dc.contributor.author | Zolotov, Adi | |
dc.contributor.author | Dekel, Avishai | |
dc.contributor.author | Mandelker, Nir | |
dc.contributor.author | Tweed, Dylan | |
dc.contributor.author | Inoue, Shigeki | |
dc.contributor.author | DeGraf, Colin | |
dc.contributor.author | Ceverino Rodríguez, Daniel | |
dc.contributor.author | Primack, Joel R. | |
dc.contributor.author | Barro, Guillermo | |
dc.contributor.author | Faber, Sandra M. | |
dc.contributor.other | UAM. Departamento de Física Teórica | es_ES |
dc.date.accessioned | 2018-07-27T16:26:45Z | |
dc.date.available | 2018-07-27T16:26:45Z | |
dc.date.issued | 2015-07-01 | |
dc.identifier.citation | Monthly Notices of the Royal Astronomical Society 450.3 (2015): 2327-2353 | es_ES |
dc.identifier.issn | 0035-8711 (print) | es_ES |
dc.identifier.issn | 1365-2966 (online) | es_ES |
dc.identifier.uri | http://hdl.handle.net/10486/684489 | |
dc.description | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved | en_US |
dc.description.abstract | We use cosmological simulations to study a characteristic evolution pattern of high redshift galaxies. Early, stream-fed, highly perturbed, gas-rich discs undergo phases of dissipative contraction into compact, star-forming systems (“blue” nuggets) at z∼4−2. The peak of gas compaction marks the onset of central gas depletion and inside-out quenching into compact ellipticals (red nuggets) by z ∼ 2. These are sometimes surrounded by gas rings or grow extended. We use cosmological simulations to study a characteristic evolution pattern of high redshift galaxies. Early, stream-fed, highly perturbed, gas-rich discs undergo phases of dissipative contraction into compact, star-forming systems (“blue” nuggets) at z∼4−2. The peak of gas compaction marks the onset of central gas depletion and inside-out quenching into compact ellipticals (red nuggets) by z ∼ 2. These are sometimes surrounded by gas rings or grow extended dry stellar envelopes. The compaction occurs at a roughly constant specific starformation rate (SFR), and the quenching occurs at a constant stellar surface density within the inner kpc ( 1). Massive galaxies quench earlier, faster, and at a higher 1 than lower-mass galaxies, which compactify and attempt to quench more than once. This evolution pattern is consistent with the way galaxies populate the SFR-radius-mass space, and with gradients and scatter across the main sequence. The compaction is triggered by an intense inflow episode, involving mergers, counter-rotating streams or recycled gas, and is commonly associated with violent disc instability. The contraction is dissipative, with the inflow rate >SFR, and the maximum 1 anti-correlated with the initial spin parameter, as predicted by Dekel & Burkert (2014). The central quenching is triggered by the high SFR and stellar/supernova feedback (possibly also AGN feedback) due to the high central gas density, while the central inflow weakens as the disc vanishes. Suppression of fresh gas supply by a hot halo allows the longterm maintenance of quenching once above a threshold halo mass, inducing the quenching downsizing dry stellar envelopes. The compaction occurs at a roughly constant specific starformation rate (SFR), and the quenching occurs at a constant stellar surface density within the inner kpc ( 1). Massive galaxies quench earlier, faster, and at a higher 1 than lower-mass galaxies, which compactify and attempt to quench more than once. This evolution pattern is consistent with the way galaxies populate the SFR-radius-mass space, and with gradients and scatter across the main sequence. The compaction is triggered by an intense inflow episode, involving mergers, counter-rotating streams or recycled gas, and is commonly associated with violent disc instability. The contraction is dissipative, with the inflow rate >SFR, and the maximum 1 anti-correlated with the initial spin parameter, as predicted by Dekel & Burkert (2014). The central quenching is triggered by the high SFR and stellar/supernova feedback (possibly also AGN feedback) due to the high central gas density, while the central inflow weakens as the disc vanishes. Suppression of fresh gas supply by a hot halo allows the longterm maintenance of quenching once above a threshold halo mass, inducing the quenching downsizing | en_US |
dc.description.sponsorship | This work was supported by ISF grant 24/12, by GIF grant G-1052-104.7/2009, by a DIP grant, by the I-CORE Program of the PBC, by ISF grant 1829/12, and by NSF grants AST-1010033 and AST-1405962. SI and CD acknowledge Lady Davis Fellowships at HU. DC acknowledges support from MINECO grant AYA2012-31101, MICINN grant AYA-2009-13875-C03-02, and a Juan de la Cierva fellowship | en |
dc.format.extent | 27 pag. | es_ES |
dc.format.mimetype | application/pdf | en |
dc.language.iso | eng | en |
dc.publisher | Oxford University Press on behalf of the Royal Astronomical Society | en_US |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en_US |
dc.rights | © 2015 The Authors | es_ES |
dc.subject.other | Galaxies: elliptical and lenticular, cD | en_US |
dc.subject.other | Galaxies: evolution | en_US |
dc.subject.other | Galaxies: formation | en_US |
dc.subject.other | Galaxies: kinematics and dynamics | en_US |
dc.subject.other | Galaxies: spiral | en_US |
dc.title | Compaction and quenching of high-z galaxies in cosmological simulations: Blue and red nuggets | en_US |
dc.type | article | en |
dc.subject.eciencia | Física | es_ES |
dc.relation.publisherversion | http://dx.doi.org/10.1093/mnras/stv740 | es_ES |
dc.identifier.doi | 10.1093/mnras/stv740 | es_ES |
dc.identifier.publicationfirstpage | 2327 | es_ES |
dc.identifier.publicationissue | 3 | es_ES |
dc.identifier.publicationlastpage | 2353 | es_ES |
dc.identifier.publicationvolume | 450 | es_ES |
dc.relation.projectID | Gobierno de España. AYA2012-31101 | es_ES |
dc.relation.projectID | Gobierno de España. AYA-2009-13875- C03-02 | es_ES |
dc.type.version | info:eu-repo/semantics/submittedVersion | en |
dc.rights.accessRights | openAccess | en |
dc.facultadUAM | Facultad de Ciencias | |