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524 results on '"García Benito, R."'

155. A bayesian-like approach to derive chemical abundances in Type-2 Active Galactic Nuclei based on photoionization models

Author

Pérez Montero, Enrique, Dors, Oli L., Vílchez, José M., García Benito, R., Cardaci, Mónica Viviana, and Hägele, Guillermo Federico

Subjects
Astronomía, galaxies: abundances, methods: data analysis, Astrophysics::Galaxy Astrophysics, ISM: abundances
Abstract

We present a new methodology for the analysis of the emission lines of the interstellar medium in the narrow-line regions around type-2 active galactic nuclei. Our aim is to provide a recipe that can be used for large samples of objects in a consistent way using different sets of optical emission lines that takes into the account possible variations from the O/H–N/O relation to use [N II] lines. Our approach consists of a bayesian-like comparison between certain observed emission-line ratios sensitive to total oxygen abundance, nitrogen-to-oxygen ratio, and ionization parameter with the predictions from a large grid of photoionization models calculated under the most usual conditions in this environment. We applied our method to a sample of Seyfert 2 galaxies with optical emission-line fluxes and determinations of their chemical properties from detailed models in the literature. Our results agree within the errors with other results and confirm the high metallicity of the objects of the sample, with N/O values consistent with a large secondary production of N, but with a large dispersion. The obtained ionization parameters for this sample are much larger than those for star-forming object at the same metallicity., Facultad de Ciencias Astronómicas y Geofísicas, Instituto de Astrofísica de La Plata

Published
2019

156. The CALIFA view on stellar angular momentum across the Hubble sequence

Author

Falcón-Barroso, J., primary, van de Ven, G., additional, Lyubenova, M., additional, Mendez-Abreu, J., additional, Aguerri, J. A. L., additional, García-Lorenzo, B., additional, Bekeraité, S., additional, Sánchez, S. F., additional, Husemann, B., additional, García-Benito, R., additional, González Delgado, R. M., additional, Mast, D., additional, Walcher, C. J., additional, Zibetti, S., additional, Zhu, L., additional, Barrera-Ballesteros, J. K., additional, Galbany, L., additional, Sánchez-Blázquez, P., additional, Singh, R., additional, van den Bosch, R. C. E., additional, Wild, V., additional, Bland-Hawthorn, J., additional, Cid Fernandes, R., additional, de Lorenzo-Cáceres, A., additional, Gallazzi, A., additional, Marino, R. A., additional, Márquez, I., additional, Peletier, R. F., additional, Pérez, E., additional, Pérez, I., additional, Roth, M. M., additional, Rosales-Ortega, F. F., additional, Ruiz-Lara, T., additional, Wisotzki, L., additional, and Ziegler, B., additional

Published
2019
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157. A few StePS forward in unveiling the complexity of galaxy evolution: light-weighted stellar ages of intermediate-redshift galaxies with WEAVE

Author

Costantin, L., primary, Iovino, A., additional, Zibetti, S., additional, Longhetti, M., additional, Gallazzi, A., additional, Mercurio, A., additional, Lonoce, I., additional, Balcells, M., additional, Bolzonella, M., additional, Busarello, G., additional, Dalton, G., additional, Ferré-Mateu, A., additional, García-Benito, R., additional, Gargiulo, A., additional, Haines, C., additional, Jin, S., additional, La Barbera, F., additional, McGee, S., additional, Merluzzi, P., additional, Morelli, L., additional, Murphy, D. N. A., additional, Peralta de Arriba, L., additional, Pizzella, A., additional, Poggianti, B. M., additional, Pozzetti, L., additional, Sánchez-Blázquez, P., additional, Talia, M., additional, Tortora, C., additional, Trager, S. C., additional, Vazdekis, A., additional, Vergani, D., additional, and Vulcani, B., additional

Published
2019
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159. The spatially resolved star formation history of mergers: A comparative study of the LIRGs IC 1623, NGC 6090, NGC 2623, and Mice

Author

Cortijo-Ferrero, C., González Delgado, R., Perez, Emile, Cid Fernandes, R., García-Benito, R., Di Matteo, P., Sanchez, Sébastien, de Amorim, A., Lacerda, E., López Fernández, R., Tadhunter, C., Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique des interactions ondes matières (LPIOM), Université Sciences et Technologies - Bordeaux 1 (UB)-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Centre National de la Recherche Scientifique (CNRS), and Université Sciences et Technologies - Bordeaux 1-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Centre National de la Recherche Scientifique (CNRS)

Subjects
techniques: imaging spectroscopy, galaxies: stellar content, galaxies: interactions, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; This paper presents the spatially resolved star formation history (2D-SFH) of a small sample of four local mergers: the early-stage mergers IC 1623, NGC 6090, and the Mice, and the more advanced merger NGC 2623, by analyzing IFS data from the CALIFA survey and PMAS in LArr mode. Full spectral fitting techniques are applied to the datacubes to obtain the spatially resolved mass growth histories, the time evolution of the star formation rate intensity (ΣSFR), and the local specific star formation rate (sSFR), over three different time scales (30 Myr, 300 Myr, and 1 Gyr). The results are compared with non-interacting Sbc–Sc galaxies, to quantify if there is an enhancement of the star formation and to trace its time scale and spatial extent. Our results for the three LIRGs (IC 1623 W, NGC 6090, and NGC 2623) show that a major phase of star formation is occurring in time scales of 107 yr to few 108 yr, with global SFR enhancements of between approximately two and six with respect to main-sequence star forming (MSSF) galaxies. In the two early-stage mergers IC 1623 W and NGC 6090, which are between first pericentre passage and coalescence, the most remarkable increase of the SFR with respect to non-interacting spirals occurred in the last 30 Myr, and it is spatially extended, with enhancements of factors between two and seven both in the centres (r < 0.5 half light radius, HLR), and in the disks (r > 1 HLR). In the more advanced merger NGC 2623 an extended phase of star formation occurred on a longer time scale of ~1 Gyr, with a SFR enhancement of a factor of approximately two-to-three larger than the one in Sbc–Sc MSSF galaxies over the same period, probably relic of the first pericentre passage epoch. A SFR enhancement in the last 30 Myr is also present, but only in NGC 2623 centre, by a factor of three. In general, the spatially resolved SFHs of the LIRG-mergers are consistent with the predictions from high spatial resolution simulations. In contrast, the star formation in the Mice, specially in Mice B, is not enhanced but inhibited with respect to Sbc–Sc MSSF galaxies. The fact that the gas fraction of Mice B is smaller than in most non-interacting spirals, and that the Mice are close to a prograde orbit, represents a new challenge for the models, which must cover a larger space of parameters in terms of the availability of gas and the orbital characteristics.

Published
2017
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164. PISCO: The PMAS/PPak Integral-field Supernova Hosts Compilation

Author

Galbany, L., primary, Anderson, J. P., additional, Sánchez, S. F., additional, Kuncarayakti, H., additional, Pedraz, S., additional, González-Gaitán, S., additional, Stanishev, V., additional, Domínguez, I., additional, Moreno-Raya, M. E., additional, Wood-Vasey, W. M., additional, Mourão, A. M., additional, Ponder, K. A., additional, Badenes, C., additional, Mollá, M., additional, López-Sánchez, A. R., additional, Rosales-Ortega, F. F., additional, Vílchez, J. M., additional, García-Benito, R., additional, and Marino, R. A., additional

Published
2018
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165. CALIFA, the Calar Alto Legacy Integral Field Area survey

Author

Sanchez, Sébastien, García-Benito, R., Zibetti, S., Walcher, C., Husemann, B., Mendoza, M., Galbany, L., Falcón-Barroso, J., Mast, D., Aceituno, J., Aguerri, J., Alves, J., Amorim, A., Ascasibar, Y., Barrado-Navascues, D., Barrera-Ballesteros, J., Bekeraitè, S., Bland-Hawthorn, J., Cano Díaz, M., Cid Fernandes, R., Cavichia, O., Cortijo, C., Dannerbauer, H., Demleitner, M., Díaz, A., Dettmar, R., de Lorenzo-Cáceres, A., del Olmo, A., Galazzi, A., García-Lorenzo, B., Gil de Paz, A., González Delgado, R., Holmes, L., Iglesias-Paramo, J., Kehrig, C., Kelz, A., Kennicutt, R., Kleemann, B., Lacerda, E., López Fernández, R., López Sánchez, A., Lyubenova, M., Marino, R., Márquez, I., Mendez-Abreu, J., Mollá, M., Monreal-Ibero, A., Ortega Minakata, R., Torres-Papaqui, J., Perez, Emile, Rosales-Ortega, F., Roth, M., Sánchez-Blázquez, P., Schilling, U., Spekkens, K., Vale Asari, N., van den Bosch, R., van de Ven, G., Vilchez, J., Wild, V., Wisotzki, L., Yildirim, A., Ziegler, B., Laboratoire de l'intégration, du matériau au système (IMS), Centre National de la Recherche Scientifique (CNRS)-Institut Polytechnique de Bordeaux-Université Sciences et Technologies - Bordeaux 1, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Department of Physics [Pittsburgh], Carnegie Mellon University [Pittsburgh] (CMU), Instituto Dom Luiz, Universidade de Lisboa (ULISBOA), Laboratory for Systems, Instrumentation and Modeling in Science and Technology for Space and the Environment (University of Lisbon and University of Beira Interior), CRLCC Val d'Aurelle - Paul Lamarque, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, Heidelberg, Germany, Astronomisches Institut der Ruhr-Universität Bochum, Ruhr-Universität Bochum [Bochum], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Avancé de Spectroscopie pour les Intéractions la Réactivité et l'Environnement - UMR 8516 (LASIRE), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Princeton University, Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid (UAM), Departamento de Tecnociencias,Centro de Ciencias Aplicadas y Desarrollo Tecnologico, Universidad Nacional Autonoma de Mexico, Universidad Nacional Autónoma de México (UNAM), Leibniz-Institut für Astrophysik Potsdam (AIP), European Southern Observatory (ESO), Millennium Institute of Astrophysics, Universidad de Chile, Instituto de Astrofisica de Canarias (IAC), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET), Centro Astronómico Hispano Alemán, Observatorio de Calar Alto (CAHA), University of Vienna [Vienna], Departamento Física [Florianópolis], Universidade Federal de Santa Catarina = Federal University of Santa Catarina [Florianópolis] (UFSC), Department of Physics and Astronomy [Baltimore], Johns Hopkins University (JHU), Sydney Institute for Astronomy (SIfA), The University of Sydney, Universidade Federal de Itajubá, SUPA School of Physics and Astronomy [University of St Andrews], University of St Andrews [Scotland]-Scottish Universities Physics Alliance (SUPA), Universidad de Granada (UGR), Departamento de Astrofisica y Ciencias de la Atmósfera, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Royal Military College of Canada (RMCC), Royal Military College of Canada, Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Departamento de Física [Universidade Federal de Santa Catarina], Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Centro de Investigaciones Energéticas Medioambientales y Tecnológicas [Madrid] (CIEMAT), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Observatório do Valongo/UFRJ [Rio de Janeiro], Universidade Federal do Rio de Janeiro (UFRJ), Universidad de Guanajuato, ANR-12-BS05-0016,STILISM,Structure du Milieu Interstellaire Local par Inversion(2012), European Project: 326466,EC:FP7:PEOPLE,FP7-PEOPLE-2012-CIG,STEMAGE(2013), European Project: 289313,EC:FP7:PEOPLE,FP7-PEOPLE-2011-ITN,DAGAL(2012), European Project: 267251,EC:FP7:PEOPLE,FP7-PEOPLE-2010-COFUND,ASTROFIT(2011), European Project: 306299,EC:FP7:ERC,ERC-2012-StG_20111012,SEDMORPH(2012), European Project: 303912,EC:FP7:PEOPLE,FP7-PEOPLE-2011-CIG,SFEHG(2012), European Project: 612701,EC:FP7:PEOPLE,FP7-PEOPLE-2013-IRSES,SELGIFS(2013), Université Sciences et Technologies - Bordeaux 1-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire de Spectrochimie Infrarouge et Raman - UMR 8516 (LASIR), Centre National de la Recherche Scientifique (CNRS)-Université de Lille, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Universidad de Chile = University of Chile [Santiago] (UCHILE), Universidad Autónoma de Madrid (UAM), Universität Heidelberg [Heidelberg] = Heidelberg University, and Universidad de Granada = University of Granada (UGR)

Subjects
[PHYS]Physics [physics], Galaxies: fundamental parameters, Techniques: imaging spectroscopy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic, ComputingMilieux_MISCELLANEOUS
Abstract

International audience; This paper describes the Third Public Data Release (DR3) of the Calar Alto Legacy Integral Field Area (CALIFA) survey. Sciencegrade quality data for 667 galaxies are made public, including the 200 galaxies of the Second Public Data Release (DR2). Data were obtained with the integral-field spectrograph PMAS/PPak mounted on the 3.5m telescope at the Calar Alto Observatory. Three different spectral setups are available, i) a low-resolution V500 setup covering the wavelength range 3745–7500 Å (4240-7140 Å unvignetted) with a spectral resolution of 6.0 Å (FWHM), for 646 galaxies, ii) a medium-resolution V1200 setup covering the wavelength range 3650–4840 Å (3650-4620 Å unvignetted) with a spectral resolution of 2.3 Å (FWHM), for 484 galaxies, and iii) the combination of the cubes from both setups (called COMBO), with a spectral resolution of 6.0 Å and a wavelength range between 3700-7500 Å (3700-7140 Å unvignetted), for 446 galaxies. The Main Sample, selected and observed according to the CALIFA survey strategy covers a redshift range between 0.005 and 0.03, spans the color-magnitude diagram and probes a wide range of stellar mass, ionization conditions, and morphological types. The Extension Sample covers several types of galaxies that are rare in the overall galaxy population and therefore not numerous or absent in the CALIFA Main Sample. All the cubes in the data release were processed using the latest pipeline, which includes improved versions of the calibration frames and an even further improved image reconstruction quality. In total, the third data release contains 1576 datacubes, including ∼1.5 million independent spectra. It is available at http://califa.caha.es/DR3.

Published
2016
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166. Nearby supernova host galaxies from the CALIFA survey

Author

Galbany, L., Stanishev, V., Mourao, A., Rodrigues, M., Flores, H., Walcher, C., Sanchez, Sébastien, García-Benito, R., Mast, D., Badenes, C., González Delgado, R., Kehrig, C., Lyubenova, M., Marino, R., Mollá, M., Meidt, S., Perez, Emile, van de Ven, G., Vílchez, J., Department of Physics [Pittsburgh], Carnegie Mellon University [Pittsburgh] (CMU), Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), inconnu, Inconnu, Instituto de Ciências Agrárias, Universidade Federal de Minas Gerais [Belo Horizonte] (UFMG), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique des interactions ondes matières (LPIOM), Université Sciences et Technologies - Bordeaux 1-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and Université Sciences et Technologies - Bordeaux 1 (UB)-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2016
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167. Star formation along the Hubble sequence: Radial structure of the star formation of CALIFA galaxies

Author

González Delgado, RM, Cid Fernandes, R, Pérez, E, García-Benito, R, López Fernández, R, Lacerda, EAD, Cortijo-Ferrero, C, De Amorim, AL, Vale Asari, N, Sánchez, SF, Walcher, CJ, Wisotzki, L, Mast, D, Alves, J, Ascasibar, Y, Bland-Hawthorn, J, Galbany, L, Kennicutt, RC, Márquez, I, Masegosa, J, Mollá, M, Sánchez-Blázquez, P, Vílchez, JM, Kennicutt, Robert [0000-0001-5448-1821], and Apollo - University of Cambridge Repository

Subjects
galaxies: star formation, galaxies: stellar content, galaxies: evolution, techniques: spectroscopic
Abstract

© ESO, 2016. The spatially resolved stellar population content of today's galaxies holds important information for understanding the different processes that contribute to the star formation and mass assembly histories of galaxies. The aim of this paper is to characterize the radial structure of the star formation rate (SFR) in galaxies in the nearby Universe as represented by a uniquely rich and diverse data set drawn from the CALIFA survey. The sample under study contains 416 galaxies observed with integral field spectroscopy, covering a wide range of Hubble types and stellar masses ranging from M∗ ∼ 109 to 7 × 1011 M⊙. Spectral synthesis techniques are applied to the datacubes to derive 2D maps and radial profiles of the intensity of the star formation rate in the recent past (ΣSFR), as well as related properties, such as the local specific star formation rate (sSFR), defined as the ratio between ΣSFR and the stellar mass surface density (μ∗). To emphasize the behavior of these properties for galaxies that are on and off the main sequence of star formation (MSSF), we stack the individual radial profiles in seven bins of galaxy morphology (E, S0, Sa, Sb, Sbc, Sc, and Sd), and several stellar masses. Our main results are: (a) the intensity of the star formation rate shows declining profiles that exhibit very small differences between spirals with values at R = 1 half light radius (HLR) within a factor two of ΣSFR ∼ 20 M⊙Gyr-1pc-2. The dispersion in the ΣSFR(R) profiles is significantly smaller in late type spirals (Sbc, Sc, Sd). This confirms that the MSSF is a sequence of galaxies with nearly constant ΣSFR. (b) sSFR values scale with Hubble type and increase radially outward with a steeper slope in the inner 1 HLR. This behavior suggests that galaxies are quenched inside-out and that this process is faster in the central, bulge-dominated part than in the disks. (c) As a whole and at all radii, E and S0 are off the MSSF with SFR much smaller than spirals of the same mass. (d) Applying the volume corrections for the CALIFA sample, we obtain a density of star formation in the local Universe of ρSFR = (0.0105 ± 0.0008) M⊙yr-1Mpc-3, in agreement with independent estimates. Most of the star formation is occurring in the disks of spirals. (e) The volume-averaged birthrate parameter, which measures the current SFR with respect to its lifetime average, b′ = 0.39 ± 0.03, suggests that the present day Universe is forming stars a about one-third of its past average rate. E, S0, and the bulge of early type spirals (Sa, Sb) contribute little to the recent SFRof the Universe, which is dominated by the disks of Sbc, Sc, and Sd spirals. (f) There is a tight relation between ΣSFR and μ∗, defining a local MSSF relation with a logarithmic slope of 0.8, similar to the global MSSF relation between SFR and M∗. This suggests that local processes are important in determining the star formation in disks, probably through a density dependence of the SFR law. The scatter in the local MSSF is driven by morphology-related offsets, with ΣSFR/μ∗ (the local sSFR) increasing from early to late type galaxies, indicating that the shut down of the star formation is more related to global processes, such as the formation of a spheroidal component.

Published
2016

168. The host of the Type I SLSN 2017egm

Author

Izzo, L., primary, Thöne, C. C., additional, García-Benito, R., additional, de Ugarte Postigo, A., additional, Cano, Z., additional, Kann, D. A., additional, Bensch, K., additional, Della Valle, M., additional, Galadí-Enríquez, D., additional, and Hedrosa, R. P., additional

Published
2018
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169. Outer-disk reddening and gas-phase metallicities: The CALIFA connection

Author

Sánchez-Blázquez, Patricia, Marino, R. A., Gil De Paz, A., Sánchez, S. F., Cardiel, N., Castillo- Morales, A., Pascual, S., Vílchez, J., Kehrig, C., Mollá, M., Méndez-Abreu, Jairo, Catalán-Torrecilla, C., Florido, E., Perez, I., Ruiz-Lara, T., Ellis, S., López-Sánchez, A. R., González Delgado, R.M, De Lorenzo-Cáceres, A., García-Benito, R., Galbany, L., Cortijo, C., Kalinova, V., Mast, D., Iglesias-Páramo, J., Papaderos, P., Walcher, C.J., Bland-Hawthorn, J., Zibetti, S., CALIFA Team, UAM. Departamento de Física Teórica, Campus de Excelencia Internacional Moncloa, Ministerio de Economía y Competitividad (España), European Commission, Ministerio de Educación, Cultura y Deporte (España), Instituto Milenio de Astrofísica (Chile), Comisión Nacional de Investigación Científica y Tecnológica (Chile), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), Consejo Nacional de Ciencia y Tecnología (México), European Research Council, and Fundação para a Ciência e a Tecnologia (Portugal)

Subjects
Astrofísica, Stellar mass, Galaxies: abundances, Hii regions, Ciencias Físicas, Metallicity, Population, FOS: Physical sciences, ISM [GALAXIES], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Type (model theory), 01 natural sciences, Flattening, ISM: abundances, purl.org/becyt/ford/1 [https], HII REGIONS, 0103 physical sciences, ABUNDANCES [ISM], Surface brightness, ABUNDANCES [GALAXIES], education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, EVOLUTION [GALAXIES], Physics, education.field_of_study, 010308 nuclear & particles physics, Star formation, Galaxies: evolution, Física, Astronomy and Astrophysics, Galaxies: photometry, PHOTOMETRY [GALAXIES], purl.org/becyt/ford/1.3 [https], Astrophysics - Astrophysics of Galaxies, Galaxy, Astronomía, Galaxies: ISM, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, CIENCIAS NATURALES Y EXACTAS
Abstract

Based on observations collected at the German-Spanish Astronomical Center, Calar Alto, jointly operated by the Max-Planck-Institut für Astronomie Heidelberg and the Instituto de Astrofísica de Andalucía (CSIC )., CALIFA Team: et al., 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-gas oxygen 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 ∼ 0.5mag 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 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., R. A. Marino is funded by the Spanish program of International Campus of Excellence Moncloa (CEI).We acknowledge support from the Plan Nacional de Investigación y Desarrollo funding programs, AyA2010-15081, AyA2012-30717 and AyA2013-46724P, of Spanish Ministerio de Economía y Competitividad (MINECO). A.G.d.P. acknowledges the support from the FP7 Marie Curie Actions of the European Commission, via the Initial Training Network DAGAL under REA grant agreement PITNGA-2011-289313. C.C.-T. thanks the support of the Spanish Ministerio de Educación, Cultura y Deporte by means of the FPU fellowship program. C.J.W. acknowledges support through the Marie Curie Career Integration Grant 303912. Support for L.G. is provided by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC 120009, awarded to The Millennium Institute of Astrophysics, MAS. L.G. acknowledges support by CONICYT through FONDECYT grant 3140566. S.F.S. thanks the CONACYT-125180 and DGAPA-IA100815 projects for providing him support in this study. J.M.A. acknowledges support from the European Research Council Starting Grant (SEDmorph; P.I. V. Wild). P.P. is supported by FCT through the Investigador FCT Contract No. IF/01220/2013 and POPH/FSE (EC) by FEDER funding through the program COMPETE. He also acknowledges support by FCT under project FCOMP-01-0124-FEDER-029170 (Reference FCT PTDC/FISAST/3214/2012), funded by FCT-MEC (PIDDAC) and FEDER (COMPETE).

Published
2016

170. The EDGE–CALIFA survey: the influence of galactic rotation on the molecular depletion time across the Hubble sequence

Author

Colombo, D, primary, Kalinova, V, additional, Utomo, D, additional, Rosolowsky, E, additional, Bolatto, A D, additional, Levy, R C, additional, Wong, T, additional, Sanchez, S F, additional, Leroy, A K, additional, Ostriker, E, additional, Blitz, L, additional, Vogel, S, additional, Mast, D, additional, García-Benito, R, additional, Husemann, B, additional, Dannerbauer, H, additional, Ellmeier, L, additional, and Cao, Y, additional

Published
2017
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172. Spatially-resolved star formation histories of CALIFA galaxies

Author

González Delgado, R. M., primary, Pérez, E., additional, Cid Fernandes, R., additional, García-Benito, R., additional, López Fernández, R., additional, Vale Asari, N., additional, Cortijo-Ferrero, C., additional, de Amorim, A. L., additional, Lacerda, E. A. D., additional, Sánchez, S. F., additional, Lehnert, M. D., additional, and Walcher, C. J., additional

Published
2017
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173. Morpho-kinematic properties of field S0 bulges in the CALIFA survey

Author

Méndez-Abreu, J., primary, Aguerri, J. A. L., additional, Falcón-Barroso, J., additional, Ruiz-Lara, T., additional, Sánchez-Menguiano, L., additional, de Lorenzo-Cáceres, A., additional, Costantin, L., additional, Catalán-Torrecilla, C., additional, Zhu, L., additional, Sánchez-Blazquez, P., additional, Florido, E., additional, Corsini, E. M., additional, Wild, V., additional, Lyubenova, M., additional, van de Ven, G., additional, Sánchez, S. F., additional, Bland-Hawthorn, J., additional, Galbany, L., additional, García-Benito, R., additional, García-Lorenzo, B., additional, Delgado, R. M. González, additional, López-Sánchez, A. R., additional, Marino, R. A., additional, Márquez, I., additional, Ziegler, B., additional, and collaboration, the CALIFA, additional

Published
2017
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174. The spatially resolved stellar population and ionized gas properties in the merger LIRG NGC 2623

Author

Cortijo-Ferrero, C., primary, González Delgado, R. M., additional, Pérez, E., additional, Sánchez, S. F., additional, Cid Fernandes, R., additional, de Amorim, A. L., additional, Di Matteo, P., additional, García-Benito, R., additional, Lacerda, E. A. D., additional, López Fernández, R., additional, Tadhunter, C., additional, Villar-Martín, M., additional, and Roth, M. M., additional

Published
2017
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176. Arm and interarm abundance gradients in CALIFA spiral galaxies

Author

Sánchez-Menguiano, L., primary, Sánchez, S. F., additional, Pérez, I., additional, Debattista, V. P., additional, Ruiz-Lara, T., additional, Florido, E., additional, Cavichia, O., additional, Galbany, L., additional, Marino, R. A., additional, Mast, D., additional, Sánchez-Blázquez, P., additional, Méndez-Abreu, J., additional, de Lorenzo-Cáceres, A., additional, Catalán-Torrecilla, C., additional, Cano-Díaz, M., additional, Márquez, I., additional, McIntosh, D. H., additional, Ascasibar, Y., additional, García-Benito, R., additional, Gónzalez Delgado, R. M., additional, Kehrig, C., additional, López-Sánchez, Á. R., additional, Mollá, M., additional, Bland-Hawthorn, J., additional, Walcher, C. J., additional, and Costantin, L., additional

Published
2017
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177. Towards a new classification of galaxies: principal component analysis of CALIFA circular velocity curves

Author

Kalinova, V., primary, Colombo, D., additional, Rosolowsky, E., additional, Kannan, R., additional, Galbany, L., additional, García-Benito, R., additional, González Delgado, R., additional, Sánchez, S. F., additional, Ruiz-Lara, T., additional, Méndez-Abreu, J., additional, Catalán-Torrecilla, C., additional, Sánchez-Menguiano, L., additional, de Lorenzo-Cáceres, A., additional, Costantin, L., additional, Florido, E., additional, Kodaira, K., additional, Marino, R. A., additional, Läsker, R., additional, and Bland-Hawthorn, J., additional

Published
2017
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178. The mass–metallicity relation revisited with CALIFA

Author

Sánchez, S. F., primary, Barrera-Ballesteros, J. K., additional, Sánchez-Menguiano, L., additional, Walcher, C. J., additional, Marino, R. A., additional, Galbany, L., additional, Bland-Hawthorn, J., additional, Cano-Díaz, M., additional, García-Benito, R., additional, López-Cobá, C., additional, Zibetti, S., additional, Vilchez, J. M., additional, Iglésias-Páramo, J., additional, Kehrig, C., additional, López Sánchez, A. R., additional, Duarte Puertas, S., additional, and Ziegler, B., additional

Published
2017
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179. Star formation in the local Universe from the CALIFA sample

Author

Catalán-Torrecilla, C., Gil De Paz, A., Castillo-Morales, A., Iglesias-Paramo, J., Sanchez, Sébastien, Kennicutt, R., Pérez-González, P., Marino, R., Walcher, C., Husemann, B., García-Benito, R., Mast, D., González Delgado, R., Muñoz-Mateos, J., Bland-Hawthorn, J., Bomans, D., Del Olmo, A., Galbany, L., Gomes, J., Kehrig, C., López-Sánchez, Á., Mendoza, M., Monreal-Ibero, A., Pérez-Torres, M., Sánchez-Blázquez, P., Vilchez, J., the CALIFA, collaboration, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'intégration, du matériau au système (IMS), Centre National de la Recherche Scientifique (CNRS)-Institut Polytechnique de Bordeaux-Université Sciences et Technologies - Bordeaux 1, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), The University of Sydney, Ruhr-Universität Bochum [Bochum], Department of Physics [Pittsburgh], Carnegie Mellon University [Pittsburgh] (CMU), Philippine General Hospital, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid (UAM), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and Universidad Autónoma de Madrid (UAM)

Subjects
[PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2015
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180. Tracing kinematic (mis)alignments in CALIFA merging galaxies

Author

Barrera-Ballesteros, J., García-Lorenzo, B., Falcón-Barroso, J., van de Ven, G., Lyubenova, M., Wild, V., Méndez-Abreu, J., Sanchez, Sébastien, Marquez, I., Masegosa, J., Monreal-Ibero, A., Ziegler, B., Del Olmo, A., Verdes-Montenegro, L., García-Benito, R., Husemann, B., Mast, D., Kehrig, C., Iglesias-Paramo, J., Marino, R., Aguerri, J., Walcher, C., Vílchez, J., Bomans, D., Cortijo-Ferrero, C., González Delgado, R., Bland-Hawthorn, J., McIntosh, D., Bekeraitė, S., Laboratoire de l'intégration, du matériau au système (IMS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Ruhr-Universität Bochum [Bochum], The University of Sydney, Centre National de la Recherche Scientifique (CNRS)-Institut Polytechnique de Bordeaux-Université Sciences et Technologies - Bordeaux 1, Université Nice Sophia Antipolis (... - 2019) (UNS), and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS]Physics [physics], [SDU]Sciences of the Universe [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2015
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181. CALIFA, the Calar Alto Legacy Integral Field Area survey

Author

García-Benito, R., Zibetti, S., Sanchez, Sébastien, Husemann, B., de Amorim, A., Castillo-Morales, A., Cid Fernandes, R., Ellis, S., Falcón-Barroso, J., Galbany, L., Gil de Paz, A., González Delgado, R., Lacerda, E., Lopez-Fernandez, R., de Lorenzo-Cáceres, A., Lyubenova, M., Marino, R., Mast, D., Mendoza, M., Perez, Emile, Vale Asari, N., Aguerri, J., Ascasibar, Y., Bekerait*error*ė, S., Bland-Hawthorn, J., Barrera-Ballesteros, J., Bomans, D., Cano-Díaz, M., Catalán-Torrecilla, C., Cortijo, C., Delgado-Inglada, G., Demleitner, M., Dettmar, R.-J., Díaz, A., Florido, E., Gallazzi, A., García-Lorenzo, B., Gomes, J., Holmes, L., Iglesias-Paramo, J., Jahnke, K., Kalinova, V., Kehrig, C., Kennicutt, R., López-Sánchez, Á., Márquez, I., Masegosa, J., Meidt, S., Mendez-Abreu, J., Mollá, M., Monreal-Ibero, A., Morisset, C., del Olmo, A., Papaderos, P., Pérez, I., Quirrenbach, A., Rosales-Ortega, F., Roth, M., Ruiz-Lara, T., Sánchez-Blázquez, P., Sánchez-Menguiano, L., Singh, R., Spekkens, K., Stanishev, V., Torres-Papaqui, J., van de Ven, G., Vilchez, J., Walcher, C., Wild, V., Wisotzki, L., Ziegler, B., Alves, J., Barrado, D., Quintana, J., Aceituno, J., Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Laboratoire de l'intégration, du matériau au système (IMS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Pittsburgh], Carnegie Mellon University [Pittsburgh] (CMU), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Philippine General Hospital, Interactions moléculaires et réactivité chimique et photochimique (IMRCP), Institut de Chimie de Toulouse (ICT), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Institut Ecologie et Environnement (INEE), Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Fédération de Recherche Fluides, Energie, Réacteurs, Matériaux et Transferts (FERMAT), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), The University of Sydney, Ruhr-Universität Bochum [Bochum], CRLCC Val d'Aurelle - Paul Lamarque, Universität Heidelberg [Heidelberg] = Heidelberg University, Astronomisches Institut der Ruhr-Universität Bochum, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Plateforme d’Investigation Technologique [Centre d’Investigation Clinique 1432 module Plurithématique - Dijon] (PIT), Cognition, Action, et Plasticité Sensorimotrice [Dijon - U1093] (CAPS), Université de Bourgogne (UB)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Bourgogne (UB)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre d'Investigation Clinique 1432 (Dijon) - Module Plurithématique : Périnatalité Cancérologie Handicap et Ophtalmologie (CIC-P803), Université de Bourgogne (UB)-Direction Générale de l'Organisation des Soins (DGOS)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Direction Générale de l'Organisation des Soins (DGOS)-Institut National de la Santé et de la Recherche Médicale (INSERM), Centre IRMf de Marseille, Université de la Méditerranée - Aix-Marseille 2, Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autónoma de Madrid (UAM), Institute for Plasma Research [Gandhinagar], Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), Fundaçao Cearense de Meteorologia e Recursos Hidricos, Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Université Sciences et Technologies - Bordeaux 1-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Institut de Chimie de Toulouse (ICT-FR 2599), Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut de Chimie du CNRS (INC)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, Heidelberg, Germany, and Universidad Autonoma de Madrid (UAM)

Subjects
[PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2015
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182. Arm and interarm abundance gradients in CALIFA spiral galaxies

Author

Sánchez-Menguiano, L, Sánchez, S.F, Pérez, I., Debattista, Victor P, Ruiz-Lara, T, Florido, E, Cavichia, O, Galbany, L, Marino, R.A, Mast, D, Sánchez-Blázquez, P, Méndez-Abreu, J, De Lorenzo-Cáceres, A, Catalán-Torrecilla, C, Cano-Díaz, M, Márquez, I, McIntosh, D.H, Ascasibar, Y, García-Benito, R, González Delgado, R.M, Kehrig, C, López-Sánchez, A.R, Molla, M, Bland-Hawthorn, J, Walcher, C.J, Costantin, L, Sánchez-Menguiano, L, Sánchez, S.F, Pérez, I., Debattista, Victor P, Ruiz-Lara, T, Florido, E, Cavichia, O, Galbany, L, Marino, R.A, Mast, D, Sánchez-Blázquez, P, Méndez-Abreu, J, De Lorenzo-Cáceres, A, Catalán-Torrecilla, C, Cano-Díaz, M, Márquez, I, McIntosh, D.H, Ascasibar, Y, García-Benito, R, González Delgado, R.M, Kehrig, C, López-Sánchez, A.R, Molla, M, Bland-Hawthorn, J, Walcher, C.J, and Costantin, L

Abstract

Spiral arms are the most singular features in disc galaxies. These structures can exhibit different patterns, namely grand design and flocculent arms, with easily distinguishable characteristics. However, their origin and the mechanisms shaping them are unclear. The overall role of spirals in the chemical evolution of disc galaxies is another unsolved question. In particular, it has not been fully explored if the H ii regions of spiral arms present different properties from those located in the interarm regions. Here we analyse the radial oxygen abundance gradient of the arm and interarm star forming regions of 63 face-on spiral galaxies using CALIFA Integral Field Spectroscopy data. We focus the analysis on three characteristic parameters of the profile: slope, zero-point, and scatter. The sample is morphologically separated into flocculent versus grand design spirals and barred versus unbarred galaxies. We find subtle but statistically significant differences betweenthe arm and interarm distributions for flocculent galaxies, suggesting that the mechanisms generating the spiral structure in these galaxies may be different to those producing grand design systems, for which no significant differences are found. We also find small differences in barred galaxies, not observed in unbarred systems, hinting that bars may affect the chemical distribution of these galaxies but not strongly enough as to be reflected in the overall abundance distribution. In light of these results, we propose bars and flocculent structure as two distinct mechanisms inducing differences in the abundance distribution between arm and interarm star forming regions.

Published
2017

183. Star formation histories in mergers: The spatially resolved properties of the early-stage merger LIRGs IC 1623 and NGC 6090

Author

Cortijo-Ferrero, C., Delgado, R. M. González, Pérez, E., Fernandes, R. Cid, Sánchez, S. F., de Amorim, A. L., Di Matteo, P., García-Benito, R., Lacerda, E. A. D., Fernández, R. López, Tadhunter, C., Cortijo-Ferrero, C., Delgado, R. M. González, Pérez, E., Fernandes, R. Cid, Sánchez, S. F., de Amorim, A. L., Di Matteo, P., García-Benito, R., Lacerda, E. A. D., Fernández, R. López, and Tadhunter, C.

Abstract

The role of major mergers in galaxy evolution is investigated through a detailed characterization of the stellar populations, ionized gas properties, and star formation rates (SFR) in the early-stage merger LIRGs IC 1623 W and NGC 6090, by analysing optical Integral Field Spectroscopy (IFS) and high resolution HST imaging. The spectra were processed with the Starlight full spectral fitting code, and the emission lines measured in the residual spectra. The results are compared with control non-interacting spiral galaxies from the CALIFA survey. Merger-induced star formation is extended and recent, as revealed by the young ages (50-80 Myr) and high contributions to light of young stellar populations (50-90$\%$), in agreement with merger simulations in the literature. These early-stage mergers have positive central gradients of the stellar metallicity, with an average $\sim$0.6 Z$_{\odot}$. Compared to non-interacting spirals, they have lower central nebular metallicity, and flatter profiles, in agreement with the gas inflow scenario. We find that they are dominated by star formation, although shock excitation cannot be discarded in some regions, where high velocity dispersion is found (170-200 km s$^{-1}$). The average SFR in these early-stage mergers ($\sim$23-32 M$_{\odot}$ yr$^{-1}$) is enhanced with respect to main-sequence Sbc galaxies by factors of 6-9, slightly above the predictions from classical merger simulations, but still possible in about 15$\%$ of major galaxy mergers, where U/LIRGs belong.

Published
2017
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184. Imprints of galaxy evolution on H II regions

Author

Sanchez-Portal, M., Pintos-Castro, I., Pérez-Martínez, R., Cepa, J., Pérez García, A., Domínguez-Sánchez, H., Bongiovanni, A., Serra, A., Alfaro, E., Altieri, B., Aragón-Salamanca, A., Balkowski, C., Biviano, A., Bremer, M., Castander, F., Castañeda, H., Castro-Rodríguez, N., Chies-Santos, A., Coia, D., Diaferio, A., Duc, P., Ederoclite, A., Geach, J., González-Serrano, I., Haines, C., McBreen, B., Metcalfe, L., Oteo, I., Pérez-Fournon, I., Poggianti, B., Polednikova, J., Ramón-Pérez, M., Rodríguez-Espinosa, J., Santos, J., Smail, I., Smith, G., Temporin, S., Valtchanov, I., Sanchez, Sébastien, Perez, Emile, Rosales-Ortega, F., Miralles-Caballero, D., López-Sánchez, A., Iglesias-Paramo, J., Marino, R., Sánchez-Menguiano, L., García-Benito, R., Mast, D., Mendoza, M., 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., Bekeraitė, S., Roth, M., Pasquali, A., Díaz, A., Bomans, D., van de Ven, G., Wisotzki, L., AUTRES, Herschel Science Centre, Agence Spatiale Européenne = European Space Agency (ESA), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Facultad de Ingenieria Mecanica y Electrica (FIME), Universidad Autonoma de Nuevo Leon [Mexique] (UANL), Instituto de Astrofisica de Canarias (IAC), Department of Experimental Physics, University College of London [London] (UCL), Department of Physics, Durham University, Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, INAF - Osservatorio Astronomico di Padova (OAPD), Institute for Computational Cosmology (ICC), INAF - Osservatorio Astronomico di Brera (OAB), Laboratoire de l'intégration, du matériau au système (IMS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), Interactions moléculaires et réactivité chimique et photochimique (IMRCP), Institut de Chimie de Toulouse (ICT), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Institut Ecologie et Environnement (INEE), Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Fédération de Recherche Fluides, Energie, Réacteurs, Matériaux et Transferts (FERMAT), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Philippine General Hospital, Department of Physics [Pittsburgh], Carnegie Mellon University [Pittsburgh] (CMU), European Space Agency (ESA), University College London, Université Sciences et Technologies - Bordeaux 1-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Institut de Chimie de Toulouse (ICT-FR 2599), Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut de Chimie du CNRS (INC)-Institut National Polytechnique (Toulouse) (Toulouse INP), and Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)

Subjects
[PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2015
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185. Ionized gas kinematics of galaxies in the CALIFA survey

Author

García-Lorenzo, B., Márquez, I., Barrera-Ballesteros, J., Masegosa, J., Husemann, B., Falcón-Barroso, J., Lyubenova, M., Sanchez, Sébastien, Walcher, J., Mast, D., García-Benito, R., Méndez-Abreu, J., van de Ven, G., Spekkens, K., Holmes, L., Monreal-Ibero, A., del Olmo, A., Ziegler, B., Bland-Hawthorn, J., Sánchez-Blázquez, P., Iglesias-Paramo, J., Aguerri, J., Papaderos, P., Gomes, J., Marino, R., González Delgado, R., Cortijo-Ferrero, C., López-Sánchez, A., Bekeraitė, S., Wisotzki, L., Bomans, D., Laboratoire de l'intégration, du matériau au système (IMS), Centre National de la Recherche Scientifique (CNRS)-Institut Polytechnique de Bordeaux-Université Sciences et Technologies - Bordeaux 1, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), The University of Sydney, Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid (UAM), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Ruhr-Universität Bochum [Bochum], Université Sciences et Technologies - Bordeaux 1 (UB)-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), Universidad Autónoma de Madrid (UAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2015
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186. Spectroscopic aperture biases in inside-out evolving early-type galaxies from CALIFA

Author

Gomes, J. M., Papaderos, P., Vílchez, J. M., Kehrig, C., Iglesias-Páramo, J., Breda, I., Lehnert, M. D., Sánchez, S. F., Ziegler, B., Dos Reis, S. N., Bland-Hawthorn, J., Lluís Galbany, Bomans, D. J., Rosales-Ortega, F. F., Walcher, C. J., García-Benito, R., Márquez, I., Del Olmo, A., Mollá, M., Marino, R. A., Catalán-Torrecilla, C., González Delgado, R. M., López-Sánchez, Á R., Califa, The Collaboration, Ministerio de Ciencia e Innovación (España), Observatorio de Calar Alto, Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), Comisión Nacional de Investigación Científica y Tecnológica (Chile), European Commission, Campus de Excelencia Internacional Moncloa, National Aeronautics and Space Administration (US), Ministerio de Economía y Competitividad (España), Junta de Andalucía, and Fundação para a Ciência e a Tecnologia (Portugal)

Subjects
Astrofísica, Aperture, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, elliptical and lenticular, cD [Galaxies], 01 natural sciences, star formation [Galaxies], Luminosity, 0103 physical sciences, ISM [Galaxies], Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxies: nuclei, Physics, COSMIC cancer database, Galaxies: star formation, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Astronomía, Galaxies: elliptical and lenticular, cD, Galaxies: ISM, Space and Planetary Science, nuclei [Galaxies], Astrophysics of Galaxies (astro-ph.GA), Equivalent width
Abstract

Integral field spectroscopy (IFS) studies based on CALIFA survey data have recently revealed ongoing low-level star formation (SF) in the periphery of a small fraction (∼10%) of local early-type galaxies (ETGs), witnessing a still ongoing inside-out galaxy growth process. A distinctive property of the nebular component in these ETGs, classified i+, is a structure with two radial zones, the inner of which displays LINER emission with a Hα equivalent width EW(Hα) ≃ 1 Å, the outer (3 Å retired>, that is, systems entirely lacking SF, and whose faint nebular emissionis solely powered by the post-AGB stellar component. The SDSS aperture progressively encompasses the outer SF zone only at higher z, at which the galaxies are unambiguously classified as >composite SF/LINER>. We also empirically demonstrate that the principal effect of a decreasing spectroscopic aperture on the classification of i+ ETGs through standard [NII]/Hα vs. [OIII]/Hβ emission-line (BPT) ratios consists of a monotonic shift upward and to the right precisely along the upper right wing of the >seagull> distribution on the BPT plane, that is, along the pathway connecting composite SF/HII galaxies with AGN/LINERs. Motivated by these observational insights, we also investigate theoretically observational biases in aperture-limited studies of inside-out growing galaxies as a function of z. To this end, we devise a simple 1D model that involves an outward-propagating exponentially decreasing SF process since z ∼ 10 and reproduces the radial extent and two-zone EW(Hα) distribution of local i+ ETGs. By simulating the 3″ spectroscopic SDSS aperture in this model, we find that SDSS studies at z ≲ 1 are progressively restricted to the inner (SF-devoid LINER) zone and miss an increasingly larger portion of the Hα-emitting periphery. This leads to the incorrect spectroscopic classification of these inside-out assembling galaxies as retired ETG/LINERs and also to a severe underestimation of their total star formation rate (SFR) in a manner inversely related to z. More specifically, the SFR inferred from the Hα luminosity registered within the SDSS fiber is reduced by 50% at z ∼ 0.86, reaching only 0.1% of its integral value at z = 0.1. We argue that the aperture-driven biases described above pertain to any morphological analog of i+ ETGs (e.g., SF-quiescent bulges within star-forming disks), regardless of whether it is viewed from the perspective of inside-out growth or inside-out SF quenching, and might be of considerable relevance to galaxy taxonomy and studies of the cosmic SFR density as a function of z., This paper is based on data from the Calar Alto Legacy Integral Field Area Survey, CALIFA (http://califa.caha.es), funded by the Spanish Ministery of Science under grant ICTS-2009-10, and the Centro Astronomico Hispano-Aleman. JMG acknowledges support by Fundacao para a Ciencia e a Tecnologia (FCT) through the Fellowship SFRH/BPD/66958/2009 and POPH/FSE (EC) by FEDER funding through the program Programa Operacional de Factores de Competitividade (COMPETE). P.P. is supported by FCT through the Investigador FCT Contract No. IF/01220/2013 and POPH/FSE (EC) by FEDER funding through the program COMPETE. J.M.G., P.P., I.B. and S.N.d.R. acknowledge support by FCT under project FCOMP-01-0124-FEDER-029170 (Reference FCT PTDC/FIS-AST/3214/2012), funded by FCT-MEC (PIDDAC) and FEDER (COMPETE). They also acknowledge support by the exchange programme >Study of Emission-Line Galaxies with Integral-Field Spectroscopy> (SELGIFS, FP7-PEOPLE-2013-IRSES-612701), funded by the EU through the IRSES scheme. SFS acknowledges support from CONACyT-180125 and PAPIIT-IA100815 grants. Support for LG 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. L.G. acknowledges support by CONICYT through FONDECYT grant 3140566. C.J.W. acknowledges support through the Marie Curie Career Integration Grant 303912. I.M. acknowledges financial support by the Junta de Andalucia through project TIC114, and the Spanish Ministry of Economy and Competitiveness (MINECO) through projects AYA2010-15169 and AYA2013-42227-P. R.A. Marino is funded by the Spanish program of International Campus of Excellence Moncloa (CEI). This research made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.

Published
2015
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187. Nearby supernova host galaxies from the CALIFA Survey

Author

Galbany, L., Stanishev, V., Mourão, A. M., Rodrigues, M., Flores, H., García Benito, R., Mast, D., Mendoza, M. A., Sánchez, S. F., Badenes, C., Barrera Ballesteros, J., Bland-Hawthorn, J., Falcón Barroso, J., García Lorenzo, B., Gomes, J. M., González Delgado, R. M., Kehrig, C., Lyubenova, M., López Sánchez, A. R., Lorenzo Cáceres, A. de, Marino, Raffaella Anna, Meidt, S., Mollá, M., Papaderos, P., Pérez Torres, M. A., Rosales Ortega, F. F., van de Ven, G., Department of Physics [Pittsburgh], Carnegie Mellon University [Pittsburgh] (CMU), Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), inconnu, Inconnu, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratory of Mycology, Institute of Biomedicine, Laboratoire de physique des interactions ondes matières (LPIOM), Université Sciences et Technologies - Bordeaux 1-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Centre National de la Recherche Scientifique (CNRS), The University of Sydney, Novae, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS]Physics [physics], Astrofísica, Astronomía, Física atmosférica, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

We use optical integral field spectroscopy (IFS) of nearby supernova (SN) host galaxies (0.005 < z < 0.03) provided by the Calar Alto Legacy Integral Field Area (CALIFA) Survey with the goal of finding correlations in the environmental parameters at the location of different SN types. In this first study of a series we focus on the properties related with star formation (SF). We recover the sequence in association of different SN types to the star-forming regions by using several indicators of the ongoing and recent SF related to both the ionized gas and the stellar populations. While the total ongoing SF is on average the same for the three SN types, SNe Ibc/IIb tend to occur closer to star-forming regions and in higher SF density locations than SNe II and SNe Ia; the latter shows the weakest correlation. SNe Ia host galaxies have masses that are on average similar to 0.3-0.8 dex higher than those of the core collapse (CC) SNe hosts because the SNe Ia hosts contain a larger fraction of old stellar populations. Using the recent SN Ia delay-time distribution and the SFHs of the galaxies, we show that the SN Ia hosts in our sample are expected to produce twice as many SNe Ia as the CC SN hosts. Since both types occur in hosts with a similar SF rate and hence similar CC SN rate, this can explain the mass difference between the SN Ia and CC SN hosts, and reinforces the finding that at least part of the SNe Ia originate from very old progenitors. By comparing the mean SFH of the eight least massive galaxies with that of the massive SF SN Ia hosts, we find that the low-mass galaxies formed their stars during a longer time (0.65%, 24.46%, and 74.89% in the intervals 0-0.42 Gyr, 0.42-2.4 Gyr, and >2.4 Gyr, respectively) than the massive SN Ia hosts (0.04%, 2.01%, and 97.95% in these intervals). We estimate that the low-mass galaxies produce ten times fewer SNe Ia and three times fewer CC SNe than the high-mass group. Therefore the ratio between the number of CC SNe and SNe Ia is expected to increase with decreasing galaxy mass. CC SNe tend to explode at positions with younger stellar populations than the galaxy average, but the galaxy properties at SNe Ia locations are one average the same as the global galaxy properties.

Published
2014
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188. Stellar Population gradients in galaxy discs from the CALIFA survey

Author

Sánchez Blázquez, P., Rosales Ortega, F. F., Méndez Abreu, J., Pérez, I., Sánchez, S. F., Zibetti, S., Aguerri, J. A. L., Bland-Hawthorn, J., Catalán Torrecilla, Cristina, Cid Fernandes, R., de Amorim, A., de Lorenzo Cáceres, A., Falcón Barroso, J., Galazzi, A., García Benito, R., Gil de Paz, Armando, González Delgado, R., Husemann, B., Iglesias Paramo, Jorge, Jungwiert, B., Marino, Raffaella Anna, Márquez, I., Mast, D., Mendoza, M. A., Molla, M., Papaderos, P., Ruiz Lara, T., van de Ven, G., Walcher, C. J., and Wisotzki, L.

Subjects
Astrofísica, Astronomía, Astrophysics of Galaxies (astro-ph.GA), Física atmosférica, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

While studies of gas-phase metallicity gradients in disc galaxies are common, very little has been done in the acquisition of stellar abundance gradients in the same regions. We present here a comparative study of the stellar metallicity and age distributions in a sample of 62 nearly face-on, spiral galaxies with and without bars, using data from the CALIFA survey. We measure the slopes of the gradients and study their relation with other properties of the galaxies. We find that the mean stellar age and metallicity gradients in the disc are shallow and negative. Furthermore, when normalized to the effective radius of the disc, the slope of the stellar population gradients does not correlate with the mass or with the morphological type of the galaxies. Contrary to this, the values of both age and metallicity at $\sim$2.5 scale-lengths correlate with the central velocity dispersion in a similar manner to the central values of the bulges, although bulges show, on average, older ages and higher metallicities than the discs. One of the goals of the present paper is to test the theoretical prediction that non-linear coupling between the bar and the spiral arms is an efficient mechanism for producing radial migrations across significant distances within discs. The process of radial migration should flatten the stellar metallicity gradient with time and, therefore, we would expect flatter stellar metallicity gradients in barred galaxies. However, we do not find any difference in the metallicity or age gradients in galaxies with without bars. We discuss possible scenarios that can lead to this absence of difference., 24 pages, 17 figures, accepted for publication in A&A

Published
2014

189. Spectroscopy of the short-hard GRB 130603B

Author

de Ugarte Postigo, A., Thöne, C. C., Rowlinson, A., García-Benito, R., Levan, A. J., Gorosabel, J., Goldoni, P., Schulze, S., Zafar, T., Wiersema, K., Sánchez-Ramírez, R., Melandri, A., D’Avanzo, P., Oates, S., D’Elia, V., De Pasquale, M., Krühler, T., van der Horst, A. J., Xu, D., Watson, D., Piranomonte, S., Vergani, S. D., Milvang-Jensen, B., Kaper, L., Malesani, D., Fynbo, J. P. U., Cano, Z., Covino, S., Flores, H., Greiss, S., Hammer, F., Hartoog, O. E., Hellmich, S., Heuser, C., Hjorth, J., Jakobsson, P., Mottola, S., Sparre, M., Sollerman, J., Tagliaferri, G., Tanvir, N. R., Vestergaard, M., and Wijers, R. A. M. J.

Subjects
galaxies: spiral, gamma-ray burst: individual: GRB 130603B, galaxies: stellar content, galaxies: distances and redshifts
Published
2014

190. Star formation histories in mergers: the spatially resolved properties of the early-stage merger luminous infrared galaxies IC 1623 and NGC 6090

Author

Cortijo-Ferrero, C., primary, González Delgado, R. M., additional, Pérez, E., additional, Cid Fernandes, R., additional, Sánchez, S. F., additional, de Amorim, A. L., additional, Di Matteo, P., additional, García-Benito, R., additional, Lacerda, E. A. D., additional, López Fernández, R., additional, and Tadhunter, C., additional

Published
2017
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191. Resolving the age bimodality of galaxy stellar populations on kpc scales

Author

Zibetti, Stefano, primary, Gallazzi, Anna R., additional, Ascasibar, Y., additional, Charlot, S., additional, Galbany, L., additional, García Benito, R., additional, Kehrig, C., additional, de Lorenzo-Cáceres, A., additional, Lyubenova, M., additional, Marino, R. A., additional, Márquez, I., additional, Sánchez, S. F., additional, van de Ven, G., additional, Walcher, C. J., additional, and Wisotzki, L., additional

Published
2017
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192. Two-dimensional multi-component photometric decomposition of CALIFA galaxies

Author

Méndez-Abreu, J., primary, Ruiz-Lara, T., additional, Sánchez-Menguiano, L., additional, de Lorenzo-Cáceres, A., additional, Costantin, L., additional, Catalán-Torrecilla, C., additional, Florido, E., additional, Aguerri, J. A. L., additional, Bland-Hawthorn, J., additional, Corsini, E. M., additional, Dettmar, R. J., additional, Galbany, L., additional, García-Benito, R., additional, Marino, R. A., additional, Márquez, I., additional, Ortega-Minakata, R. A., additional, Papaderos, P., additional, Sánchez, S. F., additional, Sánchez-Blazquez, P., additional, Spekkens, K., additional, van de Ven, G., additional, Wild, V., additional, and Ziegler, B., additional

Published
2017
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193. Stellar kinematics across the Hubble sequence in the CALIFA survey: General properties and aperture corrections

Author

Falcón-Barroso, J., Lyubenova, M., van de Ven, G., Méndez-Abreu, J., Aguerri, J. A. L., García-Lorenzo, B., Bekeraite, S., Sánchez, S. F., Husemann, B., García-Benito, R., Mast, D., Walcher, C. J., Zibetti, S., Barrera-Ballesteros, J. K., Galbany, L., Sánchez-Blázquez, P., Singh, R., Bosch, R. C. E. van den, Wild, V., Zhu, L., Bland-Hawthorn, J., Fernandes, R. Cid, de Lorenzo-Cáceres, A., Gallazzi, A., Delgado, R. M. González, Marino, R. A., Márquez, I., Pérez, E., Pérez, I., Roth, M. M., Rosales-Ortega, F. F., Ruíz-Lara, T., Wisotzki, L., Ziegler, B., collaboration, the CALIFA, Falcón-Barroso, J., Lyubenova, M., van de Ven, G., Méndez-Abreu, J., Aguerri, J. A. L., García-Lorenzo, B., Bekeraite, S., Sánchez, S. F., Husemann, B., García-Benito, R., Mast, D., Walcher, C. J., Zibetti, S., Barrera-Ballesteros, J. K., Galbany, L., Sánchez-Blázquez, P., Singh, R., Bosch, R. C. E. van den, Wild, V., Zhu, L., Bland-Hawthorn, J., Fernandes, R. Cid, de Lorenzo-Cáceres, A., Gallazzi, A., Delgado, R. M. González, Marino, R. A., Márquez, I., Pérez, E., Pérez, I., Roth, M. M., Rosales-Ortega, F. F., Ruíz-Lara, T., Wisotzki, L., Ziegler, B., and collaboration, the CALIFA

Abstract

We present the stellar kinematic maps of a large sample of galaxies from the integral-field spectroscopic survey CALIFA. The sample comprises 300 galaxies displaying a wide range of morphologies across the Hubble sequence, from ellipticals to late-type spirals. This dataset allows us to homogeneously extract stellar kinematics up to several effective radii. In this paper, we describe the level of completeness of this subset of galaxies with respect to the full CALIFA sample, as well as the virtues and limitations of the kinematic extraction compared to other well-known integral-field surveys. In addition, we provide averaged integrated velocity dispersion radial profiles for different galaxy types, which are particularly useful to apply aperture corrections for single aperture measurements or poorly resolved stellar kinematics of high-redshift sources. The work presented in this paper sets the basis for the study of more general properties of galaxies that will be explored in subsequent papers of the survey., Comment: 52 pages, 44 figures, A&A accepted. FITS tables with the stellar kinematic results are available at: http://www.caha.es/CALIFA/public_html/?q=content/science-dataproducts A full-resolution version of the manuscript is also available on the same webpage

Published
2016
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194. IMF shape constraints from stellar populations and dynamics from CALIFA

Author

Lyubenova, M., Martín-Navarro, I., van de Ven, G., Falcón-Barroso, J., Galbany, L., Gallazzi, A., García-Benito, R., Delgado, R. González, Husemann, B., La Barbera, F., Marino, R. A., Mast, D., Mendez-Abreu, J., Peletier, R. F. P., Sánchez-Blázquez, P., Sánchez, S. F., Trager, S. C., Bosch, R. C. E. van den, Vazdekis, A., Walcher, C. J., Zhu, L., Zibetti, S., Ziegler, B., Bland-Hawthorn, J., collaboration, the CALIFA, Lyubenova, M., Martín-Navarro, I., van de Ven, G., Falcón-Barroso, J., Galbany, L., Gallazzi, A., García-Benito, R., Delgado, R. González, Husemann, B., La Barbera, F., Marino, R. A., Mast, D., Mendez-Abreu, J., Peletier, R. F. P., Sánchez-Blázquez, P., Sánchez, S. F., Trager, S. C., Bosch, R. C. E. van den, Vazdekis, A., Walcher, C. J., Zhu, L., Zibetti, S., Ziegler, B., Bland-Hawthorn, J., and collaboration, the CALIFA

Abstract

In this letter we describe how we use stellar dynamics information to constrain the shape of the stellar IMF in a sample of 27 early-type galaxies from the CALIFA survey. We obtain dynamical and stellar mass-to-light ratios, $\Upsilon_\mathrm{dyn}$ and $\Upsilon_{\ast}$, over a homogenous aperture of 0.5~$R_{e}$. We use the constraint $\Upsilon_\mathrm{dyn} \ge \Upsilon_{\ast}$ to test two IMF shapes within the framework of the extended MILES stellar population models. We rule out a single power law IMF shape for 75% of the galaxies in our sample. Conversely, we find that a double power law IMF shape with a varying high-mass end slope is compatible (within 1$\sigma$) with 95% of the galaxies. We also show that dynamical and stellar IMF mismatch factors give consistent results for the systematic variation of the IMF in these galaxies., Comment: 6 pages, 3 figures, accepted for publication in MNRAS Letters

Published
2016
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195. The space density distribution of galaxies in the absolute magnitude - rotation velocity plane: a volume-complete Tully-Fisher relation from CALIFA stellar kinematics

Author

Bekeraitė, S., Walcher, C. J., Falcón-Barroso, J., Lorenzo, B. Garcia, Lyubenova, M., Sánchez, S. F., Spekkens, K., van de Ven, G., Wisotzki, L., Ziegler, B., Aguerri, J. A. L., Barrera-Ballesteros, J., Bland-Hawthorn, J., Catalán-Torrecilla, Cristina, García-Benito, R., collaboration, the CALIFA, Bekeraitė, S., Walcher, C. J., Falcón-Barroso, J., Lorenzo, B. Garcia, Lyubenova, M., Sánchez, S. F., Spekkens, K., van de Ven, G., Wisotzki, L., Ziegler, B., Aguerri, J. A. L., Barrera-Ballesteros, J., Bland-Hawthorn, J., Catalán-Torrecilla, Cristina, García-Benito, R., and collaboration, the CALIFA

Abstract

The space density distribution of galaxies in the absolute magnitude - rotation velocity plane: a volume-complete Tully-Fisher relation from CALIFA stellar kinematics, Comment: Accepted to A&A

Published
2016
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196. Star formation along the Hubble sequence: Radial structure of the star formation of CALIFA galaxies

Author

Delgado, R. M. González, Fernandes, R. Cid, Pérez, E., García-Benito, R., Fernández, R. López, Lacerda, E. A. D., Cortijo-Ferrero, C., de Amorim, A. L., Asari, N. Vale, Sánchez, S. F., Walcher, C. J., Wisotzki, L., Mast, D., Alves, J., Ascasibar, Y., Bland-Hawthorn, J., Galbany, L., Kennicutt Jr., R. C., Márquez, I., Masegosa, J., Mollá, M., Sánchez-Blázquez, P., Vílchez, J. M., collaboration, CALIFA, Delgado, R. M. González, Fernandes, R. Cid, Pérez, E., García-Benito, R., Fernández, R. López, Lacerda, E. A. D., Cortijo-Ferrero, C., de Amorim, A. L., Asari, N. Vale, Sánchez, S. F., Walcher, C. J., Wisotzki, L., Mast, D., Alves, J., Ascasibar, Y., Bland-Hawthorn, J., Galbany, L., Kennicutt Jr., R. C., Márquez, I., Masegosa, J., Mollá, M., Sánchez-Blázquez, P., Vílchez, J. M., and collaboration, CALIFA

Abstract

The aim of this paper is to characterize the radial structure of the star formation rate (SFR) in galaxies in the nearby Universe as represented by the CALIFA survey. The sample under study contains 416 galaxies observed with IFS, covering a wide range of Hubble types and stellar masses. Spectral synthesis techniques are applied to obtain radial profiles of the intensity of the star formation rate in the recent past, and the local sSFR. To emphasize the behavior of these properties for galaxies that are on and off the main sequence of star formation (MSSF) we stack the individual radial profiles in bins of galaxy morphology and stellar masses. Our main results are: a) The intensity of SFR shows declining profiles that exhibit very little differences between spirals. The dispersion between the profiles is significantly smaller in late type spirals. This confirms that the MSSF is a sequence of galaxies with nearly constant intensity of SFR b) sSFR values scale with Hubble type and increase radially outwards, with a steeper slope in the inner 1 HLR. This behavior suggests that galaxies are quenched inside-out, and that this process is faster in the central, bulge-dominated part than in the disks. c) As a whole, and at all radii, E and S0 are off the MSSF. d) Applying the volume-corrections for the CALIFA sample, we obtain a density of star formation in the local Universe of 0.0105 Msun/yr/Mpc^{-3}. Most of the star formation is occurring in the disks of spirals. e) The volume averaged birthrate parameter, b'=0.39, suggests that the present day Universe is forming stars at 1/3 of its past average rate. E, S0, and the bulge of early type spirals contribute little to the recent SFR of the Universe, which is dominated by the disks of later spirals. f) There is a tight relation between the intensity of the SFR and stellar mass, defining a local MSSF relation with a logarithmic slope of 0.8., Comment: 17 pages, 11 figures, accepted for publication in Astronomy & Astrophysics. Abridged abstract

Published
2016
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197. BaTMAn: Bayesian Technique for Multi-image Analysis

Author

Casado, J., Ascasibar, Y., García-Benito, R., Guidi, G., Choudhury, O. S., Bellocchi, E., Sánchez, S. F., Díaz, A. I., Casado, J., Ascasibar, Y., García-Benito, R., Guidi, G., Choudhury, O. S., Bellocchi, E., Sánchez, S. F., and Díaz, A. I.

Abstract

This paper describes the Bayesian Technique for Multi-image Analysis (BaTMAn), a novel image-segmentation technique based on Bayesian statistics that characterizes any astronomical dataset containing spatial information and performs a tessellation based on the measurements and errors provided as input. The algorithm iteratively merges spatial elements as long as they are statistically consistent with carrying the same information (i.e. identical signal within the errors). We illustrate its operation and performance with a set of test cases including both synthetic and real Integral-Field Spectroscopic data. The output segmentations adapt to the underlying spatial structure, regardless of its morphology and/or the statistical properties of the noise. The quality of the recovered signal represents an improvement with respect to the input, especially in regions with low signal-to-noise ratio. However, the algorithm may be sensitive to small-scale random fluctuations, and its performance in presence of spatial gradients is limited. Due to these effects, errors may be underestimated by as much as a factor of two. Our analysis reveals that the algorithm prioritizes conservation of all the statistically-significant information over noise reduction, and that the precise choice of the input data has a crucial impact on the results. Hence, the philosophy of BaTMAn is not to be used as a `black box' to improve the signal-to-noise ratio, but as a new approach to characterize spatially-resolved data prior to its analysis. The source code is publicly available at http://astro.ft.uam.es/SELGIFS/BaTMAn ., Comment: 21 pages, 7 Figure, 4 Tables

Published
2016
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198. The dependence of oxygen and nitrogen abundances on stellar mass from the CALIFA survey

Author

Pérez-Montero, E., García-Benito, R., Vílchez, J. M., Sánchez, S. F., Kehrig, C., Husemann, B., Puertas, S. Duarte, Iglesias-Pármao, J., Galbany, L., Mollá, M., Walcher, C. J., Ascasíbar, Y., Delgado, R. M. González, Marino, R. A., Masegosa, J., Pérez, E., Rosales-Ortega, F. F., Sánchez-Blázquez, P., Bland-hawthorn, J., Bomans, D., López-Sánchez, A. R., Ziegler, B., collaboration, the CALIFA, Pérez-Montero, E., García-Benito, R., Vílchez, J. M., Sánchez, S. F., Kehrig, C., Husemann, B., Puertas, S. Duarte, Iglesias-Pármao, J., Galbany, L., Mollá, M., Walcher, C. J., Ascasíbar, Y., Delgado, R. M. González, Marino, R. A., Masegosa, J., Pérez, E., Rosales-Ortega, F. F., Sánchez-Blázquez, P., Bland-hawthorn, J., Bomans, D., López-Sánchez, A. R., Ziegler, B., and collaboration, the CALIFA

Abstract

We analysed the optical spectra of HII regions extracted from a sample of 350 galaxies of the CALIFA survey. We calculated total O/H abundances and, for the first time, N/O ratios using the semi-empirical routine HII-CHI-mistry, which, according to P\'erez-Montero (2014), is consistent with the direct method and reduces the uncertainty in the O/H derivation using [NII] lines owing to the dispersion in the O/H-N/O relation. Then we performed linear fittings to the abundances as a function of the de-projected galactocentric distances. The analysis of the radial distribution both for O/H and N/O in the non-interacting galaxies reveals that both average slopes are negative, but a non-negligible fraction of objects have a flat or even a positive gradient (at least 10\% for O/H and 4\% for N/O). The slopes normalised to the effective radius appear to have a slight dependence on the total stellar mass and the morphological type, as late low-mass objects tend to have flatter slopes. No clear relation is found, however, to explain the presence of inverted gradients in this sample, and there is no dependence between the average slopes and the presence of a bar. The relation between the resulting O/H and N/O linear fittings at the effective radius is much tighter (correlation coefficient $\rho_s$ = 0.80) than between O/H and N/O slopes ($\rho_s$ = 0.39) or for O/H and N/O in the individual \hii\ regions ($\rho_s$ = 0.37). These O/H and N/O values at the effective radius also correlate very tightly (less than 0.03 dex of dispersion) with total luminosity and stellar mass. The relation with other integrated properties, such as star formation rate, colour, or morphology, can be understood only in light of the found relation with mass., Comment: Accepted for publication in A&A. 20 pages, 19 figures

Published
2016
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199. First survey of Wolf-Rayet star populations over the full extension of nearby galaxies observed with CALIFA

Author

Miralles-Caballero, D., Díaz, A. I., López-Sánchez, Á. R., Rosales-Ortega, F. F., Monreal-Ibero, A., Pérez-Montero, E., Kehrig, C., García-Benito, R., Sánchez, S. F., Walcher, C. J., Galbany, L., Iglesias-Páramo, J., Vílchez, J. M., Delgado, R. M. González, van de Ven, G., Barrera-Ballesteros, J., Lyubenova, M., Meidt, S., Falcon-Barroso, J., Mast, D., Mendoza, M. A., collaboration, the CALIFA, Miralles-Caballero, D., Díaz, A. I., López-Sánchez, Á. R., Rosales-Ortega, F. F., Monreal-Ibero, A., Pérez-Montero, E., Kehrig, C., García-Benito, R., Sánchez, S. F., Walcher, C. J., Galbany, L., Iglesias-Páramo, J., Vílchez, J. M., Delgado, R. M. González, van de Ven, G., Barrera-Ballesteros, J., Lyubenova, M., Meidt, S., Falcon-Barroso, J., Mast, D., Mendoza, M. A., and collaboration, the CALIFA

Abstract

The search of extragalactic regions with conspicuous presence of Wolf-Rayet (WR) stars outside the Local Group is challenging task due to the difficulties in detecting their faint spectral features. In this exploratory work, we develop a methodology to perform an automated search of WR signatures through a pixel-by-pixel analysis of integral field spectroscopy (IFS) data belonging to the Calar Alto Legacy Integral Field Area survey, CALIFA. This technique allowed us to build the first catalogue of Wolf-Rayet rich regions with spatially-resolved information, allowing to study the properties of these complexes in a 2D context. The detection technique is based on the identification of the blue WR bump (around He II 4686 {\AA}, mainly associated to nitrogen-rich WR stars, WN) and the red WR bump (around C IV 5808 {\AA} and associated to carbon-rich WR stars, WC) using a pixel-by-pixel analysis. We identified 44 WR-rich regions with blue bumps distributed in 25 galaxies of a total of 558. The red WR bump was identified only in 5 of those regions. We found that the majority of the galaxies hosting WR populations in our sample are involved in some kind of interaction process. Half of the host galaxies share some properties with gamma-ray burst (GRB) hosts where WR stars, as potential candidates to being the progenitors of GRBs, are found. We also compared the WR properties derived from the CALIFA data with stellar population synthesis models, and confirm that simple star models are generally not able to reproduce the observations. We conclude that other effects, such as the binary star channel (which could extend the WR phase up to 10 Myr), fast rotation or other physical processes that causes the loss of observed Lyman continuum photons, are very likely affecting the derived WR properties, and hence should be considered when modelling the evolution of massive stars., Comment: 33 pages, accepted for publication in A&A

Published
2016
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200. Aperture effects on the oxygen abundance determinations from CALIFA data

Author

Iglesias-Páramo, J., Vílchez, J. M., Rosales-Ortega, F. F., Sánchez, S. F., Puertas, S. Duarte, Petropoulou, V., de Paz, A. Gil, Galbany, L., Mollá, M., Catalán-Torrecilla, C., Morales, A. Castillo, Mast, D., Husemann, B., García-Benito, R., Mendoza, M. A., Kehrig, C., Pérez-Montero, E., Papaderos, P., Gomes, J. M., Walcher, C. J., Delgado, R. M. González, Marino, R. A., López-Sánchez, Á. R., Ziegler, B., Flores, H., Alves, J., Iglesias-Páramo, J., Vílchez, J. M., Rosales-Ortega, F. F., Sánchez, S. F., Puertas, S. Duarte, Petropoulou, V., de Paz, A. Gil, Galbany, L., Mollá, M., Catalán-Torrecilla, C., Morales, A. Castillo, Mast, D., Husemann, B., García-Benito, R., Mendoza, M. A., Kehrig, C., Pérez-Montero, E., Papaderos, P., Gomes, J. M., Walcher, C. J., Delgado, R. M. González, Marino, R. A., López-Sánchez, Á. R., Ziegler, B., Flores, H., and Alves, J.

Abstract

This paper aims at providing aperture corrections for emission lines in a sample of spiral galaxies from the Calar Alto Legacy Integral Field Area Survey (CALIFA) database. In particular, we explore the behavior of the log([OIII]5007/Hbeta)/([NII]6583/Halpha) (O3N2) and log[NII]6583/Halpha (N2) flux ratios since they are closely connected to different empirical calibrations of the oxygen abundances in star forming galaxies. We compute median growth curves of Halpha, Halpha/Hbeta, O3N2 and N2 up to 2.5R_50 and 1.5 disk R_eff. The growth curves simulate the effect of observing galaxies through apertures of varying radii. The median growth curve of the Halpha/Hbeta ratio monotonically decreases from the center towards larger radii, showing for small apertures a maximum value of ~10% larger than the integrated one. The median growth curve of N2 shows a similar behavior, decreasing from the center towards larger radii. No strong dependence is seen with the inclination, morphological type and stellar mass for these growth curves. Finally, the median growth curve of O3N2 increases monotonically with radius. However, at small radii it shows systematically higher values for galaxies of earlier morphological types and for high stellar mass galaxies. Applying our aperture corrections to a sample of galaxies from the SDSS survey at 0.02<=z<=0.3 shows that the average difference between fiber-based and aperture corrected oxygen abundances, for different galaxy stellar mass and redshift ranges, reaches typically to ~11%, depending on the abundance calibration used. This average difference is found to be systematically biased, though still within the typical uncertainties of oxygen abundances derived from empirical calibrations. Caution must be exercised when using observations of galaxies for small radii (e.g. below 0.5R_eff) given the high dispersion shown around the median growth curves., Comment: Accepted for publication in ApJ

Published
2016
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