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29 results on '"Mollá, M."'

2. Mass–metallicity and star formation rate in galaxies: A complex relation tuned to stellar age

Author

Ministerio de Ciencia e Innovación (España), Junta de Andalucía, European Commission, Duarte Puertas, Salvador, Vílchez Medina, José Manuel, Iglesias-Páramo, J., Mollá, M., Pérez Montero, Enrique, Kehrig, C., Pilyugin, L.S., Zinchenko, I. A., Ministerio de Ciencia e Innovación (España), Junta de Andalucía, European Commission, Duarte Puertas, Salvador, Vílchez Medina, José Manuel, Iglesias-Páramo, J., Mollá, M., Pérez Montero, Enrique, Kehrig, C., Pilyugin, L.S., and Zinchenko, I. A.

Abstract

Context. In this work we study the stellar mass–metallicity relation (MZR) of an extended sample of star-forming galaxies in the local Universe and its possible dependence on the star formation rate (SFR). Aims. We selected a sample of approximately 195 000 Sloan Digital Sky Survey (SDSS) star-forming galaxies up to z = 0.22 with the aim of analysing the behaviour of the MZR with respect to SFR whilst taking into account the age of their stellar populations. Methods. For the first time, with this sample, we obtained aperture corrected oxygen and nitrogen-to-oxygen abundances (O/H and N/O, respectively) and SFR using the empirical prescriptions from the Calar Alto Legacy Integral Field Area (CALIFA) survey. To perform this study we also make use of the stellar mass of the galaxies and the parameter Dn(4000) as a proxy for the age of the stellar population. Results. We derive a robust MZR locus, which is found to be fully consistent with the ‘anchoring’ points of a selected set of well-studied nearby galaxies for which the chemical abundance has been derived using the direct method. We observe a complex relation between MZR and SFR across the whole range of galaxy mass and metallicity, where the slope changes seen in the O/H–SFR plane present a pattern that seems to be tuned to the stellar age of the galaxies, and therefore stellar age has to be taken into account in the stellar mass–metallicity–SFR relation. Conclusions. In order to provide an answer to the question of whether or not the MZR depends on the SFR, it is essential to take into account the age of the stellar populations of galaxies. A strong dependence of the MZR on SFR is observed mainly for star-forming galaxies with strong SFR values and low Dn(4000). The youngest galaxies of our SDSS sample show the highest SFR measured for their stellar mass. © S. Duarte Puertas et al. 2022.

Published
2022

3. 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

4. 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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5. Arm and interarm abundance gradients in CALIFA spiral galaxies

Author

Ministerio de Economía, Industria y Competitividad (España), Junta de Andalucía, Consejo Nacional de Ciencia y Tecnología (México), National Science Foundation (US), Swiss National Science Foundation, European Research Council, Sánchez-Menguiano, L., Sánchez, S.F., Pérez, I., Debattista, V.P., Ruiz-Lara, T., Florido, E., Cavichia, O., Galbany, Lluís, Marino, R.A., Mast, D., Sánchez-Blázquez, P., Méndez-Abreu, J., de Lorenzo-Cáceres, A., Catalán-Torrecilla, C., Cano-Díaz, M., Márquez, Isabel, McIntosh, D.H., Ascasíbar, Y., García-Benito, Rubén, González Delgado, Rosa M., Kehrig, C., López-Sánchez, R., Mollá, M., Bland-Hawthorn, J., Walcher, C.J., Costantin, L., Ministerio de Economía, Industria y Competitividad (España), Junta de Andalucía, Consejo Nacional de Ciencia y Tecnología (México), National Science Foundation (US), Swiss National Science Foundation, European Research Council, Sánchez-Menguiano, L., Sánchez, S.F., Pérez, I., Debattista, V.P., Ruiz-Lara, T., Florido, E., Cavichia, O., Galbany, Lluís, Marino, R.A., Mast, D., Sánchez-Blázquez, P., Méndez-Abreu, J., de Lorenzo-Cáceres, A., Catalán-Torrecilla, C., Cano-Díaz, M., Márquez, Isabel, McIntosh, D.H., Ascasíbar, Y., García-Benito, Rubén, González Delgado, Rosa M., Kehrig, C., López-Sánchez, R., Mollá, 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.© ESO, 2017.

Published
2017

6. The dependence of oxygen and nitrogen abundances on stellar mass from the CALIFA survey

Author

Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), Junta de Andalucía, Ministerio de Ciencia e Innovación (España), Pérez Montero, Enrique, García-Benito, Rubén, Vílchez Medina, José Manuel, Sánchez, Sebastián F., Kehrig, C., Husemann, B., Duarte Puertas, Salvador, Iglesias-Páramo, J., Galbany, Lluís, Mollá, M., Walcher, C.J., Ascasíbar, Y., González Delgado, Rosa M., Marino, R.A., Masegosa, Josefa, Pérez Jiménez, Enrique, Rosales-Ortega, Fabián, Sánchez-Blázquez, P., Bland-Hawthorn, J., Bomans, D. J., López-Sánchez, A.R., Ziegler, B., Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), Junta de Andalucía, Ministerio de Ciencia e Innovación (España), Pérez Montero, Enrique, García-Benito, Rubén, Vílchez Medina, José Manuel, Sánchez, Sebastián F., Kehrig, C., Husemann, B., Duarte Puertas, Salvador, Iglesias-Páramo, J., Galbany, Lluís, Mollá, M., Walcher, C.J., Ascasíbar, Y., González Delgado, Rosa M., Marino, R.A., Masegosa, Josefa, Pérez Jiménez, Enrique, Rosales-Ortega, Fabián, Sánchez-Blázquez, P., Bland-Hawthorn, J., Bomans, D. J., López-Sánchez, A.R., and Ziegler, B.

Abstract

Context. The study of the integrated properties of star-forming galaxies is central to understand their formation and evolution. Some of these properties are extensive and therefore their analysis require totally covering and spatially resolved observations. Among these properties, metallicity can be defined in spiral discs by means of integral field spectroscopy (IFS) of individual H ii regions. The simultaneous analysis of the abundances of primary elements, as oxygen, and secondary, as nitrogen, also provides clues about the star formation history and the processes that shape the build-up of spiral discs. Aims. Our main aim is to analyse simultaneously O/H and N/O abundance ratios in H ii regions in different radial positions of the discs in a large sample of spiral galaxies to obtain the slopes and the characteristic abundance ratios that can be related to their integrated properties. Methods. We analysed the optical spectra of individual selected H ii regions extracted from a sample of 350 spiral 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 Pérez-Montero (2014, MNRAS, 441, 2663), is consistent with the direct method and reduces the uncertainty in the O/H derivation using [N ii] 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. Results. 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

Published
2016

7. CALIFA, the Calar Alto Legacy Integral Field Area survey

Author

Sánchez, S. F., primary, García-Benito, R., additional, Zibetti, S., additional, Walcher, C. J., additional, Husemann, B., additional, Mendoza, M. A., additional, Galbany, L., additional, Falcón-Barroso, J., additional, Mast, D., additional, Aceituno, J., additional, Aguerri, J. A. L., additional, Alves, J., additional, Amorim, A. L., additional, Ascasibar, Y., additional, Barrado-Navascues, D., additional, Barrera-Ballesteros, J., additional, Bekeraitè, S., additional, Bland-Hawthorn, J., additional, Cano Díaz, M., additional, Cid Fernandes, R., additional, Cavichia, O., additional, Cortijo, C., additional, Dannerbauer, H., additional, Demleitner, M., additional, Díaz, A., additional, Dettmar, R. J., additional, de Lorenzo-Cáceres, A., additional, del Olmo, A., additional, Galazzi, A., additional, García-Lorenzo, B., additional, Gil de Paz, A., additional, González Delgado, R., additional, Holmes, L., additional, Iglésias-Páramo, J., additional, Kehrig, C., additional, Kelz, A., additional, Kennicutt, R. C., additional, Kleemann, B., additional, Lacerda, E. A. D., additional, López Fernández, R., additional, López Sánchez, A. R., additional, Lyubenova, M., additional, Marino, R., additional, Márquez, I., additional, Mendez-Abreu, J., additional, Mollá, M., additional, Monreal-Ibero, A., additional, Ortega Minakata, R., additional, Torres-Papaqui, J. P., additional, Pérez, E., additional, Rosales-Ortega, F. F., additional, Roth, M. M., additional, Sánchez-Blázquez, P., additional, Schilling, U., additional, Spekkens, K., additional, Vale Asari, N., additional, van den Bosch, R. C. E., additional, van de Ven, G., additional, Vilchez, J. M., additional, Wild, V., additional, Wisotzki, L., additional, Yıldırım, A., additional, and Ziegler, B., additional

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

Author

Galbany, L., primary, Stanishev, V., additional, Mourão, A. M., additional, Rodrigues, M., additional, Flores, H., additional, Walcher, C. J., additional, Sánchez, S. F., additional, García-Benito, R., additional, Mast, D., additional, Badenes, C., additional, González Delgado, R. M., additional, Kehrig, C., additional, Lyubenova, M., additional, Marino, R. A., additional, Mollá, M., additional, Meidt, S., additional, Pérez, E., additional, van de Ven, G., additional, and Vílchez, J. M., additional

Published
2016
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9. Star formation along the Hubble sequence

Author

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

Published
2016
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10. Shape of the oxygen abundance profiles in CALIFA face-on spiral galaxies

Author

Sánchez-Menguiano, L., primary, Sánchez, S. F., additional, Pérez, I., additional, García-Benito, R., additional, Husemann, B., additional, Mast, D., additional, Mendoza, A., additional, Ruiz-Lara, T., additional, Ascasibar, Y., additional, Bland-Hawthorn, J., additional, Cavichia, O., additional, Díaz, A. I., additional, Florido, E., additional, Galbany, L., additional, Gónzalez Delgado, R. M., additional, Kehrig, C., additional, Marino, R. A., additional, Márquez, I., additional, Masegosa, J., additional, Méndez-Abreu, J., additional, Mollá, M., additional, del Olmo, A., additional, Pérez, E., additional, Sánchez-Blázquez, P., additional, Stanishev, V., additional, Walcher, C. J., additional, López-Sánchez, Á. R., additional, and the CALIFA, collaboration, additional

Published
2016
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11. CALIFA, the Calar Alto Legacy Integral Field Area survey

Author

García-Benito, R., primary, Zibetti, S., additional, Sánchez, S. F., additional, Husemann, B., additional, de Amorim, A. L., additional, Castillo-Morales, A., additional, Cid Fernandes, R., additional, Ellis, S. C., additional, Falcón-Barroso, J., additional, Galbany, L., additional, Gil de Paz, A., additional, González Delgado, R. M., additional, Lacerda, E. A. D., additional, López-Fernandez, R., additional, de Lorenzo-Cáceres, A., additional, Lyubenova, M., additional, Marino, R. A., additional, Mast, D., additional, Mendoza, M. A., additional, Pérez, E., additional, Vale Asari, N., additional, Aguerri, J. A. L., additional, Ascasibar, Y., additional, Bekerait*error*ė, S., additional, Bland-Hawthorn, J., additional, Barrera-Ballesteros, J. K., additional, Bomans, D. J., additional, Cano-Díaz, M., additional, Catalán-Torrecilla, C., additional, Cortijo, C., additional, Delgado-Inglada, G., additional, Demleitner, M., additional, Dettmar, R.-J., additional, Díaz, A. I., additional, Florido, E., additional, Gallazzi, A., additional, García-Lorenzo, B., additional, Gomes, J. M., additional, Holmes, L., additional, Iglesias-Páramo, J., additional, Jahnke, K., additional, Kalinova, V., additional, Kehrig, C., additional, Kennicutt, R. C., additional, López-Sánchez, Á. R., additional, Márquez, I., additional, Masegosa, J., additional, Meidt, S. E., additional, Mendez-Abreu, J., additional, Mollá, M., additional, Monreal-Ibero, A., additional, Morisset, C., additional, del Olmo, A., additional, Papaderos, P., additional, Pérez, I., additional, Quirrenbach, A., additional, Rosales-Ortega, F. F., additional, Roth, M. M., additional, Ruiz-Lara, T., additional, Sánchez-Blázquez, P., additional, Sánchez-Menguiano, L., additional, Singh, R., additional, Spekkens, K., additional, Stanishev, V., additional, Torres-Papaqui, J. P., additional, van de Ven, G., additional, Vilchez, J. M., additional, Walcher, C. J., additional, Wild, V., additional, Wisotzki, L., additional, Ziegler, B., additional, Alves, J., additional, Barrado, D., additional, Quintana, J. M., additional, and Aceituno, J., additional

Published
2015
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12. Stellar population gradients in galaxy discs from the CALIFA survey

Author

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

Published
2014
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13. Metallicity gradients in disks

Author

Pilkington, K., Few, C. G., Gibson, Bradley Kenneth, Calura, F., Michel-Dansac, L., Thacker, R. J., Mollá, M., Matteucci, F., Rahimi, A., Kawata, D., Kobayashi, C., Brook, C. B., Stinson, G. S., Couchman, H. M. P., Bailin, J., Wadsley, J., Pilkington, K., Few, C. G., Gibson, Bradley Kenneth, Calura, F., Michel-Dansac, L., Thacker, R. J., Mollá, M., Matteucci, F., Rahimi, A., Kawata, D., Kobayashi, C., Brook, C. B., Stinson, G. S., Couchman, H. M. P., Bailin, J., and Wadsley, J.

Abstract

Aims. We examine radial and vertical metallicity gradients using a suite of disk galaxy hydrodynamical simulations, supplemented with two classic chemical evolution approaches. We determine the rate of change of gradient slope and reconcile the differences existing between extant models and observations within the canonical “inside-out” disk growth paradigm. Methods. A suite of 25 cosmological disks is used to examine the evolution of metallicity gradients; this consists of 19 galaxies selected from the RaDES (Ramses Disk Environment Study) sample, realised with the adaptive mesh refinement code ramses, including eight drawn from the “field” and six from “loose group” environments. Four disks are selected from the MUGS (McMaster Unbiased Galaxy Simulations) sample, generated with the smoothed particle hydrodynamics (SPH) code gasoline. Two chemical evolution models of inside-out disk growth were employed to contrast the temporal evolution of their radial gradients with those of the simulations. Results. We first show that generically flatter gradients are observed at redshift zero when comparing older stars with those forming today, consistent with expectations of kinematically hot simulations, but counter to that observed in the Milky Way. The vertical abundance gradients at ~1−3 disk scalelengths are comparable to those observed in the thick disk of the Milky Way, but significantly shallower than those seen in the thin disk. Most importantly, we find that systematic differences exist between the predicted evolution of radial abundance gradients in the RaDES and chemical evolution models, compared with the MUGS sample; specifically, the MUGS simulations are systematically steeper at high-redshift, and present much more rapid evolution in their gradients. Conclusions. We find that the majority of the models predict radial gradients today which are consistent with those observed in late-type disks, but they evolve to this self-similarity in different fashions, despit

Published
2012

14. The O3N2 and N2 abundance indicators revisited: improved calibrations based on CALIFA andTe-based literature data

Author

Marino, R. A., primary, Rosales-Ortega, F. F., additional, Sánchez, S. F., additional, Gil de Paz, A., additional, Vílchez, J., additional, Miralles-Caballero, D., additional, Kehrig, C., additional, Pérez-Montero, E., additional, Stanishev, V., additional, Iglesias-Páramo, J., additional, Díaz, A. I., additional, Castillo-Morales, A., additional, Kennicutt, R., additional, López-Sánchez, A. R., additional, Galbany, L., additional, García-Benito, R., additional, Mast, D., additional, Mendez-Abreu, J., additional, Monreal-Ibero, A., additional, Husemann, B., additional, Walcher, C. J., additional, García-Lorenzo, B., additional, Masegosa, J., additional, del Olmo Orozco, A., additional, Mourão, A. M., additional, Ziegler, B., additional, Mollá, M., additional, Papaderos, P., additional, Sánchez-Blázquez, P., additional, González Delgado, R. M., additional, Falcón-Barroso, J., additional, Roth, M. M., additional, van de Ven, G., additional, and team, CALIFA, additional

Published
2013
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15. A Virtual Observatory Census to Address Dwarfs Origins (AVOCADO)

Author

Sánchez-Janssen, R., primary, Amorín, R., additional, García-Vargas, M., additional, Gomes, J. M., additional, Huertas-Company, M., additional, Jiménez-Esteban, F., additional, Mollá, M., additional, Papaderos, P., additional, Pérez-Montero, E., additional, Rodrigo, C., additional, Sánchez Almeida, J., additional, and Solano, E., additional

Published
2013
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16. Aperture corrections for disk galaxy properties derived from the CALIFA survey

Author

Iglesias-Páramo, J., primary, Vílchez, J. M., additional, Galbany, L., additional, Sánchez, S. F., additional, Rosales-Ortega, F. F., additional, Mast, D., additional, García-Benito, R., additional, Husemann, B., additional, Aguerri, J. A. L., additional, Alves, J., additional, Bekeraité, S., additional, Bland-Hawthorn, J., additional, Catalán-Torrecilla, C., additional, de Amorim, A. L., additional, de Lorenzo-Cáceres, A., additional, Ellis, S., additional, Falcón-Barroso, J., additional, Flores, H., additional, Florido, E., additional, Gallazzi, A., additional, Gomes, J. M., additional, González Delgado, R. M., additional, Haines, T., additional, Hernández-Fernández, J. D., additional, Kehrig, C., additional, López-Sánchez, A. R., additional, Lyubenova, M., additional, Marino, R. A., additional, Mollá, M., additional, Monreal-Ibero, A., additional, Mourão, A., additional, Papaderos, P., additional, Rodrigues, M., additional, Sánchez-Blázquez, P., additional, Spekkens, K., additional, Stanishev, V., additional, van de Ven, G., additional, Walcher, C. J., additional, Wisotzki, L., additional, Zibetti, S., additional, and Ziegler, B., additional

Published
2013
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17. CALIFA, the Calar Alto Legacy Integral Field Area survey

Author

Husemann, B., primary, Jahnke, K., additional, Sánchez, S. F., additional, Barrado, D., additional, Bekerait*error*ė, S., additional, Bomans, D. J., additional, Castillo-Morales, A., additional, Catalán-Torrecilla, C., additional, Cid Fernandes, R., additional, Falcón-Barroso, J., additional, García-Benito, R., additional, González Delgado, R. M., additional, Iglesias-Páramo, J., additional, Johnson, B. D., additional, Kupko, D., additional, López-Fernandez, R., additional, Lyubenova, M., additional, Marino, R. A., additional, Mast, D., additional, Miskolczi, A., additional, Monreal-Ibero, A., additional, Gil de Paz, A., additional, Pérez, E., additional, Pérez, I., additional, Rosales-Ortega, F. F., additional, Ruiz-Lara, T., additional, Schilling, U., additional, van de Ven, G., additional, Walcher, J., additional, Alves, J., additional, de Amorim, A. L., additional, Backsmann, N., additional, Barrera-Ballesteros, J. K., additional, Bland-Hawthorn, J., additional, Cortijo, C., additional, Dettmar, R.-J., additional, Demleitner, M., additional, Díaz, A. I., additional, Enke, H., additional, Florido, E., additional, Flores, H., additional, Galbany, L., additional, Gallazzi, A., additional, García-Lorenzo, B., additional, Gomes, J. M., additional, Gruel, N., additional, Haines, T., additional, Holmes, L., additional, Jungwiert, B., additional, Kalinova, V., additional, Kehrig, C., additional, Kennicutt, R. C., additional, Klar, J., additional, Lehnert, M. D., additional, López-Sánchez, Á. R., additional, de Lorenzo-Cáceres, A., additional, Mármol-Queraltó, E., additional, Márquez, I., additional, Mendez-Abreu, J., additional, Mollá, M., additional, del Olmo, A., additional, Meidt, S. E., additional, Papaderos, P., additional, Puschnig, J., additional, Quirrenbach, A., additional, Roth, M. M., additional, Sánchez-Blázquez, P., additional, Spekkens, K., additional, Singh, R., additional, Stanishev, V., additional, Trager, S. C., additional, Vilchez, J. M., additional, Wild, V., additional, Wisotzki, L., additional, Zibetti, S., additional, and Ziegler, B., additional

Published
2013
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18. Metallicity gradients in disks

Author

Pilkington, K., primary, Few, C. G., additional, Gibson, B. K., additional, Calura, F., additional, Michel-Dansac, L., additional, Thacker, R. J., additional, Mollá, M., additional, Matteucci, F., additional, Rahimi, A., additional, Kawata, D., additional, Kobayashi, C., additional, Brook, C. B., additional, Stinson, G. S., additional, Couchman, H. M. P., additional, Bailin, J., additional, and Wadsley, J., additional

Published
2012
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20. The CALIFA survey across the Hubble sequence.

Author

González Delgado, R. M., García-Benito, R., Pérez, E., Cid Fernandes, R., de Amorim, A. L., Cortijo-Ferrero, C., Lacerda, E. A. D., López Fernández, R., Vale-Asari, N., Sánchez, S. F., Mollá, M., Ruiz-Lara, T., Sánchez-Blázquez, P., Walcher, C. J., Alves, J., Aguerri, J. A. L., Bekeraité, S., Bland-Hawthorn, J., Galbany, L., and Gallazzi, A.

Subjects
HUBBLE constant, STELLAR evolution, STELLAR mass, GALACTIC evolution, STELLAR populations
Abstract

Various different physical processes contribute to the star formation and stellar mass assembly histories of galaxies. One important approach to understanding the significance of these different processes on galaxy evolution is the study of the stellar population content of today's galaxies in a spatially resolved manner. The aim of this paper is to characterize in detail the radial structure of stellar population properties of galaxies in the nearby universe, based on a uniquely large galaxy sample, considering the quality and coverage of the data. The sample under study was drawn from the CALIFA survey and contains 300 galaxies observed with integral field spectroscopy. These cover a wide range of Hubble types, from spheroids to spiral galaxies, while stellar masses range from M⋆ ~ 109 to 7 x 1011 M ⊙. We apply the fossil record method based on spectral synthesis techniques to recover the following physical properties for each spatial resolution element in our target galaxies: the stellar mass surface density (µ⋆), stellar extinction (AV), light-weighted and mass-weighted ages (L,M), and mass-weighted metallicity (log Z⋆>M). To study mean trends with overall galaxy properties, the individual radial profiles are stacked in seven bins of galaxy morphology (E, S0, Sa, Sb, Sbc, Sc, and Sd). We confirm that more massive galaxies are more compact, older, moremetal rich, and less reddened by dust. Additionally, we find that these trends are preserved spatially with the radial distance to the nucleus. Deviations from these relations appear correlated with Hubble type: earlier types are more compact, older, and more metal rich for a given M⋆, which is evidence that quenching is related to morphology, but not driven by mass. Negative gradients of L are consistent with an inside-out growth of galaxies, with the largest L gradients in Sb-Sbc galaxies. Further, the mean stellar ages of disks and bulges are correlated and with disks covering a wider range of ages, and late-type spirals hosting younger disks. However, age gradients are only mildly negative or flat beyond R ~ 2 HLR (half light radius), indicating that star formation is more uniformly distributed or that stellar migration is important at these distances. The gradients in stellar mass surface density depend mostly on stellar mass, in the sense that more massive galaxies are more centrally concentrated. Whatever sets the concentration indices of galaxies obviously depends less on quenching/morphology than on the depth of the potential well. There is a secondary correlation in the sense that at the sameM⋆ early-type galaxies have steeper gradients. The μ⋆ gradients outside 1 HLR show no dependence on Hubble type. We find mildly negative ⋆>M gradients, which are shallower than predicted from models of galaxy evolution in isolation. In general, metallicity gradients depend on stellar mass, and less on morphology, hinting that metallicity is affected by both -- the depth of the potential well and morphology/quenching. Thus, the largest ⋆>M gradients occur in Milky Way-like Sb-Sbc galaxies, and are similar to those measured above the Galactic disk. Sc spirals show flatter ⋆>M gradients, possibly indicating a larger contribution from secular evolution in disks. The galaxies from the sample have decreasing-outward stellar extinction; all spirals show similar radial profiles, independent from the stellar mass, but redder than E and S0. Overall, we conclude that quenching processes act in manners that are independent of mass, while metallicity and galaxy structure are influenced by mass-dependent processes. [ABSTRACT FROM AUTHOR]

Published
2015
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26. Imprints of galaxy evolution on H II regions.

Author

Sánchez, S. F., Pérez, E., Rosales-Ortega, F. F., Miralles-Caballero, D., López-Sánchez, A. R., Iglesias-Páramo, J., Marino, R. A., Sánchez-Menguiano, L., García-Benito, R., Mast, D., Mendoza, M. A., Papaderos, P., Ellis, S., Galbany, L., Kehrig, C., Monreal-Ibero, A., Delgado, R. González, Mollá, M., Ziegler, B., and de Lorenzo-Cáceres, A.

Subjects
GALACTIC evolution, H II regions (Astrophysics), STELLAR mass, PHOTOIONIZATION, INTERSTELLAR medium, ACTIVE galactic nuclei
Abstract

Context. H II regions in galaxies are the sites of star formation, so they are special places for understanding the build-up of stellar mass in the universe. The line ratios of this ionized gas are frequently used to characterize the ionization conditions. In particular, the oxygen abundances are assumed to trace the chemical enrichment of galaxies. Aims. We explore the connections between the ionization conditions and the properties of the overall underlying stellar population (ionizing or not-ionizing) in H II regions, in order to uncover the actual physical connection between them. Methods. We use the H II regions catalog from the CALIFA survey, which is the largest in existence with more than 5000 H II regions, to explore their distribution across the classical [O III] λ5007/Hβ vs. [N II] λ6583/Hα diagnostic diagram, and the way it depends on the oxygen abundance, ionization parameter, electron density, and dust attenuation. The location of H II regions within this diagram is compared with predictions from photoionization models. Finally, we explore the dependence of the location within the diagnostic diagram on the properties of the host galaxies, the galactocentric distances, and the properties of the underlying stellar population. Results. The H II regions with weaker ionization strengths and more metal-rich are located in the bottom righthand area of the diagram. In contrast, those regions with stronger ionization strengths and more metal poor are located in the upper lefthand end of the diagram. Photoionization models per se do not predict these correlations between the parameters and the line ratios. The H II regions located in earlier-type galaxies, closer to the center and formed in older and more metal-rich regions of the galaxies are located in the bottom-right area of the diagram. On the other hand, those regions located in late-type galaxies in the outer regions of the disks and formed on younger and more metal-poor regions lie in the top lefthand area of the diagram. The two explored line ratios show strong correlations with the age and metallicity of the underlying stellar population. Conclusions. These results indicate that although H II regions are short-lived events, they are affected by the total underlying stellar population. One may say that H II regions keep a memory of the stellar evolution and chemical enrichment that have left an imprint on both the ionizing stellar population and the ionized gas. [ABSTRACT FROM AUTHOR]

Published
2015
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28. A characteristic oxygen abundance gradient in galaxy disks unveiled with CALIFA⋆,⋆⋆.

Author

Sánchez, S. F., Rosales-Ortega, F. F., Iglesias-Páramo, J., Mollá, M., Barrera-Ballesteros, J., Marino, R. A., Pérez, E., Sánchez-Blazquez, P., González Delgado, R., Fernandes, R. Cid, de Lorenzo-Cáceres, A., Mendez-Abreu, J., Galbany, L., Falcon-Barroso, J., Miralles-Caballero, D., Husemann, B., García-Benito, R., Mast, D., Walcher, C. J., and Paz, A. Gil de

Subjects
INTERSTELLAR medium, ASTRONOMICAL spectroscopy, GALACTIC evolution, STAR formation, GALAXY formation
Abstract

We present the largest and most homogeneous catalog of Hii regions and associations compiled so far. The catalog comprises more than 7000 ionized regions, extracted from 306 galaxies observed by the CALIFA survey. We describe the procedures used to detect, select, and analyze the spectroscopic properties of these ionized regions. In the current study we focus on characterizing of the radial gradient of the oxygen abundance in the ionized gas, based on the study of the deprojected distribution of Hii regions. We found that all galaxies without clear evidence of an interaction present a common gradient in the oxygen abundance, with a characteristic slope of αO/H = -0.1 dex/re between 0.3 and 2 disk effective radii (re), and a scatter compatible with random fluctuations around this value, when the gradient is normalized to the disk effective radius. The slope is independent of morphology, the incidence of bars, absolute magnitude, or mass. Only those galaxies with evidence of interactions and/or clear merging systems present a significantly shallower gradient, consistent with previous results. The majority of the 94 galaxies with Hii regions detected beyond two disk effective radii present a flattening in the oxygen abundance. The flattening is statistically significant. We cannot provide a conclusive answer regarding the origin of this flattening. However, our results indicate that its origin is most probably related to the secular evolution of galaxies. Finally, we find a drop/truncation of the oxygen abundance in the inner regions for 26 of the galaxies. All of them are non-interacting, mostly unbarred Sb/Sbc galaxies. This feature is associated with a central star-forming ring, which suggests that both features are produced by radial gas flows induced by resonance processes. Our result suggests that galaxy disks grow inside-out, with metal enrichment driven by the local star formation history and with a small variation galaxy-by-galaxy. At a certain galactocentric distance, the oxygen abundance seems to be correlated well with the stellar mass density and total stellar mass of the galaxies, independently of other properties of the galaxies. Other processes, such as radial mixing and inflows/outflows seem to have a limited effect on shaping of the radial distribution of oxygen abundances, although they are not ruled out. [ABSTRACT FROM AUTHOR]

Published
2014
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29. The dependence of oxygen and nitrogen abundances on stellar mass from the CALIFA survey (Corrigendum).

Author

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

Subjects
OXYGEN, STELLAR mass, GALACTIC evolution
Published
2018
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