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310 results on '"Mendez-Abreu, J."'

101. The population of barred galaxies in the local universe I. Detection and characterisation of bars

Author

Aguerri, J. A. L., Mendez-Abreu, J., and Corsini, E. M.

Subjects
Astrophysics - Galaxy Astrophysics
Abstract

(Abridge) Bars are very common in the centre of the disc galaxies, and they drive the evolution of their structure. A volume-limited sample of 2106 disc galaxies extracted from the Sloan Digital Sky Survey Data Release 5 was studied to derive the bar fraction, length, and strength as a function of the morphology, size, local galaxy density, light concentration, and colour of the host galaxy. The bars were detected using the ellipse fitting method and Fourier analysis method. The ellipse fitting method was found to be more efficient in detecting bars in spiral galaxies. The fraction of barred galaxies turned out to be 45%. A bar was found in 29% of the lenticular galaxies, in 55% and 54% of the early- and late-type spirals, respectively. The bar length (normalised by the galaxy size) of late-type spirals is shorter than in early-type or lenticular ones. A correlation between the bar length and galaxy size was found with longer bars hosted by larger galaxies. The bars of the lenticular galaxies are weaker than those in spirals. Moreover, the unimodal distribution of the bar strength found for all the galaxy types argues against a quick transition between the barred and unbarred statues. There is no difference between the local galaxy density of barred and unbarred galaxies. Besides, neither the length nor strength of the bars are correlated with the local density of the galaxy neighbourhoods. In contrast, a statistical significant difference between the central light concentration and colour of barred and unbarred galaxies was found. Bars are mostly located in less concentrated and bluer galaxies. These results indicate that the properties of bars are strongly related to those of their host galaxies, but do not depend on the local environment., Comment: 15 pages, 13 figures. Accepted for publication in A&A

Published
2009
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102. Stellar Populations of Bulges in 14 Cluster Disc Galaxies

Author

Morelli, L., Pompei, E., Pizzella, A., Méndez-Abreu, J., Corsini, E. M., Coccato, L., Saglia, R. P., Sarzi, M., and Bertola, F.

Subjects
Astrophysics
Abstract

Photometry and long-slit spectroscopy are presented for 14 S0 and spiral galaxies of the Fornax, Eridanus and Pegasus cluster, and NGC 7582 group. The structural parameters of the galaxies are derived from the R-band images by performing a two-dimensional photometric decomposition of the surface-brightness distribution. This is assumed to be the sum of the contribution of a bulge and disc component characterized by elliptical and concentric isophotes with constant (but possibly different) ellipticity and position angles. The rotation curves and velocity dispersion profiles are measured from the spectra obtained along the major axis of galaxies. The radial profiles of the Hb, Mg, and Fe line-strength indices are presented too. Correlations between the central values of Mgd, , Hb, and sigma are found. The age, metallicity and alpha/Fe enhancement of the stellar population in the center and at the radius where bulge and disc give the same contribution to the total surface brightness are obtained using stellar population models with variable element abundance ratios. Three classes of bulges are identified. The youngest bulges (~2 Gyr) with ongoing star formation, intermediate-age bulges (4-8 Gyr) have solar metallicity, and old bulges (~10 Gyr) have high metallicity. Most of the sample bulges display solar alpha/Fe enhancement, no gradient in age, and a negative gradient of metallicity. The presence of negative gradient in the metallicity radial profile favors a scenario with bulge formation via dissipative collapse. (abridged), Comment: 27 pages, 16 figures, 6 tables, accepted for pubblication on MNRAS

Published
2008
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103. Confirmation of a Kinematic Diagnostic for Face-On B/P Bulges

Author

Mendez-Abreu, J., Corsini, E. M., Debattista, Victor P., De Rijcke, S., Aguerri, J. A. L., and Pizzella, A.

Subjects
Astrophysics
Abstract

We present the results of high resolution absorption-line spectroscopy of 3 face-on galaxies, NGC 98, NGC 600, and NGC 1703 with the aim of searching for box/peanut (B/P)-shaped bulges. These observations test and confirm, for the first, time the prediction that face-on B/P-shaped bulges can be recognized by two minima in the profile along the bar's major axis of the fourth Gauss-Hermite moment h_4 of the line-of-sight velocity distribution (LOSVD). In NGC 98, a clear double minimum in h_4 is present along the major axis of the bar and before the end of the bar, as predicted. In contrast, in NGC 600, which is also a barred galaxy but lacks a substantial bulge, we do not find any significant kinematic signature for a B/P-shaped bulge. In NGC 1703, which is an unbarred control galaxy, we found no evidence of a B/P bulge. We also show directly that the LOSVD is broader at the location of the h_4 minimum in NGC 98 than elsewhere. This more direct method avoids possible artifacts associated with the degeneracy between the measurement of line-of-sight velocity dispersion and h_4., Comment: 12 pages, 1 figure, accepted for publication in ApJL

Published
2008
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104. Structure and dynamics of galaxies with a low surface brightness disc. I. The stellar and ionised-gas kinematics

Author

Pizzella, A., Corsini, E. M., Sarzi, M., Magorrian, J., Mendez-Abreu, J., Coccato, L., Morelli, L., and Bertola, F.

Subjects
Astrophysics
Abstract

(abridged) Photometry and long-slit spectroscopy are presented for a sample of 6 galaxies with a low surface brightness stellar disc and a bulge. The stellar and ionised-gas kinematics were measured along the major and minor axis in half of the sample galaxies, whereas the other half was observed only along two diagonal axes. Spectra along two diagonal axes were obtained also for one of the objects with major and minor axis spectra. The kinematic measurements extend in the disc region out to a surface-brightness level mu_R~24mag/arcsec^2 reaching in all cases the flat part of the rotation curve. The stellar kinematics turns out to be more regular and symmetric than the ionised-gas kinematics, which often shows the presence of non-circular, off-plane, and non-ordered motions. This raises the question about the reliability of the use of the ionised gas as the tracer of the circular velocity in the modeling of the mass distribution, in particular in the central regions of low surface brightness galaxies., Comment: Accepted for pubblication on MNRAS (11 figures and 15 tables)

Published
2008
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105. The pseudobulge of NGC 1292

Author

Morelli, L., Pompei, E., Pizzella, A., Méndez-Abreu, J., Corsini, E. M., Coccato, L., Saglia, R. P., Sarzi, M., and Bertola, F.

Subjects
Astrophysics
Abstract

The photometric and kinematic properties of Sb NGC 1292 suggest it hosts a pseudobulge. The properties of the stellar population of such a pseudobulge are consistent with a slow buildup within a scenario of secular evolution., Comment: 2 pages, 1 figure to appear in the proceedings of "Formation and Evolution of Galaxy Disks", Rome, October 2007, Eds. J. Funes and E. M. Corsini

Published
2008

106. Properties of bars in the local universe

Author

Méndez-Abreu, J., Aguerri, J. A. L., and Corsini, E. M.

Subjects
Astrophysics
Abstract

We studied the fraction and properties of bars in a sample of about 3000 galaxies extracted from SDSS-DR5. This represents a volume limited sample with galaxies located between redshift 0.01-20, and inclination i < 60. Interacting galaxies were excluded from the sample. The fraction of barred galaxies in our sample is 45%. We found that 32% of S0s, 55% of early-type spirals, and 52% of late-type spirals are barred galaxies. The bars in S0s galaxies are weaker than those in later-type galaxies. The bar length and galaxy size are correlated, being larger bars located in larger galaxies. Neither the bar strength nor bar length correlate with the local galaxy density. On the contrary, the bar properties correlate with the properties of their host galaxies. Galaxies with higher central light concentration host less and weaker bars., Comment: 2 pages, 1 figure to appear in the proceedings of "Formation and Evolution of Galaxy Disks", Rome, October 2007, Eds. J. Funes and E. M. Corsini

Published
2008

107. Structural properties of disk galaxies: The intrinsic equatorial ellipticity of bulges

Author

Méndez-Abreu, J., Aguerri, J. A. L., Corsini, E. M., and Simonneau, E.

Subjects
Astrophysics
Abstract

The structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies were derived to study the correlations between bulge and disk parameters as well as the probability distribution function (PDF) of the intrinsic equatorial ellipticity of bulges. A new algorithm (GASP2D) was used to perform the bidimensional bulge-disk decomposition of the J-band galaxy images extracted from the archive of the 2MASS survey. The PDF of intrinsic ellipticities was derived from the distribution of the observed ellipticities of the bulges and misalignments between the the bulges and disks. About 80% of the observed bulges are not oblate but triaxial ellipsoids. Their mean axial ratio in the equatorial plane is =0.85. There is not significant dependence of their PDF on morphology, light concentration or luminosity. This has to be explained by the different scenarios of bulge formation., Comment: 2 pages, 1 figure to appear in the proceedings of "Formation and Evolution of Galaxy Disks", Rome, October 2007, Eds. J. Funes and E. M. Corsini

Published
2008

108. Structural properties of disk galaxies I. The intrinsic ellipticity of bulges

Author

Mendez-Abreu, J., Aguerri, J. A. L., Corsini, E. M., and Simonneau, E.

Subjects
Astrophysics
Abstract

(Abridged) A variety of formation scenarios was proposed to explain the diversity of properties observed in bulges. Studying their intrinsic shape can help in constraining the dominant mechanism at the epochs of their assembly. The structural parameters of a magnitude-limited sample of 148 unbarred S0--Sb galaxies were derived in order to study the correlations between bulges and disks as well as the probability distribution function (PDF) of the intrinsic equatorial ellipticity of bulges. It is presented a new fitting algorithm (GASP2D) to perform the two-dimensional photometric decomposition of galaxy surface-brightness distribution. This was assumed to be the sum of the contribution of a bulge and disk component characterized by elliptical and concentric isophotes with constant (but possibly different) ellipticity and position angles. Bulge and disk parameters of the sample galaxies were derived from the J-band images which were available in the Two Micron All Sky Survey. The PDF of the equatorial ellipticity of the bulges was derived from the distribution of the observed ellipticities of bulges and misalignments between bulges and disks. Strong correlations between the bulge and disk parameters were found. About 80% of bulges in unbarred lenticular and early-to-intermediate spiral galaxies are not oblate but triaxial ellipsoids. Their mean axial ratio in the equatorial plane is = 0.85. There is not significant dependence of their PDF on morphology, light concentration, and luminosity. The interplay between bulge and disk parameters favors scenarios in which bulges assembled from mergers and/or grew over long times through disk secular evolution. But all these mechanisms have to be tested against the derived distribution of bulge intrinsic ellipticities., Comment: 24 pages, 13 figures, accepted for publication in A&A, corrected proofs

Published
2007
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109. Imprints of galaxy evolution on H II regions: memory of the past uncovered by the CALIFA survey

Author

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

Abstract

© ESO 2014. Artículo firmado por 29 autores y la colaboración de CALIFA. We thank Prf. Dr. M. Dopita for his comments and suggestions during the reviewing process. He helped to improve significantly the interpretation of our results and the overall manuscript. S.F.S. thanks the director of CEFCA, M. Moles, for his sincere support to this project. This study makes uses of the data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey (http://califa.caha.es/). CALIFA is the first legacy survey being performed at Calar Alto. The CALIFA collaboration would like to thank the IAA-CSIC and MPIA-MPG as major partners of the observatory and CAHA itself, for the unique access to telescope time and support in manpower and infrastructures. The CALIFA collaboration also thanks the CAHA staff for the dedication to this project. This work was based on observations collected at the Centro Astronómico Hispano Aleman (CAHA) at Calar Alto, operated jointly by the Max-Planck-Institut fur Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). We thank the Viabilidad, Diseño, Acceso y Mejora funding program, ICTS-2009-10, for supporting the initial developement of this project. S.F.S. thanks the ConaCyt funding program 180125, for the support given to this project. S.ES., M. A. M. and L.S.M. thank the Plan Nacional de Investigación y Desarrollo funding programs, AYA2012-31935, of the Spanish Ministerio de Economía y Competitividad, for the support given to this project. S.F.S. thanks the Ramón y Cajal project RyC-2011-07590 of the Spanish Ministerio de Economía y Competitividad, for its support of this project. P.P. is supported by a FCT Investigator 2013 consolidation grant. He acknowledges support by the Fundacao para a Ciencia e a Tecnología (FCT) under project FCOMP-010124-FEDER-029170 (Reference FCT PTDC/FIS-AST/3214/2012), funded by FCT-MEC (PIDDAC) and FEDER (COMPETE). R.G.D., E.P., and R.G.B. thank the Plan Nacional de Investigación y Desarrollo funding, Context. H II regions in galaxies are the sites of star formation, so they are special places for understanding the build-up of stellar mass in the universe. The line ratios of this ionized gas are frequently used to characterize the ionization conditions. In particular, the oxygen abundances are assumed to trace the chemical enrichment of galaxies. Aims. We explore the connections between the ionization conditions and the properties of the overall underlying stellar population (ionizing or not-ionizing) in H II regions, in order to uncover the actual physical connection between them. Methods. We use the H II regions catalog from the CALIFA survey, which is the largest in existence with more than 5000 H II regions, to explore their distribution across the classical [O III] lambda 5007/H beta vs. [N II] lambda 6583/H alpha diagnostic diagram, and the way it depends on the oxygen abundance, ionization parameter, electron density, and dust attenuation. The location of H II regions within this diagram is compared with predictions from photoionization models. Finally, we explore the dependence of the location within the diagnostic diagram on the properties of the host galaxies, the galactocentric distances, and the properties of the underlying stellar population. Results. The H II regions with weaker ionization strengths and more metal-rich are located in the bottom righthand area of the diagram. In contrast, those regions with stronger ionization strengths and more metal poor are located in the upper lefthand end of the diagram. Photoionization models per se do not predict these correlations between the parameters and the line ratios. The H II regions located in earlier-type galaxies, closer to the center and formed in older and more metal-rich regions of the galaxies are located in the bottom-right area of the diagram. On the other hand, those regions located in late-type galaxies in the outer regions of the disks and formed on younger and more metal-poor regions lie i, Viabilidad, Diseño, Acceso y Mejora funding program, ConaCyt funding program, Spanish Ministerio de Economia y Competitividad, FCT Investigator consolidation grant, Fundacao para a Ciencia e a Tecnologia (FCT) - FCT-MEC (PIDDAC), FEDER (COMPETE), Plan Nacional de Investigación y Desarrollo, Ministry of Economy, Development, and Tourism's Millennium Science Initiative, CONICYT through FONDECYT grant, Spanish program of International Campus of Excellence Moncloa (CEI), Agence Nationale de la Recherche through the STILISM project, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Published
2023

110. The VANDELS ESO public spectroscopic survey

Author

Garilli, B., Mclure, R., Pentericci, L., Franzetti, P., Gargiulo, A., Carnall, A., Cucciati, O., Iovino, A., Amorin, R., Bolzonella, M., Bongiorno, A., Castellano, M., Cimatti, A., Cirasuolo, M., Cullen, F., Dunlop, J., Elbaz, D., Finkelstein, S., Fontana, A., Fontanot, F., Fumana, M., Guaita, L., Hartley, W., Jarvis, M., Juneau, S., Maccagni, D., Mcleod, D., Nandra, K., Pompei, E., Pozzetti, L., Scodeggio, M., Talia, M., Calabrò, A., Cresci, G., Fynbo, J., Hathi, N., Hibon, P., Koekemoer, A., Magliocchetti, M., Salvato, M., Vietri, G., Zamorani, G., Almaini, O., Balestra, I., Bardelli, S., Begley, R., Brammer, G., Bell, E., Bowler, R., Brusa, M., Buitrago, F., Caputi, C., Cassata, P., Charlot, S., Citro, A., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G., Ferguson, H., Fiore, F., Franco, M., Georgakakis, A., Giavalisco, M., Grazian, A., Hamadouche, M., Jung, I., Kim, S., Khusanova, Y., Le Fèvre, O., Longhetti, M., Lotz, J., Mannucci, F., Maltby, D., Matsuoka, K., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Roberts-Borsani, G., Rosario, D., Saldana-Lopez, A., Santini, P., Saxena, A., Schaerer, D., Schreiber, C., Stark, D., Tasca, L., Thomas, R., Vanzella, E., Wild, V., Williams, C., Zucca, E., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Astrophysique de Marseille (LAM), and 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)

Subjects
[PHYS]Physics [physics], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, cosmology: observations, galaxies: fundamental parameters, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: distances and redshifts, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: statistics, catalogs, Astrophysics::Galaxy Astrophysics
Abstract

International audience; VANDELS is an ESO Public Spectroscopic Survey designed to build a sample of high-signal-to-noise ratio, medium-resolution spectra of galaxies at redshifts between 1 and 6.5. Here we present the final Public Data Release of the VANDELS Survey, comprising 2087 redshift measurements. We provide a detailed description of sample selection, observations, and data reduction procedures. The final catalogue reaches a target selection completeness of 40% at i AB = 25. The high signal-to-noise ratio of the spectra (above 7 in 80% of the spectra) and the dispersion of 2.5 Å allowed us to measure redshifts with high precision, the redshift measurement success rate reaching almost 100%. Together with the redshift catalogue and the reduced spectra, we also provide optical mid-infrared photometry and physical parameters derived through fitting the spectral energy distribution. The observed galaxy sample comprises both passive and star forming galaxies covering a stellar mass range of 8.3 < Log( M * / M ⊙ ) < 11.7.

Published
2021
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111. The VANDELS ESO public spectroscopic survey:Final data release of 2087 spectra and spectroscopic measurements

Author

Garilli, B., McLure, R., Pentericci, L., Franzetti, P., Gargiulo, A., Carnall, A., Cucciati, O., Iovino, A., Amorin, R., Bolzonella, M., Bongiorno, A., Castellano, M., Cimatti, A., Cirasuolo, M., Cullen, F., Dunlop, J., Elbaz, D., Finkelstein, S., Fontana, A., Fontanot, F., Fumana, M., Guaita, L., Hartley, W., Jarvis, M., Juneau, S., Maccagni, D., McLeod, D., Nandra, K., Pompei, E., Pozzetti, L., Scodeggio, M., Talia, M., Calabro, A., Cresci, G., Fynbo, J. P. U., Hathi, N. P., Hibon, P., Koekemoer, A. M., Magliocchetti, M., Salvato, M., Vietri, G., Zamorani, G., Almaini, O., Balestra, I., Bardelli, S., Begley, R., Brammer, G., Bell, E. F., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, C., Cassata, P., Charlot, S., Citro, A., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G., Ferguson, H. C., Fiore, F., Franco, M., Georgakakis, A., Giavalisco, M., Grazian, A., Hamadouche, M., Jung, I., Kim, S., Khusanova, Y., Le Fevre, O., Longhetti, M., Lotz, J., Mannucci, F., Maltby, D., Matsuoka, K., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Roberts-Borsani, G., Rosario, D. J., Saldana-Lopez, A., Santini, P., Saxena, A., Schaerer, D., Schreiber, C., Stark, D., Tasca, L. A. M., Thomas, R., Vanzella, E., Wild, V., Williams, C., Zucca, E., Garilli, B., McLure, R., Pentericci, L., Franzetti, P., Gargiulo, A., Carnall, A., Cucciati, O., Iovino, A., Amorin, R., Bolzonella, M., Bongiorno, A., Castellano, M., Cimatti, A., Cirasuolo, M., Cullen, F., Dunlop, J., Elbaz, D., Finkelstein, S., Fontana, A., Fontanot, F., Fumana, M., Guaita, L., Hartley, W., Jarvis, M., Juneau, S., Maccagni, D., McLeod, D., Nandra, K., Pompei, E., Pozzetti, L., Scodeggio, M., Talia, M., Calabro, A., Cresci, G., Fynbo, J. P. U., Hathi, N. P., Hibon, P., Koekemoer, A. M., Magliocchetti, M., Salvato, M., Vietri, G., Zamorani, G., Almaini, O., Balestra, I., Bardelli, S., Begley, R., Brammer, G., Bell, E. F., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, C., Cassata, P., Charlot, S., Citro, A., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G., Ferguson, H. C., Fiore, F., Franco, M., Georgakakis, A., Giavalisco, M., Grazian, A., Hamadouche, M., Jung, I., Kim, S., Khusanova, Y., Le Fevre, O., Longhetti, M., Lotz, J., Mannucci, F., Maltby, D., Matsuoka, K., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Roberts-Borsani, G., Rosario, D. J., Saldana-Lopez, A., Santini, P., Saxena, A., Schaerer, D., Schreiber, C., Stark, D., Tasca, L. A. M., Thomas, R., Vanzella, E., Wild, V., Williams, C., and Zucca, E.

Abstract

VANDELS is an ESO Public Spectroscopic Survey designed to build a sample of high-signal-to-noise ratio, medium-resolution spectra of galaxies at redshifts between 1 and 6.5. Here we present the final Public Data Release of the VANDELS Survey, comprising 2087 redshift measurements. We provide a detailed description of sample selection, observations, and data reduction procedures. The final catalogue reaches a target selection completeness of 40% at i(AB)=25. The high signal-to-noise ratio of the spectra (above 7 in 80% of the spectra) and the dispersion of 2.5 angstrom allowed us to measure redshifts with high precision, the redshift measurement success rate reaching almost 100%. Together with the redshift catalogue and the reduced spectra, we also provide optical mid-infrared photometry and physical parameters derived through fitting the spectral energy distribution. The observed galaxy sample comprises both passive and star forming galaxies covering a stellar mass range of 8.3

Published
2021

112. New Observations with Gemini and GTC of the VHE Blazar KUV 00311–1938: About Its Redshift and Environment

Author

Pichel, A., primary, Donzelli, C., additional, Rosa-Gonzalez, D., additional, Alonso, M. Fernandez, additional, Rovero, A. C., additional, Muriel, H., additional, Mayya, Y. D., additional, Aretxaga, I., additional, González, J. Becerra, additional, Carramiñana, A., additional, Mendez-Abreu, J., additional, Vega, O., additional, Terlevich, E., additional, and Terlevich, R. J., additional

Published
2020
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114. The VANDELS ESO public spectroscopic survey

Author

McLure, R.J., Pentericci, L., Cimatti, A., Dunlop, J.S., Elbaz, D., Fontana, A., Nandra, K., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A.C., Castellano, M., Cirasuolo, M., Cucciati, O., Cullen, F., De Barros, S., Finkelstein, S.L., Fontanot, F., Franzetti, P., Fumana, M., Gargiulo, A., Garilli, B., Guaita, L., Hartley, W.G., Iovino, A., Jarvis, M.J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, Omar, Balestra, I., Bardelli, S., Bell, E.F., Bourne, N., Bowler, R.A.A., Brusa, M., Buitrago, F., Caputi, K.I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G.G., Ferguson, H.C., Fiore, F., Franco, M., Fynbo, J P U, Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N.P., Jung, I., Kim, S., Koekemoer, A.M., Khusanova, Y., Lotz, J.M., Mannucci, F., Maltby, David T., Matsuoka, K., McLeod, D.J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D.P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D.P., Tasca, L.A.M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C.C., Zamorani, G., and Zucca, E.

Subjects
surveys, galaxies: high-redshift, galaxies: star formation, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract

VANDELS is a uniquely deep spectroscopic survey of high-redshift galaxies with the VIMOS spectrograph on ESO’s Very Large Telescope (VLT). The survey has obtained ultradeep optical (0.48 < λ < 1.0 μm) spectroscopy of ≃2100 galaxies within the redshift interval 1.0 ≤ z ≤ 7.0, over a total area of ≃0.2 deg2 centred on the CANDELS Ultra Deep Survey and Chandra Deep Field South fields. Based on accurate photometric redshift pre-selection, 85 per cent of the galaxies targeted by VANDELS were selected to be at z ≥ 3. Exploiting the red sensitivity of the refurbished VIMOS spectrograph, the fundamental aim of the survey is to provide the high-signal-to-noise ratio spectra necessary to measure key physical properties such as stellar population ages, masses, metallicities, and outflow velocities from detailed absorption-line studies. Using integration times calculated to produce an approximately constant signal-to-noise ratio (20 < tint< 80 h), the VANDELS survey targeted: (a) bright star-forming galaxies at 2.4 ≤ z ≤ 5.5, (b) massive quiescent galaxies at 1.0 ≤ z ≤ 2.5, (c) fainter star-forming galaxies at 3.0 ≤ z ≤ 7.0, and (d) X-ray/Spitzer-selected active galactic nuclei and Herschel-detected galaxies. By targeting two extragalactic survey fields with superb multiwavelength imaging data, VANDELS will produce a unique legacy data set for exploring the physics underpinning high-redshift galaxy evolution. In this paper, we provide an overview of the VANDELS survey designed to support the science exploitation of the first ESO public data release, focusing on the scientific motivation, survey design, and target selection.

Published
2018

115. The VANDELS ESO spectroscopic survey

Author

McLure, R. J., Pentericci, L., Cimatti, A., Dunlop, J. S., Elbaz, D., Fontana, A., Nandra, K., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A. C., Castellano, M., Cirasuolo, M., Cucciati, O., Cullen, F., De Barros, S., Finkelstein, S. L., Fontanot, F., Franzetti, P., Fumana, M., Gargiulo, A., Garilli, B., Guaita, L., Hartley, W. G., Iovino, A., Jarvis, M. J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Mármol-Queraltó, E., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, O., Balestra, I., Bardelli, S., Bell, E. F., Bourne, N., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, K. I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G. G., Ferguson, H. C., Fiore, F., Franco, M., Fynbo, J. P. U., Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N. P., Jung, I., Kim, S., Koekemoer, A. M., Khusanova, Y., Le Fèvre, O., Lotz, J. M., Mannucci, F., Maltby, D. T., Matsuoka, K., McLeod, D. J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D. P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D. P., Tasca, L. A. M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C. C., Zamorani, G., Zucca, E., and University of St Andrews. School of Physics and Astronomy

Subjects
high-redshift [Galaxies], QC Physics, NDAS, Astrophysics::Solar and Stellar Astrophysics, QB Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, evolution [Galaxies], star formation [Galaxies], Astrophysics::Galaxy Astrophysics, QC, QB
Abstract

VANDELS is a uniquely-deep spectroscopic survey of high-redshift galaxies with the VIMOS spectrograph on ESO’s Very Large Telescope (VLT). The survey has obtained ultra-deep optical (0.48 < λ < 1.0 μm) spectroscopy of ≃2100 galaxies within the redshift interval 1.0 ≤ z ≤ 7.0, over a total area of ≃ 0.2 deg2 centred on the CANDELS UDS and CDFS fields. Based on accurate photometric redshift pre-selection, 85% of the galaxies targeted by VANDELS were selected to be at z ≥ 3. Exploiting the red sensitivity of the refurbished VIMOS spectrograph, the fundamental aim of the survey is to provide the high signal-to-noise ratio spectra necessary to measure key physical properties such as stellar population ages, masses, metallicities and outflow velocities from detailed absorption-line studies. Using integration times calculated to produce an approximately constant signal-to-noise ratio (20 < tint < 80 hours), the VANDELS survey targeted: a) bright star-forming galaxies at 2.4 ≤ z ≤ 5.5, b) massive quiescent galaxies at 1.0 ≤ z ≤ 2.5, c) fainter star-forming galaxies at 3.0 ≤ z ≤ 7.0 and d) X-ray/Spitzer-selected active galactic nuclei and Herschel-detected galaxies. By targeting two extragalactic survey fields with superb multi-wavelength imaging data, VANDELS will produce a unique legacy data set for exploring the physics underpinning high-redshift galaxy evolution. In this paper we provide an overview of the VANDELS survey designed to support the science exploitation of the first ESO public data release, focusing on the scientific motivation, survey design and target selection. Postprint

Published
2018

116. 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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118. The VANDELS ESO public spectroscopic survey: Observations and first data release

Author

Pentericci, L., primary, McLure, R. J., additional, Garilli, B., additional, Cucciati, O., additional, Franzetti, P., additional, Iovino, A., additional, Amorin, R., additional, Bolzonella, M., additional, Bongiorno, A., additional, Carnall, A. C., additional, Castellano, M., additional, Cimatti, A., additional, Cirasuolo, M., additional, Cullen, F., additional, De Barros, S., additional, Dunlop, J. S., additional, Elbaz, D., additional, Finkelstein, S. L., additional, Fontana, A., additional, Fontanot, F., additional, Fumana, M., additional, Gargiulo, A., additional, Guaita, L., additional, Hartley, W. G., additional, Jarvis, M. J., additional, Juneau, S., additional, Karman, W., additional, Maccagni, D., additional, Marchi, F., additional, Marmol-Queralto, E., additional, Nandra, K., additional, Pompei, E., additional, Pozzetti, L., additional, Scodeggio, M., additional, Sommariva, V., additional, Talia, M., additional, Almaini, O., additional, Balestra, I., additional, Bardelli, S., additional, Bell, E. F., additional, Bourne, N., additional, Bowler, R. A. A., additional, Brusa, M., additional, Buitrago, F., additional, Caputi, K. I., additional, Cassata, P., additional, Charlot, S., additional, Citro, A., additional, Cresci, G., additional, Cristiani, S., additional, Curtis-Lake, E., additional, Dickinson, M., additional, Fazio, G. G., additional, Ferguson, H. C., additional, Fiore, F., additional, Franco, M., additional, Fynbo, J. P. U., additional, Galametz, A., additional, Georgakakis, A., additional, Giavalisco, M., additional, Grazian, A., additional, Hathi, N. P., additional, Jung, I., additional, Kim, S., additional, Koekemoer, A. M., additional, Khusanova, Y., additional, Le Fèvre, O., additional, Lotz, J. M., additional, Mannucci, F., additional, Maltby, D. T., additional, Matsuoka, K., additional, McLeod, D. J., additional, Mendez-Hernandez, H., additional, Mendez-Abreu, J., additional, Mignoli, M., additional, Moresco, M., additional, Mortlock, A., additional, Nonino, M., additional, Pannella, M., additional, Papovich, C., additional, Popesso, P., additional, Rosario, D. P., additional, Salvato, M., additional, Santini, P., additional, Schaerer, D., additional, Schreiber, C., additional, Stark, D. P., additional, Tasca, L. A. M., additional, Thomas, R., additional, Treu, T., additional, Vanzella, E., additional, Wild, V., additional, Williams, C. C., additional, Zamorani, G., additional, and Zucca, E., additional

Published
2018
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119. The VANDELS ESO public spectroscopic survey:Observations and first data release

Author

Pentericci, L., McLure, R. J., Garilli, B., Cucciati, O., Franzetti, P., Iovino, A., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A. C., Castellano, M., Cimatti, A., Cirasuolo, M., Cullen, F., De Barros, S., Dunlop, J. S., Elbaz, D., Finkelstein, S. L., Fontana, A., Fontanot, F., Fumana, M., Gargiulo, A., Guaita, L., Hartley, W. G., Jarvis, M. J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Marmol-Queralto, E., Nandra, K., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, O., Balestra, I., Bardelli, S., Bell, E. F., Bourne, N., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, K. I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G. G., Ferguson, H. C., Fiore, F., Franco, M., Fynbo, J. P. U., Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N. P., Jung, I., Kim, S., Koekemoer, A. M., Khusanova, Y., Le Fevre, O., Lotz, J. M., Mannucci, F., Maltby, D. T., Matsuoka, K., McLeod, D. J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D. P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D. P., Tasca, L. A. M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C. C., Zamorani, G., Zucca, E., Pentericci, L., McLure, R. J., Garilli, B., Cucciati, O., Franzetti, P., Iovino, A., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A. C., Castellano, M., Cimatti, A., Cirasuolo, M., Cullen, F., De Barros, S., Dunlop, J. S., Elbaz, D., Finkelstein, S. L., Fontana, A., Fontanot, F., Fumana, M., Gargiulo, A., Guaita, L., Hartley, W. G., Jarvis, M. J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Marmol-Queralto, E., Nandra, K., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, O., Balestra, I., Bardelli, S., Bell, E. F., Bourne, N., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, K. I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G. G., Ferguson, H. C., Fiore, F., Franco, M., Fynbo, J. P. U., Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N. P., Jung, I., Kim, S., Koekemoer, A. M., Khusanova, Y., Le Fevre, O., Lotz, J. M., Mannucci, F., Maltby, D. T., Matsuoka, K., McLeod, D. J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D. P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D. P., Tasca, L. A. M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C. C., Zamorani, G., and Zucca, E.

Published
2018

120. 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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121. The origins of post-starburst galaxies at z < 0.05

Author

Pawlik, M M, primary, Taj Aldeen, L, additional, Wild, V, additional, Mendez-Abreu, J, additional, Lahén, N, additional, Johansson, P H, additional, Jimenez, N, additional, Lucas, W, additional, Zheng, Y, additional, Walcher, C J, additional, and Rowlands, K, additional

Published
2018
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122. 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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123. Imprints of galaxy evolution on H II regions memory of the past uncovered by the CALIFA survey

Author

Sanchez, S. F., Perez, E., Rosales-Ortega, F. F., Miralles-Caballero, D., Lopez-Sanchez, A. R., Iglesias-P��ramo, J., Marino, R. A., S��nchez-Menguiano, L., Garc��a-Benito, R., Mast, D., Mendoza, M. A., Papaderos, P., Ellis, S., Galbany, L., Kehrig, C., Monreal-Ibero, A., Delgado, R. Gonz��lez, Moll��, M., Ziegler, B., de Lorenzo-C��ceres, A., Mendez-Abreu, J., Bland-Hawthorn, J., Bekeraite, S., Roth, M. M., Pasquali, A., D��az, A., Bomans, D., van de Ven, G., Wisotzki, L., collaboration, The CALIFA, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and UAM. Departamento de Física Teórica

Subjects
evolution galaxies: ISM [Galaxies], Astrofísica, Stellar population, Stellar mass, Galaxies: abundances, FOS: Physical sciences, abundances [Galaxies], Photoionization, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, star formation [Galaxies], ISM [Galaxies], Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, QB Astronomy, Stellar evolution, Astrophysics::Galaxy Astrophysics, QC, Line (formation), QB, Physics, Galaxies: star formation, Star formation, Física atmosférica, Física, Astronomy and Astrophysics, 3rd-DAS, Galaxies: evolution galaxies: ISM, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Astronomía, QC Physics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA)
Abstract

Astronomy and Astrophysics 574 (2015): A47 reproduced with permission from Astronomy & Astrophysics, © ESO, Context. H II regions in galaxies are the sites of star formation, so they are special places for understanding the build-up of stellar mass in the universe. The line ratios of this ionized gas are frequently used to characterize the ionization conditions. In particular, the oxygen abundances are assumed to trace the chemical enrichment of galaxies. Aims. We explore the connections between the ionization conditions and the properties of the overall underlying stellar population (ionizing or not-ionizing) in H II regions, in order to uncover the actual physical connection between them. Methods. We use the H II regions catalog from the CALIFA survey, which is the largest in existence with more than 5000 H II regions, to explore their distribution across the classical [O III] λ5007/Hβ vs. [N II] λ6583/α diagnostic diagram, and the way it depends on the oxygen abundance, ionization parameter, electron density, and dust attenuation. The location of H II regions within this diagram is compared with predictions from photoionization models. Finally, we explore the dependence of the location within the diagnostic diagram on the properties of the host galaxies, the galactocentric distances, and the properties of the underlying stellar population. Results. The H II regions with weaker ionization strengths and more metal-rich are located in the bottom righthand area of the diagram. In contrast, those regions with stronger ionization strengths and more metal poor are located in the upper lefthand end of the diagram. Photoionization models per se do not predict these correlations between the parameters and the line ratios. The H II regions located in earlier-type galaxies, closer to the center and formed in older and more metal-rich regions of the galaxies are located in the bottom-right area of the diagram. On the other hand, those regions located in late-type galaxies in the outer regions of the disks and formed on younger and more metal-poor regions lie in the top lefthand area of the diagram. The two explored line ratios show strong correlations with the age and metallicity of the underlying stellar population. Conclusions. These results indicate that although H II regions are short-lived events, they are aff ected by the total underlying stellar population. One may say that H II regions keep a memory of the stellar evolution and chemical enrichment that have left an imprint on both the ionizing stellar population and the ionized gas, We thank the Viabilidad, Diseño, Acceso y Mejora funding program, ICTS-2009-10, for supporting the initial developement of this project. S.F.S. thanks the ConaCyt funding program 180125, for the support given to this project. S.F.S., M.A.M. and L.S.M. thank the Plan Nacional de Investigación y Desarrollo funding programs, AYA2012-31935, of the Spanish Ministerio de Economía y Competitividad, for the support given to this project. S.F.S. thanks the Ramón y Cajal project RyC-2011-07590 of the Spanish Ministerio de Economía y Competitividad, for its support of this project. P.P. is supported by a FCT Investigator 2013 consolidation grant. He acknowledges support by the Fundação para a Ciência e a Tecnologia (FCT) under project FCOMP-01-0124-FEDER-029170 (Reference FCT PTDC/FIS-AST/3214/2012), funded by FCT-MEC (PIDDAC) and FEDER (COMPETE). R.G.D., E.P., and R.G.B. thank the Plan Nacional de Investigación y Desarrollo funding program AYA2010-15081. Support for LG is provided by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC12009, awarded to The Millennium Institute of Astrophysics, MAS. L.G. acknowledges support by CONICYT through FONDECYT grant 3140566. R.A. Marino was also funded by the Spanish program of International Campus of Excellence Moncloa (CEI). A. M.-I. acknowledges support from Agence Nationale de la Recherche through the STILISM project (ANR-12-BS05-0016-02)

Published
2015

124. 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
Full Text
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125. A characteristic oxygen abundance gradient in galaxy disks unveiled with CALIFA

Author

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

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

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

Published
2014

126. Dark matter content of ETGs and its relation to the local density of galaxies.

Author

Nigoche-Netro, A., Ramos-Larios, G., Díaz, R., de la Fuente, E., Lagos, P., Ruelas-Mayorga, A., Mendez-Abreu, J., Kemp, S. N., Bergmann, Thaisa Storchi, Forman, William, Overzier, Roderik, and Riffel, Rogério

Abstract

We study the behaviour of the dynamical and stellar mass inside the effective radius as function of local density for early-type galaxies (ETGs). We use several samples of ETGs - ranging from 19000 to 98000 objects - from the ninth data release of the Sloan Digital Sky Survey. We consider Newtonian dynamics, different light profiles and different initial mass functions (IMF) to calculate the dynamical and stellar mass. We assume that any difference between these two masses is due to dark matter and/or a non-universal IMF. The main results are: (i) the amount of dark matter (DM) inside ETGs depends on the environment; (ii) ETGs in low-density environments span a wider DM range than ETGs in dense environments; (iii) the amount of DM inside ETGs in the most dense environments will be less than approximately 55-65 per cent of the dynamical mass; (iv) the accurate value of this upper limit depends on the impact of the IMF on the stellar mass estimation. [ABSTRACT FROM AUTHOR]

Published
2019
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127. Mass-metallicity relation explored with CALIFA I. Is there a dependence on the star-formation rate?

Author

Sanchez, S. F., Rosales-Ortega, F. F., Jungwiert, B., Iglesias-Paramo1, J., Vilchez, J. M., Marino, R. A., Walcher, C. J., Husemann, B., Mast, D., Monreal-Ibero, A., Fernandes, R. Cid, Perez, E., Delgado, R. Gonzalez, Garcia-Benito, R., Galbany, L., van de Ven, G., Jahnke, K., Flores, H., Bland-Hawthorn, J., Lopez-Sánchez, A. R., Stanishev, V., Miralles-Caballero, D., Diaz, A. I., Sanchez-Blazquez, P., Molla, M., Gallazzi1, A., Papaderos, P., Gomes, J. M., Gruel, N., Pérez, I., Ruiz-Lara, T., Florido, E., de Lorenzo-Cáceres, A., Mendez-Abreu, J., Kehrig, C., Roth, M. M., Ziegler, B., Alves, J., Wisotzki, L., Kupko, D., Quirrenbach, A., Bomans, D., and collaboration, The CALIFA

Subjects
Astrofísica, Galaxies: fundamental parameters, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Metallicity, structure [Galaxies], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, evolution [Galaxy], Galaxies: structure, 0103 physical sciences, ISM [Galaxies], Astrophysics::Solar and Stellar Astrophysics, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, spiral [Galaxies], 010308 nuclear & particles physics, Star formation, 1. No poverty, Astrophysics::Instrumentation and Methods for Astrophysics, fundamental parameters [Galaxy], Galaxies: evolution, Sigma, Física, abundances [Galaxy], Astronomy and Astrophysics, evolution [Galaxies], Galaxy, Accretion (astrophysics), Astronomía, Galaxies: ISM, Cover (topology), Space and Planetary Science, fundamental parameters [Galaxies], Galaxy: abundances, Galaxies: spiral, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We studied the global and local M-Z relation based on the first data available from the CALIFA survey (150 galaxies). This survey provides integral field spectroscopy of the complete optical extent of each galaxy (up to 2−3 effective radii), with a resolution high enough to separate individual Hii regions and/or aggregations. About 3000 individual Hii regions have been detected. The spectra cover the wavelength range between [OII]3727 and [SII]6731, with a sufficient signal-to-noise ratio to derive the oxygen abundance and star-formation rate associated with each region. In addition, we computed the integrated and spatially resolved stellar masses (and surface densities) based on SDSS photometric data. We explore the relations between the stellar mass, oxygen abundance and star-formation rate using this dataset. We derive a tight relation between the integrated stellar mass and the gas-phase abundance, with a dispersion lower than the one already reported in the literature (σΔlog (O/H) = 0.07 dex). Indeed, this dispersion is only slightly higher than the typical error derived for our oxygen abundances. However, we found no secondary relation with the star-formation rate other than the one induced by the primary relation of this quantity with the stellar mass. The analysis for our sample of ∼3000 individual Hii regions confirms (i) a local mass-metallicity relation and (ii) the lack of a secondary relation with the star-formation rate. The same analysis was performed with similar results for the specific star-formation rate. Our results agree with the scenario in which gas recycling in galaxies, both locally and globally, is much faster than other typical timescales, such like that of gas accretion by inflow and/or metal loss due to outflows. In essence, late-type/disk-dominated galaxies seem to be in a quasi-steady situation, with a behavior similar to the one expected from an instantaneous recycling/closed-box model., Nacional de Investigación y Desarrollo funding programs of the Spanish Ministerio de Ciencia e Innovación AYA2010-22111-C03-03 AYA2010-10904E, Ramon y Cajal project of the spanish Ministerio de Economía y Competitividad RyC-2011-07590, Academy of Sciences of the Czech Republic (ASCR Internal support program of international cooperation projects-PIPPMS) M100031241 M100031201, Czech Republic program for the long-term development of the research institution RVO67985815, Plan Nacional de Investigación y Desarrollo funding program AYA2010-15081, Consejo Nacional de Ciencia y Tecnología (CONACyT), Spanish grant AYA2010-15169, Junta de Andalucía TIC114, Excellence Project P08-TIC-03531, Consejo Superior de Investigaciones Científicas (CSIC), Junta para la Ampliación de Estudios, European Social Fund (ESF), spanish programme of International Campus of Excellence Moncloa, Spanish PNAYA AYA2010-21887, Spanish Government CSD2006-00070 AYA2012-38491-C02-02, Autonomic Government of Andalusia P08-TIC-4075 TIC-126, Ciencia, Portuguese Foundation for Science and Technology, European Commission European Commission Joint Research Centre European Social Fund (ESF), Portuguese Foundation for Science and Technology SFRH/BPD/66958/2009, National Science Foundation (NSF)

Published
2013

128. The origins of post-starburst galaxies at <italic>z</italic> < 0.05.

Author

Pawlik, M M, Wild, V, Lucas, W, Zheng, Y, Taj Aldeen, L, Mendez-Abreu, J, Jimenez, N, Rowlands, K, Lahén, N, Johansson, P H, and Walcher, C J

Subjects
STARBURSTS, BALMER line, GALAXY formation, STELLAR evolution, GALAXY mergers, ACTIVE galactic nuclei
Abstract

Post-starburst galaxies can be identified via the presence of prominent Hydrogen Balmer absorption lines in their spectra. We present a comprehensive study of the origin of strong Balmer lines in a volume-limited sample of 189 galaxies with 0.01 < z < 0.05, $\log ({\it M}_{\star }/{\it M}_{{\odot }})>9.5$ and projected axial ratio b/a > 0.32. We explore their structural properties, environments, emission lines, and star formation histories, and compare them to control samples of star-forming and quiescent galaxies, and simulated galaxy mergers. Excluding contaminants, in which the strong Balmer lines are most likely caused by dust-star geometry, we find evidence for three different pathways through the post-starburst phase, with most events occurring in intermediate-density environments: (1) a significant disruptive event, such as a gas-rich major merger, causing a starburst and growth of a spheroidal component, followed by quenching of the star formation (70 per cent of post-starburst galaxies at $9.5<\log (\mbox{{$M$}}_{\star }/\mbox{{$M$}}_{{\odot }})<10.5$ and 60 per cent at $\log (\mbox{{$M$}}_{\star }/\mbox{{$M$}}_{{\odot }})>10.5$ ); (2) at $9.5<\log (\mbox{{$M$}}_{\star }/\mbox{{$M$}}_{{\odot }})<10.5$ , stochastic star formation in blue-sequence galaxies, causing a weak burst and subsequent return to the blue sequence (30 per cent); (3) at $\log (\mbox{{$M$}}_{\star }/\mbox{{$M$}}_{{\odot }})>10.5$ , cyclic evolution of quiescent galaxies which gradually move towards the high-mass end of the red sequence through weak starbursts, possibly as a result of a merger with a smaller gas-rich companion (40 per cent). Our analysis suggests that active galactic nuclei (AGNs) are 'on' for $50\hbox{ per cent}$ of the duration of the post-starburst phase, meaning that traditional samples of post-starburst galaxies with strict emission-line cuts will be at least $50\hbox{ per cent}$ incomplete due to the exclusion of narrow-line AGNs. [ABSTRACT FROM AUTHOR]

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

Author

Husemann, B., Jahnke, K., Sanchez, Sébastien, Barrado, D., Bekerait*error*ė, S., Bomans, D., Castillo-Morales, A., Catalán-Torrecilla, C., Cid Fernandes, R., Falcón-Barroso, J., García-Benito, R., González Delgado, R., Iglesias-Paramo, J., Johnson, B., Kupko, D., Lopez-Fernandez, R., Lyubenova, M., Marino, R., Mast, D., Miskolczi, A., Monreal-Ibero, A., Gil de Paz, A., Perez, Emile, Pérez, I., Rosales-Ortega, F., Ruiz-Lara, T., Schilling, U., van de Ven, G., Walcher, J., Alves, J., de Amorim, A., Backsmann, N., Barrera-Ballesteros, J., Bland-Hawthorn, J., Cortijo, C., Dettmar, R.-J., Demleitner, M., Díaz, A., Enke, H., Florido, E., Flores, H., Galbany, L., Gallazzi, A., García-Lorenzo, B., Gomes, J., Gruel, N., Haines, T., Holmes, L., Jungwiert, B., Kalinova, V., Kehrig, C., Kennicutt, R., Klar, J., Lehnert, M., López-Sánchez, Á., de Lorenzo-Cáceres, A., Mármol-Queraltó, E., Márquez, I., Mendez-Abreu, J., Mollá, M., del Olmo, A., Meidt, S., Papaderos, P., Puschnig, J., Quirrenbach, A., Roth, M., Sánchez-Blázquez, P., Spekkens, K., Singh, R., Stanishev, V., Trager, S., Vilchez, J., Wild, V., Wisotzki, L., Zibetti, S., Ziegler, B., Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Ruhr-Universität Bochum [Bochum], 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), 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), 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), Instituto Dom Luiz, Universidade de Lisboa = University of Lisbon (ULISBOA), The University of Sydney, CRLCC Val d'Aurelle - Paul Lamarque, Astronomisches Institut der Ruhr-Universität Bochum, Universität Heidelberg [Heidelberg] = Heidelberg University, Department of Physics [Pittsburgh], Carnegie Mellon University [Pittsburgh] (CMU), Landessternwarte Königstuhl [ZAH] (LSW), Kiepenheuer-Institut für Sonnenphysik (KIS), 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), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Université Sciences et Technologies - Bordeaux 1-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), 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), 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), Universidade de Lisboa (ULISBOA), Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, Heidelberg, Germany, Universität Heidelberg [Heidelberg], and Universidad Autonoma de Madrid (UAM)

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

International audience

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

Author

Sanchez, Sébastien, Kennicutt, R., Gil De Paz, A., van de Ven, G., Vílchez, J., Wisotzki, L., Walcher, C., Mast, D., Aguerri, J., Albiol-Pérez, S., Alonso-Herrero, A., Alves, J., Bakos, J., Bartáková, T., Bland-Hawthorn, J., Boselli, A., Bomans, D., Castillo-Morales, A., Cortijo-Ferrero, C., de Lorenzo-Cáceres, A., Del Olmo, A., Dettmar, R.-J., Díaz, A., Ellis, S., Falcón-Barroso, J., Flores, H., Gallazzi, A., García-Lorenzo, B., González Delgado, R., Gruel, N., Haines, T., Hao, C., Husemann, B., Iglesias-Páramo, J., Jahnke, K., Johnson, B., Jungwiert, B., Kalinova, V., Kehrig, C., Kupko, D., López-Sánchez, Á., Lyubenova, M., Marino, R., Mármol-Queraltó, E., Márquez, I., Masegosa, J., Meidt, S., Mendez-Abreu, J., Monreal-Ibero, A., Montijo, C., Mourao, A., Palacios-Navarro, G., Papaderos, P., Pasquali, A., Peletier, R., Perez, Emile, Pérez, I., Quirrenbach, A., Relaño, M., Rosales-Ortega, F., Roth, M., Ruiz-Lara, T., Sánchez-Blázquez, P., Sengupta, C., Singh, R., Stanishev, V., Trager, S., Vazdekis, A., Viironen, K., Wild, V., Zibetti, S., Ziegler, B., 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 Organic Chemistry, University of Pannonia, The University of Sydney, 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), Ruhr-Universität Bochum [Bochum], Astronomisches Institut der Ruhr-Universität Bochum, 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), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, NOAA Earth System Research Laboratory (ESRL), National Oceanic and Atmospheric Administration (NOAA), 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), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), inconnu, Inconnu, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Dpto. Fisica Teorica y del Cosmos, Universidad de Granada = University of Granada (UGR), Institut de biologie et chimie des protéines [Lyon] (IBCP), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autónoma de Madrid (UAM), Imperial College London, Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Centre National de la Recherche Scientifique (CNRS)-Institut Polytechnique de Bordeaux-Université Sciences et Technologies - Bordeaux 1, Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL), Universidad de Granada (UGR), and Universidad Autonoma de Madrid (UAM)

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

International audience

Published
2012
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131. CALIFA, the Calar Alto Legacy Integral Field Area survey III. Second public data release

Author

Garcia-Benito, R., Zibetti, S., Sanchez, S. F., Husemann, B., de Amorim, A. L., Castillo-Morales, A., Cid Fernandes, R., Ellis, S. C., Falcon-Barroso, J., Galbany, L., Gil de Paz, A., Gonzalez Delgado, R. M., Lacerda, E. A. D., Lopez-Fernandez, R., de Lorenzo-Caceres, A., Lyubenova, M., Marino, R. A., Mast, D., Mendoza, M. A., Perez, E., Vale Asari, N., Aguerri, J. A. L., Ascasibar, Y., Bekeraite, S., Bland-Hawthorn, J., Barrera-Ballesteros, J. K., Bomans, D. J., Cano-Diaz, M., Catalan-Torrecilla, C., Cortijo, C., Delgado-Inglada, G., Demleitner, M., Dettmar, R. -J., Diaz, A. I., Florido, E., Gallazzi, A., Garcia-Lorenzo, B., Gomes, J. M., Holmes, L., Iglesias-Paramo, J., Jahnke, K., Kalinova, V., Kehrig, C., Kennicutt, R. C. Jr., Lopez-Sanchez, A. R., Marquez, I., Masegosa, J., Meidt, S. E., Mendez-Abreu, J., Molla, M., Monreal-Ibero, A., Morisset, C., del Olmo, A., Papaderos, P., Perez, I., Quirrenbach, A., Rosales-Ortega, F. F., Roth, M. M., Ruiz-Lara, T., Sanchez-Blazquez, P., Sanchez-Menguiano, L., Singh, R., Spekkens, K., Stanishev, Vallery, Torres-Papaqui, J. P., van de Ven, G., Vilchez, J. M., Walcher, C. J., Wild, V., Wisotzki, L., Ziegler, B., Alves, J., Barrado, D., Quintana, J. M., Aceituno, J., Garcia-Benito, R., Zibetti, S., Sanchez, S. F., Husemann, B., de Amorim, A. L., Castillo-Morales, A., Cid Fernandes, R., Ellis, S. C., Falcon-Barroso, J., Galbany, L., Gil de Paz, A., Gonzalez Delgado, R. M., Lacerda, E. A. D., Lopez-Fernandez, R., de Lorenzo-Caceres, A., Lyubenova, M., Marino, R. A., Mast, D., Mendoza, M. A., Perez, E., Vale Asari, N., Aguerri, J. A. L., Ascasibar, Y., Bekeraite, S., Bland-Hawthorn, J., Barrera-Ballesteros, J. K., Bomans, D. J., Cano-Diaz, M., Catalan-Torrecilla, C., Cortijo, C., Delgado-Inglada, G., Demleitner, M., Dettmar, R. -J., Diaz, A. I., Florido, E., Gallazzi, A., Garcia-Lorenzo, B., Gomes, J. M., Holmes, L., Iglesias-Paramo, J., Jahnke, K., Kalinova, V., Kehrig, C., Kennicutt, R. C. Jr., Lopez-Sanchez, A. R., Marquez, I., Masegosa, J., Meidt, S. E., Mendez-Abreu, J., Molla, M., Monreal-Ibero, A., Morisset, C., del Olmo, A., Papaderos, P., Perez, I., Quirrenbach, A., Rosales-Ortega, F. F., Roth, M. M., Ruiz-Lara, T., Sanchez-Blazquez, P., Sanchez-Menguiano, L., Singh, R., Spekkens, K., Stanishev, Vallery, Torres-Papaqui, J. P., van de Ven, G., Vilchez, J. M., Walcher, C. J., Wild, V., Wisotzki, L., Ziegler, B., Alves, J., Barrado, D., Quintana, J. M., and Aceituno, J.

Abstract

This paper describes the Second Public Data Release (DR2) of the Calar Alto Legacy Integral Field Area (CALIFA) survey. The data for 200 objects are made public, including the 100 galaxies of the First Public Data Release (DR1). Data were obtained with the integral-field spectrograph PMAS /PPak mounted on the 3.5 m telescope at the Calar Alto observatory. Two different spectral setups are available for each galaxy, (i) a low-resolution V500 setup covering the wavelength range 3745-7500 angstrom with a spectral resolution of 6.0 angstrom (FWHM); and (ii) a medium-resolution V1200 setup covering the wavelength range 3650-4840 angstrom with a spectral resolution of 2.3 angstrom (FWHM). The sample covers a redshift range between 0.005 and 0.03, with a wide range of properties in the color-magnitude diagram, stellar mass, ionization conditions, and morphological types. All the cubes in the data release were reduced with the latest pipeline, which includes improved spectrophotometric calibration, spatial registration, and spatial resolution. The spectrophotometric calibration is better than 6% and the median spatial resolution is 2 4. In total, the second data release contains over 1.5 million spectra., Funding Agencies|Spanish Ministerio de Ciencia e Innovacion [AYA2010-15081, AYA2010-15196]; EU Marie Curie Integration Grant "SteMaGE" [PCIG12-GA-2012-326466]; Spanish Ministry of Economy and Competitiveness (MINECO) [AYA2010-21322-C03-02, AIB-2010-DE-00227]; FP7 Marie Curie Actions of the European Commission, via the Initial Training Network DAGAL under REA [289313]; Ministry of Economy, Development, and Tourisms Millennium Science Initiative [IC12009]; CONICYT through FONDECYT [3140566]; Fundacao para a Ciencia e a Tecnologia (FCT) from FCT (Portugal) [SFRH/BPD/66958/2009]; Spanish programme of International Campus of Excellence Moncloa (CEI); European Research Council; Junta de Andalucia [TIC 114, PO08-TIC-3531]; Agence Nationale de la Recherche through the STILISM project [ANR-12-BS05-0016-02]; Ministerio de Economia y Competitividad [AYA2010-21887-C04-02]; FCT Investigador Contract - FCT/MCTES (Portugal); POPH/FSE (EC); FCT - FCT-MEC (PIDDAC) [FCOMP-01-0124-FEDER-029170, FCT PTDC/FIS-AST/3214/2012]; FEDER (COMPETE); Spanish Ministerio de Educacion, Cultura y Deporte by FPU; Ramon y Cajal program from the Spanish Ministry of Economy and Competitiveness (MINECO) [ATA2010-21322-C03-02]; Marie Curie Career Integration Grant [303912]; European Research Council Starting Grant (SEDMorph P.I. V. Wild); European Career Re-integration Grant; Ramon y Cajal programme [RyC-2011-09461, AYA2013-47742-C4-3-P]; EU [FP7-PEOPLE-2013-IRSES-612701]; [267251]; [PTDC/FIS-AST/3214/2012]

Published
2015
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133. The incidence of bar-like kinematic flows in CALIFA galaxies

Author

Holmes, L., primary, Spekkens, K., additional, Sánchez, S. F., additional, Walcher, C. J., additional, García-Benito, R., additional, Mast, D., additional, Cortijo-Ferrero, C., additional, Kalinova, V., additional, Marino, R. A., additional, Mendez-Abreu, J., additional, and Barrera-Ballesteros, J. K., additional

Published
2015
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134. CALIFA, the Calar alto legacy integral field area survey:II. First public data release

Author

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

Abstract

We present the first public data release (DR1) of the Calar Alto Legacy Integral Field Area (CALIFA) survey. It consists of science-grade optical datacubes for the first 100 of eventually 600 nearby (0.005 < z < 0.03) galaxies, obtained with the integral-field spectrograph PMAS/PPak mounted on the 3.5 m telescope at the Calar Alto observatory. The galaxies in DR1 already cover a wide range of properties in color-magnitude space, morphological type, stellar mass, and gas ionization conditions. This offers the potential to tackle a variety of open questions in galaxy evolution using spatially resolved spectroscopy. Two different spectral setups are available for each galaxy, (i) a low-resolution V500 setup covering the nominal wavelength range 3745-7500 Å with a spectral resolution of 6.0 Å (FWHM), and (ii) a medium-resolution V1200 setup covering the nominal wavelength range 3650-4840 Å with a spectral resolution of 2.3 Å (FWHM). We present the characteristics and data structure of the CALIFA datasets that should be taken into account for scientific exploitation of the data, in particular the effects of vignetting, bad pixels and spatially correlated noise. The data quality test for all 100 galaxies showed that we reach a median limiting continuum sensitivity of 1.0 × 10-18 erg s-1 cm-2 Å-1 arcsec-2 at 5635 Å and 2.2 × 10 -18 erg s-1 cm-2 Å-1 arcsec-2 at 4500 Å for the V500 and V1200 setup respectively, which corresponds to limiting r and g band surface brightnesses of 23.6 mag arcsec-2 and 23.4 mag arcsec-2, or an unresolved emission-line flux detection limit of roughly 1 × 10-17 erg s-1 cm-2 arcsec-2 and 0.6 × 10 -17 erg s-1 cm-2 arcsec-2, respectively. The median spatial resolution is 3-7, and the absolute spectrophotometric calibration is

Published
2013

135. The effects of spatial resolution on integral field spectrograph surveys at different redshifts − The CALIFA perspective

Author

Mast, D., primary, Rosales-Ortega, F. F., additional, Sánchez, S. F., additional, Vílchez, J. M., additional, Iglesias-Paramo, J., additional, Walcher, C. J., additional, Husemann, B., additional, Márquez, I., additional, Marino, R. A., additional, Kennicutt, R. C., additional, Monreal-Ibero, A., additional, Galbany, L., additional, de Lorenzo-Cáceres, A., additional, Mendez-Abreu, J., additional, Kehrig, C., additional, del Olmo, A., additional, Relaño, M., additional, Wisotzki, L., additional, Mármol-Queraltó, E., additional, Bekeraitè, S., additional, Papaderos, P., additional, Wild, V., additional, Aguerri, J. A. L., additional, Falcón-Barroso, J., additional, Bomans, D. J., additional, Ziegler, B., additional, García-Lorenzo, B., additional, Bland-Hawthorn, J., additional, López-Sánchez, Á. R., additional, and van de Ven, G., additional

Published
2014
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136. 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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138. Shape asymmetry: a morphological indicator for automatic detection of galaxies in the post-coalescence merger stages.

Author

Pawlik, M. M., Wild, V., Walcher, C. J., Johansson, P. H., Villforth, C., Rowlands, K., Mendez-Abreu, J., and Hewlett, T.

Subjects
GALACTIC evolution, STARBURSTS, ASTRONOMICAL observations, STELLAR evolution
Abstract

We present a new morphological indicator designed for automated recognition of galaxies with faint asymmetric tidal features suggestive of an ongoing or past merger. We use the new indicator, together with pre-existing diagnostics of galaxy structure to study the role of galaxy mergers in inducing (post-) starburst spectral signatures in local galaxies, and investigate whether (post-) starburst galaxies play a role in the build-up of the 'red sequence'. Our morphological and structural analysis of an evolutionary sample of 335 (post-) starburst galaxies in the Sloan Digital Sky Survey DR7 with starburst ages 0 < tSB < 0.6 Gyr, shows that 45 per cent of galaxies with young starbursts (tSB < 0.1 Gyr) show signatures of an ongoing or past merger. This fraction declines with starburst age, and we find a good agreement between automated and visual classifications. The majority of the oldest (post-) starburst galaxies in our sample (tSB ∼ 0.6 Gyr) have structural properties characteristic of early-type discs and are not as highly concentrated as the fully quenched galaxies commonly found on the 'red sequence' in the present day Universe. This suggests that, if (post-) starburst galaxies are a transition phase between active star-formation and quiescence, they do not attain the structure of presently quenched galaxies within the first 0.6 Gyr after the starburst. [ABSTRACT FROM AUTHOR]

Published
2016
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140. The effects of spatial resolution on integral field spectrograph surveys at different redshifts - The CALIFA perspective.

Author

Mast, D., Rosales-Ortega, F. F., Sánchez, S. F., Vílchez, J. M., Iglesias-Paramo, J., Walcher, C. J., Husemann, B., Márquez, I., Marino, R. A., Kennicutt, R. C., Monreal-Ibero, A., Galbany, L., Lorenzo-Cáceres, A. de, Mendez-Abreu, J., Kehrig, C., Olmo, A. del, Relaño, M., Wisotzki, L., Mármol-Queraltó, E., and Bekeraitè, S.

Subjects
REDSHIFT, ASTRONOMICAL photography, GALAXIES, IONIZATION of gases, ASTROPHYSICS
Abstract

Context. Over the past decade, 3D optical spectroscopy has become the preferred tool for understanding the properties of galaxies and is now increasingly used to carry out galaxy surveys. Low redshift surveys include SAURON, DiskMass, ATLAS3D, PINGS, and VENGA. At redshifts above 0.7, surveys such as MASSIV, SINS, GLACE, and IMAGES have targeted the most luminous galaxies to study mainly their kinematic properties. The on-going CALIFA survey (z ~ 0.02) is the first of a series of upcoming integral field spectroscopy (IFS) surveys with large samples representative of the entire population of galaxies. Others include SAMI and MaNGA at lower redshift and the upcoming KMOS surveys at higher redshift. Given the importance of spatial scales in IFS surveys, the study of the effects of spatial resolution on the recovered parameters becomes important. Aims. We explore the capability of the CALIFA survey and a hypothetical higher redshift survey to reproduce the properties of a sample of objects observed with better spatial resolution at lower redshift. Methods. Using a sample of PINGS galaxies, we simulated observations at different redshifts. We then studied the behaviour of different parameters as the spatial resolution degrades with increasing redshift. Results. We show that at the CALIFA resolution, we are able to measure and map common observables in a galaxy study: the number and distribution of Hii regions (Ha flux structure), the gas metallicity (using the O3N2 method), the gas ionization properties (through the [Nii]/Ha and [O iii]/Hß line ratios), and the age of the underlying stellar population (using the D4000 index). This supports the aim of the survey to characterise the observable properties of galaxies in the Local Universe. Our analysis of simulated IFS data cubes at higher redshifts highlights the importance of the projected spatial scale per spaxel as the most important figure of merit in the design of an integral field survey. [ABSTRACT FROM AUTHOR]

Published
2014
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141. The O3N2 and N2 abundance indicators revisited: improved calibrations based on CALIFA and Te-based literature data.

Author

Marino, R. A., Rosales-Ortega, F. F., Sánchez, S. F., Gil de Paz, A., Vílchez, J., Miralles-Caballero, D., Kehrig, C., Pérez-Montero, E., Stanishev, V., Iglesias-Páramo, J., Díaz, A. I., Castillo-Morales, A., Kennicutt, R., López-Sánchez, A. R., Galbany, L., García-Benito, R., Mast, D., Mendez-Abreu, J., Monreal-Ibero, A., and Husemann, B.

Subjects
COSMIC abundances, CALIBRATION, INTEGRAL field spectroscopy, GALACTIC evolution, EMISSION-line galaxies, FLUX (Energy), GAS phase reactions, REDSHIFT
Abstract

The use of integral field spectroscopy is since recently allowing to measure the emission line fluxes of an increasingly large number of star-forming galaxies, both locally and at high redshift. Many studies have used these fluxes to derive the gas-phase metallicity of the galaxies by applying the so-called strong-line methods. However, the metallicity indicators that these datasets use were empirically calibrated using few direct abundance data points (Te-based measurements). Furthermore, a precise determination of the prediction intervals of these indicators is commonly lacking in these calibrations. Such limitations might lead to systematic errors in determining the gas-phase metallicity, especially at high redshift, which might have a strong impact on our understanding of the chemical evolution of the Universe. The main goal of this study is to review the most widely used empirical oxygen calibrations, O3N2 and N2, by using new direct abundance measurements. We pay special attention to (1) the expected uncertainty of these calibrations as a function of the index value or abundance derived and (2) the presence of possible systematic offsets. This is possible thanks to the analysis of the most ambitious compilation of Te-based Hii regions to date. This new dataset compiles the Te-based abundances of 603 Hii regions extracted from the literature but also includes new measurements from the CALIFA survey. Besides providing new and improved empirical calibrations for the gas abundance, we also present a comparison between our revisited calibrations with a total of 3423 additional CALIFA Hii complexes with abundances derived using the ONS calibration from the literature. The combined analysis of Te-based and ONS abundances allows us to derive their most accurate calibration to date for both the O3N2 and N2 singleratio indicators, in terms of all statistical significance, quality, and coverage of the parameters space. In particular, we infer that these indicators show shallower abundance dependencies and statistically significant offsets compared to others'. The O3N2 and N2 indicators can be empirically applied to derive oxygen abundances calibrations from either direct abundance determinations with random errors of 0.18 and 0.16, respectively, or from indirect ones (but based on a large amount of data), reaching an average precision of 0.08 and 0.09 dex (random) and 0.02 and 0.08 dex (systematic; compared to the direct estimations), respectively. [ABSTRACT FROM AUTHOR]

Published
2013
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142. Withdrawn as Duplicate: IMF shape constraints from stellar populations and dynamics from CALIFA.

Author

Lyubenova, M, Martín-Navarro, I, Ven, G van de, Falcón-Barroso, J, Galbany, L, Gallazzi, A, García-Benito, R, Delgado, R González, Husemann, B, Barbera, F La, 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, and Walcher, C J

Subjects
STELLAR dynamics, STELLAR populations, POPULATION dynamics, STELLAR initial mass function, HILBERT-Huang transform, GEOMETRIC shapes
Published
2019
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144. VizieR Online Data Catalog: CALIFA face-on spiral galaxies oxygen (Sanchez-Menguiano+, 2016)

Author

Sanchez-Menguiano, L., Sanchez, S. F., Perez, I., Garcia-Benito, R., Husemann, B., Mast, D., Mendoza, A., Ruiz-Lara, T., Ascasibar, Y., Bland-Hawthorn, J., Cavichia, O., Diaz, A. I., Florido, E., Lluís Galbany, Gonzalez Delgado, R. M., Kehrig, C., Marino, R. A., Marquez, I., Masegosa, J., Mendez-Abreu, J., Molla, M., Del Olmo, A., Perez, E., Sanchez-Blazquez, P., Stanishev, V., Walcher, C. J., Lopez-Sanchez, A. R., and (The Califa Collaboration)

145. VizieR Online Data Catalog: 2D decomposition of CALIFA galaxies (Mendez-Abreu+, 2017)

Author

Mendez-Abreu, J., Ruiz-Lara, T., Sanchez-Menguiano, L., Lorenzo-Caceres, A., Costantin, L., Catalan-Torrecilla, C., Florido, E., Aguerri, J. A. L., Bland-Hawthorn, J., Corsini, E. M., Dettmar, R. J., Lluís Galbany, Garcia-Benito, R., Marino, R. A., Marquez, I., Ortega-Minakata, R. A., Papaderos, P., Sanchez, S. F., Sanchez-Blazquez, P., Spekkens, K., Ven, G., Wild, V., and Ziegler, B.

146. VizieR Online Data Catalog: CALIFA DR2 (Garcia-Benito+, 2015)

Author

Garcia-Benito, R., Zibetti, S., Sanchez, S. F., Husemann, B., Amorim, A. L., Castillo-Morales, A., Cid Fernandes, R., Ellis, S. C., Falcon-Barroso, J., Galbany, L., Gil Paz, A., Gonzalez Delgado, R. M., Lacerda, E. A. D., Lopez-Fernandez, R., Lorenzo-Caceres, A., Lyubenova, M., Marino, R. A., Mast, D., Mendoza, M. A., Perez, E., Vale Asari, N., Aguerri, J. A. L., Ascasibar, Y., Bekeraite, S., Bland-Hawthorn, J., Barrera-Ballesteros, J. K., Bomans, D. J., Cano-Diaz, M., Catalan-Torrecilla, C., Cortijo, C., Delgado-Inglada, G., Demleitner, M., Dettmar, R. -J, Diaz, A. I., Florido, E., Gallazzi, A., Garcia-Lorenzo, B., Gomes, J. M., Holmes, L., Iglesias-Paramo, J., Jahnke, K., Kalinova, V., Kehrig, C., Kennicutt, R. C. Jr, Lopez-Sanchez, A. R., Marquez, I., Masegosa, J., Meidt, S. E., Mendez-Abreu, J., Molla, M., Monreal-Ibero, A., Morisset, C., Del Olmo, A., Papaderos, P., Perez, I., Quirrenbach, A., Rosales-Ortega, F. F., Roth, M. M., Ruiz-Lara, T., Sanchez-Blazquez, P., Sanchez-Menguiano, L., Singh, R., Spekkens, K., Stanishev, V., Torres-Papaqui, J. P., Glenn van de Ven, Vilchez, J. M., Walcher, C. J., Wild, V., Wisotzki, L., Ziegler, B., Alves, J., Barrado, D., Quintana, J. M., and Aceituno, J.

147. VizieR Online Data Catalog: CALIFA galaxies observational hints (Ruiz-Lara+, 2017)

Author

Ruiz-Lara, T., Perez, I., Florido, E., Sanchez-Blazquez, P., Mendez-Abreu, J., Sanchez-Menguiano, L., Sanchez, S. F., Lyubenova, M., Falcon-Barroso, J., Glenn van de Ven, Marino, R. A., Lorenzo-Caceres, A., Catalan-Torrecilla, C., Costantin, L., Bland-Hawthorn, J., Galbany, L., Garcia-Benito, R., Husemann, B., Kehrig, C., Marquez, I., Mast, D., Walcher, C. J., Zibetti, S., Ziegle, B., and Califa Team

148. VizieR Online Data Catalog: Merging galaxies (mis)alignments (Barrera-Ballesteros+, 2015)

Author

Barrera-Ballesteros, J. K., Garcia-Lorenzo, B., Falcon-Barroso, J., Ven, G., Lyubenova, M., Wild, V., Mendez-Abreu, J., Sanchez, S. F., Marquez, I., Masegosa, J., Ana Monreal Ibero, Ziegler, B., Del Olmo, A., Verdes-Montenegro, L., Garcia-Benito, R., Husemann, B., Mast, D., Kehrig, C., Iglesias-Paramo, J., Marino, R. A., Aguerri, J. A. L., Walcher, C. J., Vilchez, J. M., Bomans, D. J., Cortijo-Ferrero, C., Gonzalez Delgado, R. M., Bland-Hawthorn, J., Mcintosh, D. H., Bekeraite, S., and Califa, Collaboration

149. VizieR Online Data Catalog: CALIFA color/metallicity gradients connections (Marino+, 2016)

Author

Marino, R. A., Gil, Paz A., Sanchez, S. F., Sanchez-Blazquez, P., Cardiel, N., Castillo-Morales, A., Pascual, S., Vilchez, J., Kehrig, C., Molla, M., Mendez-Abreu, J., Catalan-Torrecilla, C., Florido, E., Perez, I., Ruiz-Lara, T., Ellis, S., Lopez-Sanchez, A. R., Gonzalez Delgado, R. M., Lorenzo-Caceres, A., Garcia-Benito, R., Lluís Galbany, Zibetti, S., Cortijo, C., Kalinova, V., Mast, D., Iglesias-Paramo, J., Papaderos, P., Walcher, C. J., and Bland-Hawthorn, J.

150. MEGARA, the Next Generation Optical MOS and IFU for GTC

Author

Gil Paz, A., Gallego, J., Carrasco, E., Iglesias, J., Sanchez, F., Vilchez, J., Garcia Vargas, M., Andres, P., Arrillaga, X., Aviles, J., Bonache, J., Carrera, M., Castillo, A., Castillo, E., Raquel Cedazo, Dormido, J., Eliche Moral, C., Esteban, S., Ferrusca, D., Gonzalez, E., Lefort, B., Lopez, J. A., Maldonado, M., Marino, R., Martinez, I., Morales, I., Mujica, E., Paez, G., Pascual, S., Perez, A., Sanchez, A., Sanchez, E., Tulloch, S., Velazquez, M., Zamorano, J., Aguerri, A., Barrado, D., Bertone, E., Cardiel, N., Cava, A., Cenarro, J., Chavez, M., Garcia, M., Gonzalez Delgado, R., Guichard, J., Guzman, R., Herrero, A., Huelamo, N., Hughes, D., Jimenez, J., Kehrig, C., Marquez, I., Masegosa, J., Mayya, D., Mendez Abreu, J., Molla, M., Munoz Tunon, C., Peimbert, M., Perez Gonzalez, P., Perez Montero, E., Rodriguez, M., Rodriguez Espinosa, J. M., Rodriguez, L., Rosa, D., Sanchez Almeida, J., Sanchez Contreras, C., Sanchez Blazquez, P., Sanchez, S. F., Sarajedini, A., Silich, S., Simon-Diaz, S., Tenorio Tagle, G., Terlevich, E., Terlevich, R., Torres-Peimbert, S., Trujillo, I., Tsamis, Y., Vega, O., and Villar, V.

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