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dc.contributor.authorSánchez-Menguiano, L.
dc.contributor.authorSánchez, S. F.
dc.contributor.authorPérez, I.
dc.contributor.authorGarciá-Benito, R.
dc.contributor.authorHusemann, B.
dc.contributor.authorMast, D.
dc.contributor.authorMendoza, A.
dc.contributor.authorRuiz-Lara, T.
dc.contributor.authorAscasibar, Y.
dc.contributor.authorBland-Hawthorn, J.
dc.contributor.authorCavichia, O.
dc.contributor.authorDiáz, A. I.
dc.contributor.authorFlorido, E.
dc.contributor.authorGalbany, L.
dc.contributor.authorGónzalez Delgado, R. M.
dc.contributor.authorKehrig, C.
dc.contributor.authorMarino, R. A.
dc.contributor.authorMárquez, I.
dc.contributor.authorMasegosa, J.
dc.contributor.authorMéndez-Abreu, Jairo
dc.contributor.authorMollá, M.
dc.contributor.authordel Olmo, A.
dc.contributor.authorPérez, E.
dc.contributor.authorSánchez-Blázquez, P.
dc.contributor.authorStanishev, V.
dc.contributor.authorWalcher, C. J.
dc.contributor.authorLópez-Sánchez, A. R.
dc.contributor.authorcollaboration the CALIFA
dc.date.accessioned2016-04-11T14:00:03Z
dc.date.available2016-04-11T14:00:03Z
dc.date.issued2016-03-01
dc.identifier.citationSánchez-Menguiano , L , Sánchez , S F , Pérez , I , Garciá-Benito , R , Husemann , B , Mast , D , Mendoza , A , Ruiz-Lara , T , Ascasibar , Y , Bland-Hawthorn , J , Cavichia , O , Diáz , A I , Florido , E , Galbany , L , Gónzalez Delgado , R M , Kehrig , C , Marino , R A , Márquez , I , Masegosa , J , Méndez-Abreu , J , Mollá , M , del Olmo , A , Pérez , E , Sánchez-Blázquez , P , Stanishev , V , Walcher , C J , López-Sánchez , A R & collaboration the CALIFA 2016 , ' Shape of the oxygen abundance profiles in CALIFA face-on spiral galaxies ' , Astronomy & Astrophysics , vol. 587 , A70 , pp. 1-21 . https://doi.org/10.1051/0004-6361/201527450en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 241556367
dc.identifier.otherPURE UUID: fc4cd280-9b8e-4a4d-bc45-444134bd105a
dc.identifier.otherScopus: 84959019750
dc.identifier.otherWOS: 000371589800081
dc.identifier.urihttp://hdl.handle.net/10023/8594
dc.descriptionY.A. acknowledges financial support from the Ramón y Cajal programme (RyC-2011-09461). Y.A. and A.I.D. acknowledge support from the project AYA2013-47742-C4-3-P from the Spanish MINECO, as well as the “Study of Emission-Line Galaxies with Integral-Field Spectroscopy” (SELGIFS) programme, funded by the EU (FP7-PEOPLE-2013-IRSES-612701). Support for L.G. is provided by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. LG acknowledges support by CONICYT through FONDECYT grant 3140566. R.M.G.D. acknowledges support from the Spanish grant AYA2014-57490-P, and from the “Junta de Andalucía” P12-FQM2828 project. RAM thanks the Spanish program of International Campus of Excellence Moncloa (CEI). IM and A.d.O. acknowledge support from the Spanish MINECO grant AYA2013-42227P. JMA acknowledges support from the European Research Council Starting Grant (SEDmorph, P.I. V. Wild). Support for MM has been provided by DGICYT grant AYA2013-47742-C4-4-P. PSB acknowledges support from the Ramón y Cajal programme, grant ATA2010-21322-C03-02 from the Spanish MINECO. CJW acknowledges support through the Marie Curie Career Grant Integration 303912.en
dc.description.abstractWe measured the gas abundance profiles in a sample of 122 face-on spiral galaxies observed by the CALIFA survey and included all spaxels whose line emission was consistent with star formation. This type of analysis allowed us to improve the statistics with respect to previous studies, and to properly estimate the oxygen distribution across the entire disc to a distance of up to 3-4 disc effective radii (re). We confirm the results obtained from classical H ii region analysis. In addition to the general negative gradient, an outer flattening can be observed in the oxygen abundance radial profile. An inner drop is also found in some cases. There is a common abundance gradient between 0.5 and 2.0 re of αO/H =-0.075 dex/re with a scatter of σ = 0.016 dex/re when normalising the distances to the disc effective radius. By performing a set of Kolmogorov-Smirnov tests, we determined that this slope is independent of other galaxy properties, such as morphology, absolute magnitude, and the presence or absence of bars. In particular, barred galaxies do not seem to display shallower gradients, as predicted by numerical simulations. Interestingly, we find that most of thegalaxies in the sample with reliable oxygen abundance values beyond ~2 effective radii (57 galaxies) present a flattening of the abundance gradient in these outer regions. This flattening is not associated with any morphological feature, which suggests that it is a common property of disc galaxies. Finally, we detect a drop or truncation of the abundance in the inner regions of 27 galaxies in the sample; this is only visible for the most massive galaxies.
dc.format.extent21
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© ESO 2016. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://dx.doi.org/10.1051/0004-6361/201527450en
dc.subjectGalaxies: abundancesen
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: ISMen
dc.subjectGalaxies: spiralen
dc.subjectTechniques: imaging spectroscopyen
dc.subjectTechniques: spectroscopicen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectAstronomy and Astrophysicsen
dc.subjectSpace and Planetary Scienceen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleShape of the oxygen abundance profiles in CALIFA face-on spiral galaxiesen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201527450
dc.description.statusPeer revieweden


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