Galaxy and mass assembly (GAMA): The mass-metallicity relationship

dc.contributor.authorFoster, C
dc.contributor.authorHopkins, Andrew M.
dc.contributor.authorGunawardhana, M
dc.contributor.authorLara-Lopez, M A
dc.contributor.authorSharp, Robert
dc.contributor.authorSteele, O
dc.contributor.authorTaylor, E N
dc.contributor.authorDriver, Simon P
dc.contributor.authorBaldry, Ivan
dc.contributor.authorBamford, Steven P.
dc.contributor.authorLiske, Jochen
dc.contributor.authorColless, Matthew
dc.contributor.authorBauer, Amanda E
dc.date.accessioned2015-12-10T23:31:32Z
dc.date.issued2012
dc.date.updated2016-02-24T08:50:57Z
dc.description.abstractContext. The mass-metallicity relationship (MMR) of star-forming galaxies is well-established, however there is still some disagreement with respect to its exact shape and its possible dependence on other observables. Aims.We measure the MMR in the Galaxy And Mass Assembly (GAMA) survey. We compare our measured MMR to that measured in the Sloan Digital Sky Survey (SDSS) and study the dependence of the MMR on various selection criteria to identify potential causes for disparities seen in the literature. Methods.We use strong emission line ratio diagnostics to derive oxygen abundances. We then apply a range of selection criteria for the minimum signal-to-noise in various emission lines, as well as the apparent and absolute magnitude to study variations in the inferred MMR. Results. The shape and position of the MMR can differ significantly depending on the metallicity calibration and selection used. After selecting a robust metallicity calibration amongst those tested, we find that the mass-metallicity relation for redshifts 0.061 ≲ z ≲ 0.35 in GAMA is in reasonable agreement with that found in the SDSS despite the difference in the luminosity range probed. Conclusions. In view of the significant variations of the MMR brought about by reasonable changes in the sample selection criteria and method, we recommend that care be taken when comparing the MMR from different surveys and studies directly. We also conclude that there could be a modest level of evolution over 0.06 ≤ z ≤ 0.35 within the GAMA sample.
dc.identifier.issn0004-6361
dc.identifier.urihttp://hdl.handle.net/1885/68680
dc.publisherSpringer
dc.rightsAuthor/s retain copyrighten_AU
dc.sourceAstronomy and Astrophysics
dc.subjectKeywords: Emission lines; Galaxies: abundances; Galaxies: fundamental parameters; Galaxies: star formation; Galaxies: statistics; Metallicities; Red shift; Sample selection; Selection criteria; Signal to noise; Sloan Digital Sky Survey; Star forming galaxy; Astroph Galaxies: abundances; Galaxies: fundamental parameters; Galaxies: star formation; Galaxies: statistics
dc.titleGalaxy and mass assembly (GAMA): The mass-metallicity relationship
dc.typeJournal article
dcterms.accessRightsOpen Accessen_AU
local.bibliographicCitation.startpageA79
local.contributor.affiliationFoster, C, European Southern Observatory
local.contributor.affiliationHopkins, Andrew M., Australian Astronomical Observatory
local.contributor.affiliationGunawardhana, M, University of Sydney
local.contributor.affiliationLara-Lopez, M A, Australian Astronomical Observatory
local.contributor.affiliationSharp, Robert, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationSteele, O, University of Portsmouth
local.contributor.affiliationTaylor, E N, University of Sydney
local.contributor.affiliationDriver, Simon P, University of St Andrews
local.contributor.affiliationBaldry, Ivan, Liverpool John Moores University
local.contributor.affiliationBamford, Steven P., University of Nottingham
local.contributor.affiliationLiske, Jochen, European Southern Observatory
local.contributor.affiliationColless, Matthew, Australian Astronomical Observatory
local.contributor.affiliationBauer, Amanda E, Australian Astronomical Observatory
local.contributor.authoremailu4954956@anu.edu.au
local.contributor.authoruidSharp, Robert, u4954956
local.description.notesImported from ARIES
local.identifier.absfor020103 - Cosmology and Extragalactic Astronomy
local.identifier.ariespublicationf5625xPUB1797
local.identifier.ariespublicationu4630950xPUB132
local.identifier.citationvolume547
local.identifier.doi10.1051/0004-6361/201220050
local.identifier.scopusID2-s2.0-84868314594
local.identifier.thomsonID000311031700079
local.identifier.uidSubmittedByf5625
local.type.statusPublished Version

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