Can Supernovae Quench Star Formation in High-z Galaxies?

Gelli, Viola; Salvadori, Stefania; Ferrara, Andrea; Pallottini, Andrea

doi:10.3847/1538-4357/ad23ec

Cited by 6 publications

(2 citation statements)

References 38 publications

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“…The choice of feedback model has also been shown to impact the overall size-mass relation at low masses (e.g., Pillepich et al 2018), with the caveat that the sample is not separated into star-forming and quiescent populations. At higher redshifts, supernovae have been proposed as potential drivers of low-mass galaxy quenching, though they have been shown to not impart sufficient energy to halt star formation in the Looser et al (2024) or Strait et al (2023) high-redshift mini-quenched galaxy candidates (Gelli et al 2024(Gelli et al , 2023. Quenching via environmental interactions would result in minimal structural changes to the stellar light of low-mass galaxies, while stellar feedback quenching makes galaxies larger (Übler et al 2014).…”

Section: Structural Evolution At Low Massesmentioning

confidence: 99%

Two Distinct Classes of Quiescent Galaxies at Cosmic Noon Revealed by JWST PRIMER and UNCOVER

Cutler,

Whitaker,

Weaver

et al. 2024

ApJL

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We present a measurement of the low-mass quiescent size–mass relation at cosmic noon (1 < z < 3) from the JWST PRIMER and UNCOVER treasury surveys, which highlights two distinct classes of quiescent galaxies. While the massive population is well studied at these redshifts, the low-mass end has been previously underexplored due to a lack of observing facilities with sufficient sensitivity and spatial resolution. We select a conservative sample of low-mass quiescent galaxy candidates using rest-frame UVJ colors and specific star formation rate criteria and measure galaxy morphology in both rest-frame UV/optical wavelengths (F150W) and rest-frame near-infrared (F444W). We confirm an unambiguous flattening of the low-mass quiescent size–mass relation, which results from the separation of the quiescent galaxy sample into two distinct populations at log ( M ⋆ / M ⊙ ) ∼ 10.3 : low-mass quiescent galaxies that are notably younger and have disky structures, and massive galaxies consistent with spheroidal morphologies and older median stellar ages. These separate populations imply mass quenching dominates at the massive end while other mechanisms, such as environmental or feedback-driven quenching, form the low-mass end. This stellar mass-dependent slope of the quiescent size–mass relation could also indicate a shift from size growth due to star formation (low masses) to growth via mergers (massive galaxies). The transition mass between these two populations also corresponds with other dramatic changes and characteristic masses in several galaxy evolution scaling relations (e.g., star formation efficiency, dust obscuration, and stellar-to-halo mass ratios), further highlighting the stark dichotomy between low-mass and massive galaxy formation.

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Section: Structural Evolution At Low Massesmentioning

confidence: 99%

Two Distinct Classes of Quiescent Galaxies at Cosmic Noon Revealed by JWST PRIMER and UNCOVER

Cutler,

Whitaker,

Weaver

et al. 2024

ApJL

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“…Quenching could be caused by internal feedback from active galactic nuclei (AGN) and supernova (SN) feedback or by external physical processes including galaxy-galaxy interactions and environmental stripping. With a minimal physical model, Gelli et al (2023) suggests that SN feedback is not powerful enough to quench galaxies of ∼10 8 M e at high redshift. The fact that many high-z quenched galaxies are found to host luminous AGN (Ito et al 2022;Carnall et al 2023b;Belli et al 2023;D'Eugenio et al 2023;Davies et al 2024;Shimakawa et al 2024) suggests an important contribution to quenching from feedback from their central supermassive black holes (SMBHs).…”

Section: Introductionmentioning

confidence: 99%

The First Quenched Galaxies: When and How?

Xie 谢,

De Lucia,

Fontanot

et al. 2024

ApJL

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Many quiescent galaxies discovered in the early Universe by JWST raise fundamental questions on when and how these galaxies became and stayed quenched. Making use of the latest version of the semianalytic model GAEA that provides good agreement with the observed quenched fractions up to z ∼ 3, we make predictions for the expected fractions of quiescent galaxies up to z ∼ 7 and analyze the main quenching mechanism. We find that in a simulated box of 685 Mpc on a side, the first quenched massive (M ⋆ ∼ 1011 M ⊙), Milky Way–mass, and low-mass (M ⋆ ∼ 109.5 M ⊙) galaxies appear at z ∼ 4.5, z ∼ 6.2, and before z = 7, respectively. Most quenched galaxies identified at early redshifts remain quenched for more than 1 Gyr. Independently of galaxy stellar mass, the dominant quenching mechanism at high redshift is accretion disk feedback (quasar winds) from a central massive black hole, which is triggered by mergers in massive and Milky Way–mass galaxies and by disk instabilities in low-mass galaxies. Environmental stripping becomes increasingly more important at lower redshift.

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Super-early JWST galaxies, outflows, and Lyαvisibility in the Epoch of Reionization

Ferrara

2024

A&A

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The overabundance of super-early (redshift $z>10$) luminous ($M_ UV < -20$) blue galaxies detected by JWST has been explained as being due to negligible dust attenuation in these systems. We show that this model correctly reproduces the UV luminosity function at $z>10$ and the star formation rate (SFR) density evolution. The model also predicts, in agreement with data, that the cosmic specific SFR (sSFR) grows as $ sSFR $. At $z 10$, the cosmic sSFR crosses the critical value $ sSFR^ $, and approximately $45$<!PCT!> of the galaxies become super-Eddington, driving outflows reaching velocities of $ where $ and $f_M$ are the star formation efficiency and fraction of the halo gas expelled in the outflow, respectively. This prediction is consistent with the outflow velocities measured in 12 super-Eddington galaxies of the JWST /JADES sample. Such outflows clear the dust, thus boosting the galaxy luminosity. They also dramatically enhance the visibility of the Lyalpha line from $z>10$ galaxies by introducing a velocity offset. The observed Lyalpha properties in GN-z11 ($z=10.6$) are simultaneously recovered by the outflow model if $ HI 20.1$, implying that the outflow is largely ionized. We make analogous predictions for the Lyalpha visibility of other super-early galaxies, and we compare the model with Lyalpha surveys at $z>7$, finding that essentially all super-Eddington (sub-Eddington) galaxies are (not) detected in Lyalpha . Finally, the sSFR positively correlates with the LyC escape fraction, as outflows carve ionized transparent channels through which LyC photons leak.

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Can Supernovae Quench Star Formation in High-z Galaxies?

Cited by 6 publications

References 38 publications

Two Distinct Classes of Quiescent Galaxies at Cosmic Noon Revealed by JWST PRIMER and UNCOVER

Two Distinct Classes of Quiescent Galaxies at Cosmic Noon Revealed by JWST PRIMER and UNCOVER

The First Quenched Galaxies: When and How?

Super-early JWST galaxies, outflows, and Lyαvisibility in the Epoch of Reionization

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