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Metallicity gradient of the thick disc progenitor at high redshift

Kawata, Daisuke; Prieto, Carlos Allende; Brook, Chris B.; Casagrande, Luca; Ciuca, Ioana; Gibson, Brad K.; Grand, Robert J. J.; Hayden, Michael R.; Hunt, Jason A. S.

Description

We have developed a novel Markov Chain Monte Carlo chemical 'painting' technique to explore possible radial and vertical metallicity gradients for the thick disc progenitor. In our analysis, we match an N-body simulation to the data from the Apache Point Observatory Galactic Evolution Experiment survey.We assume that the thick disc has a constant scaleheight and has completed its formation at an early epoch, after which time radial mixing of its stars has taken place. Under these assumptions,...[Show more]

dc.contributor.authorKawata, Daisuke
dc.contributor.authorPrieto, Carlos Allende
dc.contributor.authorBrook, Chris B.
dc.contributor.authorCasagrande, Luca
dc.contributor.authorCiuca, Ioana
dc.contributor.authorGibson, Brad K.
dc.contributor.authorGrand, Robert J. J.
dc.contributor.authorHayden, Michael R.
dc.contributor.authorHunt, Jason A. S.
dc.date.accessioned2021-05-13T00:14:11Z
dc.date.available2021-05-13T00:14:11Z
dc.identifier.issn0035-8711
dc.identifier.urihttp://hdl.handle.net/1885/232986
dc.description.abstractWe have developed a novel Markov Chain Monte Carlo chemical 'painting' technique to explore possible radial and vertical metallicity gradients for the thick disc progenitor. In our analysis, we match an N-body simulation to the data from the Apache Point Observatory Galactic Evolution Experiment survey.We assume that the thick disc has a constant scaleheight and has completed its formation at an early epoch, after which time radial mixing of its stars has taken place. Under these assumptions, we find that the initial radial metallicity gradient of the thick disc progenitor should not be negative, but either flat or even positive, to explain the current negative vertical metallicity gradient of the thick disc. Our study suggests that the thick disc was built-up in an inside-out and upside-down fashion, and older, smaller and thicker populations are more metal poor. In this case, star-forming discs at different epochs of the thick disc formation are allowed to have different radial metallicity gradients, including a negative one, which helps to explain a variety of slopes observed in high-redshift disc galaxies. This scenario helps to explain the positive slope of the metallicity-rotation velocity relation observed for the Galactic thick disc. On the other hand, radial mixing flattens the slope of an existing gradient.
dc.description.sponsorshipDK and IC acknowledge the support of the UK’s Science & Technology Facilities Council (STFC Grants ST/K000977/1 and ST/N000811/1). CAP is thankful to the Spanish MINECO for funding through grant AYA2014-56359-P. LC gratefully acknowledges support from the Australian Research Council (grants DP150100250, FT160100402). RJJG acknowledges support by the DFG Research Centre SFB-881 ‘The Milky Way System’, through project A1. JH is supported by a Dunlap Fellowship at the Dunlap Institute for Astronomy & Astrophysics, funded through an endowment established by the Dunlap family and the University of Toronto.
dc.format.mimetypeapplication/pdf
dc.language.isoen_AU
dc.publisherBlackwell Publishing Ltd
dc.rights© 2017 The Authors
dc.sourceMonthly Notices of the Royal Astronomical Society
dc.subjectmethods: numerical
dc.subjectGalaxy: disc
dc.subjectGalaxy: kinematics and dynamics
dc.titleMetallicity gradient of the thick disc progenitor at high redshift
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume473
dcterms.dateAccepted2017-09-20
dc.date.issued2017-09-25
local.identifier.absfor020104 - Galactic Astronomy
local.identifier.ariespublicationa383154xPUB9262
local.publisher.urlhttps://academic.oup.com/
local.type.statusPublished Version
local.contributor.affiliationKawata, Daisuke, UCL, Mullard Space Science Laboratory
local.contributor.affiliationPrieto, Carlos Allende, Instituto de Astrof´ısica de Canarias
local.contributor.affiliationBrook, Chris B., Instituto de Astrofisica de Canarias
local.contributor.affiliationCasagrande, Luca, College of Science, ANU
local.contributor.affiliationCiuca, Ioana, University College London
local.contributor.affiliationGibson, Brad K., University of Hull, E.A. Milne Centre for Astrophysics
local.contributor.affiliationGrand, Robert J. J., Heidelberger Institut für Theoretische Studien
local.contributor.affiliationHayden, Michael R., Universite de Nice Sophia Antipolis
local.contributor.affiliationHunt, Jason A. S., University of Toronto
dc.relationhttp://purl.org/au-research/grants/arc/DP150100250
dc.relationhttp://purl.org/au-research/grants/arc/FT160100402
local.bibliographicCitation.issue1
local.bibliographicCitation.startpage867
local.bibliographicCitation.lastpage878
local.identifier.doi10.1093/MNRAS/STX2464
dc.date.updated2020-11-23T11:47:50Z
local.identifier.scopusID2-s2.0-85040258364
dcterms.accessRightsOpen Access
dc.provenancehttps://v2.sherpa.ac.uk/id/publication/24618..."Published version can be made open access on institutional repository" from SHERPA/RoMEO site (as at 13.5.2021)
CollectionsANU Research Publications

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