The age gradients of galaxies in EAGLE: outside-in quenching as the origin of young bulges in cluster galaxies

Pfeffer, Joel; Bekki, Kenji; Couch, Warrick J.; Koribalski, Bärbel S.; Forbes, Duncan A.

doi:10.48550/arxiv.2201.03137

Cited by 1 publication

(3 citation statements)

References 96 publications

(164 reference statements)

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“…For example, Johnston et al (2021) also found evidence of younger luminosity-weighted ages in the bulges and discs than their mass-weighted ages, which they attributed to more recent star formation that contributes towards only a small fraction of the mass of the galaxy. Simulations by Pfeffer et al (2022) also found evidence of negative age gradients across cluster galaxies, which they attributed to outside-in quenching of star formation as the galaxies fall into the clusters.…”

Section: General Properties Of Bulges and Discsmentioning

confidence: 94%

“…Evidence of a dependence on environment has been seen before. For example, using EAGLE simulations (Schaye et al 2015;Crain et al 2015), Pfeffer et al (2022) found that cluster S0 galaxies tend to display positive age gradients, which corresponds to outside-in quenching, while more isolated S0 galaxies showed more negative age gradients, reflecting inside-out quenching. Bedregal et al (2011) and Finn et al (2018) found the same result for galaxies in local clusters.…”

Section: Dependence On Environmentmentioning

confidence: 99%

“…For example, gas stripping processes may produce stellar population gradients across the galaxy where the star formation becomes truncated first in the outskirts while continuing for some time in the inner regions (e.g. Pfeffer et al 2022). On the other hand, minor mergers might trigger a short episode of enhanced star formation across the entire galaxy, using up all the gas at around the same time and producing flatter age gradients (Mehlert et al 2003;Ogando et al 2005;Kuntschner et al 2010;Eigenthaler & Zeilinger 2013).…”

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confidence: 99%

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BUDDI-MaNGA II: The Star-Formation Histories of Bulges and Discs of S0s

Johnston,

Häußler,

Jegatheesan

et al. 2022

Preprint

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Many processes have been proposed to explain the quenching of star formation in spiral galaxies and their transformation into S0s. These processes affect the bulge and disc in different ways, and so by isolating the bulge and disc spectra, we can look for these characteristic signatures. In this work, we used to cleanly extract the spectra of the bulges and discs of 78 S0 galaxies in the MaNGA Survey. We compared the luminosity and mass weighted stellar populations of the bulges and discs, finding that bulges are generally older and more metal rich than their discs. When considering the mass and environment of each galaxy, we found that the galaxy stellar mass plays a more significant role on the formation of the bulges. Bulges in galaxies with masses 10 10 𝑀 built up the majority of their mass rapidly early in their lifetimes, while those in lower mass galaxies formed over more extended timescales and more recently. No clear difference was found in the formation or quenching processes of the discs as a function of galaxy environment. We conclude that more massive S0 galaxies formed through an inside-out scenario, where the bulge formed first and evolved passively while the disc underwent a more extended period of star formation. In lower mass S0s, the bulges and discs either formed together from the same material, or through an outside-in scenario. Our results therefore imply multiple formation mechanisms for S0 galaxies, the pathway of which is chiefly determined by a galaxy's current stellar mass.

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Section: General Properties Of Bulges and Discsmentioning

confidence: 94%