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

Author

Sánchez, S. F., Pérez, E., Rosales Ortega, F. F., Miralles Caballero, D., López Sánchez, A. R., Iglesias Páramo, J., Marino, Raffaella Anna, Sánchez Menguiano, L., García Benito, R., Mast, D., Mendoza, M. A., Papaderos, P., Ellis, S., Galbany, L., Kehrig, C., Monreal Ibero, A., González Delgado, R., Mollá, M., Ziegler, B., de Lorenzo Cáceres, A., Mendez Abreu, J., Bland-Hawthorn, J., Bekeraite, S., Roth, M. M., Pasquali, A., Diaz, A., Bomans, D., van de Ven, G., Wisotzki, L., Sánchez, S. F., Pérez, E., Rosales Ortega, F. F., Miralles Caballero, D., López Sánchez, A. R., Iglesias Páramo, J., Marino, Raffaella Anna, Sánchez Menguiano, L., García Benito, R., Mast, D., Mendoza, M. A., Papaderos, P., Ellis, S., Galbany, L., Kehrig, C., Monreal Ibero, A., González Delgado, R., Mollá, M., Ziegler, B., de Lorenzo Cáceres, A., Mendez Abreu, J., Bland-Hawthorn, J., Bekeraite, S., Roth, M. M., Pasquali, A., Diaz, A., Bomans, D., van de Ven, G., and Wisotzki, L.

Abstract

© 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 (http://califa.caha.es/). 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, 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 i, Viabilidad, Diseño, Acceso y Mejora funding program, ConaCyt funding program, Spanish Ministerio de Economia y Competitividad, FCT Investigator consolidation grant, Fundacao para a Ciencia e a Tecnologia (FCT) - FCT-MEC (PIDDAC), FEDER (COMPETE), Plan Nacional de Investigación y Desarrollo, Ministry of Economy, Development, and Tourism's Millennium Science Initiative, CONICYT through FONDECYT grant, Spanish program of International Campus of Excellence Moncloa (CEI), Agence Nationale de la Recherche through the STILISM project, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Published
2023

2. A characteristic oxygen abundance gradient in galaxy disks unveiled with CALIFA

Author

Sanchez, S. F., Rosales-Ortega, F. F., Iglesias-Paramo, J., Molla, M., Barrera-Ballesteros, J., Marino, R. A., Perez, E., Sanchez-Blazquez, P., Delgado, R. Gonzalez, Fernandes, R. Cid, de Lorenzo-Caceres, A., Mendez-Abreu, J., Galbany, L., Falcon-Barroso, J., Miralles-Caballero, D., Husemann, B., Garcia-Benito, R., Mast, D., Walcher, C. J., de Paz, A. Gil, Garcia-Lorenzo, B., Jungwiert, B., Vilchez, J. M., Jilkova, Lucie, Lyubenova, M., Cortijo-Ferrero, C., Diaz, A. I., Wisotzki, L., Marquez, I., Bland-Hawthorn, J., Ellis, S., van de Ven, G., Jahnke, K., Papaderos, P., Gomes, J. M., Mendoza, M. A., Lopez-Sanchez, Á. R., collaboration, The CALIFA, Science & Technology Facilities Council, and University of St Andrews. School of Physics and Astronomy

Subjects
Absolute magnitude, Astrofísica, HII regions, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Potsdam multiaperture spectrophotometer, FOS: Physical sciences, abundances [Galaxies], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, star formation [Galaxies], 01 natural sciences, Resonance (particle physics), Galactic chemical evolution, Flattening, H-II REGIONS, Radial gas-flows, Abundance (ecology), Ionization, ISM [Galaxies], 0103 physical sciences, Mass-metallicity relation, QB Astronomy, 10. No inequality, 010303 astronomy & astrophysics, Digital sky survey, Astrophysics::Galaxy Astrophysics, QB, abundances [ISM], Effective radius, Physics, Emission-line kinematics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Plasma, evolution [Galaxies], Galaxy, Astronomía, Space and Planetary Science, Inside-out growth, Star forming galaxies, Integral field spectroscopy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the largest and most homogeneous catalog of HII regions and associations compiled so far. The catalog comprises more than 7000 ionized regions, extracted from 306 galaxies observed by the CALIFA survey. We describe the procedures used to detect, select, and analyse the spectroscopic properties of these ionized regions. In the current study we focus on the characterization of the radial gradient of the oxygen abundance in the ionized gas, based on the study of the deprojected distribution of HII regions. We found that all galaxies without clear evidence of an interaction present a common gradient in the oxygen abundance, with a characteristic slope of alpha = -0.1 dex/re between 0.3 and 2 disk effective radii, and a scatter compatible with random fluctuations around this value, when the gradient is normalized to the disk effective radius. The slope is independent of morphology, incidence of bars, absolute magnitude or mass. Only those galaxies with evidence of interactions and/or clear merging systems present a significant shallower gradient, consistent with previous results. The majority of the 94 galaxies with H ii regions detected beyond 2 disk effective radii present a flattening in the oxygen abundance. The flattening is statistically significant. We cannot provide with a conclusive answer regarding the origin of this flattening. However, our results indicate that its origin is most probably related to the secular evolution of galaxies. Finally, we find a drop/truncation of the oxygen abundance in the inner regions for 26 of the galaxies. All of them are non-interacting, mostly unbarred, Sb/Sbc galaxies. This feature is associated with a central star-forming ring, which suggests that both features are produced by radial gas flows induced by resonance processes., 25 Pages, 15 Figures, Accepted for publishing in A&A

Published
2014

3. Kinematic alignment of non-interacting CALIFA galaxies Quantifying the impact of bars on stellar and ionised gas velocity field orientations

Author

Barrera-Ballesteros, J. K., Falcón-Barroso, J., García-Lorenzo, B., van de Ven, G., Aguerri, J. A. L., Mendez-Abreu, J., Spekkens, K., Sánchez, S. F., Husemann, B., Mast, D., García-Benito, R., Iglesias-Paramo, J., del Olmo, A., Márquez, I., Masegosa, J., Kehrig, C., Marino, R. A., Verdes-Montenegro, L., Ziegler, B., MacIntosh, D. H., Bland-Hawthorn, J., Walcher, C. J., and collaboration, the CALIFA

Subjects
Physics, Astrofísica, Field (physics), 010308 nuclear & particles physics, Bar (music), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Kinematics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Astronomía, Gravitational potential, Space and Planetary Science, Position (vector), Astrophysics of Galaxies (astro-ph.GA), Orientation (geometry), 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Disc, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present 80 stellar and ionised gas velocity maps from the Calar Alto Legacy Integral Field Area (CALIFA) survey in order to characterize the kinematic orientation of non-interacting galaxies. The study of galaxies in isolation is a key step towards understanding how fast-external processes, such as major mergers, affect kinematic properties in galaxies. We derived the global and individual (projected approaching and receding sides) kinematic position angles (PAs) for both the stellar and ionised gas line-of-sight velocity distributions. When compared to the photometric PA, we find that morpho-kinematic differences are smaller than 22 degrees in 90% of the sample for both components; internal kinematic misalignments are generally smaller than 16 degrees. We find a tight relation between the global stellar and ionised gas kinematic PA consistent with circular-flow pattern motions in both components. This relation also holds generally in barred galaxies across the bar and galaxy disk scales. Our findings suggest that even in the presence of strong bars, both the stellar and the gaseous components tend to follow the gravitational potential of the disk. As a result, kinematic orientation can be used to assess the degree of external distortions in interacting galaxies., Accepted for publication in A&A

Published
2014

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

Author

Sánchez, S. F., Pérez, E., Rosales Ortega, F. F., Miralles Caballero, D., López Sánchez, Á. R., Iglesias Páramo, J., Marino, Raffaella Anna, Sánchez Menguiano, L., García Benito, R., Mast, D., Mendoza, M. A., Papaderos, P., Ellis, S., Galbany, L., Kehrig, C., Monreal Ibero, A., González Delgado, R., Mollá, M., Ziegler, B., De Lorenzo Cáceres, A., Mendez Abreu, J., Bland-Hawthorn, J., Bekeraite, S., Roth, M. M., Pasquali, A., Diaz, A., Bomans, D., van de Ven, G., Wisotzki, L., Sánchez, S. F., Pérez, E., Rosales Ortega, F. F., Miralles Caballero, D., López Sánchez, Á. R., Iglesias Páramo, J., Marino, Raffaella Anna, Sánchez Menguiano, L., García Benito, R., Mast, D., Mendoza, M. A., Papaderos, P., Ellis, S., Galbany, L., Kehrig, C., Monreal Ibero, A., González Delgado, R., Mollá, M., Ziegler, B., De Lorenzo Cáceres, A., Mendez Abreu, J., Bland-Hawthorn, J., Bekeraite, S., Roth, M. M., Pasquali, A., Diaz, A., Bomans, D., van de Ven, G., and Wisotzki, L.

Abstract

© 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 (http://califa.caha.es/). 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, 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 i, Viabilidad, Diseño, Acceso y Mejora funding program, ConaCyt funding program, Spanish Ministerio de Economia y Competitividad, FCT Investigator consolidation grant, Fundacao para a Ciencia e a Tecnologia (FCT) - FCT-MEC (PIDDAC), FEDER (COMPETE), Plan Nacional de Investigación y Desarrollo, Ministry of Economy, Development, and Tourism's Millennium Science Initiative, CONICYT through FONDECYT grant, Spanish program of International Campus of Excellence Moncloa (CEI), Agence Nationale de la Recherche through the STILISM project, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Published
2015

5. Outer-disk reddening and gas-phase metallicities: The CALIFA connection

Author

Marino, Raffaella Anna, Gil De Paz, Armando, Sánchez, S. F., Sánchez Blázquez, Patricia, Cardiel López, Nicolás, Castillo Morales, María África, Pascual Ramírez, Sergio, Vílchez, J., Kehrig, C., Mollá, M., Mendez Abreu, J., Catalán Torrecilla, Cristina, Florido, E., Perez, I., Ruiz Lara, T., Ellis, S., López Sánchez, Á. R., González Delgado, R. M., De Lorenzo Cáceres, A., García Benito, R., Galbany, L., Zibetti, S., Cortijo, C., Kalinova, V., Mast, D., Iglesias Páramo, J., Papaderos, P., Walcher, C. J., Bland Hawthorn, J., CALIFA Team, Marino, Raffaella Anna, Gil De Paz, Armando, Sánchez, S. F., Sánchez Blázquez, Patricia, Cardiel López, Nicolás, Castillo Morales, María África, Pascual Ramírez, Sergio, Vílchez, J., Kehrig, C., Mollá, M., Mendez Abreu, J., Catalán Torrecilla, Cristina, Florido, E., Perez, I., Ruiz Lara, T., Ellis, S., López Sánchez, Á. R., González Delgado, R. M., De Lorenzo Cáceres, A., García Benito, R., Galbany, L., Zibetti, S., Cortijo, C., Kalinova, V., Mast, D., Iglesias Páramo, J., Papaderos, P., Walcher, C. J., Bland Hawthorn, J., and CALIFA Team

Abstract

We study, for the first time in a statistically significant and well-defined sample, the relation between the outer-disk ionized-gas metallicity gradients and the presence of breaks in the surface brightness profiles of disk galaxies. Sloan Digital Sky Survey (SDSS) g′- and r′-band surface brightness, (g′ – r′) color, and ionized-gasoxygen abundance profiles for 324 galaxies within the Calar Alto Legacy Integral Field Area (CALIFA) survey are used for this purpose. We perform a detailed light-profile classification, finding that 84% of our disks show down- or up-bending profiles (Type II and Type III, respectively), while the remaining 16% are well fitted by one single exponential (Type I). The analysis of the color gradients at both sides of this break shows a U-shaped profile for most Type II galaxies with an average minimum (g′ − r′) color of ~0.5 mag and an ionized-gas metallicity flattening associated with it only in the case of low-mass galaxies. Comparatively, more massive systems show a rather uniform negative metallicity gradient. The correlation between metallicity flattening and stellar mass for these systems results in p-values as low as 0.01. Independent of the mechanism having shaped the outer light profiles of these galaxies, stellar migration or a previous episode of star formation in a shrinking star-forming disk, it is clear that the imprint in their ionized-gas metallicity was different for low- and high-mass Type II galaxies. In the case of Type III disks, a positive correlation between the change in color and abundance gradient is found (the null hypothesis is ruled out with a p-value of 0.02), with the outer disks of Type III galaxies with masses ≤10^10 M_⊙ showing a weak color reddening or even a bluing. This is interpreted as primarily due to a mass downsizing effect on the population of Type III galaxies that recently experienced an enhanced inside-out growth., Unión Europea - FP7, Ministerio de Economía, Comercio y Empresa (España), Campus de Excelencia Internacional Moncloa, Unión Europea - Acciones Marie Curie, Ministerio de Educación, Formación Profesional y Deportes (España), Ministry of Economy, Development, and Tourism's Millennium Science Initiative, Fondo Nacional de Desarrollo Científico, Tecnológico y de Innovación Tecnológica (Chile), Iniciativa Científica Milenio (Chile), FCT Investigator Programme (Portugal), Ministério da Educação e Ciência (Portugal), Dirección General Asuntos del Personal Académico - Universidad Nacional Autónoma de México, Fondo Europeo de Desarrollo Regional, Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016 I+D+i - Ministerio de Economía, Comercio y Empresa (España), Ministerio Economía, Fomento y Turismo (Chile), Millennium Institute of Astrophysics, Comisión Nacional de Investigación Científica y Tecnológica (Chile), Universidad Nacional Autónoma de México, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

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