The Roles of Mass and Environment in the Quenching of Galaxies

Contini, E.; Gu, Qiusheng; Kang, Xi; Rhee, Jinsu; Yi, Sukyoung K.

doi:10.3847/1538-4357/ab3b03

Cited by 14 publications

(12 citation statements)

References 83 publications

(136 reference statements)

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“…For instance, for what concerns the environmental quenching, when we look at the dependence of the SFR or SSFR on the environment since redshift z ∼ 1 (when the environment is believed to play a remarkable role), we find no dependence (see, e.g. Muzzin et al 2012;Laganá & Ulmer 2018;Contini et al 2019b, and references therein for many other works supporting it), which either means that the environment does not play an important role or it acts so fast such that it does not influence the star formation of active galaxies but increases the fraction of quiescent galaxies. Many other studies (e.g., van den Bosch et al 2008;Quadri et al 2012;Omand et al 2014;Balogh et al 2016;Nantais et al 2016;Darvish et al 2016;Fossati et al 2017;Jian et al 2017;Kawinwanichakij et al 2017;van der Burg et al 2018;Papovich et al 2018;Pintos-Castro et al 2019), which have looked at the efficiencies of the environmental and mass quenching, have been able to quantify the two quenching modes, albeit with different results in terms of mutual dependence among the two modes, redshift, stellar mass and halo mass dependence.…”

Section: Introductionmentioning

confidence: 95%

“…In Contini et al (2019b) (hereafter PapI) we took advantage of an analytic model of galaxy formation that was tuned to match the observed evolution of the stellar mass function from redshift z ∼ 2.3 down to the present time and give a reasonable prediction of the evolution of the SFR-M * relation in the same redshift range, to investigate galaxy quenching by looking at the SFR and SSFR of star forming and quiescent galaxies as a function of both stellar mass and environment. Our goal was mainly to understand the roles of environmental and mass quenching at different redshifts.…”

Section: Introductionmentioning

confidence: 99%

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The Roles of Mass and Environment in the Quenching of Galaxies. II.

Contini

Kang

et al. 2020

ApJ

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We take advantage of an analytic model of galaxy formation coupled to the merger tree of an N-body simulation to study the roles of environment and stellar mass in the quenching of galaxies. The model has been originally set in order to provide the observed evolution of the stellar mass function as well as reasonable predictions of the star formation rate-stellar mass relation, from high redshift to the present time. We analyse the stellar mass and environmental quenching efficiencies and their dependence on stellar mass, halo mass (taken as a proxy for the environment) and redshift. Our analysis shows that the two quenching efficiencies are redshift, stellar and halo mass dependent, and that the halo mass is also a good proxy for the environment. The environmental quenching increases with decreasing redshift and is inefficient below log M * ∼ 9.5, reaches the maximum value at log M * ∼ 10.5, and decreases again, becoming poorly efficient at very high stellar mass (log M * 11.5). Central and satellites galaxies are mass quenched differently: for the former, the quenching efficiency depends very weakly on redshift, but strongly on stellar mass; for the latter, it strongly depends on both stellar mass and redshift in the range 10 log M * 11. According to the most recent observational results, we find that the two quenching efficiencies are not separable: intermediate mass galaxies are environmental quenched faster, as well as intermediate/massive galaxies in more massive haloes. At stellar masses lower than log M * 9.5 both quenching mechanisms become inefficient, independently of the redshift.

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Section: Introductionmentioning

confidence: 95%

Section: Introductionmentioning

confidence: 99%

The Roles of Mass and Environment in the Quenching of Galaxies. II.

Contini

Kang

et al. 2020

ApJ

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“…Cosmological simulations are a powerful tool that allows us to disentangle the effects associated with the different processes that are typically coupled in a non-linear fashion. In the last years, analytic models (Fujita 2004;Mok et al 2014;Contini et al 2020), semi-analytic (De Lucia et al 2012;Wetzel et al 2013;Henriques et al 2017;Stevens & Brown 2017;Cora et al 2018;Contini et al 2019) and hydrodynamical simulations (e.g. Bahé et al 2013;Bahé & McCarthy 2015;Taylor et al 2017;Wright et al 2019;Pallero et al 2019;Donnari et al 2020) have allowed us to explore the relative importance of the different mechanisms that bring a galaxy to a final quenched state.…”

Section: Introductionmentioning

confidence: 99%

Too dense to go through: the role of low-mass clusters in the pre-processing of satellite galaxies

Pallero

Gómez

Padilla

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We study the evolution of satellite galaxies in clusters of the C-EAGLE simulations, a suite of 30 high-resolution cosmological hydrodynamical zoom-in simulations based on the EAGLE code. We find that the majority of galaxies that are quenched at z = 0 (≳ 80${{\ \rm per\ cent}}$) reached this state in a dense environment (log10M200[M⊙] ≥13.5). At low redshift, regardless of the final cluster mass, galaxies appear to reach their quenching state in low mass clusters. Moreover, galaxies quenched inside the cluster that they reside in at z = 0 are the dominant population in low-mass clusters, while galaxies quenched in a different halo dominate in the most massive clusters. When looking at clusters at z > 0.5, their in-situ quenched population dominates at all cluster masses. This suggests that galaxies are quenched inside the first cluster they fall into. After galaxies cross the cluster’s r200 they rapidly become quenched (≲ 1Gyr). Just a small fraction of galaxies ($\lesssim 15{{\ \rm per\ cent}}$) is capable of retaining their gas for a longer period of time, but after 4Gyr, almost all galaxies are quenched. This phenomenon is related to ram pressure stripping and is produced when the density of the intracluster medium reaches a threshold of ρICM ∼ 3 × 10−5 nH (cm−3). These results suggest that galaxies start a rapid-quenching phase shortly after their first infall inside r200 and that, by the time they reach r500, most of them are already quenched.

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confidence: 99%

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

Pallero,

Gómez,

Padilla

et al. 2020

Preprint

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We study the evolution of satellite galaxies in clusters of the C-EAGLE simulations, a suite of 30 high-resolution cosmological hydrodynamical zoom-in simulations based on the EAGLE code. We find that the majority of galaxies that are quenched at z = 0 ( 80%) reached this state in a dense environment (log 10 M 200 [M ]≥13.5). At low redshift, regardless of the final cluster mass, galaxies appear to reach their quenching state in low mass clusters. Moreover, galaxies quenched inside the cluster that they reside in at z = 0 are the dominant population in low-mass clusters, while galaxies quenched in a different halo dominate in the most massive clusters. When looking at clusters at z > 0.5, their in-situ quenched population dominates at all cluster masses. This suggests that galaxies are quenched inside the first cluster they fall into. After galaxies cross the cluster's r 200 they rapidly become quenched ( 1Gyr). Just a small fraction of galaxies ( 15%) is capable of retaining their gas for a longer period of time, but after 4Gyr, almost all galaxies are quenched. This phenomenon is related to ram pressure stripping and is produced when the density of the intracluster medium reaches a threshold of ρ ICM ∼ 3 × 10 −5 n H (cm −3 ). These results suggest that galaxies start a rapid-quenching phase shortly after their first infall inside r 200 and that, by the time they reach r 500 , most of them are already quenched.

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The Roles of Mass and Environment in the Quenching of Galaxies

Cited by 14 publications

References 83 publications

The Roles of Mass and Environment in the Quenching of Galaxies. II.

The Roles of Mass and Environment in the Quenching of Galaxies. II.

Too dense to go through: the role of low-mass clusters in the pre-processing of satellite galaxies

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

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