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dc.contributor.authorMaltby, David T.
dc.contributor.authorAlmaini, Omar
dc.contributor.authorWild, Vivienne
dc.contributor.authorHatch, Nina A.
dc.contributor.authorHartley, William G.
dc.contributor.authorSimpson, Chris
dc.contributor.authorRowlands, Kate
dc.contributor.authorSocolovsky, Miguel
dc.date.accessioned2018-07-23T15:30:05Z
dc.date.available2018-07-23T15:30:05Z
dc.date.issued2018-10-11
dc.identifier.citationMaltby , D T , Almaini , O , Wild , V , Hatch , N A , Hartley , W G , Simpson , C , Rowlands , K & Socolovsky , M 2018 , ' The structure of post-starburst galaxies at 0.5 < z < 2 : evidence for two distinct quenching routes at different epochs ' , Monthly Notices of the Royal Astronomical Society , vol. 480 , no. 1 , pp. 381-401 . https://doi.org/10.1093/mnras/sty1794en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 255012028
dc.identifier.otherPURE UUID: 0d69f277-21c0-48aa-b928-5817607f29d4
dc.identifier.otherBibCode: 2018MNRAS.tmp.1706M
dc.identifier.otherScopus: 85052571344
dc.identifier.otherWOS: 000442567900031
dc.identifier.urihttp://hdl.handle.net/10023/15660
dc.descriptionFunding: DTM acknowledges support from STFC. NAH acknowledges support from STFC throughan Ernest Rutherford Fellowship.en
dc.description.abstractWe present an analysis of the structure of post-starburst (PSB) galaxies in the redshift range 0.5 < z < 2, using a photometrically-selected sample identified in the Ultra Deep Survey (UDS) field. We examine the structure of ∼80 of these transient galaxies using radial light μ(r) profiles obtained from CANDELS Hubble Space Telescope near-infrared/optical imaging, and compare to a large sample of ∼2000 passive and star-forming galaxies. For each population, we determine their typical structural properties (effective radius re, Sérsic index n) and find significant differences in PSB structure at different epochs. At high redshift (z > 1), PSBs are typically massive (M∗>1010M⊙M∗>1010M⊙), very compact and exhibit high Sérsic indices, with structures that differ significantly from their star-forming progenitors but are similar to massive passive galaxies. In contrast, at lower redshift (0.5 < z < 1), PSBs are generally of low mass (M∗<1010M⊙M∗<1010M⊙) and exhibit compact but less concentrated profiles (i.e. lower Sérsic indices), with structures similar to low-mass passive discs. Furthermore, for both epochs we find remarkably consistent PSB structure across the optical/near-infrared wavebands (which largely trace different stellar populations), suggesting that any preceding starburst and/or quenching in PSBs was not strongly centralized. Taken together, these results imply that PSBs at z > 1 have been recently quenched during a major disruptive event (e.g. merger or protogalactic collapse) which formed a compact remnant, while at z < 1 an alternative less disruptive process is primarily responsible. Our results suggest that high-z PSBs are an intrinsically different population to those at lower redshifts, and indicate different quenching routes are active at different epochs.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2018, the Author(s). This work has been made available online in accordance with the publisher’s policies. This is the author created accepted version manuscript following peer review and as such may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1093/mnras/sty1794en
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: fundamental parametersen
dc.subjectGalaxies: high-redshiften
dc.subjectGalaxies: structureen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe structure of post-starburst galaxies at 0.5 < z < 2 : evidence for two distinct quenching routes at different epochsen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/sty1794
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2018MNRAS.tmp.1706Men


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