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© The Authors 2023. DMD acknowledges financial support from the Talentia Senior Program (through the incentive ASE-136) from Secretaría General de Universidades, Investigación y Tecnología, de la Junta de Andalucía. DMD acknowledges funding from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709) and project (PDI2020-114581GBC21/ AEI / 10.13039/501100011033). SRF acknowledges financial support from the Spanish Ministry of Economy and Competitiveness (MINECO) under grant number AYA2016-75808-R, AYA2017-90589-REDT and S2018/NMT-429, and from the CAM-UCM under grant number PR65/19-22462. SRF acknowledges support from a Spanish postdoctoral fellowship, under grant number 2017- T2/TIC-5592. MAGF acknowledges financial support from the Spanish Ministry of Science and Innovation through the project PID2020-114581GB-C22. JR acknowledges support from the State Research Agency (AEI-MCINN) of the Spanish Ministry of Science and Innovation under the grant “The structure and evolution of galaxies and their central regions” with reference PID2019- 105602GB-I00/10.13039/501100011033. JR also acknowledges funding from University of La Laguna through the Margarita Salas Program from the Spanish Ministry of Universities ref. UNI/551/2021-May 26, and under the EU Next Generation. MA acknowledges the financial support from the Spanish Ministry of Science and Innovation and the European Union – NextGenerationEU through the Recovery and Resilience Facility project ICTS-MRR-2021-03-CEFCA. This project uses data from observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. We acknowledge support from the Spanish Ministry for Science, Innovation and Universities and FEDER funds through gra, Secretaría General de Universidades, Investigación y Tecnología, de la Junta de Andalucía, State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa”, Ministerio de Economía y Competitividad (MINECO), Comunidad de Madrid, Spanish postdoctoral fellowship, Ministerio de Ciencia e Innovación (MICIN), State Research Agency (AEI-MCINN) of the Spanish Ministry of Science and Innovation under the grant “The structure and evolution of galaxies and their central regions”, University of La Laguna through the Margarita Salas Program from the Spanish Ministry of Universities, European Union – NextGenerationEU through the Recovery and Resilience Facility project, Ministerio de Ciencia, Innovación y Universidades, FEDER funds, US Department of Energy, US National Science Foundation, Ministerio de Ciencia e Innovación, Science and Technology Facilities Council of the United Kingdom, Higher Education Funding Council for England, National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, Kavli Institute of Cosmological Physics at the University of Chicago, Center for Cosmology and Astro-Particle Physics at the Ohio State University, Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico, Ministério da Ciência, Tecnologia e Inovacão, Deutsche Forschungsgemeinschaft, Argonne National Laboratory, University of California at Santa Cruz, University of Cambridge, Centro de Investigaciones Enérgeticas, Medioambientales y Tecnológicas-Madrid, University of Chicago, University College London, DES-Brazil Consortium, University of Edinburgh, Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, University of Illinois at UrbanaChampaign, Institut de Ciències de l’Espai (IEEC/CSIC), Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, LudwigMaximilians Universität München and the associated Excellence Cluster Universe, University of Michigan, National Optical Astronomy Observatory, University of Nottingham, Ohio State University, University of Pennsylvania, University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, University of Sussex, Texas A&M University, NASA through the NASA Hubble Fellowship, Association of Universities for Research in Astronomy, Incorporated, under NASA contract, Japanese MEXT scholarship and its Grant-in-Aid for Scientific Research, European Research Council (ERC), Ministerio de Economía y Competitividad, Ministerio de Ciencia e Innovación, European Union – NextGenerationEU through the Recovery and Resilience Facility, Universidad Complutense de Madrid, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2023 The Author(s). Artículo firmado por 23 autores. We sincerely thank the referee for the thorough reading and insightful comments that helped to improve the quality of this work. This research has been funded by grants PGC2018- 093499-B-I00 and RTI2018-096188-B-I00 funded by MCIN/ AEI/10.13039/501100011033. Á.G.A. acknowledges the support of the Universidad Complutense de Madrid through the predoctoral grant CT17/17-CT18/17. A.Y. is supported by an appointment to the NASA Postdoctoral Program (NPP) at NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities under contract with NASA. L.C. acknowledges financial support from Comunidad de Madrid under Atracción de Talento grant 2018-T2/TIC-11612. R.M. M. acknowledges support from Spanish Ministerio de Ciencia, Innovación y Universidades through grant PGC2018-093499- B-I00, from MDM-2017-0737 Unidad de Excelencia “Maria de Maeztu”-Centro de Astrobiología (INTA-CSIC) by the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/ 10.13039/501100011033 and by “ERDF A way of making Europe,” and also from the Instituto Nacional de Técnica Aeroespacial SHARDS-JWST project through the PRE-SHARDSJWST/2020 grant., Ministerio de Ciencia e Innovación (MCIN), Universidad Complutense de Madrid through the predoctoral grant, NASA Postdoctoral Program (NPP) at NASA Goddard Space Flight Center, Comunidad de Madrid under Atracción de Talento grant, Unidad de Excelencia “Maria de Maeztu”, Agencia Estatal de Investigación (España), Instituto Nacional de Técnica Aeroespacial SHARDS-JWST, ERDF "A way of making Europe", Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© TheAuthors 2023. Artículo firmado por 29 autores. We thank the anonymous referee for their useful report. This work was supported by the Evolution of Galaxies project, of references AYA2017-88007-C3-1-P, AYA2017-88007-C3-2-P, AYA2018-RTI-096188-BI00, PID2019-107408GB-C41, PID2019-106027GB-C41, PID2021-122544NB-C41, and MDM-2017-0737 (Unidad de Excelencia María de Maeztu, CAB), within the Programa estatal de fomento de la investigación científica y técnica de excelencia del Plan Estatal de Investigación Científica y Técnica y de Innovación (2013-2016) of the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/10.13039/501100011033 and by `ERDF A way of making Europe'. This article is based on observations made with the Gran Telescopio Canarias (GTC) at Roque de los Muchachos Observatory on the island of La Palma, with the Willian Herschel Telescope (WHT) at Roque de los Muchachos Observatory on the island of La Palma and on observations at Kitt Peak National Observatory, NSF's National Optical-Infrared Astronomy Research Laboratory (NOIRLab Prop. ID: 2018A-0056; PI: Gonzalez-Serrano, J.I.), which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. J.N. acknowledges the support of the National Science Centre, Poland through the SONATA BIS grant 2018/30/E/ST9/00208. E.B. and I.C.G. acknowledge support from DGAPA-UNAM grant IN113320. M.P. acknowledges the support from the Space Science and Geospatial Institute under the Ethiopian Ministry of Innovation and Technology (MInT). E.A. and M.P. acknowledge the support from the State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa award to the Instituto de Astrofísica de An, Context. Extragalactic surveys are a key tool for better understanding the evolution of galaxies. Both deep and wide-field surveys serve to provide a clearer emerging picture of the physical processes that take place in and around galaxies, and to identify which of these processes are the most important in shaping the properties of galaxies. Aims. The Lockman Spectroscopic Redshift Survey using Osiris (Lockman-SpReSO) aims to provide one of the most complete optical spectroscopic follow-ups of the far-infrared (FIR) sources detected by the Herschel Space Observatory in the Lockman Hole (LH) field. The optical spectroscopic study of the FIR-selected galaxies supplies valuable information about the relation between fundamental FIR and optical parameters, including extinction, star formation rate, and gas metallicity. In this article, we introduce and provide an in-depth description of the Lockman-SpReSO project and of its early results. Methods. We selected FIR sources from Herschel observations of the central 24 arcmin x24 arcmin of the LH field with an optical counterpart up to 24.5 R_(C)(AB). The sample comprises 956 Herschel FIR sources, plus 188 additional interesting objects in the field. These are point X-ray sources, cataclysmic variable star candidates, high-velocity halo star candidates, radio sources, very red quasi-stellar objects, and optical counterparts of sub-millimetre galaxies. The faint component of the catalogue (R_(C)(AB) ≥ 20) was observed using the OSIRIS instrument on the 10.4 m Gran Telescopio Canarias in multi-object spectroscopy (MOS) mode. The bright component was observed using two multi-fibre spectrographs: the AF2-WYFFOS at the William Herschel Telescope and the HYDRA instrument at the WYIN telescope. Results. From an input catalogue of 1144 sources, we measured a secure spectroscopic redshift in the range 0.03 ≲ z ≲ 4.96 for 357 sources with at least two identified spectral lines. In addition, for 99 sources that show only one emission, he Spanish Ministry of SciPrograma estatal de fomento de la investigación científica y técnica de excelencia del Plan Estatal de Investigación Científica y Técnica y de Innovación (2013-2016), Unidad de Excelencia María de Maeztu, CAB, ERDF "A way of making Europe", National Science Centre, Poland through the SONATA BIS, DGAPA-UNAM, Space Science and Geospatial Institute under the Ethiopian Ministry of Innovation and Technology (MInT), Centro de Excellence Severo Ochoa, Universidad de La Laguna. Proyecto de Internacionalización y Excelencia, Programa Tomás de Iriarte 2022, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

We investigate spatially resolved emission-line ratios in a sample of 219 galaxies (0.6 < z < 1.3) detected using the G102 grism on the Hubble Space Telescope Wide Field Camera 3 taken as part of the CANDELS Ly alpha Emission at Reionization survey to measure ionization profiles and search for low-luminosity active galactic nuclei (AGN). We analyze [O iii] and H beta emission-line maps, enabling us to spatially resolve the [O iii]/H beta emission-line ratio across the galaxies in the sample. We compare the [O iii]/H beta ratio in galaxy centers and outer annular regions to measure ionization differences and investigate the potential of sources with nuclear ionization to host AGN. We investigate some of the individual galaxies that are candidates to host strong nuclear ionization and find that they often have low stellar mass and are undetected in X-rays, as expected for low-luminosity AGN in low-mass galaxies. We do not find evidence for a significant population of off-nuclear AGN or other clumps of off-nuclear ionization. We model the observed distribution of [O iii]/H beta spatial profiles and find that most galaxies are consistent with a small or zero difference between their nuclear and off-nuclear line ratios, but 6%-16% of galaxies in the sample are likely to host nuclear [O iii]/H beta that is similar to 0.5 dex higher than in their outer regions. This study is limited by large uncertainties in most of the measured [O iii]/H beta spatial profiles; therefore, deeper data, e.g., from deeper HST/WFC3 programs or from JWST/NIRISS, are needed to more reliably measure the spatially resolved emission-line conditions of individual high-redshift galaxies.

© ESO 2013. The authors are very grateful to the referee, Frédéric Bournaud, for the input that helped to improve this publication significantly. We also thank Olga Sil'chenko for stimulating the present study, as well as Miguel Querejeta and Eija Laurikainen for interesting and useful comments. Supported by the Spanish Ministry of Science and Innovation (MICINN) under projects AYA2009-10368, AYA2006-12955, AYA2010-21887-C04-04, AYA2009-11137, and AYA2012-30717, and by the Madrid Regional Government through the AstroMadrid Project (CAM S2009/ESP-1496, http://www.laeff.cab.inta-csic.es/projects/astromadrid/main/index.php). Funded by the Spanish MICINN under the Consolider-Ingenio 2010 Program grant CSD2006-00070: "First Science with the GTC" (http://www.iac.es/consolider-ingenio-gtc/), and by the Spanish programme of International Campus of Excellence Moncloa (CEI). A.C.G.G. is a Ramón y Cajal Fellow of the Spanish MICINN. This research is based in part on services provided by the GAVO data center. It has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration., Context. Galaxy mergers are widely discussed as one possible evolution mechanism for lenticular galaxies (S0s), because even minor mergers induce structural changes that are difficult to reconcile with the strong bulge-disk coupling observed in the photometric scaling relations of these galaxies. Aims. We check if the evolution induced onto S0s by dry intermediate and minor mergers can reproduce the S0 photometric scaling relations. Methods. We analyse the bulge-disk decompositions of the collisionless N-body simulations of intermediate and minor mergers onto S0s presented previously to determine the evolution induced by the mergers in several relevant photometric planes. Results. The mergers induce an evolution in the photometric planes that is compatible with the data of S0s, even in the relations that indicate a strong bulge-disk coupling. Mergers drive the formation of the observed photometric relation in some cases and induce a slight dispersion compatible with data in others. Therefore, this evolutionary mechanism tends to preserve the observational photometric relations. In the photometric planes where the morphological types segregate, the mergers always induce evolution towards the region populated by S0s. No clear trends with the mass ratio of the encounter, the central satellite density, or the spin-orbit coupling are found for the range of values studied. Long-pericentre orbits generate more concentrated disks and expanded bulges than initially, while short-pericentre orbits do the opposite. The structural coupling of the bulge and the disk is preserved or reinforced in the models because mergers trigger internal secular processes in the primary disk that induce significant bulge growth. This happens even though the encounters do not induce bars in the disks. Conclusions. Intermediate and minor mergers can be considered to be plausible mechanisms for the evolution of S0s if one includes their photometric scaling relations, because they can preserve and e, Ministerio de Ciencia e Innovación (MICINN), España, Comunidad de Madrid, Campus de Excelencia Internacional (CEI) Moncloa, Depto. de Física de Materiales, Fac. de Ciencias Físicas, TRUE, pub

Reproduced by permission of the AAS. © 2009. The American Astronomical Society. All rights reserved. We thank J. Cenarro for his help on investigating the spectra for potential problems and for providing the GC data. We are also grateful to Russell Smith for providing the data from the Hectospec Coma cluster survey and double checking our measurements. R. G. gratefully acknowledges University of Yale for the awarded nights at WIYN telescope. P. Sánchez Blázquez acknowledges the support by a Marie Curie Intra-European Fellowship within the 6th European Community Framework Programme. We also thank the anonymous referee whose suggestions have improved this work., We present line-strength measurements for 74 early-type galaxies in the core of the Coma cluster reaching down to velocity dispersions, sigma, of 30 km s(-1). The index-sigma relations for our sample, including galaxies with sigma < 100 km s(-1) (low-sigma), differ in shape depending on which index is used. We note two types of relations for the metallic indices: one showing a break in the slope around similar to 100 km s(-1) and another group with strong linear relations between an index and log s. We find no connection between the behavior of index-sigma relations with either alpha- or Fe-peak elements. However, we find indications that the relations are tighter for indices which do not depend on the microturbulent velocities of stellar atmospheres. We confirm previous results that low-sigma galaxies including dE/dS0s are on average younger, less metal rich, and have lower [alpha/Fe] in comparison with E/S0s. Our data show that these trends derived for high-sigma galaxies extend down to dE/dS0s. This is a factor of similar to 2 lower in sigma than previously published work. We confirm that the observed anticorrelation between age and metallicity for high-sigma galaxies is consistent with the effects of correlated errors. Low-sigma galaxies also show a similar relation between age and metallicity as a result of correlated errors. However, they are offset from this relationship so that, on average, they are less metal rich and younger than their high-sigma counterparts., Marie Curie Intra-European Fellowship, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO, 2011. We thank the MAGPOP EU Marie Curie Training Network for financial support for the collaborating research visits and observations that led to this paper. E.T. acknowledges the financial support by the Spanish research project AYA2007-67752-C03-03. We thank Consolider-GTC project for partial financial support. This paper made use of the following public databases: SDSS, NED, HyperLEDA, GOLDMine. We are grateful to the anonymous referee for a critical report that has improved the quality of the paper., We present new medium resolution kinematic data for a sample of 21 dwarf early-type galaxies (dEs) mainly in the Virgo cluster, obtained with the WHT and INT telescopes at the Roque de los Muchachos Observatory (La Palma, Spain). These data are used to study the origin of the dwarf elliptical galaxy population inhabiting clusters. We confirm that dEs are not dark matter dominated galaxies, at least not up to the half-light radius. We also find that the observed galaxies in the outer parts of the cluster are mostly rotationally supported systems with disky morphological shapes. Rotationally supported dEs have rotation curves similar to those of star-forming galaxies of similar luminosity and follow the Tully-Fisher relation. This is expected if dE galaxies are the descendants of low-luminosity star-forming systems that have recently entered the cluster environment and lost their gas due to a ram-pressure stripping event, quenching their star formation activity and transforming into quiescent systems, but conserving their angular momentum., Ministerio de Ciencia e Innovación (MICINN), Marie Curie Actions (UE), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2006. This paper has been supported by the “Plan Andaluz de Investigación” (FQM-108) and by the “Secretaría de Estado de Política Científica y Tecnológica” (AYA2004-08251-C02-02, ESP2004-06870-C02-02). We are indebted to Andrés González Carmona who helped us with the statistical analysis. We also acknowledge the LEDA data base organisation, which was highly useful for this research. Thanks to the anonymous referee for valuable comments and suggestions that have contributted to improve the final version of the paper., The results obtained in Paper I are used to study possible relationships between the truncation radius of stellar discs in the NIR and structural parameters of the galaxies. The NIR truncation radius is larger for brighter galaxies, being proportional to V(m)(c) with c approximate to 3/2, and with V(m) being the asymptotic rotation velocity at large radii (when the rotation curve becomes flat), and is lower for higher wavelengths. When it is normalized to the scalelength, the truncation is an increasing function of the central surface brightness and is lower for late type galaxies, although these correlations are weaker. These relations are in agreement with the scenario of magnetically driven truncations., Plan Andaluz de Investigación, Secretaría de Estado de Política Científica y Tecnológica, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2007. We are grateful to Nicolás Cardiel for his help in technical issues in the reduction process. The INT is operated on the island of La Palma by the Royal Greenwich Observatory at the Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. This work was supported by the Spanish research project AYA 2003-01840., This is the first paper presenting our long-term project aimed at studying the nature of bulges through analyzing their stellar population gradients. We present deep spectroscopic observations along the minor axis and the data reduction for a sample of 32 bulges of edge-on spiral galaxies. We explain in detail our procedures for measuring their dynamical parameters (rotation curves and velocity dispersion profiles) and line-strength indices, including the conversion to the Lick/IDS system. Tables giving the values of the dynamical parameters and line-strength indices at each galactocentric radius are presented (in electronic form) for each galaxy of the sample. The derived line-strength gradients from this dataset will be analyzed in a forthcoming paper to set constraints on the different scenarios for the formation of the bulges., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

This article has been accepted for publication in Monthly notices of the Royal Astronomical Society © 2011 The Authors © 2011 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. This work was based on observations made with European Southern Observatory (ESO) telescopes at Paranal Observatory under programme ID 070.A 0332. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This work has been supported by the Programa Nacional de Astronomía y Astrofísica of the Spanish Ministry of Science and Innovation under grants AYA2007-67752-C03-03 and AYA2006-15698-C02-02., We present absorption-line index gradients for a sample of S0 galaxies in the Fornax cluster. The sample has been selected to span a wide range in galaxy mass, and the deep FORS2 spectroscopy on the VLT allows us to explore the stellar populations all the way to the outer disc-dominated regions of these galaxies. We find that globally, in both bulges and discs, star formation ceased earliest in the most massive systems, as a further manifestation of downsizing. However, within many galaxies, we find an age gradient which indicates that star formation ended first in the outermost regions. Metallicity gradients, when detected, are always negative such that the galaxy centres are more metal-rich. This finding fits with a picture in which star formation continued in the central regions, with enriched material, after it had stopped in the outskirts. Age and metallicity gradients are correlated, suggesting that large differences in star formation history between the inner and outer parts of S0 galaxies yield large differences in their chemical enrichment. In agreement with previous results, we conclude that the radial variations in the stellar populations of S0 galaxies are compatible with the hypothesis that these galaxies are the descendants of spiral galaxies whose star formation has ceased. With the addition of radial gradient information, we are able to show that this shutdown of star formation occurred from the outside inward, with the later star formation in the central regions offering a plausible mechanism for enhancing the bulge light in these systems, as the transformation to more bulge-dominated S0 galaxies requires., National Aeronautics and Space Administration, National Science Foundation, Spanish Ministry of Science and Innovation, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

This article has been accepted for publication in Monthly notices of the Royal Astronomical Society. © 2007 The Authors. Journal compilation. © 2007 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck-Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). Based in part on observations with the NASA/ESA HST, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. We thank Dr R. Gredel, former director of Calar Alto, for supporting this work and providing us with the telescope time for finishing it. We thank support from the Spanish Plan Nacional de Astronomía programme AYA2005-09413-C02-02, of the Spanish Ministery of Education and Science and the Plan Andaluz de Investigación of Junta de Andalucía as research group FQM322. We thank Dr R. Peletier, who kindly read the article cleaning the English. His comments on the science content have helped us to increase the quality of this article., We present a study of the stellar populations and morphologies of galaxies in the core of the galaxy cluster Abell 2218. Integral field spectroscopy (IFS) observations were performed using PMAS in the PPAK mode covering a field of view of similar to 74 x 64 arcsec(2) centred on the core of the cluster, in order to obtain spectroscopy of an unbiased flux-limited sample of cluster galaxies. 43 objects were detected in the IFS data, 31 of them with enough signal-to-noise ratio to derive the redshift, all of them brighter than I < 21.5 mag. 28 are at the redshift of the cluster (17 with previously unknown redshift). Individual spectra of the cluster members were extracted and compared with single stellar population models to derive the luminosity-weighted ages and metallicities. In addition, deep Hubble Space Telescope (HST)/ACS F475W-, F555W-, F625W- and F850LP-band images centred on the cluster core were obtained from the HST archive (z(lim) similar to 28 mag). A detailed morphological analysis of all the galaxies within the field of view of these images down to z(lim) < 22.5 mag was performed classifying them as late-type, intermediate and early-type, on the basis of their Sersic indices. The literature was scanned to look for spectroscopically confirmed cluster members located within the field of view of the ACS image. The final sample of 59 galaxies comprises our reported sample of 28 galaxies in the core, and 31 additional galaxies in the outer regions. In addition, multiband broad-band photometry was extracted from the literature for all objects. The morphologically segregated colour-magnitude diagram shows that the early-type galaxies cover the range of brighter and redder colours (the so-called 'red sequence'). A large fraction of spiral galaxies (similar to 50 per cent) is found, most of them fainter than the limit of previous studies. They cover a wide range in colours, from blue colours typical of Butcher-Oemler galaxies to red colours similar to those of ea, Spanish Plan Nacional de Astronomía of the Spanish Ministery of Education and Science, Plan Andaluz de Investigación of Junta de Andalucía, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2009. The American Astronomical Society. All rights reserved. We thank Francesca Matteucci and Reynier Peletier for several very useful discussions. The expert guidance of the referee, Judy Cohen, is gratefully acknowledged. This work has been partially supported by the Spanish research project AYA2007-67752-C03-03, the Marie Curie Intra-European Fellowship scheme within the 6th European Community Framework Programme (PSB), UK's Science & Technology Facilities Council (BKG). E. T. acknowledges the support of the University of Central Lancashire's Livesey Award scheme (PSB)., For the first time, we undertake a systematic examination of the nitrogen abundances using the NH3360 feature for a sample of 35 early-type galaxies spanning a range of masses and local environment. The nitrogen-sensitive molecular feature at 3360Å has been employed in conjunction with a suite of atomic- and molecular-sensitive indices to provide unique and definitive constraints on the chemical content of these systems. By employing NH3360, we are now able to break the carbon, nitrogen, and oxygen degeneracies inherent to the use of the cyanogen (CN) index. We demonstrate that the NH3360 feature shows little dependency upon the velocity dispersion (our proxy for mass) of the galaxies, contrary to what is seen for carbon-and magnesium-sensitive indices. At face value, these results are at odds with conclusions drawn previously using indices sensitive to both carbon and nitrogen, such as CN. With the aid of stellar population models, we find that the N/Fe ratios in these galaxies are consistent with being mildly enhanced with respect to the solar ratio. We also explore the dependence of these findings upon environment, by analyzing the co-added spectra of galaxies in the field and the Coma cluster. We confirm the previously found differences in carbon abundances between galaxies in low-and high-density environments, while showing that these differences do not seem to exist for nitrogen. We discuss the implications of these findings for the derivation of the star-formation histories in early-type galaxies, and for the origin of carbon and nitrogen themselves., Ministerio de Ciencia e Innovación (MICINN), Programa Nacional de Astronomía y Astrofísica (PNAyA), MCINN, Marie Skłodowska-Curie actions (UE), UK's Science & Technology Facilities Council (BKG), University of Central Lancashire's Livesey Award scheme (PSB), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2014. The authors would like to thank the anonymous reviewer for a very helpful and constructive referee report. We would also like to acknowledge I. Chilingarian, P. Di Matteo, F. Combes, A.-L. Melchior, and B. Semelin for creating the GalMer database. We also appreciate valuable comments by P.G. Pérez González and E. Laurikainen, as well as the GALFIT code made publicly available by his author C. Peng. We also acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr). This research has made use of the NASA's Astrophysics Data System and NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. M.Q. acknowledges financial support to the DAGAL network from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme FP7/2007-2013/ under REA grant agreement number PITN-GA-2011-289313. Supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under projects AYA2006-12955, AYA2009-10368, AYA2012-30717, and AYA2012-31277, and by the Madrid Regional Government through the AstroMadrid Project (CAM S2009/ESP-1496, http://www.laeff.cab.inta-csic.es/projects/astromadrid/main/index. php). Funded by the Spanish MICINN under the Consolider-Ingenio 2010 Programme grant CSD2006-0070: "First Science with the GTC" (http://www.iac.es/consolider-ingenio-gtc/), and by the Spanish programme of International Campus of Excellence Moncloa (CEI)., Context. Observations reveal a strong structural coupling between bulge and disc in S0 galaxies, which seems difficult to explain if they have formed from supposedly catastrophic events such as major mergers. Aims. We face this question by quantifying the bulge-disc coupling in dissipative simulations of major and minor mergers that result in realistic S0s. Methods. We have studied the dissipative N-body binary merger simulations from the GalMer database that give rise to realistic, relaxed E/S0 and S0 remnants (67 major and 29 minor mergers). We simulate surface brightness profiles of these S0-like remnants in the K band, mimicking typical observational conditions, to perform bulge-disc decompositions analogous to those carried out in real S0s. Additional components have been included when needed. The global bulge-disc structure of these remnants has been compared with real data. Results. The S0-like remnants distribute in the B/T - r(e) - h(d) parameter space consistently with real bright S0s, where B/T is the bulge-to- total luminosity ratio, r(e) is the bulge effective radius, and h(d) is the disc scalelength. Major mergers can rebuild a bulge-disc coupling in the remnants after having destroyed the structures of the progenitors, whereas minor mergers directly preserve them. Remnants exhibit B/T and r(e)/h(d) spanning a wide range of values, and their distribution is consistent with observations. Many remnants have bulge Sersic indices ranging 1 < n < 2, flat appearance, and contain residual star formation in embedded discs, a result which agrees with the presence of pseudobulges in real S0s. Conclusions. Contrary to the popular view, mergers (and in particular, major events) can result in S0 remnants with realistically coupled bulge-disc structures in less than similar to 3 Gyr. The bulge-disc coupling and the presence of pseudobulges in real S0s cannot be used as an argument against the possible major-merger origin of these galaxies., Comunidad de Madrid, Unión Europea. FP7, National Aeronautics and Space Administration, Spanish Ministry of Economy and Competitiveness (MINECO), Spanish MICINN, Spanish programme of International Campus of Excellence Moncloa (CEI), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

This article has been accepted for publication in Monthly notices of the Royal Astronomical Society. © 2007 The Authors. Journal compilation © 2007 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. This paper has been supported by the ‘Plan Andaluz de Investigación’ (FQM-108) and by the ‘Secretaría de Estado de Política Científica y Tecnológica’ (AYA2000-2046-C02-01, AYA2004- 08251-C02-02, ESP2004-06870-CO2-02). This research has made use of the NASA/IPAC Extragalactic Database which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We have used observations made with the NASA/ESA HST, obtained from the data archive at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. J. Jiménez Vicente acknowledges support from the Consejería de Educación y Ciencia de la Junta de Andalucía. A. Castillo Morales acknowledges the support from Universidad Complutense de Madrid (AYA2003-01676). We thank J. Knapen and A. Zurita for their help with the astrometric calibration of our images. We also acknowledge the support of the RTN Euro3D: ‘Promoting 3D spectroscopy in Europe’. Thanks to the anonymous referee for valuable comments and suggestions that have contributed to improve this paper., We analyse new integral-field spectroscopy of the inner region (central 2.5 kpc) of the spiral galaxy NGC 4321 to study the peculiar kinematics of this region. Fourier analysis of the velocity residuals obtained by subtracting an axisymmetric rotation model from the H alpha velocity field indicates that the distortions are global features generated by an m = 2 perturbation of the gravitational potential which can be explained by the nuclear bar. This bar has been previously observed in the near-infrared but not in the optical continuum dominated by star formation. We detect the optical counterpart of this bar in the 2D distribution of the old stellar population (inferred from the equivalent width map of the stellar absorption lines). We apply the Tremaine-Weinberg method to the stellar velocity field to calculate the pattern speed of the inner bar, obtaining a value of Omega(b) = 160 +/- 70 km s(-1) kpc(-1). This value is considerably larger than the one obtained when a simple bar model is considered. However, the uncertainties in the pattern speed determination prevent us from giving support to alternative scenarios., Plan Andaluz de Investigación, Secretaría de Estado de Política Científica y Tecnológica, NASA, Consejería de Educación y Ciencia de la Junta de Andalucía, Universidad Complutense de Madrid, RTN Euro3D: Promoting 3D spectroscopy in Europe, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© EDP Sciencies. Based on observations made with the Isaac Newton Telescope operated on the island of La Palma by the Royal Greenwich Observatory in the Spanish Observatorio del Roque de los Muchachos of the Instituto Astrofísica. This research has been support in part by the grant No. PB96-0645 from the Spanish Programa Sectorial de Promoción General del Conocimiento., UCM1612+1308 is a new emission-line galaxy identified in the context of the Universidad Complutense de Madrid (UCM) survey. This object was classified as Blue Compact Galaxy (BCG) from photometric data. A detailed spectroscopic study from new optical observations is presented now. The physical conditions and chemical composition are derived. The ionic abundances yield to a metallicity of 0.23±0.01Z_⊙ and a very low nitrogen to oxygen abundances ratio, log (N/O)= -1.74±0.07, supporting a primary nucleosynthesis origin for the nitrogen. The same value has been obtained for the sulfur to oxygen ratio. The comparison of the helium abundance with the oxygen and nitrogen abundances evidences a quickly enrichment of oxygen produced by massive stars. The ionizing cluster has been analyzed yielding a relatively low ionization parameter, log bar Ū=-3, total number of stars, log N^* = 6.18, stellar mass, log M^* = 5.71 M_⊙, and gas mass log M_g = 7.42M_⊙. A lower limit of the dust mass, log M_dust = 5.65M_⊙, has been obtained from the IRAS fluxes. The observed data and derived parameters, when interpreted with the evolutionary synthesis models by Leitherer & Heckman (1995), point out to an instantaneous burst with an age of log t= 6.7yr., Programa Sectorial de Promoción General del Conocimiento (MEC), España, Ministerio de Educación y Cultura (MEC), España, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2012. The authors thank the anonymous referee for the provided input that helped to improve this publication significantly. We also thank Olga Sil'chenko for stimulating the present study, as well as Peter Erwin and Miguel Querejeta for interesting and useful comments. Supported by the Spanish Ministry of Science and Innovation (MICINN) under projects AYA2009-10368, AYA2006-12955, AYA2010-21887-C04-04, and AYA2009-11137, and by the Madrid Regional Government through the AstroMadrid Project (CAM S2009/ESP-1496, http://www.laeff.cab.inta-csic.es/projects/astromadrid/main/index.php). Funded by the Spanish MICINN under the Consolider-Ingenio 2010 Program grant CSD2006-00070: "First Science with the GTC" (http://www.iac.es/consolider-ingenio-gtc/). ACGG is a Ramón y Cajal Fellow of the Spanish MICINN. This research is based in part on services provided by the GAVO data center. It has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. S. D. H. & G., Context. Recent studies have argued that galaxy mergers are not important drivers for the evolution of S0's, on the basis that mergers cannot preserve the coupling between the bulge and disk scale-lengths observed in these galaxies and the lack of correlation of their ratio with the S0 Hubble type. However, about 70% of present-day S0's reside in groups, an environment where mergers and tidal interactions dominate galaxy evolution. Aims. We investigate whether the remnants resulting from collision-less N-body simulations of intermediate and minor mergers onto S0 galaxies evolve fulfilling global structural relations observed between the bulges and disks of these galaxies. Methods. Different initial bulge-to-disk ratios of the primary S0 have been considered, as well as different satellite densities, mass ratios, and orbits of the encounter. We have analysed the final morphology of the remnants in images simulating the typical observing conditions of S0 surveys. We derive bulge+disk decompositions of the final remnants to compare their global bulge-to-disk structure with observations. Results. We show that all remnants present undisturbed S0 morphologies according to the prescriptions of specialized surveys. The dry intermediate and minor mergers induce noticeable bulge growth (S0c --> S0b and S0b --> S0a), but affect negligibly to the bulge and disk scale-lengths. Therefore, if a coupling between these two components exists prior to the merger, the encounter does not break this coupling. This fact provides a simple explanation for the lack of correlation between the ratio of bulge and disk scale-lengths and the S0 Hubble type reported by observations. Conclusions. These models prove that dry intermediate and minor mergers can induce global structural evolution within the sequence of S0 Hubble types compatible with observations, meaning that these processes should not be discarded from the evolutionary scenarios of S0's just on the basis of the strong coupling observ, Ministerio de Ciencia e Innovación (MCINN), Consolider-Ingenio Program, Comunidad de Madrid, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. We received financial support through the Spanish research project AYA2010-21322-C03-03, from the Spanish Ministerio de Economía y Competitividad. PSB is supported by the Ministerio de Economía y Competitividad (MINECO) through its Ramón y Cajal program. IP acknowledges the support by the Spanish Ministerio de Economía y Competitividad (MINECO) (via grants AYA2010-21322-C03-02, AYA2010-21322-C03-03, AYA2007-67625-C02-02 and Consolider-Ingenio CSD2010-00064) and by the Junta de Andalucía (FQM-108)., Numerical simulations predict that bars represent a very important agent for triggering gas inflows, which in turn could lead to central star formation. Bars thus are thought to contribute to the formation of the bulge. This process changes both the gaseous-phase and the stellar-phase metallicities in the centres of galaxies. With the aim of quantifying the importance of this process, we present a comparative study of the gaseous-phase and stellar-phase metallicities in the centres of members of a sample of barred and unbarred galaxies from SDSS. We do not find a significant difference in the metallicity (neither gaseous nor stellar) between barred and unbarred galaxies, but we find different trends in the metallicities of early- and late-type galaxies, with larger differences in the metallicity in the early-type subsample. Our results contradict some previous research in this field, but we find a possible origin of the discrepancies between previous works and our results., Ministerio de Economía y Competitividad (MINECO), CONSOLIDER - INGENIO (MINECO), Junta de Andalucía, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO, 2014. Artículo firmado por 22 autores. We thank our anonymous referee, who very carefully read this paper. The authors wish to thank the entire S4G team for their efforts in this project. We thank Pertti Rautiainen for useful discussions on the ring formation in his simulations, Simón Díaz García for helping with fundamental statistical concepts, and Glenn van de Ven for his useful comments. We acknowledge financial support to the DAGAL network from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme FP7/2007-2013/under REA grant agreement number PITN-GA-2011-289313. E.A. and A.B. acknowledge financial support from the CNES (Centre National d'Etudes Spatiales - France). K.S., J.-C.M.-M., T.K., and T.M. acknowledge support from the National Radio Observatory, which is a facility of the National Radio Astronomy Observatory operated under cooperative agreement by Associated Universities, Inc. S.C., H.S., E.L., M.H.-H., and J.L. acknowledge support from the Academy of Finland. This work is based on observations and archival data made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We are grateful to the dedicated staff at the Spitzer Science Center for their help and support in planning and execution of this Exploration Science program. We also gratefully acknowledge support from NASA JPL/Spitzer grant RSA 1374189 provided for the S4G project. This research has made use of SAOImage DS9, developed by Smithsonian Astrophysical Observatory. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration., Context. Resonance rings and pseudorings (here collectively called rings) are thought to be related to the gathering of material near dynamical resonances caused by non-axisymmetries in galaxy discs. This means that they are the result of secular evolution processes that redistribute material and angular momentum in discs. Studying them may give clues on the formation and growth of bars and other disc non-axisymmetries. Aims. Our aims are to produce a catalogue and an atlas of the rings detected in the Spitzer Survey of Stellar Structure in Galaxies (S^4G) and to conduct a statistical study of the data in the catalogue. Methods. We traced the contours of rings previously identified and fitted them with ellipses. We found the orientation of bars by studying the galaxy ellipse fits from the S^4G pipeline 4. We used the galaxy orientation data obtained by the S^4G pipeline 4 to obtain intrinsic ellipticities and orientations of rings and the bars. Results. ARRAKIS contains data on 724 ringed galaxies in the S^4G. The frequency of resonance rings in the S^4G is of 16 ± 1% and 35 ± 1% for outer and inner features, respectively. Outer rings are mostly found in Hubble stages − 1 ≤ T ≤ 4. Inner rings are found in a broad distribution that covers the range − 1 ≤ T ≤ 7. We confirm that outer rings have two preferred orientations, namely parallel and perpendicular to the bar. We confirm a tendency for inner rings to be oriented parallel to the bar, but we report the existence of a significant fraction (maybe as large as 50%) of inner features that have random orientations with respect to the bar. These misaligned inner rings are mostly found in late-type galaxies (T ≥ 4). We find that the fraction of barred galaxies hosting outer (inner) rings is ~1.7 times (~1.3 times) that in unbarred galaxies. Conclusions. We confirm several results from previous surveys as well as predictions from simulations of resonant rings and/or from manifold flux tube theory. We report that a signifi, Unión Europea. FP7, CNES (Centre National d'Etudes Spatiales - France), NASA JPL/Spitzer, Acción Marie Curie "People Programme" (UE), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

This article has been accepted for publication in Monthly notices of the Royal Astronomical Society. © 2007 The Authors. Journal compilation © 2007 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. This paper has been supported by the Secretaría de Estado de Política Científica y Tecnológica (AYA2004-08251-C02-02, ESP2004-06870-C02-02, AYA2006-02358). This research has made use of NED which is operated by the JPL, Caltech, under contract with NASA. We have used observations made with the NASA/ESA HST, obtained from the data archive at the STScI. JJV acknowledges support from the Consejería de Educación y Ciencia de la Junta de Andalucía. A.C.M. acknowledges the support from the Ministerio de Educación y Ciencia. We also acknowledge the support of the RTN Euro3D: Promoting 3D spectroscopy in Europe. We are grateful to the anonymous referee for valuable comments that have helped to improve the quality of the paper., We report the discovery of a galactic wind in the central region of the galaxy M100. This result is based on a careful 2D spectroscopic study performed on observations made with the fibre system INTEGRAL on the William Herschel Telescope. The primary evidence of the wind is the presence of blueshifted interstellar NaD absorption lines. The velocity field of the absorbers show a clear rotation pattern but which is globally blueshifted (similar to -115 km s(-1)) with respect to the systemic velocity of the galaxy. The emission lines also present a blueward component arising from the ionized gas phase of the galactic wind. The velocity field of the ionized gas wind component shows no evidence of rotation but exhibits a pattern that can be interpreted in terms of the projection of an outflowing cone or shell. The wind component has [N II]/H alpha ratios of about 1.8, typical of shock ionization. The ionized component of the wind can be identified with an expanding shell of shocked gas, and the neutral component with disc gas entrained in the wind at the interface of the expanding shell with the galactic interstellar medium. The galactic wind seems to be driven uniquely by the nuclear starburst. Our analysis indicates that a non-negligible fraction of the wind material might escape to the intergalactic medium (IGM). In this case, if the wind detected in M100 were representative of similar phenomena in other galaxies with low to moderate activity, the current estimates of metal and dust content of the IGM might be drastically underestimated., Secretaría de Estado de Política Científica y Tecnológica, Consejería de Educación y Ciencia de la Junta de Andalucía, Ministerio de Educación y Ciencia, RTN Euro3D: Promoting 3D spectroscopy in Europe, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

The edge-on spiral galaxy NGC4013 has been mapped in the J=2-1 and 1-0 lines of (CO)-C-12 with the IRAM 30m telescope (HPBW 13'' and 21''). CO emission is detected within a galactocentric radius, R similar to 100'' (5.5 Kpc), The radial molecular gas distribution consists of a ring-like source (of radius r(ring) similar to 1.5 kPc)) and a fast rotating nuclear disk (of radius r(nucl) similar to 500 pc)., Unidad Deptal. de Astronomía y Geodesia, Fac. de Ciencias Matemáticas, TRUE, pub

© 2014. The American Astronomical Society. E.T. thanks Laura Ferrarese for very useful suggestions on ellipse-fitting and Tomer Tal, Guillermo Barro, and Michele Cappellari for very helpful discussions. E.T. and P.G. thank Alice Wu and Ajinkya Nene, students of the 2014 Science Internship Program (SIP) for high school students that takes place every summer at UCSC, for their contribution to this manuscript. The authors thank the anonymous referee for useful suggestions that helped improve the manuscript. E.T. acknowledges the financial support of the Fulbright Program jointly with the Spanish Ministry of Education. P.G. acknowledges the NSF grant AST-1010039. T.L. was supported within the framework of the Excellence Initiative by the German Research Foundation (DFG) through the Heidelberg Graduate School of Fundamental Physics (grant number GSC 129/1). R.F.P., J.F.B., G.v.d.V., E.L., and H.S. acknowledge the DAGAL network from the People Programme (Marie Curie Actions) of the European Unions Seventh Framework Programme FP7/2007 2013/ under REA grant agreement number PITN GA-2011-289313. J.J. thanks the ARC for financial support (DP130100388). G.H. acknowledges support by the FWF project P21097-N16. This work has made use of the GOLDMine database (Gavazzi et al. 2003) and the NASA/IPAC Extragalactic Database (NED.26), We present spatially resolved kinematics and global stellar populations and mass-to-light ratios for a sample of 39 dwarf early-type (dE) galaxies in the Virgo cluster studied as part of the SMAKCED stellar absorption-line spectroscopy and imaging survey. This sample is representative of the early-type population in the Virgo cluster in the absolute magnitude range -19.0 < M-r < -16.0 and of all morphological subclasses found in this galaxy population. For each dE, we measure the rotation curve and velocity dispersion profile and fit an analytic function to the rotation curve. We study the significance of the departure of the rotation curve from the best-fit analytic function (poorly fit) and of the difference between the approaching and receding sides of the rotation curve (asymmetry). Our sample includes two dEs with kinematically decoupled cores that have been previously reported. We find that 62 +/- 8% (23 out of the 39) of the dEs have a significant anomaly in their rotation curve. Analysis of the images reveals photometric anomalies for most galaxies. However, there is no clear correlation between the significance of the photometric and kinematic anomalies. We measure age-sensitive (H-beta and H-gamma A) and metallicity sensitive (Fe4668 and Mgb) Lick spectral indices in the LIS-5 angstrom system. This population of galaxies exhibits a wide range of ages and metallicities; we also find that 4 dEs show clear evidence of emission partially filling in the Balmer absorption lines. Finally, we estimate the total masses and dark matter fractions of the dEs and plot them in the mass-size, themass-velocity dispersion, and the fundamental plane scaling relations. The dEs seem to be the bridge between massive early-type galaxies and dSphs, and have a median total mass within the R-e of logM(e) = 9.1 +/- 0.2 and a median dark matter fraction within the R-e of f(DM) = 46 +/- 18%. Any formation model for the dE galaxy class must account for this diversity of kinematic and, Unión Europea. FP7, Fulbright Program, Ministerio de Educación, NSF, German Research Foundation (DFG) through the Heidelberg Graduate School of Fundamental Physics, DAGAL network from the People Programme (Marie Curie Actions) of the European Unions Seventh Framework Programme FP7/2007-2013/ under REA, ARC, FWF, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2003. Valuable discussions with A. Vazdekis, and J. J. González are gratefully acknowledged. The data employed in Appendix A was obtained with the 1m JKT, 2.5m INT and the 4.2m WHT at La Palma Observatory, and with the 3.5m Telescope at Calar Alto Observatory. The JKT, INT and WHT are operated on the island of La Palma by the Royal Greenwich Observatory at the Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. The Calar Alto Observatory is operated jointly by the Max-Planck-Institute fur Astronomie, Heidelberg, and the Spanish Comisión Nacional de Astronomía. This work was supported by the Spanish Programa Nacional de Astronomía y Astrofísica under grant AYA2000-977., It is well known that, when analyzed in the light of current synthesis model predictions, variations in the physical properties of single stellar populations (e.g. age, metallicity, initial mass function, element abundance ratios) may have a similar effect in their integrated spectral energy distributions. The confusion is even worsened when more realistic scenarios, i.e. composite star formation histories, are considered. This is, in fact, one of the major problems when facing the study of stellar populations in star clusters and galaxies. Typically, the observational efforts have aimed to find the most appropriate spectroscopic indicators in order to avoid, as far as possible, degeneracies in the parameter space. However, from a practical point of view, the most suited observables are not, necessarily, those that provide more orthogonality in that parameter space, but those that give the best balance between parameter degeneracy and sensitivity to signal-to-noise ratio per Angstrom, S/N(Angstrom). In order to achieve the minimum combined total error in the derived physical parameters, this work discusses how the functional dependence of typical line-strength indices and colors on S/N(Angstrom) allows to define a suitability parameter which helps to obtain more realistic combinations of spectroscopic data. As an example, we discuss in more detail the problem of breaking the well known age-metallicity degeneracy in relatively old stellar populations, comparing the suitability of different spectroscopic diagrams for a simple stellar population of solar metallicity and of 12 Gyr in age., Spanish Programa Nacional de Astronomía y Astrofísica, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2012 RAS. Artículo firmado por 24 autores. This work has been supported by the Programa Nacional de Astronomía y Astrofísica of the Spanish Ministry of Science and Innovation under grant AYA2010-21322-C03-02. We acknowledge financial support from the DAGAL network from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme FP7/2007-2013/ under REA grant agreement number PITN-GA-2011-289313.Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University., The mechanism causing breaks in the radial surface brightness distribution of spiral galaxies is not yet well known. Despite theoretical efforts, there is not a unique explanation for these features and the observational results are not conclusive. In an attempt to address this problem, we have selected a sample of 34 highly inclined spiral galaxies present both in the Sloan Digital Sky Survey and in the Spitzer Survey of Stellar Structure in Galaxies. We have measured the surface brightness profiles in the five Sloan optical bands and in the 3.6µm Spitzer band. We have also calculated the color and stellar surface mass density profiles using the available photometric information, finding two differentiated features: an innermost break radius at distances of ∼ 8 ± 1 kpc [0.77 ± 0.06 R_25] and a second characteristic radius, or truncation radius, close to the outermost optical extent (∼ 14 ± 2 kpc [1.09 ± 0.05 R_25]) of the galaxy. We propose in this work that the breaks might be a phenomena related to a threshold in the star formation, while truncations are more likely a real drop in the stellar mass density of the disk associated with the maximum angular momentum of the stars., Unión Europea. FP7, Ministerio de Economía y Competitividad (MINECO), Programa Nacional de Astronomía y Astrofísica, España, Alfred P. Sloan Foundation, National Science Foundation (NFS), EE.UU., US Department of Energy Office of Science, University of Arizona, Carnegie Mellon University, Brookhaven National Laboratory, University of Cambridge, University of Florida, French Participation Group, German Participation Group, Brazilian Participation Group, Harvard University, Instituto de Astrofísica de Canarias (IAC), Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, Yale University, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2015. The American Astronomical Society. All rights reserved. Artículo firmado por 18 autores., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly notices of the Royal Astronomical Society following peer review. The version of record Gaseous-phase metallicities and stellar populations in the centres of barred galaxies is available online at: http://arxiv.org/pdf/1406.6885.pdf. © 0000 RAS. We received financial support through the Spanish research project AYA2010-21322-C03-03, from the Spanish Ministerio de Economía y Competitividad. PSB is supported by the Ministerio de Economía y Competitividad (MINECO) through its Ramón y Cajal program. IP acknowledges the support by the Spanish Ministerio de Economía y Competitividad (MINECO) (via grants AYA2010-21322-C03-02, AYA2010-21322-C03-03, AYA2007-67625-C02-02 and Consolider-Ingenio CSD2010-00064) and by the Junta de Andalucia (FQM-108)., Numerical simulations predict that bars represent a very important agent for triggering gas inflows, which in turn could lead to central star formation. Bars thus are thought to contribute to the formation of the bulge. This process changes both the gaseous-phase and the stellar-phase metallicities in the centres of galaxies. With the aim of quantifying the importance of this process, we present a comparative study of the gaseous-phase and stellar-phase metallicities in the centres of members of a sample of barred and unbarred galaxies from SDSS. We do not find a significant difference in the metallicity (neither gaseous nor stellar) between barred and unbarred galaxies, but we find different trends in the metallicities of early- and late-type galaxies, with larger differences in the metallicity in the early-type subsample. Our results contradict some previous research in this field, but we find a possible origin of the discrepancies between previous works and our results., Spanish research project from Spanish Ministerio de Economía y Competitividad, Ministerio de Economia y Competitividad (MINECO), Spanish Ministerio de Economiía y Competitividad (MINECO), Junta de Andalucía, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2003. The American Astronomical Society. This work was based on data obtained on the German Spanish Astronomical Centre, Calar Alto, operated by the Max-Planck-Institut for Astronomy, Heidelberg, jointly with the Spanish National Commission for Astronomy. It has profited from the GCN data base at NASA maintained by Scott Barthelmy, NASA. This paper is partly based on observations collected at the European Southern Observatory, La Silla and Paranal, Chile (ESO Programme 165.H- 0464). We thank the observers and the staff at ESO for performing the SOFI and the ISAAC observations. This study has made use of the SIMBAD database, operated at CDS, Strasbourg, France. S. K. acknowledges helpful comments by Johan Fynbo, Jens Hjorth, Attila Mészáros, Holger Pedersen, and Paul Vreeswijk. J. M. C. C. acknowledges the receipt of a FPI doctoral fellowship from Spain’s Ministerio de Ciencia y Tecnología. We thank an anonymous referee for a prompt and very helpful reply., We report rapid follow-up K'-band observations of the error box of the bright High Energy Transient Explorer burst GRB 020819. We find that any afterglow was fainter than K' = 19 only 9 hr after the burst. Because no optical afterglow was found, GRB 020819 represents a typical "dark burst.'' At first, we discuss if extinction by cosmic dust in the GRB host galaxy could explain the faintness of the afterglow of GRB 020819. We then turn to the entire ensemble of K-band dark afterglows. We find that extinction by cosmic dust in the GRB host galaxies is still a possible explanation for the faintness of many afterglows. In all investigated cases a combination of only a modest extinction with a modest redshift can explain the observations. However, the required extinction is very high if these bursts occurred at redshifts smaller than unity, perhaps arguing for alternative models to explain the nature of the dark bursts., FPI doctoral fellowship from Spain’s Ministerio de Ciencia y Tecnología, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2015. The American Astronomical Society. All rights reserved. This research used data collected with the Subaru Telescope operated by the National Astronomical Observatory of Japan and with the GALEX operated for NASA by the Caltech under NASA contract NAS5-98034, and used the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, Caltech, under contract with NASA. We thank an anonymous referee for constructive comments, Fumiaki Nakata for help in observations, Eric Greisen for HI data, and the Pan-STARRS1 Surveys collaboration for the photometric catalog. This research is supported by NASA through grant NNX14AF74G. J.K. also acknowledges support from the NSF (AST-1211680)., We report the discovery of a new dwarf galaxy (NGC 6503-d1) during the Subaru extended ultraviolet disk survey. It is a likely companion of the spiral galaxy NGC 6503. The resolved images, in the B, V, R, i, and H alpha bands, show an irregular appearance due to bright stars with underlying, smooth and unresolved stellar emission. It is classified as the transition type (dwarf irregular (dIrr)/dwarf spheroidal (dSph)) between the dIrr and dSph types. Its structural properties are similar to those of the dwarfs in the Local Group, with an absolute magnitude M-V similar to -10.5, half-light radius r(e) similar to 400 pc, and central surface brightness mu(0,V) similar to 25.2. Despite the low stellar surface brightness environment, one H II region was detected, though its H alpha luminosity is low, indicating an absence of any appreciable O-stars at the current epoch. The presence of multiple stellar populations is indicated by the color-magnitude diagram of similar to 300 bright resolved stars and the total colors of the dwarf, with the majority of its total stellar mass similar to 4 x 10(6) M-circle dot in an old stellar population., Caltech under NASA, NASA, NSF, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2005. The American Astronomical Society. All rights reserved. We thank an unknown referee for his/her criticism. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA’s support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d’Etudes Spatiales of France and the Korean Ministry of Science and Technology. The authors would like to take this opportunity to thank the members of the GALEX SODA team for their valiant efforts in the timely reduction of the complex observational data set covering the full expanse of the Virgo Cluster., We study the UV properties of a volume-limited sample of early-type galaxies in the Virgo Cluster combining new GALEX far-ultraviolet (1530 Å) and near-ultraviolet (2310 Å) data with spectrophotometric data available at other wavelengths. The sample includes 264 elliptical, lenticular, and dwarf galaxies spanning a large range in luminosity (M_B ≤ -15). While the NUV to optical or near-IR color-magnitude relations (CMRs) are similar to those observed at optical wavelengths, with a monotonic reddening of the color index with increasing luminosity, the (FUV - V) and (FUV - H) CMRs show a discontinuity between massive and dwarf objects. An even more pronounced dichotomy is observed in the (FUV - NUV) CMR. For elliptical galaxies, the (FUV - NUV) color becomes bluer with increasing luminosity and with increasing reddening of the optical or near-IR color indices. For the dwarfs, the opposite trend is observed. These observational evidences are consistent with the idea that the UV emission is dominated by hot, evolved stars in giant systems, while in dwarf ellipticals residual star formation activity is more common., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO, 2012. We thank the Viabilidad, Diseño, Acceso y Mejora funding programme, ICTS-2009-10, of the Spanish Ministerio de Ciencia e Innovación, for the support given to this project. This paper makes use of the Sloan Digital Sky Survey data. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. Finally, we want to thank the anonymous referee for useful comments that helped us to improve the article considerably., Context. We carry out a detailed 2-D study of the ionised gas in the local universe galaxy UGC 9837. In nearby galaxies, like the galaxy in question here, the spatial distribution of the physical properties can be studied in detail, providing benchmarks for galaxy formation models. Aims. Our aim is to derive detailed and spatially resolved physical properties of the ionised gas of UGC 9837. In addition, we derive an integrated spectrum of the galaxy and study how varying spatial coverage affects the derived integrated properties. We also study how the same properties would be seen if the galaxy was placed at a higher redshift and observed as part of one of the high-z surveys. Methods. UGC 9837 was observed using the PMAS PPAK integral-field unit. The spectra were reduced and calibrated and the stellar and ionised components separated. Using strong emission line ratios of the ionised gas, the source of ionisation, the dust extinction, the star formation rate, the electron density, and the oxygen abundance derived from a total integrated spectrum, central integrated spectrum, and individual fibre spectra are studied. Finally, the same properties are studied in a spectrum whose spatial resolution is degraded to simulate high-z observations. Results. The spatial distribution of the ionised gas properties is consistent with inside-out growing scenario of galaxies. We also find that lack of spatial coverage would bias the results derived from the integrated spectrum leading, e.g., to an underestimation of ionisation and overestimation of metallicity, if only the centre of the galaxy was covered by the spectrum. Our simulation of high-z observations shows that part of the spatial information, such as dust and SFR distribution would be lost, while shallower gradients in metallicity and ionisation strength would be detected., Ministerio de Ciencia e Innovación (MICINN), España, Alfred P. Sloan Foundation, National Science Foundation (NSF), EE.UU., U.S. Department of Energy, National Aeronautics and Space Administration (NASA), Japanese Monbukagakusho, Max Planck Society, Higher Education Funding Council for England, Astrophysical Research Consortium, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO, 2010 Artículo firmado por 35 autores. We thank the following people for providing various data sets/information to us: D. Clowe (Magellan/IMACS images), S. M. Chung and A. H. González (IMACS spectroscopic redshifts), J.-G. Cuby (VLT/HAWKI images), D. Johansson, C. Horellou, and the LABOCA team (LABOCA map), and D. Hughes, I. Aretxaga, and the AzTEC team (AzTEC map and far-infrared photometric redshifts). We thank the NASA Herschel Science Center for its excellent user support, and the International Space Science Institute in Berne for their support through the International team 181. EE would like to thank D. Elbaz for communicating his results before publication. This work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech., The Herschel Lensing Survey (HLS) will conduct deep PACS and SPIRE imaging of ~40 massive clusters of galaxies. The strong gravitational lensing power of these clusters will enable us to penetrate through the confusion noise, which sets the ultimate limit on our ability to probe the Universe with Herschel. Here we present an overview of our survey and a summary of the major results from our science demonstration phase (SDP) observations of the Bullet cluster (z = 0.297). The SDP data are rich and allow us to study not only the background high-redshift galaxies (e. g., strongly lensed and distorted galaxies at z = 2.8 and 3.2) but also the properties of cluster-member galaxies. Our preliminary analysis shows a great diversity of far-infrared/submillimeter spectral energy distributions (SEDs), indicating that we have much to learn with Herschel about the properties of galaxy SEDs. We have also detected the Sunyaev-Zel'dovich (SZ) effect increment with the SPIRE data. The success of this SDP program demonstrates the great potential of the Herschel Lensing Survey to produce exciting results in a variety of science areas., National Aeronautics and Space Administration (NASA), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2011 The Authors. © 201Monthly Notices of the Royal Astronomical Society. © 2011 RAS. CRA acknowledges financial support from STFC PDRA (ST/G001758/1). CRA, PGPG and GB acknowledge the Spanish Ministry of Science and Innovation (MICINN) through project Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC (http://www.iac.es/consolider-ingenio-gtc/). PGPG and GB acknowledge support from the Spanish Programa Nacional de Astronomía y Astrofísica under grants AYA2009-10368 and AYA2009-07723-E. KJI is supported through the Emmy Noether programme of the German Science Foundation (DFG). This work has made use of the Rainbow Cosmological Surveys Data base, which is operated by the Universidad Complutense de Madrid (UCM). This work is based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. This research has made use of the NED which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The authors specially acknowledge Tomer Tal for providing access to the OBEY images, as well as David Carter, Richard Pogge, Philip Massey, Giovanni Carraro and Carlos López SanJuan for their valuable help. We finally acknowledge useful comments from the anonymous referee., We present the results of a comparison between the optical morphologies of a complete sample of 46 southern 2 Jy radio galaxies at intermediate redshifts (0.05 < z < 0.7) and those of two control samples of quiescent early-type galaxies: 55 ellipticals at redshifts z ≤ 0.01 from the Observations of Bright Ellipticals at Yale (OBEY) survey, and 107 early-type galaxies at redshifts 0.2 < z < 0.7 in the Extended Groth Strip (EGS). Based on these comparisons, we discuss the role of galaxy interactions in the triggering of powerful radio galaxies (PRGs). We find that a significant fraction of quiescent ellipticals at low and intermediate redshifts show evidence for disturbed morphologies at relatively high surface brightness levels, which are likely the result of past or on-going galaxy interactions. However, the morphological features detected in the galaxy hosts of the PRGs (e.g. tidal tails, shells, bridges, etc.) are up to 2 mag brighter than those present in their quiescent counterparts. Indeed, if we consider the same surface brightness limits, the fraction of disturbed morphologies is considerably smaller in the quiescent population (53 per cent at z < 0.2 and 48 per cent at 0.2 ≤ z < 0.7) than in the PRGs (93 per cent at z < 0.2 and 95 per cent at 0.2 ≤ z < 0.7 considering strong-line radio galaxies only). This supports a scenario in which PRGs represent a fleeting active phase of a subset of the elliptical galaxies that have recently undergone mergers/interactions. However, we demonstrate that only a small proportion (≲20 per cent) of disturbed early-type galaxies are capable of hosting powerful radio sources., Ministerio de Ciencia e Innovación (MICINN), Science and Technology Facilities Council (STFC), Reino Unido, Programa Nacional de Astronomía y Astrofísica (PNAyA), España, Deutsche Forschungsgemeinschaft (DFG), Alemania, National Aeronautics and Space Administration (NASA), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2008. We thank the anonymous referee for suggestions that improved the paper and Ignacio Trujillo, Carlos López, David Abreu, Marc Vallbe, Enrique García Dabo, Alfonso Aragón Salamanca, David Koo, and Reynier Peletier, for useful discussions. This work was supported by the Spanish Programa Nacional de Astronomía y Astrofísica through project number AYA2006-12955. Some/all of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NAG5-7584 and by other grants and contracts. This work uses data obtained with support of the National Science Foundation grants AST 95-29028 and AST 00-71198., Context. Analysis of bulges to redshifts of up to z∽1 have provided ambiguous results as to whether bulges as a class are old structures akin to elliptical galaxies or younger products of the evolution of their host disks. Aims. We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. Methods. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 (Wide-Field Planetary Camera 2 at the Hubble Space Telescope) Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measures quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85 kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6 '' diameter apertures. Colour transformations and K-corrections are calculated using SEDs covering bands UBVIJK, from the GOYA photometric survey. Results. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1 < z < 1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and rest-frame) and magnitudes (apparent and absolute), as well a, Programa Nacional de Astronomia y Astrofisica (PNAYA), España, NASA, Ministerio de Economía y Competitividad (MINECO), España, National Science Foundation (NFS), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO, 2011. We thank the referee, Matt Bershady, for his useful comments. We acknowledge the Viabilidad, Diseño, Acceso y Mejora funding program, ICTS-2009-10, and the Plan Nacional de Investigación y Desarrollo funding program AYA2010-22111-C03-03 and AYA-2010-10904-E, of the Spanish Ministerio de Ciencia e Innovación (MICINN), for the support given to this project. E.M.Q. acknowledges financial support from the research projects AYA2007-67752-C03-03 and AYA2010-21322-C03-02. E.M.Q., R.M. and A.G.P. thank support from Consolider-GTC and AstroMadrid S2009/ESP-1496 - from the Comunidad de Madrid -. R.M. and A.G.P. acknowledge financial support from the project AYA2005-09413-C02-02. J.V.M. and J.I.P. are funded by the grants AYA2007-67965-C03-02 - from the Spanish MICINN and TIC114 - from the Junta de Andalucía -. We also thank the director of CEFCA, Dr. M. Moles, for his sincere support of this project. This paper makes use of the Sloan Digital Sky Survey data. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max, Aims. Integral field spectroscopy (IFS) is a powerful approach to studying nearby galaxies since it enables a detailed analysis of their resolved physical properties. Here we present our study of a sample of nearby galaxies selected to exploit the two-dimensional information provided by the IFS. Methods. We observed a sample of 48 galaxies from the local universe with the PPaK integral field spectroscopy unit (IFU), of the PMAS spectrograph, mounted at the 3.5 m telescope at Calar Alto Observatory (Almeria, Spain). Two different setups were used during these studies (low – V300 – and medium – V600 – resolution mode) covering a spectral range of around 3700–7000 ÅÅ. We developed a full automatic pipeline for the data reduction, which includes an analysis of the quality of the final data products. We applied a decoupling method to obtain the ionised gas and stellar content of these galaxies, and derive the main physical properties of the galaxies. To assess the accuracy in the measurements of the different parameters, we performed a set of simulations to derive the expected relative errors obtained with these data. In addition, we extracted spectra for two types of aperture, one central and another integrated over the entire galaxy, from the datacubes. The main properties of the stellar populations and ionised gas of these galaxies and an estimate of their relative errors are derived from those spectra, as well as from the whole datacubes. Results. We compare the central spectrum extracted from our datacubes and the SDSS spectrum for each of the galaxies for which this is possible, and find close agreement between the derived values for both samples. We find differences on the properties of galaxies when comparing a central and an integrated spectra, showing the effects of the extracted aperture on the interpretation of the data. Finally, we present two-dimensional maps of some of the main properties derived with the decoupling procedure., Comunidad de Madrid, Ministerio de Ciencia e Innovación (MICINN), Junta de Andalucia, Alfred P. Sloan Foundation, National Science Foundation, US Department of Energy, National Aeronautics and Space Administration (NASA), Japanese Monbukagakusho, Max Planck Society, Higher Education Funding Council for England, Viabilidad, Diseño, Acceso y Mejora funding program, Astrophysical Research Consortium, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2007. The American Astronomical Society. All rights reserved. Artículo firmado por 26 autores. We wish to acknowledge Jakob Walcher for kindly extracting for us useful data from stochastic realizations of star formation models. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA’s support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d’Etudes Spatiales of France and the Korean Ministry of Science and Technology. The grating, window, and aspheric corrector were supplied by France. We acknowledge the dedicated team of engineers, technicians, and administrative staff from JPL/Caltech; Orbital Sciences Corporation; University of California, Berkeley; Laboratory Astrophysique Marseille; and the other institutions who made this mission possible. This work was partly supported by grant R01-2006-000-10716-0 (SKY) from the Basic Research Program of the Korea Science and Engineering Foundation. A. G. d. P. is financed by the MAGPOP EU Marie Curie Research Training Network., We use GALEX/optical photometry to construct color-color relationships for early-type galaxies sorted by morphological type. We have matched objects in the GALEX GR1 public release and the first IR1.1 internal release, with the RC3 early-type galaxies having a morphological type -5.5 ≤ T < − 1.5, with mean error on T < 1.5 and mean error on (B − V)_T < 0.05. After visual inspection of each match, we are left with 130 galaxies with reliable GALEX pipeline photometry in the far-UV and near-UV bands. This sample is divided into ellipticals (-5.5 ≤ T < − 3.5) and lenticulars (-3.5 ≤ T < − 1.5). After correction for Galactic extinction, the color-color diagrams FUV − NUV versus (B − V)_Tc are plotted for the two subsamples. We find a tight anticorrelation between the FUV − NUV and (B − V)Tc colors for ellipticals, with the UV color getting bluer when the (B − V)Tc gets redder. This relationship very likely is an extension of the color-metallicity relationship in the GALEX NUV band. We suspect that the main source of the correlation is metal line blanketing in the NUV band. The FUV − NUV versus B − V correlation has larger scatter for lenticular galaxies; we speculate that this reflects the presence of low-level star formation. If the latter objects (i.e., those that are blue both in FUV − NUV and in B − V) are interpreted as harboring recent star formation activity, this would be the case for a few percent (~4%) of ellipticals and ~15% of lenticulars; this would mean about 10% of early-type galaxies have residual star formation in our full sample of 130 early-type galaxies. We also plot FUV − NUV versus the Mg2 index and central velocity dispersion. We find a tight anticorrelation between FUV − NUV and the Mg2 index; we suspect that this reflects blanketing in the NUV band being correlated with overall metallicity. We find a marginal anticorrelation of FUV − V_T with Mg_2 for elliptical galaxies., Korea Science and Engineering Foundation, Marie Curie Action Research Training Network, Unión Europea. FP6, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© The American Astronomical Society. We thank the IAC for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN and the Spanish CICYT is gratefully acknowledged. This work was also supported by ETH Research Grant TH 34/04 3 and the Polish MNiI Grant 1P03D01028., Using the Major Atmospheric Gamma Imaging Cerenkov Telescope ( MAGIC), we have observed the nearest ultraluminous infrared galaxy, Arp 220, for about 15 hr. No significant signal was detected within the dedicated amount of observation time. The first upper limits to the very high energy gamma-ray flux of Arp 220 are herein reported and compared with theoretical expectations., German BMBF, German MPG, Italian INFN, Spanish CICYT, ETH, Polish MNiI, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

This article has been accepted for publication in Monthly notices of the Royal Astronomical Society © 2014 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. DZ acknowledges financial support from NASA ADAP NNX12AE27G and NYU CCPP for its hospitality during long-term visits. The authors acknowledge the support from the FP7 Marie Curie Actions of the European Commission, via the Initial Training Network DAGAL under REA grant agreement PITN-GA-2011-289313. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA., We extend our initial study of the connection between the UV colour of galaxies and both the inferred stellar mass-to-light ratio, Upsilon(*), and a mass-to-light ratio referenced to Salpeter initial mass function (IMF) models of the same age and metallicity, Upsilon(*)/Upsilon(Sal), using new UV magnitude measurements for a much larger sample of early-type galaxies, ETGs, with dynamically determined mass-to-light ratios. We confirm the principal empirical finding of our first study, a strong correlation between the GALEX FUV-NUV colour and Upsilon(*). We show that this finding is not the result of spectral distortions limited to a single passband (e.g. metallicity-dependent line-blanketing in the NUV band), or of the analysis methodology used to measure Upsilon(*), or of the inclusion or exclusion of the correction for stellar population effects as accounted for using Upsilon(*)/Upsilon(Sal). The sense of the correlation is that galaxies with larger Upsilon(*), or larger Upsilon(*)/Upsilon(Sal), are bluer in the UV. We conjecture that differences in the low-mass end of the stellar IMF are related to the nature of the extreme horizontal branch stars generally responsible for the UV flux in ETGs. If so, then UV colour can be used to identify ETGs with particular IMF properties and to estimate Upsilon(*). We also demonstrate that UV colour can be used to decrease the scatter about the Fundamental Plane and Manifold, and to select peculiar galaxies for follow-up with which to further explore the cause of variations in Upsilon(*) and UV colour., Unión Europea. FP7, NASA ADAP, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

We present the first detection of the [NII] 122 mu m and [O III ] 52 mu m lines for a reionization-epoch galaxy. Based on these lines and previous [C II ] 158 mu m and [O III ] 88 mu m measurements, using two different radiati ve transfer models of the interstellar medium, we estimate an upper limit on electron density of < 500 cm(-3) and an approximate gas-phase metallicity of Z/Z(circle dot) similar to 1.1 +/- 0.2 for A1689-zD1, a gravitationally lensed dusty galaxy at z = 7.133. Other measurements or indicators of metallicity so far in galaxy interstellar media at z greater than or similar to 6 are typically an order of magnitude lower than this. The unusually high metallicity makes A1689-zD1 inconsistent with the fundamental metallicity relation, although there is likely significant dust obscuration of the stellar mass, which may partly resolve the inconsistency. Given a solar metallicity, the dust-to-metals ratio is a factor of several lower than expected, hinting that galaxies be yond z similar to 7 may hav e lower dust formation efficiency . Finally , the inferred nitrogen enrichment compared to oxygen, on which the metallicity measurement depends, indicates that star formation in the system is older than about 250 Myr, pushing the beginnings of this galaxy to z > 10.

Context. Determining when the first galaxies formed remains an outstanding goal of modern observational astronomy. Theory and current stellar population models imply that the first galaxies formed at least at z = 14 15. But to date, only one galaxy at z > 13 (GS-z13-0) has been spectroscopically confirmed.Aims. The galaxy `HD1' was recently proposed to be a z similar to 13:27 galaxy based on its potential Lyman break and tentative [O iii] 88 mu m detection with ALMA. We hereby aim to test this scenario with new ALMA Band 4 observations of what would be the [C II] 158 mu m emission if HD1 is at z similar to 13:27.Methods. We carefully analyse the new ALMA Band 4 observations and re-analyse the existing ALMA Band 6 data on the source to determine the proposed redshift.Results. We find a tentative 4 sigma feature in the Band 4 data that is spatially o ffset by 1:'' 7 and spectrally o ffset by 190 km s(-1) from the previously reported 3.8 sigma `[O III] 88 mu m' feature. Through various statistical tests, we demonstrate that these tentative features are fully consistent with both being random noise features.Conclusions. We conclude that we are more likely to be recovering noise features than both [O III] 88 mu m and [C II] 158 mu m emission from a source at z similar to 13 :27. Although we find no credible evidence of a z similar to 13 :27 galaxy, we cannot entirely rule out this scenario. Non-detections are also possible for a z similar to 13 source with a low interstellar gas-phase metallicity or ionisation parameter and/or high gas density. Moreover, the new continuum and line upper limits provide no strong evidence for or against a lower-redshift scenario. Determining where and exactly what type of galaxy HD1 is, will now likely require JWST /NIRSpec spectroscopy.

Star-forming and starburst galaxies (SBGs), which are well-known cosmic-ray (CR) reservoirs, are expected to emit gamma rays and neutrinos predominantly via hadronic collisions. In this work we analyze the 10-year Fermi-Low Energy Technique (LAT) spectral energy distributions of 13 nearby galaxies by means of a physical model that accounts for high-energy proton transport in starburst nuclei and includes the contribution of primary and secondary electrons. In particular, we test the hypothesis that the observed gamma-ray fluxes are mostly due to star-forming activity, which is in agreement with the available star formation rates coming from infrared (IR) and ultraviolet (UV) observations. Through this observation-based approach, we determine the most-likely neutrino counterparts from star-forming and SBGs and quantitatively assess the ability of current and upcoming neutrino telescopes to detect them as point-like sources. We also generate mock gamma-ray data to simulate the Cherenkov Telescope Array (CTA) performance in detecting these sources. Moreover, we propose a test to discriminate between the two different CR transport models for the starburst nuclei by looking at the different gamma-ray expectations. We point out that current data already gives a slight preference to CR models, which are dominated by advection.

How passive galaxies form, and the physical mechanisms which prevent star formation over long timescales, are some of the most outstanding questions in understanding galaxy evolution. The properties of quiescent galaxies over cosmic time provide crucial information to identify the quenching mechanisms. Passive galaxies have been confirmed and studied out to z similar to 4, but all of these studies have been limited to massive systems (mostly with log(M-star/M-2) > 10.8). Using JWST-NIRISS grism slitless spectroscopic data from the GLASS-JWST Early Release Science program, we present spectroscopic confirmation of two quiescent galaxies at z(spec) = 2.650(-0.006)(+0.004) and -z(spec) = 2.433(-0.016)(+0.032) (3 sigma errors) with -stellar masses of ( log M-star/M-?) = 10.59(-0.05)(+0.11) and ( log M-star/M-?) = 10.07(-0.03)(+0.06) -(corrected for magnification factors of mu = 2.0 and mu = 2.1, respectively). The latter represents the first spectroscopic confirmation of the existence of low-mass quiescent galaxies at cosmic noon, showcasing the power of JWST to identify and characterize this enigmatic population.

We present the combination of the Canada-France-Hawaii Telescope (CHFT) Large Area U-bands Deep Survey (CLAUDS) and the Hyper-Suprime-Cam (HSC) Subaru Strategic Program (HSC-SSP) data over their four deep fields. We provide photometric catalogs for u, u* (CFHT-MegaCam), g, r, i, z, and y (Subaru-HSC) bands over similar to 20 deg(2), complemented in two fields by data from the Visible and Infrared Survey Telescope for Astronomy (VISTA) Deep Extragalactic Observations (VIDEO) survey and the UltraVISTA survey, thus extending the wavelength coverage toward near-infrared with VIRCAM Y, J, H, and K-s observations over 5.5 deg(2). The extraction of the photometry was performed with two different softwares: the HSC pipeline hscPipe and the standard and robust SExtractor software. Photometric redshifts were computed with template-fitting methods using the new Phosphoros code for the hscPipe photometry and the well-known Le Phare code for the SExtractor photometry. The products of these methods were compared with each other in detail. We assessed their quality using the large spectroscopic sample available in those regions, together with photometry and photometric redshifts from COSMOS2020, the latest version of the Cosmic Evolution Survey catalogs. We find that both photometric data sets are in good agreement in Ugrizy down to magnitude similar to 26, and to magnitude similar to 24.5 in the YJHK(s) bands. We achieve good performance for the photometric redshifts, reaching precisions of sigma(NMAD) less than or similar to 0.04 down to m(i) similar to 25, even using only the CLAUDS and HSC bands. At the same magnitude limit, we measured an outlier fraction of eta less than or similar to 10% when using the Ugrizy bands, and down to eta less than or similar to 6% when considering near-infrared data. The hscPipe plus Phosphoros pipeline performs slightly worse in terms of photometric-redshifts precision and outlier fraction than its SExtractor plus Le Phare counterpart, which

Short gamma-ray bursts (SGRBs) are produced by the coalescence of compact binary systems which are remnants of massive stars. GRB 160410A is classified as a short-duration GRB with extended emission and is currently the farthest SGRB with a redshift determined from an afterglow spectrum and also one of the brightest SGRBs to date. The fast reaction to the Neil Gehrels Swift Observatory alert allowed us to obtain a spectrum of the afterglow using the X-shooter spectrograph at the Very Large Telescope (VLT). The spectrum shows several absorption features at a redshift of z = 1.7177, in addition, we detect two intervening systems at z = 1.581 and z = 1.444. The spectrum shows Ly alpha in absorption with a column density of log (N(H i)/cm(2)) = 21.2 +/- 0.2 which, together with Fe ii, C ii, Si ii, Al ii, and O i, allow us to perform the first study of chemical abundances in a SGRB host galaxy. We determine a metallicity of [X/H] = -2.3 +/- 0.2 for Fe ii and -2.5 +/- 0.2 for Si ii and no dust depletion. We also find no evidence for extinction in the afterglow spectral energy distribution modelling. The environment has a low degree of ionization and the C iv and Si iv lines are completely absent. We do not detect an underlying host galaxy down to deep limits. Additionally, we compare GRB 160410A to GRB 201221D, another high-z short GRB that shows absorption lines at z = 1.045 and an underlying massive host galaxy.

We present a pilot, untargeted extragalactic carbon monoxide (CO) emission-line survey using ALMACAL, a project utilizing ALMA calibration data for scientific purposes. In 33 deep (T-exp' > 40 min) ALMACAL fields, we report six CO emission-line detections above S/N > 4, one-third confirmed by MUSE observations. With this pilot survey, we probe a cosmologically significant volume of similar to 10(5) cMpc(3), widely distributed over many pointings in the southern sky, making the survey largely insusceptible to the effects of cosmic variance. We derive the redshift probability of the CO detections using probability functions from the SHARK semi-analytical model of galaxy formation. By assuming typical CO excitations for the detections, we put constraints on the cosmic molecular gas mass density evolution over the redshift range 0 < z < 1.5. The results of our pilot survey are consistent with the findings of other untargeted emission-line surveys and the theoretical model predictions and currently cannot rule out a non-evolving molecular gas mass density. Our study demonstrates the potential of using ALMA calibrator fields as a multi-sightline untargeted CO emission-line survey. Applying this approach to the full ALMACAL database will provide an accurate, free of cosmic variance, measurement of the molecular luminosity function as a function of redshift.

Analysis of a large galaxy sample shows that black hole activity is greater in galaxies in which the stellar and gas kinematics are misaligned. This observation suggests that the misalignment, driven by external gas accretion, fuels the central supermassive black holes.External accretion events such as a galaxy merger or the accretion of gas from the immediate environment of a galaxy can create a large misalignment between the gas and the stellar kinematics. Numerical simulations have suggested that misaligned structures may promote the inflow of gas to the nucleus of the galaxy and the accretion of gas by the central supermassive black hole. We show for the first time that galaxies with a strong misalignment between the ionized gas and stellar kinematic angles have a higher observed fraction of active black holes than galaxies with aligned rotation of gas and stars. The increase in black hole activity suggests that the process of formation and/or the presence of misaligned structures are connected with the fuelling of active supermassive black holes.