Imprints of galaxy evolution on H II regions. Memory of the past uncovered by the CALIFA survey

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Show simple item record Sánchez, S. F. Pérez, E. Rosales Ortega, F. Fabián Miralles-Caballero, D. López-Sánchez, A. R. Iglesias-Páramo, J. Marino, R. A. Sánchez-Menguiano, L. García-Benito, R. Mast, D. Mendoza, M. A. Papaderos, P. Ellis, S. Galbany, L. Kehrig, C. Monreal-Ibero, Ana Mollá, M. Ziegler, B. De Lorenzo-Cáceres, A. Méndez-Abreu, Jairo Bland-Hawthorn, J. Bekeraitė, S. Roth, M. M. Pasquali, A. Díaz, A. Bomans, D. Van De Ven, Glenn Wisotzki, L. González Delgado, R.
dc.contributor.other UAM. Departamento de Física Teórica es_ES 2016-05-31T15:04:55Z 2016-05-31T15:04:55Z 2015-01-01
dc.identifier.citation Astronomy and Astrophysics 574 (2015): A47 en_US
dc.identifier.issn 0004-6361 (print) es_ES
dc.identifier.issn 1432-0746 (online) es_ES
dc.description Astronomy and Astrophysics 574 (2015): A47 reproduced with permission from Astronomy & Astrophysics, © ESO en_US
dc.description.abstract Context. H II regions in galaxies are the sites of star formation, so they are special places for understanding the build-up of stellar mass in the universe. The line ratios of this ionized gas are frequently used to characterize the ionization conditions. In particular, the oxygen abundances are assumed to trace the chemical enrichment of galaxies. Aims. We explore the connections between the ionization conditions and the properties of the overall underlying stellar population (ionizing or not-ionizing) in H II regions, in order to uncover the actual physical connection between them. Methods. We use the H II regions catalog from the CALIFA survey, which is the largest in existence with more than 5000 H II regions, to explore their distribution across the classical [O III] λ5007/Hβ vs. [N II] λ6583/α diagnostic diagram, and the way it depends on the oxygen abundance, ionization parameter, electron density, and dust attenuation. The location of H II regions within this diagram is compared with predictions from photoionization models. Finally, we explore the dependence of the location within the diagnostic diagram on the properties of the host galaxies, the galactocentric distances, and the properties of the underlying stellar population. Results. The H II regions with weaker ionization strengths and more metal-rich are located in the bottom righthand area of the diagram. In contrast, those regions with stronger ionization strengths and more metal poor are located in the upper lefthand end of the diagram. Photoionization models per se do not predict these correlations between the parameters and the line ratios. The H II regions located in earlier-type galaxies, closer to the center and formed in older and more metal-rich regions of the galaxies are located in the bottom-right area of the diagram. On the other hand, those regions located in late-type galaxies in the outer regions of the disks and formed on younger and more metal-poor regions lie in the top lefthand area of the diagram. The two explored line ratios show strong correlations with the age and metallicity of the underlying stellar population. Conclusions. These results indicate that although H II regions are short-lived events, they are aff ected by the total underlying stellar population. One may say that H II regions keep a memory of the stellar evolution and chemical enrichment that have left an imprint on both the ionizing stellar population and the ionized gas en_US
dc.description.sponsorship We thank the Viabilidad, Diseño, Acceso y Mejora funding program, ICTS-2009-10, for supporting the initial developement of this project. S.F.S. thanks the ConaCyt funding program 180125, for the support given to this project. S.F.S., M.A.M. and L.S.M. thank the Plan Nacional de Investigación y Desarrollo funding programs, AYA2012-31935, of the Spanish Ministerio de Economía y Competitividad, for the support given to this project. S.F.S. thanks the Ramón y Cajal project RyC-2011-07590 of the Spanish Ministerio de Economía y Competitividad, for its support of this project. P.P. is supported by a FCT Investigator 2013 consolidation grant. He acknowledges support by the Fundação para a Ciência e a Tecnologia (FCT) under project FCOMP-01-0124-FEDER-029170 (Reference FCT PTDC/FIS-AST/3214/2012), funded by FCT-MEC (PIDDAC) and FEDER (COMPETE). R.G.D., E.P., and R.G.B. thank the Plan Nacional de Investigación y Desarrollo funding program AYA2010-15081. Support for LG is provided by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC12009, awarded to The Millennium Institute of Astrophysics, MAS. L.G. acknowledges support by CONICYT through FONDECYT grant 3140566. R.A. Marino was also funded by the Spanish program of International Campus of Excellence Moncloa (CEI). A. M.-I. acknowledges support from Agence Nationale de la Recherche through the STILISM project (ANR-12-BS05-0016-02) en_US
dc.format.extent 17 pag. es_ES
dc.format.mimetype application/pdf en
dc.language.iso eng en
dc.publisher EDP Sciences en_US
dc.relation.ispartof Astronomy and Astrophysics en_US
dc.rights © ESO 2015 en_US
dc.subject.other Galaxies: abundances en_US
dc.subject.other Galaxies: evolution galaxies: ISM en_US
dc.subject.other Galaxies: star formation en_US
dc.title Imprints of galaxy evolution on H II regions. Memory of the past uncovered by the CALIFA survey en_US
dc.type article en
dc.subject.eciencia Física es_ES
dc.relation.publisherversion es_ES
dc.identifier.doi 10.1051/0004-6361/201424873 es_ES
dc.identifier.publicationfirstpage A47 es_ES
dc.identifier.publicationlastpage A47 es_ES
dc.identifier.publicationvolume 574 es_ES
dc.relation.projectID Gobierno de España. AYA2012-31935 es_ES
dc.relation.projectID Gobierno de España. RyC-2011-07590 es_ES
dc.relation.projectID Gobierno de España. AYA2010- 15081 es_ES
dc.type.version info:eu-repo/semantics/publishedVersion en
dc.rights.accessRights openAccess en
dc.authorUAM Rosales Ortega, Fernando Fabián (264791)

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