2024-03-28T12:06:59Zhttp://digital.csic.es/dspace-oai/requestoai:digital.csic.es:10261/1675342020-12-13T09:25:11Zcom_10261_97com_10261_4col_10261_350
Observational hints of radial migration in disc galaxies from CALIFA
Ruiz-Lara, T.
Pérez, I.
Florido, E.
Sánchez-Blázquez, P.
Méndez-Abreu, J.
Sánchez Menguiano, Laura
Sánchez, S.F.
Lyubenova, M.
Falcón-Barroso, Jesús
Van De Ven, G.
Marino, R.A.
de Lorenzo-Cáceres, A.
Catalán-Torrecilla, C.
Costantin, L.
Bland-Hawthorn, J.
Galbany, Lluís
García-Benito, Rubén
Husemann, B.
Kehrig, C.
Márquez, Isabel
Mast, D.
Walcher, C.J.
Zibetti, S.
Ziegler, B.
Consejo Nacional de Ciencia y Tecnología (México)
Swiss National Science Foundation
European Research Council
Ministerio de Economía y Competitividad (España)
National Science Foundation (US)
Junta de Andalucía
Ministerio de Ciencia e Innovación (España)
European Commission
Galaxies: structure
Galaxies: formation
Galaxies: evolution
Galaxies: stellar content
Galaxies: spiral
Context. According to numerical simulations, stars are not always kept at their birth galactocentric distances but they have a tendency to migrate. The importance of this radial migration in shaping galactic light distributions is still unclear. However, if radial migration is indeed important, galaxies with different surface brightness (SB) profiles must display differences in their stellar population properties. Aims. We investigate the role of radial migration in the light distribution and radial stellar content by comparing the inner colour, age, and metallicity gradients for galaxies with different SB profiles. We define these inner parts, avoiding the bulge and bar regions and up to around three disc scale lengths (type I, pure exponential) or the break radius (type II, downbending; type III, upbending). Methods. We analysed 214 spiral galaxies from the CALIFA survey covering different SB profiles. We made use of GASP2D and SDSS data to characterise the light distribution and obtain colour profiles of these spiral galaxies. The stellar age and metallicity profiles were computed using a methodology based on full-spectrum fitting techniques (pPXF, GANDALF, and STECKMAP) to the Integral Field Spectroscopic CALIFA data. Results. The distributions of the colour, stellar age, and stellar metallicity gradients in the inner parts for galaxies displaying different SB profiles are unalike as suggested by Kolmogorov-Smirnov and Anderson-Darling tests. We find a trend in which type II galaxies show the steepest profiles of all, type III show the shallowest, and type I display an intermediate behaviour. Conclusions. These results are consistent with a scenario in which radial migration is more efficient for type III galaxies than for type I systems, where type II galaxies present the lowest radial migration efficiency. In such a scenario, radial migration mixes the stellar content, thereby flattening the radial stellar properties and shaping different SB profiles. However, in light of these results we cannot further quantify the importance of radial migration in shaping spiral galaxies, and other processes, such as recent star formation or satellite accretion, might play a role.© 2017 ESO.
This research has been supported by the Spanish Ministry of Science and Innovation (MICINN) under grants AYA2014-53506-P, AYA2007-67625-C02-02, AYA2014-56795-P and Consolider-Ingenio CSD2010-00064; and by the Junta de Andalucia (FQM-108). L.G. was supported in part by the US National Science Foundation under Grant AST-1311862. I.M. would like to thank support under grants AYA2013-42227-P and AYA2016-76682-C3-1-P. S.Z. has been supported by the EU Marie Curie Career Integration Grant SteMaGE No. PCIG12-GA-2012-326466 (Call Identifier: FP7-PEOPLE-2012 CIG). J.F.B. thanks the support received under grant AYA2016-77237-C3-1-P. A.d.L.C. acknowledges support from the CONACyT-125180, DGAPA-IA100815 and DGAPA-IA101217 projects. R.A.M. acknowledges support by the Swiss National Science Foundation. J.M.A. thanks support from the support from the European Research Council Starting Grant (SEDmorph; P.I. V. Wild) and MINECO through the grant AYA2013-43188-P.
Peer Reviewed
2018-07-11T06:44:44Z
2018-07-11T06:44:44Z
2017
2018-07-11T06:44:44Z
artículo
http://purl.org/coar/resource_type/c_6501
doi: 10.1051/0004-6361/201730705
issn: 1432-0746
Astronomy and Astrophysics 604: A4 (2017)
http://hdl.handle.net/10261/167534
10.1051/0004-6361/201730705
http://dx.doi.org/10.13039/501100003141
http://dx.doi.org/10.13039/501100000781
http://dx.doi.org/10.13039/501100003329
http://dx.doi.org/10.13039/100000001
http://dx.doi.org/10.13039/501100004837
http://dx.doi.org/10.13039/501100000780
http://dx.doi.org/10.13039/501100011011
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info:eu-repo/grantAgreement/EC/FP7/326466
info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2014-53506-P
info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2007-67625-C02-02
info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2014-56795-P
info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2013-42227-P
info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2016-76682-C3-1-P
info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2016-77237-C3-1-P
info:eu-repo/grantAgreement/MINECO/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2013-43188-P
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