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dc.contributor.authorYesuf, Hassen M.
dc.contributor.authorFaber, S.M.
dc.contributor.authorTrump, Jonathan R.
dc.contributor.authorKoo, David C.
dc.contributor.authorFang, Jerome J.
dc.contributor.authorLiu, F.S.
dc.contributor.authorWild, Vivienne
dc.contributor.authorHayward, Christopher C.
dc.date.accessioned2014-09-23T10:01:05Z
dc.date.available2014-09-23T10:01:05Z
dc.date.issued2014-07-14
dc.identifier.citationYesuf , H M , Faber , S M , Trump , J R , Koo , D C , Fang , J J , Liu , F S , Wild , V & Hayward , C C 2014 , ' From starburst to quiescence : testing AGN feedback in rapidly Quenching post-starburst galaxies ' , Astrophysical Journal , vol. 792 , no. 2 , 84 . https://doi.org/10.1088/0004-637X/792/2/84en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 150540359
dc.identifier.otherPURE UUID: 3ee403b3-5ace-4898-bbcb-08e2ec988830
dc.identifier.otherArXiv: http://arxiv.org/abs/1407.3834v1
dc.identifier.otherScopus: 84906751867
dc.identifier.otherBibCode: 2014ApJ...792...84Y
dc.identifier.otherWOS: 000341172200002
dc.identifier.urihttp://hdl.handle.net/10023/5472
dc.descriptionWe acknowledge financial support from the NSF grant AST-0808133. C.C.H. is grateful to the Klaus Tschira Foundation for financial support.en
dc.description.abstractPost-starbursts are galaxies in transition from the blue cloud to the red sequence. Although they are rare today, integrated over time they may be an important pathway to the red sequence. This work uses SDSS, GALEX, and WISE observations to identify the evolutionary sequence from starbursts to fully quenched post-starbursts in the narrow mass range log M(Msun) = 10.3-10.7, and identifies "transiting" post-starbursts which are intermediate between these two populations. In this mass range, ∼0.3% of galaxies are starbursts, ∼0.1% are quenched post-starbursts, and ∼0.5% are the transiting types in between. The transiting post-starbursts have stellar properties that are predicted for fast-quenching starbursts and morphological characteristics that are already typical of early-type galaxies. The AGN fraction, as estimated from optical line ratios, of these post-starbursts is about 3 times higher (∼>36 ± 8%) than that of normal star-forming galaxies of the same mass, but there is a significant delay between the starburst phase and the peak of nuclear optical AGN activity (median age difference of ∼> 200 ± 100$ Myr), in agreement with previous studies. The time delay is inferred by comparing the broad-band near NUV-to-optical photometry with stellar population synthesis models. We also find that starbursts and post-starbursts are significantly more dust-obscured than normal star-forming galaxies in the same mass range. About 20% of the starbursts and 15% of the transiting post-starbursts can be classified as the "Dust-Obscured Galaxies" (DOGs), while only 0.8% of normal galaxies are DOGs.The time delay between the starburst phase and AGN activity suggests that AGN do not play a primary role in the original quenching of starbursts but may be responsible for quenching later low-level star formation during the post-starburst phase.
dc.format.extent22
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2014. The American Astronomical Society. All rights reserved. This is an Accepted Manuscript of an article published online in the Astrophysical Journal on 7 July 2014, available online: http://iopscience.iop.org/0004-637X/792/2/84/articleen
dc.subjectGalaxies: activeen
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: formationen
dc.subjectGalaxies: starbursten
dc.subjectGalaxies: stellar contenten
dc.subjectGalaxies: structureen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleFrom starburst to quiescence : testing AGN feedback in rapidly Quenching post-starburst galaxiesen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/792/2/84
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2014ApJ...792...84Yen


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