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dc.contributor.authorDonnari, Martina
dc.contributor.authorPillepich, Annalisa
dc.contributor.authorJoshi, Gandhali D
dc.contributor.authorNelson, Dylan
dc.contributor.authorGenel, Shy
dc.contributor.authorMarinacci, Federico
dc.contributor.authorRodriguez-Gomez, Vicente
dc.contributor.authorPakmor, Rüdiger
dc.contributor.authorTorrey, Paul
dc.contributor.authorVogelsberger, Mark
dc.contributor.authorHernquist, Lars
dc.date.accessioned2022-05-06T17:18:02Z
dc.date.available2022-05-06T17:18:02Z
dc.date.issued2020
dc.identifier.urihttps://hdl.handle.net/1721.1/142405
dc.description.abstract© 2020 The Author(s). We use the IllustrisTNG hydrodynamical simulations to show how the fractions of quenched galaxies vary across different environments and cosmic time, and to quantify the role AGN feedback and pre-processing play in quenching group and cluster satellites. At z = 0, we select galaxies with Mstars = 109-12 M⊙ residing within (≤R200c) massive groups and clusters of total host mass M200c = 1013-15.2 M⊙ in TNG100 and TNG300. The model predicts a quenched fraction of ∼70-90 per cent (on average) for centrals and satellites of mass ≳1010.5 M⊙, regardless of host mass, cosmic time (0 ≤ z ≤ 0.5), cluster-centric distance, and time since infall in the z = 0 host. Low-mass central galaxies (≲ 1010 M⊙), on the other hand, are rarely quenched unless they become members of groups (1013-14 M⊙) or clusters (≥1014 M⊙), where the quenched fraction rises to ∼ 80 per cent. Typically, the fraction of low-mass passive galaxies is higher closer to the host centre and for progressively more massive hosts. The population of low-mass satellites accreted more than ∼ 4-6 Gyr ago in massive hosts is almost entirely passive, thus suggesting an upper limit for the time needed for environmental quenching to occur. In fact, about 30 per cent of group and cluster satellites that are quenched at z = 0 were already quenched before falling into their current host, and the bulk of them quenched as early as 4-10 billion years ago. For low-mass galaxies (Mstars ≲1010-10.5 M⊙), this is due to pre-processing, whereby current satellites may have been members of other hosts, and hence have undergone environmental processes, before falling into their final host, this mechanism being more common and more effective for the purposes of quenching for satellites found today in more massive hosts. On the other hand, massive galaxies quench on their own and because of AGN feedback, regardless of whether they are centrals or satellites.en_US
dc.language.isoen
dc.publisherOxford University Press (OUP)en_US
dc.relation.isversionof10.1093/MNRAS/STAA3006en_US
dc.rightsAttribution-NonCommercial-ShareAlike 4.0 Internationalen_US
dc.rights.urihttps://creativecommons.org/licenses/by-nc-sa/4.0/en_US
dc.sourcearXiven_US
dc.titleQuenched fractions in the IllustrisTNG simulations: the roles of AGN feedback, environment, and pre-processingen_US
dc.typeArticleen_US
dc.identifier.citationDonnari, Martina, Pillepich, Annalisa, Joshi, Gandhali D, Nelson, Dylan, Genel, Shy et al. 2020. "Quenched fractions in the IllustrisTNG simulations: the roles of AGN feedback, environment, and pre-processing." Monthly Notices of the Royal Astronomical Society, 500 (3).
dc.contributor.departmentMIT Kavli Institute for Astrophysics and Space Research
dc.relation.journalMonthly Notices of the Royal Astronomical Societyen_US
dc.eprint.versionAuthor's final manuscripten_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dc.date.updated2022-05-06T17:09:18Z
dspace.orderedauthorsDonnari, M; Pillepich, A; Joshi, GD; Nelson, D; Genel, S; Marinacci, F; Rodriguez-Gomez, V; Pakmor, R; Torrey, P; Vogelsberger, M; Hernquist, Len_US
dspace.date.submission2022-05-06T17:09:20Z
mit.journal.volume500en_US
mit.journal.issue3en_US
mit.licenseOPEN_ACCESS_POLICY
mit.metadata.statusAuthority Work and Publication Information Neededen_US


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