The environmental dependence of rapidly quenching and rejuvenating galaxies

Cressida, Cleland,; McGee, Sean L.

doi:10.1093/mnras/staa3267

Cited by 9 publications

(6 citation statements)

References 61 publications

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“…This rejuvenation phenomenon is also discovered in the observation (e.g. Thomas et al 2010;Chauke et al 2019;Cleland & McGee 2021). It is possible that the merger or some other gas supply mechanism is responsible for that.…”

Section: Discussionsupporting

confidence: 60%

The Formation and Evolution of Massive Galaxies

Jing,

Rong,

Wang

et al. 2021

Preprint

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The discovery of massive galaxies at high redshifts, especially the passive ones, poses a big challenge for the current standard galaxy formation models. Here we use the semi-analytic galaxy formation model developed by Henriques et al. to explore the formation and evolution of massive galaxies (MGs, stellar-mass M * > 10 11 M ). Different from previous works, we focus on the ones just formed (e.g. just reach 10 11 M ). We find that most of the MGs are formed around z = 0.6, with the earliest formation at z > 4. Interestingly, although most of the MGs in the local Universe are passive, we find that only 13% of the MGs are quenched at the formation time. Most of the quenched MGs at formation already hosts a very massive supermassive black hole (SMBH) which could power the very effective AGN feedback. For the star-forming MGs, the ones with more massive SMBH prefer to quench in shorter timescales; in particular, those with M SMBH > 10 7.5 M have a quenching timescale of ∼ 0.5 Gyr and the characteristic M SMBH depends on the chosen stellar mass threshold in the definition of MGs as a result of their co-evolution. We also find that the "in-situ" star formation dominates the stellar mass growth of MGs until they are formed. Over the whole redshift range, we find the quiescent MGs prefer to stay in more massive dark matter halos, and have more massive SMBH and less cold gas masses. Our results provide a new angle on the whole life of the growth of MGs in the Universe.

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Section: Discussionsupporting

confidence: 60%

The Formation and Evolution of Massive Galaxies

Jing,

Rong,

Wang

et al. 2021

Preprint

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“…Some of them will pass away again just less than 1Gyr, while a small fraction of them will keep star formation more than a few Gyr, and even keep alive at present. This rejuvenation phenomenon is also discovered in the observation (e.g., Thomas et al 2010;Chauke et al 2019;Cleland & McGee 2021). It is possible that the merger or some other gas supply mechanism is responsible for that.…”

Section: Discussionsupporting

confidence: 59%

The formation and evolution of massive galaxies

Jing

Wang

et al. 2021

Res. Astron. Astrophys.

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The discovery of massive galaxies at high redshifts, especially the passive ones, poses a big challenge for the current standard galaxy formation models. Here we use the semi-analytic galaxy formation model developed by Henriques et al. to explore the formation and evolution of massive galaxies (MGs, stellar-mass M * > 1011 M ⊙). Different from previous works, we focus on the ones just formed (e.g. just reach ≃ 1011 M ⊙). We find that most of the MGs are formed around z = 0.6, with the earliest formation at z > 4. Interestingly, although most of the MGs in the local Universe are passive, we find that only 13% of the MGs are quenched at the formation time. Most of the quenched MGs at formation already host a very massive supermassive black hole (SMBH) which could power the very effective AGN feedback. For the star-forming MGs, the ones with more massive SMBH prefer to quench in shorter timescales; in particular, those with M SMBH > 107.5 M ⊙ have a quenching timescale of ∼ 0.5 Gyr and the characteristic M SMBH depends on the chosen stellar mass threshold in the definition of MGs as a result of their co-evolution. We also find that the “in-situ” star formation dominates the stellar mass growth of MGs until they are formed. Over the whole redshift range, we find the quiescent MGs prefer to stay in more massive dark matter halos, and have more massive SMBH and less cold gas masses. Our results provide a new angle on the whole life of the growth of MGs in the Universe.

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“…Starvation and strangulation begin earlier in ancient infallers (T > 5 Gyr; inf Pasquali et al 2019) compared to recent infallers (T < 2.5 Gyr; inf Pasquali et al 2019). Ancient infallers also tend to orbit closer to the halo center (inner orbits), where the external quenching processes are strongest (van de Voort et al 2017;Cleland & McGee 2021). Indeed, Gallazzi et al (2021) found ancient infallers to have older ages, higher…”

Section: The Environment-driven Quenching Scenariomentioning

confidence: 99%

SDSS-IV MaNGA: The Effect of Stellar Mass and Halo Mass on the Assembly Histories of Satellite Galaxies

Oyarzún

Bundy

Westfall

et al. 2023

ApJ

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We combine an unprecedented MaNGA sample of over 3000 passive galaxies in the stellar mass range 109–1012 M ⊙ with the Sloan Digital Sky Survey group catalog by Tinker to quantify how central and satellite formation, quantified by radial profiles in stellar age, [Fe/H], and [Mg/Fe], depends on the stellar mass of the galaxy (M *) and the mass of the host halo (M h ). After controlling for M * and M h , the stacked spectra of centrals and satellites beyond the effective radius (r e ) show small, yet significant differences in multiple spectral features at the 1% level. According to spectral fitting with the code alf, a primary driver of these differences appears to be [Mg/Fe] variations, suggesting that stellar populations in the outskirts of satellites formed more rapidly than the outer populations of centrals. To probe the physical mechanisms that may be responsible for this signal, we examined how satellite stellar populations depend on M h . We find that satellites in high-M h halos show older stellar ages, lower [Fe/H], and higher [Mg/Fe] compared to satellites in low-M h halos, especially for M * = 109.5–1010.5 M ⊙. These signals lend support to environmentally driven processes that quench satellite galaxies, although variations in the merger histories of central and satellite galaxies also emerge as a viable explanation.

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The environmental dependence of rapidly quenching and rejuvenating galaxies

Cited by 9 publications

References 61 publications

The Formation and Evolution of Massive Galaxies

The Formation and Evolution of Massive Galaxies

The formation and evolution of massive galaxies

SDSS-IV MaNGA: The Effect of Stellar Mass and Halo Mass on the Assembly Histories of Satellite Galaxies

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