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

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

doi:10.3847/1538-4357/ab6730

Cited by 40 publications

(35 citation statements)

References 69 publications

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“…Alternately, this could be interpreted in terms of the quenching timescale, suggesting that massive satellites quench earlier than their lower mass counterparts. We note that this interpretation is at least qualitatively consistent 7 with those of Wetzel et al (2013); Rhee et al (2020), who also suggest a shorter quenching timescale for massive satellites (see also Contini et al 2020, who found similar results for cluster satellites at higher redshift).…”

Section: Quenching In the Coma Clustersupporting

confidence: 90%

Star formation histories of Coma cluster galaxies matched to simulated orbits hint at quenching around first pericenter

Upadhyay

Oman

Trager

2021

A&A

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Context. The star formation in galaxies in present-day clusters has almost entirely been shut down, but the exact mechanism that quenched these galaxies is still uncertain. Aims. By tracing the orbital and star formation histories of galaxies within the Coma cluster, we seek to understand the role of the high-density cluster environment in quenching these galaxies. Methods. We combine star formation histories extracted from high-signal-to-noise spectra of 11 early-type galaxies around the center of the Coma cluster with probability distributions for their orbital parameters obtained using an N-body simulation to connect their orbital and star formation histories. Results. We find that all 11 galaxies likely quenched near their first pericentric approach. Higher stellar mass galaxies (log(M⋆/M⊙) > 10) had formed a higher fraction of their stellar mass (more than ∼90%) than their lower mass counterparts (∼80−90%) by the time they fell into the cluster (when they cross 2.5rvir). We find that the expected infall occurred around z ∼ 0.6, followed by the first pericentric passage ∼4 Gyr later. Galaxies in our sample formed a significant fraction of their stellar mass, up to 15%, between infall and first pericenter, and had assembled more than ∼98% of their cumulative stellar mass by first pericenter. Conclusions. Unlike previous low-redshift studies that suggest that star formation continues until about first apocenter or later, the high percentage of stellar mass already formed by first pericenter in our sample galaxies points to star formation ceasing within a gigayear after the first pericentric passage. We consider the possible physical mechanisms driving quenching and find that our results resemble the situation in clusters at z ∼ 1, where active stripping of gas (ram-pressure or tidally driven) seems to be required to quench satellites by their first pericentric passage. However, a larger sample will be required to conclusively account for the unknown fraction of preprocessed satellites in the Coma cluster.

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Section: Quenching In the Coma Clustersupporting

confidence: 90%

Star formation histories of Coma cluster galaxies matched to simulated orbits hint at quenching around first pericenter

Upadhyay

Oman

Trager

2021

A&A

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“…Figure 9 shows that the stellar masses for BSF galaxies with logM * = 10.2 are lower than those of RQ galaxies, which have logM * = 10.6. According to models by Contini et al (2020), environmental quenching efficiencies for these masses are 0.5 and 0.6, respectively. This means that the mass quenching efficiency is similarly low for both.…”

Section: Galaxy Evolution In the Supercluster And In The Cocoonmentioning

confidence: 99%

“…External processes depend on environmental densities, on galaxy orbital properties, and also on galaxy masses. They are most effective at lower redshifts and for intermediate mass galaxies (Contini et al 2020). Tidal interactions between galaxies are external processes and they can transform the morphology of galaxies significantly.…”

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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“…There is evidence that the quenching processes that are driven by mass and environment are largely separable, at least in the local (z 1) Universe (Baldry et al 2006;Peng et al 2010;Muzzin et al 2012;Kovač et al 2014;Guglielmo et al 2015;van der Burg et al 2018). This is to say that there are no cross-terms; the effectiveness of environmental quenching does not depend on stellar mass, and the self/mass-quenching itself does not depend on the environment (but for different interpretations, see De Lucia et al 2012;Contini et al 2020). We note that the separability of these processes does not mean that they are physically unrelated processes; galaxies may quench due to shock heating of their cold gas component due to interactions with the hot (host) halo; this is generally referred to as "halo quenching", a process that may become efficient for both centrals and satellites in host-haloes M halo 10 12 M (Dekel & Birnboim 2006;Cattaneo et al 2008).…”

Section: Introductionmentioning

confidence: 99%

The GOGREEN Survey: A deep stellar mass function of cluster galaxies at 1.0 < z < 1.4 and the complex nature of satellite quenching

Burg

Rudnick

Balogh

et al. 2020

A&A

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We study the stellar mass functions (SMFs) of star-forming and quiescent galaxies in 11 galaxy clusters at 1.0 < z < 1.4 drawn from the Gemini Observations of Galaxies in Rich Early ENvironments (GOGREEN) survey. Based on more than 500 h of Gemini/GMOS spectroscopy and deep multi-band photometry taken with a range of observatories, we probe the SMFs down to a stellar mass limit of 109.7 M⊙ (109.5 M⊙ for star-forming galaxies). At this early epoch, the fraction of quiescent galaxies is already highly elevated in the clusters compared to the field at the same redshift. The quenched fraction excess (QFE) represents the fraction of galaxies that would be star-forming in the field but are quenched due to their environment. The QFE is strongly mass dependent, and increases from ∼30% at M⋆ = 109.7 M⊙ to ∼80% at M⋆ = 1011.0 M⊙. Nonetheless, the shapes of the SMFs of the two individual galaxy types, star-forming and quiescent galaxies, are identical between cluster and field to high statistical precision. Nevertheless, along with the different quiescent fractions, the total galaxy SMF is also environmentally dependent, with a relative deficit of low-mass galaxies in the clusters. These results are in stark contrast with findings in the local Universe, and therefore require a substantially different quenching mode to operate at early times. We discuss these results in light of several popular quenching models.

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

Cited by 40 publications

References 69 publications

Star formation histories of Coma cluster galaxies matched to simulated orbits hint at quenching around first pericenter

Star formation histories of Coma cluster galaxies matched to simulated orbits hint at quenching around first pericenter

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

The GOGREEN Survey: A deep stellar mass function of cluster galaxies at 1.0 < z < 1.4 and the complex nature of satellite quenching

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