Star formation quenching in the infall region around galaxy clusters

Salerno, Juán Manuel; Muriel, H.; Coenda, Valeria; Cora, S. A.; Pereyra, Luis; Ruiz, Andrés N.; Vega-Martínez, Cristian A

doi:10.1093/mnras/stac2980

Cited by 5 publications

(2 citation statements)

References 112 publications

(101 reference statements)

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“…This is an underrated, but important way in which galaxies can be pre-processed prior to entering the clusters [e.g. [7][8][9][10][11].…”

Section: Jcap02(2024)051mentioning

confidence: 99%

An AstroSat/UVIT study of galaxies in the cluster Abell 2199

Mahajan,

Singh,

Raychaudhury

2024

J. Cosmol. Astropart. Phys.

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We present the newly acquired data for an AstroSat/UVIT field centred on a face-on spiral starburst galaxy UGC 10420, located in the X-ray bright cluster Abell 2199 (z = 0.031). We have analysed the FUV BaF2 data for this field along with the archival FUV and NUV data from the GALEX mission, optical photometric data from the SDSS, spectroscopic data from the literature, and low-frequency radio data from the LoTSS survey, respectively. The stars were separated from the galaxies using the SDSS photometric pipeline classification, while the spectroscopic redshifts available for 35% of the detected UVIT sources were used to identify member galaxies of the cluster Abell 2199. We find that (a) the non-cluster galaxies are on average fainter than the cluster galaxies at fixed magnitude, (b) stars and galaxies are indistinguishable in the r vs. NUV–r plane, and (c) bright stars are ∼ 1.5 mag bluer than the galaxies in the FUV–r vs. NUV–r colour-colour plane. Besides UGC 10420 which is the only known cluster galaxy with an extended-UV disk, we identify five more galaxies with asymmetric FUV morphology and extended radio emission in this field. All the asymmetric member galaxies of Abell 2199, lie within the virial boundaries of the cluster. This observation, together with the fact that these asymmetric cluster galaxies have low-frequency radio tails or FUV emission pointing away from the cluster centre leads us to hypothesise that these galaxies are likely undergoing ram-pressure stripping (RPS) under the influence of cluster-environment related mechanisms. A comparison of optical and FUV star formation rate of UVIT detected galaxies shows enhanced star formation in half of the RPS candidates, suggesting that environment-related mechanisms may lead to a burst of star formation in RPS galaxies. Our analysis indicates the presence of at least two more groups or clusters at z ∼ 0.077 and 0.260, coincident with Abell 2199 along the line of sight of the field of view studied here.

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“…This is an underrated, but important way in which galaxies can be pre-processed prior to entering the clusters [e.g. [7][8][9][10][11].…”

Section: Jcap02(2024)051mentioning

confidence: 99%

An AstroSat/UVIT study of galaxies in the cluster Abell 2199

Mahajan,

Singh,

Raychaudhury

2024

J. Cosmol. Astropart. Phys.

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“…The decreasing number fraction of quenched fractions after infall for more massive hosts indicates that there are more pre-processed satellites in the more massive hosts (e.g., Hou et al 2014;van der Burg et al 2018;Bahé et al 2019). Because satellites in more massive hosts can have more massive infalling groups than less massive hosts (e.g., Hou et al 2014;van der Burg et al 2018;Sarron et al 2019;Donnari et al 2021a), they are more likely to be quenched than those in lowmass hosts (e.g., Reeves et al 2023;Salerno et al 2022). Indeed, among the total number of quenched satellites, 25.8% of those in low-mass hosts and 50.2% of those in high-mass hosts are members of other structures when they fall into the final low-and high-mass hosts (e.g., Han et al 2018;Donnari et al 2021a).…”

Section: The Effects Of Pre-and Post-processing On the Quenched Fractionmentioning

confidence: 99%

Galaxy Quenching with Mass Growth History of Galaxy Groups and Clusters: The Importance of Post-processing

Park,

Chun,

Shin

et al. 2023

ApJ

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We investigate the fraction of quenched satellite galaxies in host galaxy groups and clusters using TNG300 in the IllustrisTNG cosmological magnetohydrodynamical simulations. The simulations show that most satellites are quenched after they fall into their final hosts, and that post-processing is a more dominant mechanism of galaxy quenching than pre-processing. We find that the fraction of quenched satellites at z = 0 increases with host mass, which implies that more massive hosts have higher quenching efficiency because they have more massive groups infalling. Furthermore, we find that hosts that have many early-infall satellites show a higher fraction of quenched satellites at z = 0 than those that have many late-infall satellites, which results in a scatter of the quenched fraction of satellites in a given mass range of hosts at z = 0. Our results highlight the significance of the mass of hosts and the different infall times of satellites in understanding galaxy quenching.

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When the well runs dry: modelling environmental quenching of high-mass satellites in massive clusters at z ≳ 1

Baxter,

Cooper,

Balogh

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We explore models of massive (>1010 M⊙) satellite quenching in massive clusters at z ≳ 1 using an MCMC framework, focusing on two primary parameters: Rquench (the host-centric radius at which quenching begins) and τquench (the time-scale upon which a satellite quenches after crossing Rquench). Our MCMC analysis shows two local maxima in the 1D posterior probability distribution of Rquench at approximately 0.25 and 1.0 R200. Analysing four distinct solutions in the τquench–Rquench parameter space, nearly all of which yield quiescent fractions consistent with observational data from the GOGREEN survey, we investigate whether these solutions represent distinct quenching pathways and find that they can be separated between ‘starvation’ and ‘core quenching’ scenarios. The starvation pathway is characterized by quenching time-scales that are roughly consistent with the total cold gas (H2 + H i) depletion time-scale at intermediate z, while core quenching is characterized by satellites with relatively high line-of-sight velocities that quench on short time-scales (∼0.25 Gyr) after reaching the inner region of the cluster (<0.30 R200). Lastly, we break the degeneracy between these solutions by comparing the observed properties of transition galaxies from the GOGREEN survey. We conclude that only the ‘starvation’ pathway is consistent with the projected phase-space distribution and relative abundance of transition galaxies at z ∼ 1. However, we acknowledge that ram pressure might contribute as a secondary quenching mechanism.

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Star formation quenching in the infall region around galaxy clusters

Cited by 5 publications

References 112 publications

An AstroSat/UVIT study of galaxies in the cluster Abell 2199

An AstroSat/UVIT study of galaxies in the cluster Abell 2199

Galaxy Quenching with Mass Growth History of Galaxy Groups and Clusters: The Importance of Post-processing

When the well runs dry: modelling environmental quenching of high-mass satellites in massive clusters at z ≳ 1

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