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dc.contributor.authorChaplin, William J.
dc.contributor.authorSerenelli, Aldo M.
dc.contributor.authorMiglio, Andrea
dc.contributor.authorMorel, Thierry
dc.contributor.authorMackereth, J. Ted
dc.contributor.authorVincenzo, Fiorenzo
dc.contributor.authorKjeldsen, Hans
dc.contributor.authorBasu, Sarbani
dc.contributor.authorBall, Warrick H.
dc.contributor.authorStokholm, Amalie
dc.contributor.authorVerma, Kuldeep
dc.contributor.authorMosumgaard, Jakob Rørsted
dc.contributor.authorSilva Aguirre, Victor
dc.contributor.authorMazumdar, Anwesh
dc.contributor.authorRanadive, Pritesh
dc.contributor.authorAntia, H. M.
dc.contributor.authorLebreton, Yveline
dc.contributor.authorOng, Joel
dc.contributor.authorAppourchaux, Thierry
dc.contributor.authorBedding, Timothy R.
dc.contributor.authorChristensen-Dalsgaard, Jørgen
dc.contributor.authorCreevey, Orlagh
dc.contributor.authorGarcía, Rafael A.
dc.contributor.authorHandberg, Rasmus
dc.contributor.authorHuber, Daniel
dc.contributor.authorKawaler, Steven D.
dc.contributor.authorLund, Mikkel N.
dc.contributor.authorMetcalfe, Travis S.
dc.contributor.authorStassun, Keivan G.
dc.contributor.authorBazot, Michäel
dc.contributor.authorBeck, Paul G.
dc.contributor.authorBell, Keaton J.
dc.contributor.authorBergemann, Maria
dc.contributor.authorBuzasi, Derek L.
dc.contributor.authorBenomar, Othman
dc.contributor.authorBossini, Diego
dc.contributor.authorBugnet, Lisa
dc.contributor.authorCampante, Tiago L.
dc.contributor.authorOrhan, Zeynep Çelik
dc.contributor.authorCorsaro, Enrico
dc.contributor.authorGonzález-Cuesta, Lucía
dc.contributor.authorDavies, Guy R.
dc.contributor.authorDi Mauro, Maria Pia
dc.contributor.authorEgeland, Ricky
dc.contributor.authorElsworth, Yvonne P.
dc.contributor.authorGaulme, Patrick
dc.contributor.authorGhasemi, Hamed
dc.contributor.authorGuo, Zhao
dc.contributor.authorHall, Oliver J.
dc.contributor.authorHasanzadeh, Amir
dc.contributor.authorHekker, Saskia
dc.contributor.authorHowe, Rachel
dc.contributor.authorJenkins, Jon M.
dc.contributor.authorJiménez, Antonio
dc.contributor.authorKiefer, René
dc.contributor.authorKuszlewicz, James S.
dc.contributor.authorKallinger, Thomas
dc.contributor.authorLatham, David W.
dc.contributor.authorLundkvist, Mia S.
dc.contributor.authorMathur, Savita
dc.contributor.authorMontalbán, Josefina
dc.contributor.authorMosser, Benoit
dc.contributor.authorBedón, Andres Moya
dc.contributor.authorNielsen, Martin Bo
dc.contributor.authorÖrtel, Sibel
dc.contributor.authorRendle, Ben M.
dc.contributor.authorRicker, George R.
dc.contributor.authorRodrigues, Thaíse S.
dc.contributor.authorRoxburgh, Ian W.
dc.contributor.authorSafari, Hossein
dc.contributor.authorSchofield, Mathew
dc.contributor.authorSeager, Sara
dc.contributor.authorSmalley, Barry
dc.contributor.authorStello, Dennis
dc.contributor.authorSzabó, Róbert
dc.contributor.authorTayar, Jamie
dc.contributor.authorThemeßl, Nathalie
dc.contributor.authorThomas, Alexandra E. L.
dc.contributor.authorVanderspek, Roland K.
dc.contributor.authorvan Rossem, Walter E.
dc.contributor.authorVrard, Mathieu
dc.contributor.authorWeiss, Achim
dc.contributor.authorWhite, Timothy R.
dc.contributor.authorWinn, Joshua N.
dc.contributor.authorYıldız, Mutlu
dc.date.accessioned2020-12-23T18:28:10Z
dc.date.available2020-12-23T18:28:10Z
dc.date.issued2020-01
dc.date.submitted2019-10
dc.identifier.issn2397-3366
dc.identifier.urihttps://hdl.handle.net/1721.1/128912
dc.description.abstractOver the course of its history, the Milky Way has ingested multiple smaller satellite galaxies1. Although these accreted stellar populations can be forensically identified as kinematically distinct structures within the Galaxy, it is difficult in general to date precisely the age at which any one merger occurred. Recent results have revealed a population of stars that were accreted via the collision of a dwarf galaxy, called Gaia–Enceladus1, leading to substantial pollution of the chemical and dynamical properties of the Milky Way. Here we identify the very bright, naked-eye star ν Indi as an indicator of the age of the early in situ population of the Galaxy. We combine asteroseismic, spectroscopic, astrometric and kinematic observations to show that this metal-poor, alpha-element-rich star was an indigenous member of the halo, and we measure its age to be 11.0 ± 0.7 (stat) ± 0.8 (sys) billion years. The star bears hallmarks consistent with having been kinematically heated by the Gaia–Enceladus collision. Its age implies that the earliest the merger could have begun was 11.6 and 13.2 billion years ago, at 68% and 95% confidence, respectively. Computations based on hierarchical cosmological models slightly reduce the above limits.en_US
dc.language.isoen
dc.publisherSpringer Science and Business Media LLCen_US
dc.relation.isversionofhttp://dx.doi.org/10.1038/s41550-019-0975-9en_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.sourcearXiven_US
dc.titleAge dating of an early Milky Way merger via asteroseismology of the naked-eye star ν Indien_US
dc.typeArticleen_US
dc.identifier.citationChaplin, William J. et al. "Age dating of an early Milky Way merger via asteroseismology of the naked-eye star ν Indi." Nature Astronomy 4, 4 (January 2020): 382–389 © 2020 The Author(s)en_US
dc.contributor.departmentMassachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciencesen_US
dc.relation.journalNature Astronomyen_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.updated2020-04-28T17:34:30Z
dspace.date.submission2020-04-28T17:34:35Z
mit.journal.volume4en_US
mit.journal.issue4en_US
mit.licensePUBLISHER_POLICY


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