Do galaxy global relationships emerge from local ones? The SDSS IV MaNGA surface mass density-metallicity relation

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dc.contributor.authorBarrera Ballesteros, Jorge K.
dc.contributor.authorHeckman, Timothy M.
dc.contributor.authorZhu, Guangtun B.
dc.contributor.authorZakamska, Nadia L.
dc.contributor.authorSanchez, Sebastian F.
dc.contributor.authorLaw, David
dc.contributor.authorWake, David
dc.contributor.authorGreen, Jenny E.
dc.contributor.authorBizyaev, Dmitry
dc.contributor.authorOravetz, Daniel
dc.contributor.authorSimmons, Audrey
dc.contributor.authorMalanushenko, Elena
dc.contributor.authorPan, Kaike
dc.contributor.authorRoman Lopes, Alexandre
dc.contributor.authorLane, Richard R.
dc.date.accessioned2024-01-10T12:38:24Z
dc.date.available2024-01-10T12:38:24Z
dc.date.issued2016
dc.description.abstractWe present the stellar surface mass density versus gas metallicity (Sigma(*)-Z) relation for more than 500 000 spatially resolved star-forming resolution elements (spaxels) from a sample of 653 disc galaxies included in the SDSS IV MaNGA survey. We find a tight relation between these local properties, with higher metallicities as the surface density increases. This relation extends over three orders of magnitude in the surface mass density and a factor of 4 in metallicity. We show that this local relationship can simultaneously reproduce two well-known properties of disc galaxies: their global mass-metallicity relationship and their radial metallicity gradients. We also find that the Sigma(*)-Z relation is largely independent of the galaxy's total stellar mass and specific star formation rate (sSFR), except at low stellar mass and high sSFR. These results suggest that in the present-day universe local properties play a key role in determining the gas-phase metallicity in typical disc galaxies.
dc.description.funderAlfred P. Sloan Foundation
dc.description.funderUS Department of Energy Office of Science
dc.description.funderCenter for High-Performance Computing at the University of Utah
dc.description.funderBrazilian Participation Group
dc.description.funderCarnegie Institution for Science
dc.description.funderCarnegie Mellon University
dc.description.funderChilean Participation Group
dc.description.funderFrench Participation Group
dc.description.funderHarvard-Smithsonian Center for Astrophysics
dc.description.funderInstituto de Astrofisica de Canarias
dc.description.funderJohns Hopkins University
dc.description.funderKavli Institute for the Physics and Mathematics of the Universe (IPMU) / University of Tokyo
dc.description.funderLawrence Berkeley National Laboratory
dc.description.funderLeibniz Institut fur Astrophysik Potsdam (AIP)
dc.description.funderMax-Planck-Institut fur Astronomie (MPIA Heidelberg)
dc.description.funderMax-Planck-Institut fur Astrophysik (MPA Garching)
dc.description.funderMax-Planck-Institut fur Extraterrestrische Physik (MPE)
dc.description.funderNational Astronomical Observatory of China
dc.description.funderNew Mexico State University
dc.description.funderNew York University
dc.description.funderUniversity of Notre Dame
dc.description.funderObservatario Nacional / MCTI
dc.description.funderOhio State University
dc.description.funderPennsylvania State University
dc.description.funderShanghai Astronomical Observatory
dc.description.funderUnited Kingdom Participation Group
dc.description.funderUniversidad Nacional Autonoma de Mexico
dc.description.funderUniversity of Arizona
dc.description.funderUniversity of Colorado Boulder
dc.description.funderUniversity of Oxford
dc.description.funderUniversity of Portsmouth
dc.description.funderUniversity of Utah
dc.description.funderUniversity of Virginia
dc.description.funderUniversity of Washington
dc.description.funderUniversity of Wisconsin
dc.description.funderVanderbilt University
dc.description.funderYale University
dc.fechaingreso.objetodigital2024-05-06
dc.format.extent10 páginas
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stw1984
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stw1984
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/77038
dc.identifier.wosidWOS:000393566000019
dc.information.autorucFísica;Lane R;S/I;1021384
dc.issue.numero3
dc.language.isoen
dc.nota.accesoSin adjunto
dc.pagina.final2522
dc.pagina.inicio2513
dc.publisherOXFORD UNIV PRESS
dc.revistaMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
dc.rightsregistro bibliográfico
dc.subjecttechniques: imaging spectroscopy
dc.subjectgalaxies: abundances
dc.subjectgalaxies: fundamental parameters
dc.subjectgalaxies: ISM
dc.subjectDIGITAL SKY SURVEY
dc.subjectSTAR-FORMING GALAXIES
dc.subjectH-II REGIONS
dc.subject2.5 M TELESCOPE
dc.subjectSPIRAL GALAXIES
dc.subjectABUNDANCE GRADIENTS
dc.subjectPHYSICAL-PROPERTIES
dc.subjectOXYGEN ABUNDANCES
dc.subjectSTELLAR CONTENT
dc.subjectHIGH-REDSHIFT
dc.titleDo galaxy global relationships emerge from local ones? The SDSS IV MaNGA surface mass density-metallicity relation
dc.typeartículo
dc.volumen463
sipa.codpersvinculados1021384
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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