The GOGREEN survey: constraining the satellite quenching time-scale in massive clusters at <i>z</i> ≳ 1

Baxter, Devontae C; Cooper, Michael C.; Balogh, Michael L.; Carleton, Timothy; Cerulo, P.; Lucia, G. De; Demarco, R.; McGee, Sean L.; Muzzin, Adam; Nantais, Julie; Pintos-Castro, Irene; Reeves, Andrew M. M.; Rudnick, Gregory; Sarron, Florian; Burg, R. F. J. van der; Vulcani, Benedetta; Wilson, Gillian; Zaritsky, Dennis

doi:10.1093/mnras/stac2149

Cited by 8 publications

(1 citation statement)

References 160 publications

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“…Most commonly, the quenching time has been defined as the period for which a satellite remains star forming after infall into its host halo (Rocha et al 2012;Weisz et al 2015;Foltz et al 2018). Other studies define quenching time as the time at which the specific star formation rate falls below 10 −11 yr −1 (Akins et al 2021) or use both (Baxter et al 2022). However, in this work, we choose to use the time at which a galaxy had formed 90% of its present-day stellar mass, τ 90 , as our definition of quenching time.…”

Section: % 15%mentioning

confidence: 99%

Devouring the Centaurus A Satellites: Modeling Dwarf Galaxies with Galacticus

Weerasooriya,

Bovill,

Taylor

et al. 2024

ApJ

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For the first time, systematic studies of dwarf galaxies are being conducted throughout the Local Volume, including the dwarf satellites of the nearby giant elliptical galaxy Centaurus A (NGC 5128). Given Centaurus A's mass (roughly 10 times larger than that of the Milky Way), AGN activity, and recent major mergers, investigating the dwarf galaxies of Centaurus A and their star formation physics is imperative. However, simulating the faintest dwarfs around a galaxy of Centaurus A's mass with sufficient resolution in a hydrodynamic simulation is computationally expensive and currently infeasible. In this study, we seek to reproduce the properties of Centaurus A dwarfs using the semianalytic model Galacticus to model dwarfs within a 700 kpc region around Centaurus A, corresponding approximately to its splashback radius. We investigate the effects of host halo mass and environment and predict observable properties of Centaurus A dwarfs using astrophysical prescriptions and parameters previously tuned to match properties of the Milky Way’s satellite galaxies. This approach allows us to approximately replicate cumulative luminosity functions, and luminosity–metallicity and luminosity–half-light-radii relations observed in the Centaurus A satellites. We provide predictions for the velocity dispersions, and star formation histories of Centaurus A dwarfs. The agreement between our predicted star formation histories for Centaurus A dwarfs and those of the Milky Way dwarfs implies the presence of universal processes governing star formation in dwarf galaxies. Overall, our findings shed light on the star formation physics of dwarf galaxies in the Centaurus A system, revealing insights into their properties and dependence on the host environment.

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Section: % 15%mentioning

confidence: 99%

Devouring the Centaurus A Satellites: Modeling Dwarf Galaxies with Galacticus

Weerasooriya,

Bovill,

Taylor

et al. 2024

ApJ

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Galaxy populations in the most distant SPT-SZ clusters

Strazzullo

Pannella

Mohr

et al. 2023

A&A

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We investigate structural properties of massive galaxy populations in the central regions (< 0.7r 500 ) of five very massive (M 200 > 4 × 10 14 M ⊙ ), high-redshift (1.4 ≲ z ≲ 1.7) galaxy clusters from the 2500 deg 2 South Pole Telescope Sunyaev Zel'dovich effect (SPT-SZ) survey. We probe the connection between galaxy structure and broad stellar population properties at stellar masses of log(M/M ⊙ )>10.85. We find that quiescent and star-forming cluster galaxy populations are largely dominated by bulge-and diskdominated sources, respectively, with relative contributions being fully consistent with those of field counterparts. At the same time, the enhanced quiescent galaxy fraction observed in these clusters with respect to the coeval field is reflected in a significant morphology-density relation, with bulge-dominated galaxies already clearly dominating the massive galaxy population in these clusters at z ∼ 1.5. At face value, these observations show no significant environmental signatures in the correlation between broad structural and stellar population properties. In particular, the Sersic index and axis ratio distribution of massive, quiescent sources are consistent with field counterparts, in spite of the enhanced quiescent galaxy fraction in clusters. This consistency suggests a tight connection between quenching and structural evolution towards a bulge-dominated morphology, at least in the probed cluster regions and galaxy stellar mass range, irrespective of environment-related processes affecting star formation in cluster galaxies. We also probe the stellar mass -size relation of cluster galaxies, and find that star-forming and quiescent sources populate the mass-size plane in a manner largely similar to their field counterparts, with no evidence of a significant size difference for any probed sub-population. In particular, both quiescent and bulge-dominated cluster galaxies have average sizes at fixed stellar mass consistent with their counterparts in the field.

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The relationship between cluster environment and molecular gas content of star-forming galaxies in the eagle simulation

Manuwal

Stevens

2023

Monthly Notices of the Royal Astronomical Society

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We employ the eagle hydrodynamical simulation to uncover the relationship between cluster environment and H2 content of star-forming galaxies at redshifts spanning 0 ≤ z ≤ 1. To do so, we divide the star-forming sample into those that are bound to clusters and those that are not. We find that, at any given redshift, the galaxies in clusters generally have less H2 than their non-cluster counterparts with the same stellar mass (corresponding to an offset of ≲ 0.5 dex), but this offset varies with stellar mass and is virtually absent at M⋆ ≲ 109.3 M⊙. The H2 deficit in star-forming cluster galaxies can be traced back to a decline in their H2 content that commenced after first infall into a cluster, which occurred later than a typical cluster galaxy. Evolution of the full cluster population after infall is generally consistent with ‘slow-then-rapid’ quenching, but galaxies with M⋆ ≲ 109.5 M⊙ exhibit rapid quenching. Unlike most cluster galaxies, star-forming ones were not pre-processed in groups prior to being accreted by clusters. For both of these cluster samples, the star formation efficiency remained oblivious to the infall. We track the particles associated with star-forming cluster galaxies and attribute the drop in H2 mass after infall to poor replenishment, depletion due to star formation, and stripping of H2 in cluster environments. These results provide predictions for future surveys, along with support and theoretical insights for existing molecular gas observations that suggest there is less H2 in cluster galaxies.

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The GOGREEN survey: constraining the satellite quenching time-scale in massive clusters at z ≳ 1

Cited by 8 publications

References 160 publications

Devouring the Centaurus A Satellites: Modeling Dwarf Galaxies with Galacticus

Devouring the Centaurus A Satellites: Modeling Dwarf Galaxies with Galacticus

Galaxy populations in the most distant SPT-SZ clusters

The relationship between cluster environment and molecular gas content of star-forming galaxies in the eagle simulation

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