Imprints of galaxy evolution on H II regions: memory of the past uncovered by the CALIFA survey



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Sánchez, S. F. and Pérez, E. and Rosales Ortega, F. F. and Miralles Caballero, D. and López Sánchez, A. R. and Iglesias Páramo, J. and Marino, Raffaella Anna and Sánchez Menguiano, L. and García Benito, R. and Mast, D. and Mendoza, M. A. and Papaderos, P. and Ellis, S. and Galbany, L. and Kehrig, C. and Monreal Ibero, A. and González Delgado, R. and Mollá, M. and Ziegler, B. and de Lorenzo Cáceres, A. and Mendez Abreu, J. and Bland-Hawthorn, J. and Bekeraite, S. and Roth, M. M. and Pasquali, A. and Diaz, A. and Bomans, D. and van de Ven, G. and Wisotzki, L. (2015) Imprints of galaxy evolution on H II regions: memory of the past uncovered by the CALIFA survey. Astronomy & Astrophysics, 574 . ISSN 0004-6361

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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] lambda 5007/H beta vs. [N II] lambda 6583/H alpha 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 affected 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.

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© ESO 2014. Artículo firmado por 29 autores y la colaboración de CALIFA. We thank Prf. Dr. M. Dopita for his comments and suggestions during the reviewing process. He helped to improve significantly the interpretation of our results and the overall manuscript. S.F.S. thanks the director of CEFCA, M. Moles, for his sincere support to this project. This study makes uses of the data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey ( CALIFA is the first legacy survey being performed at Calar Alto. The CALIFA collaboration would like to thank the IAA-CSIC and MPIA-MPG as major partners of the observatory and CAHA itself, for the unique access to telescope time and support in manpower and infrastructures. The CALIFA collaboration also thanks the CAHA staff for the dedication to this project. This work was based on observations collected at the Centro Astronómico Hispano Aleman (CAHA) at Calar Alto, operated jointly by the Max-Planck-Institut fur Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). 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.ES., 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 Fundacao para a Ciencia e a Tecnología (FCT) under project FCOMP-010124-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).

Uncontrolled Keywords:Integral field spectroscopy; Star-forming galaxies; Mass-metallicity relation; Spectral energy-distribution; Potsdam multiaperture spectrophotometer; Oxygen abundance gradient; Ionized gaseous nebulae; Active galactic nuclei; Small-magellanic-cloud; Emission-line spectra
Subjects:Sciences > Physics > Astrophysics
Sciences > Physics > Astronomy
Sciences > Physics > Atmospheric physics
ID Code:29623
Deposited On:21 Apr 2015 12:15
Last Modified:10 Dec 2018 15:05

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