

(65 citation statements)

References 127 publications

(174 reference statements)

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“…This fact is known as the environmental quenching of galaxy star formation, which has been firmly established in the nearby Universe (e.g. Dressler 1980;Blanton & Moustakas 2009;Peng et al 2010;Wetzel et al 2012;Haines et al 2015;Roberts et al 2019) and also observed out to z ∼ 1 and beyond (e.g. Muzzin et al 2014;Foltz et al 2018;Ji et al 2018;Old et al 2020).…”

Section: Introductionmentioning

confidence: 92%

“…Despite RPS being a mechanism to quench galaxies (e.g. Gunn & Gott 1972;Quilis et al 2000;Roediger & Hensler 2005;Bekki 2009;Steinhauser et al 2016;Roberts et al 2019), star formation may be briefly enhanced during the early stages of the ram pressure interaction, as predicted by simulations (e.g. Bekki & Couch 2003;Steinhauser et al 2012;Troncoso Iribarren et al 2016Ramos-Martínez et al 2018) and seen in observations (e.g.…”

Section: Introductionmentioning

confidence: 98%

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LoTSS jellyfish galaxies

Roberts

Weeren

McGee

et al. 2021

A&A

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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 L144 MHz − 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.

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Section: Introductionmentioning

confidence: 92%

Section: Introductionmentioning

confidence: 98%

LoTSS jellyfish galaxies

Roberts

Weeren

McGee

et al. 2021

A&A

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“…External processes or environmental quenching are due to stripping away galactic gas by the ram pressure from a cluster's or group's hot gas (Gunn & Gott 1972;McCarthy et al 2008;Roberts et al 2019;Yun et al 2019), cold gas removal by viscous stripping (Nulsen 1982), starvation due to the prevention of fresh gas from reaching galaxies by removal their feeding primordial filaments (Aragon Calvo et al 2019;Maier et al 2019), harassment due to multiple high-speed mergers (Moore et al 1996). External processes depend on environmental densities, on galaxy orbital properties, and also on galaxy masses.…”

Section: Introductionmentioning

confidence: 99%

Multiscale cosmic web detachments, connectivity, and preprocessing in the supercluster SCl A2142 cocoon

Einasto

Deshev

Tenjes

et al. 2020

A&A

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Context. Superclusters of galaxies and their surrounding low-density regions (cocoons) represent dynamically evolving environments in which galaxies and their systems form and evolve. While evolutionary processes of galaxies in dense environments are extensively studied at present, galaxy evolution in low-density regions has received less attention. Aims. We study the properties, connectivity, and galaxy content of groups and filaments in the A2142 supercluster (SCl A2142) cocoon to understand the evolution of the supercluster with its surrounding structures and the galaxies within them. Methods. We calculated the luminosity-density field of SDSS galaxies and traced the SCl A2142 cocoon boundaries by the lowest luminosity-density regions that separate SCl A2142 from other superclusters. We determined galaxy filaments and groups in the cocoon and analysed the connectivity of groups, the high density core (HDC) of the supercluster, and the whole of the supercluster. We compared the distribution and properties of galaxies with different star-formation properties in the supercluster and in the cocoon. Results. The supercluster A2142 and the long filament that is connected to it forms the longest straight structure in the Universe detected so far, with a length of approximately 75 h −1 Mpc. The connectivity of the cluster A2142 and the whole supercluster is C = 6 − 7; poor groups exhibit C = 1 − 2. Long filaments around the supercluster's main body are detached from it at the turnaround region. Among various local and global environmental trends with regard to the properties of galaxies and groups, we find that galaxies with very old stellar populations lie in systems across a wide range of richness from the richest cluster to poorest groups and single galaxies. They lie even at local densities as low as D1 < 1 in the cocoon and up to D1 > 800 in the supercluster. Recently quenched galaxies lie in the cocoon mainly in one region and their properties are different in the cocoon and in the supercluster. The star-formation properties of single galaxies are similar across all environments. Conclusions. The collapsing main body of SCl A2142 with the detached long filaments near it are evidence of an important epoch in the supercluster evolution. There is a need for further studies to explore possible reasons behind the similarities between galaxies with very old stellar populations in extremely different environments, as well as mechanisms for galaxy quenching at very low densities. The presence of long, straight structures in the cosmic web may serve as a test for cosmological models.

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“…The stellar mass trend indicates that massive galaxies can be significantly self-quenched prior to their infall into clusters. Cumulative mass quenching for those galaxies or gas depletion with a short timescale in more massive galaxies (e.g., Boselli et al 2014a;Saintonge et al 2017) might be the main contributor (e.g., Roberts et al 2019). Moreover, the values of ex-situ-quenching timescale are generally lower than those of field samples, likely indicating the role of pre-processing at play in the galaxy group environments.…”

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confidence: 97%

YZiCS: Unveiling the Quenching History of Cluster Galaxies Using Phase-space Analysis

Rhee

Smith

Choi

et al. 2020

ApJS

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We used the time since infall (TSI) of galaxies, obtained from the Yonsei Zoom-in Cluster Simulation, and the star formation rate (SFR) from the Sloan Digital Sky Survey (SDSS) Data Release 10 to study how quickly star formation of disk galaxies is quenched in cluster environments. We first confirm that both simulated and observed galaxies are consistently distributed in phase space. We then hypothesize that the TSI and SFR are causally connected; thus, both the TSI and SFR of galaxies at each position of phase space can be associated through abundance matching. Using a flexible model, we derive the star formation history (SFH) of cluster galaxies that best reproduces the relationship between the TSI and SFR at z ∼ 0.08. According to this SFH, we find that the galaxies with M * > 10 9.5 M generally follow the so-called "delayed-then-rapid" quenching pattern. Our main results are as following: (i) Part of the quenching takes place outside clusters through mass quenching and pre-processing. The e-folding timescale of this "ex-situ quenching phase" is roughly 3 Gyr with a strong inverse mass dependence. (ii) The pace of quenching is maintained roughly for 2 Gyr ("delay time") during the first crossing time into the cluster. During the delay time, quenching remains gentle probably because gas loss happens primarily on hot and neutral gases. (iii) Quenching becomes more dramatic (e-folding timescale of roughly 1 Gyr) after delay time, probably because ram pressure stripping is strongest near the cluster center. Counter-intuitively, more massive galaxies show shorter quenching timescales mainly because they enter their clusters with lower gas fractions due to ex-situ quenching.

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Quenching Low-mass Satellite Galaxies: Evidence for a Threshold ICM Density

Cited by 60 publications

References 127 publications

LoTSS jellyfish galaxies

LoTSS jellyfish galaxies

Multiscale cosmic web detachments, connectivity, and preprocessing in the supercluster SCl A2142 cocoon

YZiCS: Unveiling the Quenching History of Cluster Galaxies Using Phase-space Analysis

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