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© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Artículo firmado por 19 autores. Herschel is a European Space Agency (ESA) space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. TDR was supported by an ESA Research Fellowship at the European Space Astronomy Centre (ESAC), in Madrid, Spain. RJI acknowledges support from the ERC in the form of the Advanced Investigator Program, 321302, COSMICISM. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson Merit Award.; Based on observations made with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programmes #11689, 13389, 13495, 13496, 13498, 13504. This publication also uses data products from the Wide-field Infrared Survey Explorer ( WISE), which is a joint project of UCLA and JPL, Caltech, funded by NASA. This research made use of the NASA/IPAC Infrared Science Archive, which is operated by JPL, Caltech, under contract with NASA.; We made use of a private version of the Rainbow Cosmological Surveys Database, operated by the Universidad Complutense de Madrid (UCM), and PGP-G acknowledges support from Spanish Government MINECO grant AYA2012-31277.; This work also utilizes gravitational lensing models produced by PIs Ebeling (CATS) and Merten & Zitrin, funded as part of the HST Frontier Fields program conducted by STScI. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. The lens models were obtained from the Mikulski Archive for Space Telescopes (MAST)., We present a complete census of all Herschel-detected sources within the six massive lensing clusters of the HST Frontier Fields (HFF). We provide a robust legacy catalogue of 263 sources with Herschel fluxes, primarily based on imaging from the Herschel Lensing Survey and PEP/HerMES Key Programmes. We optimally combine Herschel, Spitzer and WISE infrared (IR) photometry with data from HST, VLA and ground-based observatories, identifying counterparts to gain source redshifts. For each Herschel-detected source we also present magnification factor (mu), intrinsic IR luminosity and characteristic dust temperature, providing a comprehensive view of dust-obscured star formation within the HFF. We demonstrate the utility of our catalogues through an exploratory overview of the magnified population, including more than 20 background sub-LIRGs unreachable by Herschel without the assistance gravitational lensing., Unión Europea. FP7, Ministerio de Economía y Competitividad (MINECO), ERC Advanced Investigator programme DUSTYGAL, ESA Research Fellowship at the European Space Astronomy Centre (ESAC), in Madrid, Spain, European Research Council (ERC), Science and Technology Facilities Council (STFC), Reino Unido, Royal Society, Reino Unido, National Aeronautics and Space Administration (NASA), Gobierno de España, HST Frontier Fields program, Hubble Space Telescopy (HST), Royal Society Wolfson Research Merit Award, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2001. This paper is based on observations obtained at the German-Spanish Astronomical Centre, Calar Alto, Spain, operated by the Max-Planck Institute für Astronomie (MPIE), Heidelberg, jointly with the Spanish Commission for Astronomy. It is also partly based on observations made with the Jacobus Kapteyn 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 de Astrofísica de Canarias and the 1.52 m telescope of the EOCA/OAN 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. We have also use of the LEDA database, http://www-obs.univ-lyon1.fr. This research was also supported by the Spanish Programa Sectorial de Promoción General del Conocimiento under grants PB96-0610 and PB96- 0645. P. G. Pérez González acknowledges the receipt of a “Formación de Profesorado Universitario” fellowship from the Spanish “Ministerio de Educación y Cultura”. We would like to thank C. E. García Dabó and S. Pascual for their help during part of the observing runs and stimulating conversations. We thank M. N. Estévez for carefully reading the manuscript and making some useful remarks. We are also grateful to Dr. E. Emsellem for his helpful comments and suggestions., We present Johnson B surface photometry for the UCM Survey galaxies. One-dimensional bulge-disk decomposition is attempted, discussing on fitting functions and computational procedures. The results from this decomposition, jointly with concentration indices and an asymmetry coefficient, are employed to study the morphological properties of these galaxies. We also compare our results with the previous morphological classification established using Gunn r imaging data and with other samples of galaxies. No major statistical differences in morphology are found between red and blue data, although some characteristics such as size and luminosity concentration vary. We find a correlation between luminosity and size. Several parameters are used to segregate the objects according to their morphological type., National Aeronautics and Space Administration (NASA), Programa Sectorial de Promoción General del Conocimiento (MEC), España, Ministerio de Educación y Cultura (MEC), España, Programa Formación de Profesorado Universitario (MEC), España, 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. The authors are grateful to the anonymous referee for helpful comments, M. Krumpe for discussions that improved this paper, J. Aird for providing optical identifications of X-ray sources and O. Ilbert for making available photometric redshift PDFs for galaxies in the COSMOS survey field. GM acknowledges financial support from the Marie-Curie Reintegration Grant PERG03-GA-2008-230644 and the THALES project 383549, which is jointly funded by the European Union and the Greek Government in the framework of the programme 'Education and lifelong learning'. PGP-G acknowledges support from the Spanish Programa Nacional de Astronomía y Astrofísica under grant AYA2012-31277. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM), partnered with the University of California Observatories at Santa Cruz (UCO/Lick,UCSC). Funding for the DEEP2 Galaxy Redshift Survey has been provided in part by NSF grants AST95-09298, AST-0071048, AST-0071198, AST-0507428, and AST-0507483 as well as NASA LTSA grant NNG04GC89G. Funding for the DEEP3 Galaxy Redshift Survey has been provided by NSF grants AST-0808133, AST-0807630, and AST-0806732. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada France Hawaii Telescope which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the CFHTLS, a collaborative project of NRC and CNRS., We combine multi-wavelength data in the AEGIS-XD and C-COSMOS surveys to measure the typical dark matter halo mass of X-ray selected active galactic nuclei (AGN) [L_X(2–10 keV) > 10^42 erg s^− 1] in comparison with far-infrared selected star-forming galaxies detected in the Herschel/PEP survey (PACS Evolutionary Probe; L_IR > 10^11 L_⊙) and quiescent systems at z ≈ 1. We develop a novel method to measure the clustering of extragalactic populations that uses photometric redshift probability distribution functions in addition to any spectroscopy. This is advantageous in that all sources in the sample are used in the clustering analysis, not just the subset with secure spectroscopy. The method works best for large samples. The loss of accuracy because of the lack of spectroscopy is balanced by increasing the number of sources used to measure the clustering. We find that X-ray AGN, far-infrared selected star-forming galaxies and passive systems in the redshift interval 0.6 < z < 1.4 are found in haloes of similar mass, log M_DMH/(M_⊙ h^−1) ≈ 13.0. We argue that this is because the galaxies in all three samples (AGN, star-forming, passive) have similar stellar mass distributions, approximated by the J-band luminosity. Therefore, all galaxies that can potentially host X-ray AGN, because they have stellar masses in the appropriate range, live in dark matter haloes of log M_DMH/(M_⊙ h^−1) ≈ 13.0 independent of their star formation rates. This suggests that the stellar mass of X-ray AGN hosts is driving the observed clustering properties of this population. We also speculate that trends between AGN properties (e.g. luminosity, level of obscuration) and large-scale environment may be related to differences in the stellar mass of the host galaxies., Unión Europea. FP7, Programa Nacional de Astronomía y Astrofísica (PNAyA), MINECO, España, Gobierno de Grecia, National Science Foundation (NSF), EE.UU., National Aeronautics and Space Administration (NASA), EE.UU., Acciones Marie Skłodowska-Curie (UE), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2015. The American Astronomical Society. Artículo firmado por 25 autores. The authors would like to thank the referee for her/his valuable comments and helpful suggestions concerning the presentation of this paper, which helped to improve the manuscript. The work of A.C. is supported by the STARFORM Sinergia Project funded by the Swiss National Science Foundation, and also benefited from a MERAC Funding and Travel Award. A.C. acknowledges the kind hospitality of the Departamento de Astrofísica y ciencias de la Atmósfera, Universidad Complutense de Madrid, and of the Department d'Astronomia i Astrofisica, Universitat de Valencia. A.C. and E.R. are grateful to M. Cava for many useful discussions and suggestions. E.R. acknowledges the kind hospitality of the Observatoire de Geneve, Universite de Geneve. P.G.P.-G. acknowledges support from the Spanish Programa Nacional de Astronomía y Astrofísica under grants AYA2012-31277. A.V.G. acknowledges support from the ERC via an Advanced Grant under grant agreement no. 321323-NEOGAL. N.C. acknowledges support from the Spanish Ministry of Economy and Competitiveness under grant AYA2013-46724-P. A.A.H. and A.H.C. acknowledge financial support from the Spanish Ministry of Economy and Competitiveness through grant AYA2012-31447, which is partly funded by the FEDER program. A.J.C. is a Ramón y Cajal Fellow of the Spanish Ministry of Science and Innovation and acknowledges financial support from the Spanish Ministry of Economy and Competitiveness through grant AYA2012-30789, partly funded by the FEDER program. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM). Based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma., In this paper, we present a comprehensive analysis of star-forming galaxies (SFGs) at intermediate redshifts (z ~ 1). We combine the ultra-deep optical spectro-photometric data from the Survey for High-z Absorption Red and Dead Sources (SHARDS) with deep UV-to-FIR observations in the GOODS-N field. Exploiting two of the 25 SHARDS medium-band filters, F687W17 and F823W17, we select [O II] emission line galaxies at z ~ 0.84 and z ~ 1.23 and characterize their physical properties. Their rest-frame equivalent widths (EWrf([O ii])), line fluxes, luminosities, star formation rates (SFRs), and dust attenuation properties are investigated. The evolution of EW_rf([O II]) closely follows the SFR density evolution of the universe, with a trend of EW_rf([O II]) ∞ (1 + z)^3 up to redshift z ≃1, followed by a possible flattening. The SF properties of the galaxies selected on the basis of their [O II] emission are compared with complementary samples of SFGs selected by their MIR and FIR emission, and also with a general mass-selected sample of galaxies at the same redshifts. We demonstrate observationally that the UVJ diagram (or, similarly, a cut in the specific SFR) is only partially able to distinguish the quiescent galaxies from the SFGs. The SFR–M_* relation is investigated for the different samples, yielding a logarithmic slope ~1, in good agreement with previous results. The dust attenuations derived from different SFR indicators (UV(1600), UV(2800), [O II], IR) are compared and show clear trends with respect to both the stellar mass and total SFR, with more massive and highly star-forming galaxies being affected by stronger dust attenuation., Unión Europea. FP7, Ministerio de Economía y Competitividad (MINECO), España, STARFORM Sinergia Project - Swiss National Science Foundation, MERAC, Programa Nacional de Astronomía y Astrofísica, España, ERC, Programa Fondos FEDER (UE), Ministerio de Ciencia en Innovación (MICINN), España, Programa Ramón y Cajal, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Conference on Ground-Based and Airborne Instrumentation for Astronomy (5th. 2014. Montreal, Canada). © 2014 SPIE, the international society for optics and photonics., MEGARA (Multi-Espectrógrafo en GTC de Alta Resolución para Astronomía) is an optical Integral-Field Unit (IFU) and Multi-Object Spectrograph (MOS) designed for the GTC 10.4m telescope in La Palma. MEGARA offers two IFU fiber bundles, one covering 12.5x11.3 arcsec^2 with a spaxel size of 0.62 arcsec (Large Compact Bundle; LCB) and another one covering 8.5x6.7 arcsec^2 with a spaxel size of 0.42 arcsec (Small Compact Bundle; SCB). The MEGARA MOS mode will allow observing up to 100 objects in a region of 3.5x3.5 arcmin^2 around the two IFU bundles. Both the LCB IFU and MOS capabilities of MEGARA will provide intermediate-to-high spectral resolutions (R_FWHM∽6,000, 12,000 and 18,700, respectively for the low-, mid-and high-resolution Volume Phase Holographic gratings) in the range 3650-9700 ÅÅ. These values become R_FWHM∽7,000, 13,500, and 21,500 when the SCB is used. A mechanism placed at the pseudo-slit position allows exchanging the three observing modes and also acts as focusing mechanism. The spectrograph is a collimator-camera system that has a total of 11 VPHs simultaneously available (out of the 18 VPHs designed and being built) that are placed in the pupil by means of a wheel and an insertion mechanism. The custom-made cryostat hosts an E2V231-84 4kx4k CCD. The UCM (Spain) leads the MEGARA Consortium that also includes INAOE (Mexico), IAA-CSIC (Spain), and UPM (Spain). MEGARA is being developed under a contract between GRANTECAN and UCM. The detailed design, construction and AIV phases are now funded and the instrument should be delivered to GTC before the end of 2016., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2012 The Authors. © 2012 Monthly Notices of the Royal Astronomical Society © 2012 RAS. We thank the anonymous referee for a careful and constructive reading of the manuscript that helped us to improve the quality of the paper. We are grateful to Lulu Liu for providing us with their measurements of the fraction of galaxies with satellites obtained from the SDSS, used here as a local (z = 0) comparison. We thank Juan Betancort for his valuable input on several aspects of the statistical analysis in this paper. We are grateful to Sergio Pascual for his very useful help with programming questions. We would like also to acknowledge fruitful discussions with Javier Cenarro, Luis Díaz, Rosa Domínguez, César González, Carlos López San Juan, José Onorbe, Thorsten Naab and Vicent Quilis. IT is a Ramón y Cajal Fellow of the Spanish Ministry of Science and Innovation. 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. PGP and GB acknowledge support from the Spanish Programa Nacional de Astronomía y Astrofísica under grants AYA2009-10368 and AYA2009-07723-E. This work has made use of the Rainbow Cosmological Surveys Data base, which is operated by the Universidad Complutense de Madrid (UCM)., The accretion of minor satellites has been postulated as the most likely mechanism to explain the significant size evolution of massive galaxies over cosmic time. Using a sample of 629 massive (M_star~ 10^11 M_⊙) galaxies from the near-infrared Palomar/DEEP-2 survey, we explore what fraction of these objects have satellites with 0.01 < M_sat/M_central < 1 (1:100) up to z= 1 and what fraction have satellites with 0.1 < M_sat/M_central < 1 (1:10) up to z= 2 within a projected radial distance of 100 kpc. We find that the fraction of massive galaxies with satellites, after background correction, remains basically constant and close to 30 per cent for satellites with a mass ratio down to 1:100 up to z= 1, and close to 15 per cent for satellites with a 1:10 mass ratio up to z= 2. The family of spheroid-like massive galaxies presents a 2–3 times larger fraction of objects with satellites than the group of disc-like massive galaxies. A crude estimation of the number of 1:3 mergers a massive spheroid-like galaxy has experienced since z~2 is around 2. For a disc-like galaxy this number decreases to ~1., Ministerio de Ciencia e Innovación (MICINN), Programa Nacional de Astronomía y Astrofísica (PNAyA), España, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2015. The American Astronomical Society. All rights reserved. We thank the two anonymous referees for contributing to significantly improve this work. M.H.C acknowledges D. Gratadour for kindly giving us access to the GPU cluster at LESIA. G.C.V gratefully acknowledges financial support from CONICYT-Chile through its doctoral scholarship and grant DPI20140090. S.M. acknowledges financial support from the Institut Universitaire de France (IUF), of which she is senior member. G.B., D.C.K., and S.M.F. acknowledge support from NSF grant AST-08-08133 and NASA grant HST-GO-12060.10A., We present a catalog of visual-like H-band morphologies of ~50.000 galaxies (H_f160w < 24.5) in the 5 CANDELS fields (GOODS-N, GOODS-S, UDS, EGS, and COSMOS). Morphologies are estimated using Convolutional Neural Networks (ConvNets). The median redshift of the sample is < z> 1.25. The algorithm is trained on GOODS-S, for which visual classifications are publicly available, and then applied to the other 4 fields. Following the CANDELS main morphology classification scheme, our model retrieves for each galaxy the probabilities of having a spheroid or a disk, presenting an irregularity, being compact or a point source, and being unclassifiable. ConvNets are able to predict the fractions of votes given to a galaxy image with zero bias and ~10% scatter. The fraction of mis-classifications is less than 1%. Our classification scheme represents a major improvement with respect to Concentration-Asymmetry-Smoothness-based methods, which hit a 20%–30% contamination limit at high z., Comisión Nacional de Investigación Científica y Tecnológica de Chile (CONICYT), Institut Universitaire de France (IUF), National Science Foundation (NSF), EE.UU., National Aeronautics and Space Administration (NASA), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO, 2010. We are grateful to the referee for his valuable suggestions and comments which helped us to improve the paper. The authors acknowledge support by DGI of the Spanish Ministerio de Educación y Ciencia under grants AYA2007-68034-C03-02/-01, FEDER funds, Plan Andaluz de Investigación Desarrollo e Innovación (PAIDI) of Junta de Andalucía as research group FQM-322 and the excellence fund FQM-5418. J.A.C., J.F.A.C. and G.E.R are researchers of CONICET. J.F.A.C was supported by grant PICT 2007-02177 (SecyT). G. E. R. and J.A.C were supported by grant PICT 0700848 BID 1728/OC-AR (ANPCyT) and PIP 2010-0078 (CONICET). J.L.S. acknowledges support by the Spanish Ministerio de Innovación y Tecnología under grant AYA2008-06423-C03-03. P. G. P.-G. acknowledges support from the Ramón y Cajal Program, financed by the Spanish Government and/or the European Union. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc., Aims. We report results of an X-ray study of the supernova remnant (SNR) G344.7-0.1 and the point-like X-ray source located at the geometrical center of the SNR radio structure. Methods. The morphology and spectral properties of the remnant and the central X-ray point-like source were studied using data from the XMM-Newton and Chandra satellites. Archival radio data and infrared Spitzer observations at 8 and 24 mu m were used to compare and study its multi-band properties at different wavelengths. Results. The XMM-Newton and Chandra observations reveal that the overall X-ray emission of G344.7-0.1 is extended and correlates very well with regions of bright radio and infrared emission. The X-ray spectrum is dominated by prominent atomic emission lines. These characteristics suggest that the X-ray emission originated in a thin thermal plasma, whose radiation is represented well by a plane-parallel shock plasma model (PSHOCK). Our study favors the scenario in which G344.7-0.1 is a 6 x 10^3 year old SNR expanding in a medium with a high density gradient and is most likely encountering a molecular cloud on the western side. In addition, we report the discovery of a soft point-like X-ray source located at the geometrical center of the radio SNR structure. The object presents some characteristics of the so-called compact central objects (CCO). However, its neutral hydrogen absorption column (N_H) is inconsistent with that of the SNR. Coincident with the position of the source, we found infrared and optical objects with typical early-K star characteristics. The X-ray source may be a foreground star or the CCO associated with the SNR. If this latter possibility were confirmed, the point-like source would be the farthest CCO detected so far and the eighth member of the new population of isolated and weakly magnetized neutron stars., Dirección General de Investigación Científica y Técnica (DGICT), MINECO, Fondo Europeo de Desarrollo Regional (FEDER), UE, Plan Andaluz de Investigación Desarrollo e Innovación (PAIDI), Secretaría de Ciencia y Tecnología (SecyT), Argentina, Agencia Nacional de Promoción Científica y Tecnológica (ANPCyT), Aregntina, Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Argentina, Ministerio de Ciencia e Innovación (MICINN), España, Gobierno de España, Dirección General de Investigación (DGI), MEC, Ministerio de Educación y Ciencia (MEC), España, Ministerio de Economía y Competitividad (MINECO), España, Junta de Andalucía, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2011 The American Astronomical Society. This wor0k is partially funded by the Spanish MICINN under the Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC. J. M. M. acknowledges funding from a Graduate Alumni Fellowship at the University of Florida. The Spanish MICINN provides support to M. B., M. P., and A. H. through grant AYA2009-11137 and to J. G. through grant AYA2009-10368. Our observations were made with the GTC Telescope at the Spanish Observatorio del Roque de los Muchachos, which is managed by the Instituto de Astrofísica de Canarias. We are grateful to the personnel who took the observations and to Ana Matkovic for her help with the use of the REDucmE software. We also thank the anonymous referee for useful comments that improved the presentation of this Letter., We present Gran-Telescopio-Canarias/OSIRIS optical spectra of four of the most compact and massive early-type galaxies (ETGs) in the Groth Strip Survey at redshift z similar to 1, with effective radii R-e = 0.5-2.4 kpc and photometric stellarmasses M-star = (1.2-4) x 10(11)M(circle dot). We find that these galaxies have velocity dispersions sigma = 156-236 km s(-1). The spectra are well fitted by single stellar population models with approximately 1 Gyr of age and solar metallicity. We find that (1) the dynamical masses of these galaxies are systematically smaller by a factor of similar to 6 than the published stellarmasses using BRIJK photometry, and (2) when estimating stellarmasses as 0.7xM(dyn), a combination of passive luminosity fading with mass/size growth due to minor mergers can plausibly evolve our objects to match the properties of the local population of ETGs., Spanish MICINN, University of Florida, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2012 SPIE. Conference on Ground-Based and Airborne Telescopes (4º. 2012. Amsterdam, Netherlands). This project is partly funded by the Spanish Ministry of Science and Innovation (MICINN) under project AYA2009-10368, by the Madrid Regional Government through the AstroMadrid Project (CAM S2009/ESP- 1496) and by the Spanish MICINN under the Consolider Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC. This work is being done in the framework of the Moncloa Campus of International Excellence (UCM-UPM)., In these proceedings we give a summary of the characteristics and current status of the MEGARA instrument, the future optical IFU and MOS for the 10.4-m Gran Telescopio Canarias (GTC). MEGARA is being built by a Consortium of public research institutions led by the Universidad Complutense de Madrid (UCM, Spain) that also includes INAOE (Mexico), IAA-CSIC (Spain) and UPM (Spain). The MEGARA IFU includes two different fiber bundles, one called LCB (Large Compact Bundle) with a field-of-view of 12.5x11.3 arcsec(2) and a spaxel size of 0.62 arcsec yielding spectral resolutions between R=6,800-17,000 and another one called SCB (Small Compact Bundle) covering 8.5x6.7 arcsec(2) with hexagonally-shaped and packed 0.42-arcsec spaxels and resolutions R=8,000-20,000. The MOS component allows observing up to 100 targets in 3.5x3.5 arcmin(2). Both the IFU bundles and the set of 100 robotic positioners of the MOS will be placed at one of the GTC Folded-Cass foci while the spectrographs (one in the case of the MEGARA-Basic concept) will be placed at the Nasmyth platform. On March 2012 MEGARA passed the Preliminary Design Review and its first light is expected to take place at the end of 2015., Spanish Ministry of Science and Innovation (MICINN), Madrid Regional Government, Spanish MICINN, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

©2013 The American Astronomical Society. We acknowledge support from the Spanish Programa Nacional de Astronomía y Astrofísica under grants AYA2009-07723-E and AYA2009-10368. SHARDS has been funded by the Spanish MICINN/MINECO under the Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC. O.G.-M., C.M.-T., J.M.R.-E., and J.R.-Z. wish to acknowledge support from grant AYA2010-21887-C04-04. A.A.-H. and A.H.-C. acknowledge financial support from the Universidad de Cantabria through the Augusto G. Linares Program. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. Based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. We thank all the GTC Staff for their support and enthusiasm with the SHARDS project, and we especially acknowledge the help from Antonio Cabrera and René Rutten. The work is also based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck-Institut fur Astronomie and the Instituto de Astrofísica de Andalucia (CSIC). We thank the referee for her/his very useful and positive comments., We present the Survey for High-z Absorption Red and Dead Sources (SHARDS), an ESO/GTC Large Program carried out using the OSIRIS instrument on the 10.4 m Gran Telescopio Canarias (GTC). SHARDS is an ultra-deep optical spectro-photometric survey of the GOODS-N field covering 130 arcmin(2) at wavelengths between 500 and 950 nm with 24 contiguous medium-band filters (providing a spectral resolution R similar to 50). The data reach an AB magnitude of 26.5 (at least at a 3 sigma level) with sub-arcsec seeing in all bands. SHARDS' main goal is to obtain accurate physical properties of intermediate-and high-z galaxies using well-sampled optical spectral energy distributions (SEDs) with sufficient spectral resolution to measure absorption and emission features, whose analysis will provide reliable stellar population and active galactic nucleus (AGN) parameters. Among the different populations of high-z galaxies, SHARDS' principal targets are massive quiescent galaxies at z > 1, whose existence is one of the major challenges facing current hierarchical models of galaxy formation. In this paper, we outline the observational strategy and include a detailed discussion of the special reduction and calibration procedures which should be applied to the GTC/OSIRIS data. An assessment of the SHARDS data quality is also performed. We present science demonstration results on the detection and study of emission-line galaxies (star-forming objects and AGNs) at z = 0-5. We also analyze the SEDs for a sample of 27 quiescent massive galaxies with spectroscopic redshifts in the range 1.0 < z less than or similar to 1.4. We discuss the improvements introduced by the SHARDS data set in the analysis of their star formation history and stellar properties. We discuss the systematics arising from the use of different stellar population libraries, typical in this kind of study. Averaging the results from the different libraries, we find that the UV-to-MIR SEDs of the massive quiescent galaxies at, Spanish Programa Nacional de Astronomia y Astrofisica, Spanish MICINN/MINECO under the Consolider-Ingenio 2010 Program, Universidad de Cantabria through the Augusto G. Linares Program, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2015 RAS. We thank the referee for helpful comments that have improved this paper. We also thank Johannes Buchner for helpful discussions and providing machine-readable results. We acknowledge helpful discussions with Ranjan Vasudevan. The scientific results reported in this article are based to a significant degree on observations made by the Chandra X-ray Observatory. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM). This study makes use of data from AEGIS, a multiwavelength sky survey conducted with the Chandra, GALEX, Hubble, Keck, CFHT, MMT, Subaru, Palomar, Spitzer, VLA, and other telescopes and supported in part by the National Science Foundation (NSF), NASA, and the STFC. Funding for the DEEP2 Galaxy Redshift Survey has been provided by NSF grants AST-95-09298, AST-0071048, AST-0507428, and AST-0507483 as well as NASA LTSA grant NNG04GC89G. Funding for the DEEP3 Galaxy Redshift Survey has been provided by NSF grants AST-0808133, AST-0807630, and AST-0806732. This work made use of images and/or data products provided by the NDWFS (Jannuzi & Dey 1999), which is supported by the National Optical Astronomy Observatory (NOAO). NOAO is operated by AURA, Inc., under a cooperative agreement with the NSF. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the NSF, 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. Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Some of the data used in this, We present new measurements of the evolution of the X-ray luminosity functions (XLFs) of unabsorbed and absorbed active galactic nuclei (AGNs) out to z ~ 5. We construct samples containing 2957 sources detected at hard (2-7 keV) X-ray energies and 4351 sources detected at soft (0.5-2 keV) energies from a compilation of Chandra surveys supplemented by wide-area surveys from ASCA and ROSAT. We consider the hard and soft X-ray samples separately and find that the XLF based on either (initially neglecting absorption effects) is best described by a new flexible model parametrization where the break luminosity, normalization, and faint-end slope all evolve with redshift. We then incorporate absorption effects, separately-modelling the evolution of the XLFs of unabsorbed (20 < log N_H < 22) and absorbed (22 < log N_H < 24) AGNs, seeking a model that can reconcile both the hard-and soft-band samples. We find that the absorbed AGN XLF has a lower break luminosity, a higher normalization, and a steeper faint-end slope than the unabsorbed AGN XLF out to z ~ 2. Hence, absorbed AGNs dominate at low luminosities, with the absorbed fraction falling rapidly as luminosity increases. Both XLFs undergo strong luminosity evolution which shifts the transition in the absorbed fraction to higher luminosities at higher redshifts. The evolution in the shape of the total XLF is primarily driven by the changing mix of unabsorbed and absorbed populations., Unión Europea (UE), Ministerio de Economía y Competitividad (MINECO), España, National Science Foundation (NSF), National Aeronautics and Space Administration (NASA), EE.UU., Science and Technology Facilities Council (STFC), Long Term Space Astrophysics Program (LTSA-NASA), National Optical Astronomy Observatory (NOAO), Alfred P. Sloan Foundation, US Department of Energy Office of Science, NASA Office of Space Science, COFUND Junior Research Fellowship from the Institute of Advanced Study, Durham University, ERC Advanced Grant FEEDBACK at the University of Cambridge, NSF CAREER, Greek Government, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2011 The Authors. © 2011 Monthly Notices of the Royal Astronomical Society. © 2011 RAS. We acknowledge support from the UK Science and Technology Facilities Council (STFC), the Leverhulme Trust and the University of Nottingham. PGP-G acknowledges support from the Spanish Programa Nacional de Astronomía y Astrofísica under grants AYA2009 D07723 DE, AYA 2009-10368 and CSD2006-00070, and the Ramón y Cajal Program financed by the Spanish Government and the European Union., We present a study of the star-forming properties of a stellar mass-selected sample of galaxies in the GOODS (Great Observatories Origins Deep Survey) NICMOS Survey (GNS), based on deep Hubble Space Telescope (HST) imaging of the GOODS North and South fields. Using a stellar mass-selected sample, combined with HST/ACS and Spitzer data to measure both ultraviolet (UV) and infrared-derived star formation rates (SFRs), we investigate the star forming properties of a complete sample of ∼1300 galaxies down to log M_*= 9.5 at redshifts 1.5 < z < 3. Eight per cent of the sample is made up of massive galaxies with M_*≥ 10^11 M_⊙. We derive optical colours, dust extinctions and UV and infrared SFR to determine how the SFR changes as a function of both stellar mass and time. Our results show that SFR increases at higher stellar mass such that massive galaxies nearly double their stellar mass from star formation alone over the redshift range studied, but the average value of SFR for a given stellar mass remains constant over this ∼2 Gyr period. Furthermore, we find no strong evolution in the SFR for our sample as a function of mass over our redshift range of interest; in particular we do not find a decline in the SFR among massive galaxies, as is seen at z < 1. The most massive galaxies in our sample (log M_*≥ 11) have high average SFRs with values SFR_UV, corr= 103 ± 75 M_⊙ yr^−1, and yet exhibit red rest-frame (U−B) colours at all redshifts. We conclude that the majority of these red high-redshift massive galaxies are red due to dust extinction. We find that A_2800 increases with stellar mass, and show that between 45 and 85 per cent of massive galaxies harbour dusty star formation. These results show that even just a few Gyr after the first galaxies appear, there are strong relations between the global physical properties of galaxies, driven by stellar mass or another underlying feature of galaxies strongly related to the stellar mass., Ministerio de Economía y Competitividad (MINECO), Unión Europea (UE), Leverhulme Trust, Science and Technology Facilities Council (STFC), Reino Unido, University of Nottingham, Programa Nacional de Astronomía y Astrofísica (PNAyA), España, Ayudas para contratos Ramón y Cajal (RYC), MINECO, Gobierno de España, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. The authors acknowledge the referee's comments, which led to improvements in this work. They also thank Carlos Hernández Monteagudo for his very useful advice. LADG acknowledges support from the 'Caja Rural de Teruel' to develop this research. AJC is a Ramón y Cajal Fellow of the Spanish Ministry of Economy and Competitiveness. This work was supported by the 'Programa Nacional de Astronomía y Astrofísica' of the Spanish Ministry of Economy and Competitiveness under grants AYA2012-30789, AYA2010-21322-C03-02, AYA2009-10368 and AYA2009-07723-E. This work made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM)., Using a compilation of 379 massive (stellar mass M ≳ 10^11 M_⊙) spheroid-like galaxies from the near-infrared Palomar/DEEP-2 survey, we investigated, up to z ∼ 1, whether the presence of companions depends on the size of the host galaxy. We explored the presence of companions for mass ratios with respect to the central massive galaxy down to 1 : 10 and 1 : 100, and within projected distances of 30, 50 and 100 kpc of these objects. We found evidence that these companions are equally distributed around both compact and extended massive spheroid-like galaxies. This suggests that, at least since z ∼ 1, the merger activity in these objects is nearly homogeneous across the whole population and that the merger history is not affected by the size of the host galaxy. Our results could indicate that compact and extended massive spheroid-like galaxies are increasing in size at the same rate., Ministerio de Economía y Competitividad (MINECO), Caja Rural de Teruel, Programa Nacional de Astronomía y Astrofísica (PNAyA), España, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2010 The Authors. Journal compilation, © 2010 RAS. The authors wish to thank the anonymous referee for constructive suggestions that improved the paper and Alison Coil for useful comments. AG acknowledges financial support from the Marie-Curie Reintegration Grant PERG03-GA-2008-230644. PGP-G acknowledges support from the Spanish Ministry of Science and Innovation under grants AYA 2006-02358, AYA 2006-15698-C02-02 and CSD2006-100070, and from the Ramón y Cajal Program financed by the Spanish Government and the European Union. This study makes use of data from AEGIS, a multiwavelength sky survey conducted with the Chandra, GALEX, Hubble, Keck, CFHT, MMT, Subaru, Palomar, Spitzer, VLA and other telescopes and supported in part by the NSF, NASA and the STFC., We explore the nature of Infrared Excess sources (IRX), which are proposed as candidates for luminous [L_X(2–10 keV) > 10^43 erg s^−1] Compton thick (NH > 2 × 1024 cm−2) QSOs at z≈ 2. Lower redshift, z≈ 1, analogues of the distant IRX population are identified by first redshifting to z= 2 the spectral energy distributions (SEDs) of all sources with secure spectroscopic redshifts in the AEGIS (6488) and the GOODS-North (1784) surveys and then selecting those that qualify as IRX sources at that redshift. A total of 19 galaxies are selected. The mean redshift of the sample is z≈ 1. We do not find strong evidence for Compton thick QSOs in the sample. For nine sources with X-ray counterparts, the X-ray spectra are consistent with Compton thin active galactic nucleus (AGN). Only three of them show tentative evidence for Compton thick obscuration. The SEDs of the X-ray undetected population are consistent with starburst activity. There is no evidence for a hot dust component at the mid-infrared associated with AGN heated dust. If the X-ray undetected sources host AGN, an upper limit of L_X(2–10 keV) = 10^43 erg s^−1 is estimated for their intrinsic luminosity. We propose that a large fraction of the z≈ 2 IRX population is not Compton thick quasi-stellar objects (QSOs) but low-luminosity [L_X(2–10 keV) < 10^43 erg s^−1], possibly Compton thin, AGN or dusty starbursts. It is shown that the decomposition of the AGN and starburst contribution to the mid-IR is essential for interpreting the nature of this population, as star formation may dominate this wavelength regime., Unión Europea. FP7, Ministerio de Ciencia e Innovación (MICINN), Acciones Marie Skłodowska-Curie (UE), Gobierno de España, National Science Foundation (NSF), EE.UU., National Aeronautics and Space Administration (NASA), Science and Technology Facilities Council (STFC), Reino Unido, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

©Wiley & Sons. This paper is partially based on data from CAHA, the German-Spanish Astronomical Centre, Calar Alto, operated by the Max-Planck-Institute for Astronomy, Heidelberg, jointly with the Spanish National Commission for Astronomy. Also partially based on data obtained with the 2.3m Bok Telescope of the University of Arizona on Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. Also partially based on observations made with the Isaac Newton and Jacobus Kapteyn Telescopes, operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. This research has made use of the NASA/IPAC Extragalactic Database (NED) and the NASA/IPAC Infrared Science Archive which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. 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. PGPG wishes to acknowledge the Spanish Ministry of Education and Culture for the reception of a Formación de Profesorado Universitario fellowship. AGdP acknowledges financial support from NASA through a Long Term Space Astrophysics grant to B.F. Madore. During the course of this work AAH has been supported by the National Aeronautics and Space Administration grant NAG 5-3042 through the University of Arizona and Contract 960785 through the Jet Propulsion Laboratory. AAS acknowledges generous financial support from the Royal Society. We also would like to thank George and, We present an analysis of the integrated properties of the stellar populations in the Universidad Complutense de Madrid (UCM) Survey of Halpha-selected galaxies. In this paper, the first of a series, we describe in detail the techniques developed to model star-forming galaxies using a mixture of stellar populations, and taking into account the observational uncertainties. We assume a recent burst of star formation superimposed on a more evolved population. The effects of the nebular continuum, line emission and dust attenuation are taken into account. We also test different model assumptions, including the choice of specific evolutionary synthesis model, initial mass function, star formation scenario and the treatment of dust extinction. Quantitative tests are applied to determine how well these models fit our multiwavelength observations for the UCM sample. Our observations span the optical and near-infrared, including both photometric and spectroscopic data. Our results indicate that extinction plays a key role in this kind of study, revealing that low- and high-obscured objects may require very different extinction laws and must be treated differently. We also demonstrate that the UCM Survey galaxies are best described by a short burst of star formation occurring within a quiescent galaxy, rather than by continuous star formation. A detailed discussion on the inferred parameters, such as the age, burst strength, metallicity, star formation rate, extinction and total stellar mass for individual objects, is presented in Paper II of this series., National Aeronautics and Space Administration (NASA), National Science Foundation (NSF), EE.UU., Ministerio de Educación, Cultura y Deporte (MECD), España, University of Arizona, Jet Propulsion Laboratory, EE.UU., Royal Society, RU, Plan Nacional de Astronomía y Astrofísica (MICINN), España, Ministerio de ciencia e Innovación (MICINN), España, 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 Journal © 2012 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. We thank the anonymous referee for their useful comments that helped to improve this paper. AH-C and AA-H acknowledge funding by the Universidad de Cantabria Augusto González Linares programme and the Spanish Plan Nacional de Astronomía y Astrofísica under grant AYA2012-31447. PE and PGP-G acknowledge support from the Spanish Plan Nacional grant AYA2012-31277. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM), partnered with the University of California Observatories at Santa Cruz (UCO/Lick, UCSC). Based on observations made with the GTC, installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma., We analyse the stellar populations in the host galaxies of 53 X-ray selected optically dull active galactic nuclei (AGN) at 0.34 < z < 1.07 with ultradeep (m(AB) = 26.5, 3 sigma) optical medium-band (R similar to 50) photometry from the Survey for High-z Absorption Red and Dead Sources (SHARDS). The spectral resolution of SHARDS allows us to consistently measure the strength of the 4000 angstrom brk, D-n(4000), a reliable age indicator for stellar populations. We confirm that most X-ray selected moderate-luminosity AGN (L-X < 10(44) erg s(-1)) are hosted by massive galaxies (typically M-* > 10(10.5) M circle dot) and that the observed fraction of galaxies hosting an AGN increases with the stellar mass. A careful selection of random control samples of inactive galaxies allows us to remove the stellar mass and redshift dependences of the AGN fraction to explore trends with several stellar age indicators. We find no significant differences in the distribution of the rest-frame U - V colour for AGN hosts and inactive galaxies, in agreement with previous results. However, we find significantly shallower 4000 angstrom bres in AGN hosts, indicative of younger stellar populations. With the help of a model-independent determination of the extinction, we obtain extinction-corrected U - V colours and light-weighted average stellar ages. We find that AGN hosts have younger stellar populations and higher extinction compared to inactive galaxies with the same stellar mass and at the same redshift. We find a highly significant excess of AGN hosts with D-n(4000) similar to 1.4 and light-weighted average stellar ages of 300-500 Myr, as well as a deficit of AGN in intrinsic red galaxies. We interpret failure in recognizing these trends in previous studies as a consequence of the balancing effect in observed colours of the age-extinction degeneracy., Universidad de Cantabria Augusto Gonzalez Linares programme, Spanish Plan Nacional de Astronomía y Astrofísica, Spanish Plan Nacional grant, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2009 The American Astronomical Society. All rights reserved. We thank the anonymous referee for detailed comments. Support for this work was provided by NASA through contract 1255094 issued by JPL/California Institute of Technology. J.M.L. acknowledges support from Leo Goldberg Fellowship sponsored by the National Optical Astronomy Observatory. P.G.P.-G. acknowledges support from the Spanish Programa Nacional de Astronomía y Astrofísica under grants AYA 2006– 02358 and AYA 2006–15698–C02–02, and from the Ramón y Cajal Program financed by the Spanish Government and the European Union., We present a morphology study of intermediate-redshift (0.2 < z < 1.2) luminous infrared galaxies (LIRGs) and general field galaxies in the GOODS fields using a revised asymmetry measurement method optimized for deep fields. By taking careful account of the importance of the underlying sky-background structures, our new method does not suffer from systematic bias and offers small uncertainties. By redshifting local LIRGs and low-redshift GOODS galaxies to different higher redshifts, we have found that the redshift dependence of the galaxy asymmetry due to surface-brightness dimming is a function of the asymmetry itself, with larger corrections for more asymmetric objects. By applying redshift-, infrared (IR)-luminosity- and optical-brightness-dependent asymmetry corrections, we have found that intermediate-redshift LIRGs generally show highly asymmetric morphologies, with implied merger fractions ~50% up to z = 1.2, although they are slightly more symmetric than local LIRGs. For general field galaxies, we find an almost constant relatively high merger fraction (20%-30%). The B-band luminosity functions (LFs) of galaxy mergers are derived at different redshifts up to z = 1.2 and confirm the weak evolution of the merger fraction after breaking the luminosity-density degeneracy. The IR LFs of galaxy mergers are also derived, indicating a larger merger fraction at higher IR luminosity. The integral of the merger IR LFs indicates a dramatic evolution of the merger-induced IR energy density [(1 + z)^~(5-6)], and that galaxy mergers start to dominate the cosmic IR energy density at z greater than or ~ 1., Ministerio de Economía y Competitividad (MINECO), National Aeronautics and Space Administration (NASA), Leo Goldberg Fellowship, National Optical Astronomy Observatory (NOAO), EE.UU., Programa Nacional de Astronomía y Astrofísica (PNAyA), España, Unión Europea (UE), Ayudas para contratos Ramón y Cajal (RYC), MINECO, 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. Artículo firmado por 13 autores. JMRE, OGM and NCR (CDS2006-00070, AYA2012-39168-C03-01), CMT and JMMH (AYA2010-21887-C04-04, AYA2010-21887-C04-02 and AYA2012-39362-C02-01) and AHC (AYA2012-31447) acknowledge support from the Spanish MINECO under the PNAyA grants given in parenthesis. OGM acknowledges a Juan de La Cierva Fellowship (MINECO). We are very grateful to the GTC support staff for their help with the observations. SHARDS is funded by the Spanish MINECO with grant AYA2012-31277. The Rainbow data base is partially funded by the Spanish MINECO under grant AYA2012-31277 and the US NSF grant AST-08-08133. Based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma., We are undertaking a search for high-redshift low-luminosity Lyman Alpha sources in the SHARDS (Survey for High-z Absorption Red and Dead Sources) survey. Among the pre-selected Lyman Alpha sources two candidates were spotted, located 3.19 arcsec apart, and tentatively at the same redshift. Here, we report on the spectroscopic confirmation with Gran Telescopio Canarias of the Lyman Alpha emission from this pair of galaxies at a confirmed spectroscopic redshifts of z=5.07. Furthermore, one of the sources is interacting/merging with another close companion that looks distorted. Based on the analysis of the spectroscopy and additional photometric data, we infer that most of the stellar mass of these objects was assembled in a burst of star formation 100 Myr ago. A more recent burst (2 Myr old) is necessary to account for the measured Lyman Alpha flux. We claim that these two galaxies are good examples of Lyman Alpha sources undergoing episodic star formation. Besides, these sources very likely constitute a group of interacting Lyman Alpha emitters (LAEs)., Ayudas para contratos Juan de la Cierva (MINECO), Ministerio de Economía y Competitividad (MINECO), National Science Fpundation (NSF), Programa Nacional de Astronomía y Astrofísica (PNAyA), MINECO, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2015. The American Astronomical Society. We would like to thank the referee for a useful and constructive report that clearly helped in improving the manuscript. M.H.C. warmly thanks P. Behroozi for kindly sharing the mass growth and merger rates of massive galaxies used in this paper. P.G.P.-G. acknowledges funding from Spanish Government MINECO Grant AYA2012-31277. G. C. V. gratefully acknowledges funding from CONICYT (Chile) through their Doctoral Scholarship. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM), partnered with the University of California Observatories at Santa Cruz (UCO/Lick, UCSC). This work is based on observations taken by the 3D-HST Treasury Program (GO 12177 and 1232) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc, under NASA contract NAS5-26555., We quantify the morphological evolution of z ~ 0 massive galaxies (M_*/M_∼ ∼10^11.2 +/- 0.3) from z ~ 3 in the 5 CANDELS fields. The progenitors are selected using abundance matching techniques to account for the mass growth. At z < 1, the population matches the massive end of the Hubble sequence, with 30% of pure spheroids, 50% of galaxies with equally dominant disk and bulge components, and 20% of disks. At z ~ 2-3 however, there is a majority of irregular systems (~ 60%-70%) with still 30% of pure spheroids. We then analyze the stellar populations, star formation rates (SFRs), gas fractions, and structural properties for the different morphologies independently. Our results suggest two distinct channels for the growth of bulges in massive galaxies. Around ~ 30%-40% were already bulges at z ~ 2.5, with low average SFRs and gas fractions (10%-15%), high Sersic indices (n > 3-4), and small effective radii (R_e ∼1 kpc), pointing toward an even earlier formation through gas-rich mergers or violent disk instabilities. Between z ~ 2.5 and z ~ 0, they rapidly increase their size by a factor of ~ 4-5, are quenched, and slightly increase their Sersic indices (n ~ 5) but their global morphology remains unaltered. The structural evolution is independent of the gas fractions, suggesting that it is driven by ex situ events. The remaining 60% experience a gradual morphological transformation, from clumpy disks to more regular bulge +disk systems, essentially happening at z > 1. This results in the growth of a significant bulge component (n ~ 3) for 2/3 of the systems, possibly through the migration of clumps, while the remaining 1/3 retain a rather small bulge (n ~ 1.5-2). The transition phase between disturbed and relaxed systems and the emergence of the bulge is correlated with a decrease in the star formation activity and the gas fractions, suggesting a morphological quenching process as a plausible mechanism for the formation of these bulges., Ministerio de Economía y Competitividad (MINECO), España, Comisión Nacional de Investigación Científica y Tecnológica (CONICYT), Chile, Association of Universities for Research in Astronomy, NASA, EE.UU., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2015. The American Astronomical Society. We acknowledge support from the Spanish Government grants AYA2010-21322-C03-02 and AYA2012-31277, and the ERC Advanced Grant 321323-NEOGAL. This work is based on SHARDS observations made with the Gran Telescopio Canarias (GTC), and the Rainbow Cosmological Surveys Database, operated by UCM partnered with UCO/Lick, UCSC. I.M.N. thanks Carsten Weidner, Jesús Falcón Barroso, and Mike Beasley for their careful reading and comments on the manuscript., We explore the stellar initial mass function (IMF) of a sample of 49 massive quiescent galaxies (MQGs) at 0.9 < z < 1.5. We base our analysis on intermediate resolution spectro-photometric data in the GOODS-N field taken in the near-infrared and optical with the Hubble Space Telescope Wide Field Camera 3 G141 grism and the Survey for High-z Absorption Red and Dead Sources. To constrain the slope of the IMF, we have measured the TiO2 spectral feature, whose strength depends strongly on the content of low-mass stars, as well as on stellar age. Using ultraviolet to near-infrared individual and stacked spectral energy distributions, we have independently estimated the stellar ages of our galaxies. Knowing the age of the stellar population, we interpret the strong differences in the TiO2 feature as an IMF variation. In particular, for the heaviest z similar to 1 MQGs (M > 10(11) M-circle dot), we find an average age of 1.7 +/- 0.3 Gyr and a bottom-heavy IMF (Gamma(b) = 3.2 +/- 0.2). Lighter MQGs (2 x 10(10) < M < 10(11) M-circle dot) at the same redshift are younger on average (1.0 +/- 0.2 Gyr) and present a shallower IMF slope (Gamma(b) = 2.7(-0.4)(+0.3)). Our results are in good agreement with the findings about the IMF slope in early-type galaxies of similar mass in the present-day universe. This suggests that the IMF, a key characteristic of the stellar populations in galaxies, is bottom-heavier for more massive galaxies and has remained unchanged in the last similar to 8 Gyr., Spanish Government, ERC, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Thanks to R. Sheth for comments on an early draft. Thanks to the anonymous referee for a constructive and quick report., We quantify the evolution of the stellar mass functions (SMFs) of star-forming and quiescent galaxies as a function of morphology from z ∼ 3 to the present. Our sample consists of ∼50 000 galaxies in the CANDELS fields (∼880 arcmin^2), which we divide into four main morphological types, i.e. pure bulge-dominated systems, pure spiral disc-dominated, intermediate two-component bulge+disc systems and irregular disturbed galaxies. At z ∼ 2, 80 per cent of the stellar mass density of star-forming galaxies is in irregular systems. However, by z ∼ 0.5, irregular objects only dominate at stellar masses below 10^9 M_⊙. A majority of the star-forming irregulars present at z ∼ 2 undergo a gradual transformation from disturbed to normal spiral disc morphologies by z ∼ 1 without significant interruption to their star formation. Rejuvenation after a quenching event does not seem to be common except perhaps for the most massive objects, because the fraction of bulge-dominated star-forming galaxies with M^*/M_⊙ > 10^10.7 reaches 40 per cent at z < 1. Quenching implies the presence of a bulge: the abundance of massive red discs is negligible at all redshifts over 2 dex in stellar mass. However, the dominant quenching mechanism evolves. At z > 2, the SMF of quiescent galaxies above M^* is dominated by compact spheroids. Quenching at this early epoch destroys the disc and produces a compact remnant unless the star-forming progenitors at even higher redshifts are significantly more dense. At 1 < z < 2, the majority of newly quenched galaxies are discs with a significant central bulge. This suggests that mass quenching at this epoch starts from the inner parts and preserves the disc. At z < 1, the high-mass end of the passive SMF is globally in place and the evolution mostly happens at stellar masses below 10^10 M_⊙. These low-mass galaxies are compact, bulge-dominated systems, which were environmentally quenched: destruction of the disc through ram-pressure stripping is the likely proc, 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 © 2013 MNRAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. MAL-G and JL-S acknowledge support by the Spanish Ministerio de Ciencía e Innovación under grant AYA2008-06423-C03-03. JFA-C is a researcher of the CONICET and acknowledges support by grant PICT 2007-02177 (SecyT). PGP-G acknowledges support from the Spanish Programa Nacional de Astronomía y Astrofísica under grants AYA2009-10368 and AYA2009-07723-E. We would like to acknowledge the anonymous referee for a fruitful discussion about the results of this work. His/her comments on the text content have allowed us to notoriously improve this manuscript., Nearby star-forming regions are ideal laboratories to study high-energy emission of different stellar populations, from very massive stars to brown dwarfs. NGC 2023 is a reflection nebula situated to the south of the Flame Nebula (NGC 2024) and at the edge of the H II region IC 434, which also contains the Horsehead Nebula (Barnard 33). NGC 2023, NGC 2024, Barnard 33 and the surroundings of the O-type supergiant star zeta Ori constitute the south part of the Orion B molecular complex. In this work, we present a comprehensive study of X-ray emitters in the region of NGC 2023 and its surroundings. We combine optical and infrared data to determine physical properties (mass, temperature, luminosity and the presence of accretion discs) of the stars detected in an XMM-Newton observation. This study has allowed us to analyse spectral energy distribution of these stars for the first time and determine their evolutionary stage. Properties of the X-ray emitting plasma of these stars are compared to those found in other nearby star-forming regions. The results indicate that the stars that are being formed in this region have characteristics, in terms of physical properties and luminosity function, similar to those found in the Taurus-Auriga molecular complex., Spanish Ministerio de Ciencía e Innovación, SecyT, Spanish Programa Nacional de Astronomía y Astrofísica, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2009. The American Astronomical Society. NASA’s Chandra X-Ray Observatory was launched in July 1999. The Chandra Data Archive (CDA) is part of the Chandra X-Ray Center (CXC) which is operated for NASA by the Smithsonian Astrophysical Observatory. This work is based on observations obtained with XMMNewton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and NASA. 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 of the GALEX Mission, developed in cooperation with the Centre National d’Etudes Spatiales of France and the Korean Ministry of Science and Technology. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California, Institute of Technology under a contract with NASA. This work is based on observations obtained with MegaPrime/ MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l’Univers of the Centre National de la Reserche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy data Centre as part of the CFHT Legacy Survey, a collaborative project of NRC and CNRS. This work is based on observations obtained at the Hale Telescope, Palomar Observatory, as part of a collaborative agreement between the California Institute of Technology, its divisions Caltech Optical Observatories and the Jet Propulsion Laboratory (operated for NASA), and Cornell University. Many images of this article are based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute (STScI). STScI is operated by the Association, We have employed a reliable technique of classification of active galactic nuclei (AGNs) based on the fit of well sampled spectral energy distributions (SEDs) with a complete set of AGN and starburst galaxy templates. We have compiled UV, optical, and IR data for a sample of 116 AGNs originally selected for their X-ray and mid-IR emissions (96 with single detections and 20 with double optical counterparts). This is the most complete compilation of multiwavelength data for such a large sample of AGN in the Extended Groth Strip. Through these SEDs, we are able to obtain highly reliable photometric redshifts and to distinguish between pure and host-dominated AGNs. For the objects with unique detection we find that they can be separated into five main groups, namely: Starburst-dominated AGNs (24% of the sample), Starburst-contaminated AGNs (7%), Type-1 AGNs (21%), Type-2 AGNs (24%), and Normal galaxy hosting AGN (24%). We find these groups concentrated at different redshifts: Type-2 AGNs and Normal galaxy hosting AGNs are concentrated at low redshifts, whereas Starburst-dominated AGNs and Type-1 AGNs show a larger span. Correlations between hard/soft X-ray and UV, optical and IR luminosities are reported for the first time for such a sample of AGNs spanning a wide range of redshifts. For the 20 objects with double detection, the percentage of Starburst-dominated AGNs increases up to 48%., Ministerio de Economía y Competitividad (MINECO), Unión Europea (UE), Centre National d’Etudes Spatiales, Francia, Ministerio de Educación y Ciencia (MEC), España, Gobierno de España, National Science Foundation (NSF), European Space Agency (ESA), Ministerio de Ciencia y Tecnología, Corea del Sur, Jet Propulsion Laboratory, California, Institute of Technology, Caltech, National Research Council (NRC), Canada, Centre National de la Reserche Scientifique (CNRS), Francia, University of Hawaii, Cornell University, Association of Universities for Research in Astronomy, Inc., Programa Consolider-Ingenio, Programa Ramón y Cajal, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO, 2013. We are grateful to the referee for comments that helped improve the paper. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. N.C.-M., F.J.C., S.M. and X.B. acknowledge financial support provided by the Spanish Ministry of Economy and Competitiveness through grant AYA2010-21490-C02-01. S.M., F.J.C. and A.A.-H. acknowledge financial support by the Spanish Ministry of Economy and Competitiveness through grants AYA2010-21490-C02-01 and AYA2012-31447. SM acknowledges financial support from the JAE-Doc program (Consejo Superior de Investigaciones Científicas, cofunded by FSE). A.A.-H. acknowledges support from the Universidad de Cantabria through the Augusto G. Linares program. P.G.P.-G. acknowledges support from the Spanish Programa Nacional de Astronomía y Astrofísica under grants AYA2009-07723-E and AYA2009-10368. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM). We acknowledge financial contribution from the agreement ASI-INAF I/009/10/0 and from the INAF-PRIN-2011., Context. Accretion onto supermassive black holes is believed to occur mostly in obscured active galactic nuclei (AGN). Such objects are proving rather elusive in surveys of distant galaxies, including those at X-ray energies. Aims. Our main goal is to determine whether the revised IRAC criteria of Donley et al. (2012, ApJ, 748, 142; objects with an infrared (IR) power-law spectral shape), are effective at selecting X-ray type-2 AGN (i.e., absorbed N_H > 10^22 cm^-2). Methods. We present the results from the X-ray spectral analysis of 147 AGN selected by cross-correlating the highest spectral quality ultra-deep XMM-Newton and the Spitzer/IRAC catalogues in the Chandra Deep Field South. Consequently it is biased towards sources with high S/N X-ray spectra. In order to measure the amount of intrinsic absorption in these sources, we adopt a simple X-ray spectral model that includes a power-law modified by intrinsic absorption at the redshift of each source and a possible soft X-ray component. Results. We find 21/147 sources to be heavily absorbed but the uncertainties in their obscuring column densities do not allow us to confirm their Compton-Thick nature without resorting to additional criteria. Although IR power-law galaxies are less numerous in our sample than IR non-power-law galaxies (60 versus 87 respectively), we find that the fraction of absorbed (N_H^intr > 10^22 cm^-2) AGN is significantly higher (at about 3 sigma level) for IR-power-law sources (similar to 2/3) than for those sources that do not meet this IR selection criteria (~1/2). This behaviour is particularly notable at low luminosities, but it appears to be present, although with a marginal significance, at all luminosities. Conclusions. We therefore conclude that the IR power-law method is efficient in finding X-ray-absorbed sources. We would then expect that the long-sought dominant population of absorbed AGN is abundant among IR power-law spectral shape sources not detected in X-rays., Ministerio de Economía y Competitividad (MINECO), European Space Agency (ESA), National Aeronautics and Space Administration (NASA), Consejo Superior de Investigaciones Científicas (CSIC), Universidad de Cantabria (UC), Programa Nacional de Astronomía y Astrofísica (PNAyA), España, Programa JAE-Doc (CSIC), Fondo Social Europeo (FSE), Unión Europea (UE), Programa Augusto G. Linares (UC), 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 Journal © 2013 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. AH-C and AA-H acknowledge funding by the Universidad de Cantabria Augusto González Linares program. We acknowledge support from the Spanish Programa Nacional de Astronomía y Astrofísica under grants AYA2009-07723-E and AYA2009-10368. SHARDS has been funded by the Spanish MICINN/MINECO under the Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM). Based on observations made with the GTC, installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. We thank all the GTC Staff for their support and enthusiasm with the SHARDS project, and we would like to especially acknowledge the help from Antonio Cabrera and Rene Rutten. We also thank the anonymous referee for their useful comments that helped to improve this paper., We report on results from the analysis of a stellar mass-selected (log (M-*/M-circle dot) >= 9.0) sample of 1644 galaxies at 0.65 < z < 1.1 with ultradeep (m(AB) < 26.5) optical medium-band (R similar to 50) photometry from the Survey for High-z Absorption Red and Dead Sources (SHARDS). The spectral resolution of SHARDS allows us to consistently measure the strength of the 4000 A spectral break [D-n(4000), an excellent age indicator for the stellar populations of quiescent galaxies] for all galaxies at z similar to 0.9 down to log (M-*/M-circle dot) similar to 9. The D-n(4000) index cannot be resolved from broad-band photometry, and measurements from optical spectroscopic surveys are typically limited to galaxies at least 10 times more massive. When combined with the rest-frame U - V colour, (U - V)(r), D-n(4000) provides a powerful diagnostic of the extinction affecting the stellar population that is relatively insensitive to degeneracies with age, metallicity or star formation history. We use this novel approach to estimate de-reddened colours and light-weighted stellar ages for individual sources. We explore the relationships linking stellar mass, (U - V)(r), and D-n(4000) for the sources in the sample, and compare them to those found in local galaxies. The main results are: (a) both D-n(4000) and (U - V)(r) correlate with M-*. The dispersion in D-n(4000) values at a given M-* increases with M-*, while the dispersion for (U - V)(r) decreases due to the higher average extinction prevalent in massive star-forming galaxies. (b) For massive galaxies, we find a smooth transition between the blue cloud and red sequence in the intrinsic U - V colour, in contrast with other recent results. (c) At a fixed stellar age, we find a positive correlation between extinction and stellar mass. (d) The fraction of sources with declining or halted star formation increases steeply with the stellar mass, from similar to 5 per cent at log (M-*/M-circle dot) = 9.0-9.5 to similar to 80 p, Universidad de Cantabria Augusto Gonzalez Linares program, Spanish Programa Nacional de Astronomia y Astrofisica, Spanish MICINN/MINECO under the Consolider-Ingenio Program, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2010. The American Astronomical Society. This work was supported by the Spanish Programa Nacional de Astronomía y Astrofísica through the project numbers AYA2006-12955, AYA2006-02358, and AYA 2006-15698-C02-02. This work was partially funded by the Spanish MEC under the Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC (http://www.iac.es/consolider-ingenio-gtc/).This work is based on HST/ACS images from GOODS HST Treasury Program, which is supported by NASA through grants HST-GO-09425.01-A and HST-GO-09583.01, and in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, Caltech under NASA contract 1407.P. G. P. G. acknowledges support from the Ramón y Cajal Program financed by the Spanish Government and the European Union., We study the evolution of galaxy structure since z ~ 1 to the present. From a Great Observatories Origins Deep Survey South (GOODS-S) multi-band catalog, we define (blue) luminosity- and mass-weighted samples, limited by MB ≤ –20 and M sstarf ≥ 1010 M ☉, comprising 1122 and 987 galaxies, respectively. We extract early-type (ET; E/S0/Sa) and late-type (LT; Sb-Irr) subsamples by their position in the concentration-asymmetry plane, in which galaxies exhibit a clear bimodality. We find that the ET fraction, f ET, rises with cosmic time, with a corresponding decrease in the LT fraction, f LT, in both luminosity- and mass-selected samples. However, the evolution of the comoving number density is very different: the decrease in the total number density of MB ≤ –20 galaxies since z = 1 is due to the decrease in the LT population, which accounts for ~75% of the total star formation rate in the range under study, while the increase in the total number density of M sstarf ≥ 1010 M ☉ galaxies in the same redshift range is due to the evolution of ETs. This suggests that we need a structural transformation between LT galaxies that form stars actively and ET galaxies in which the stellar mass is located. Comparing the observed evolution with the gas-rich major merger rate in GOODS-S, we infer that only ~20% of the new ET galaxies with M sstarf ≥ 1010 M ☉ appeared since z ~ 1 can be explained by this kind of mergers, suggesting that minor mergers and secular processes may be the driving mechanisms of the structural evolution of intermediate-mass (M sstarf ~ 4 × 1010 M ☉) galaxies since z ~ 1., Programa Nacional de Astronomía y Astrofísica (MICINN), España, Ministerio de Educación y Ciencia (MEC), España, National Aeronautics and Space Administration (NASA), Gobierno de España, Unión Europea (UE), Programa Consolider-Ingenio (MINECO), España, Ministerio de Economía y Competitividad (MINECO), España, GOODS HST Treasury Program (NASA), Jet Propulsion Laboratory, Caltech, Programa Ramón y Cajal, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© The European Southern Observatory (ESO). This paper is based on observations obtained at the German-Spanish Astronomical Centre, Calar Alto, Spain, operated by the Max-Planck Institut für Astronomie (MPIA), Heidelberg, jointly with the Spanish Commission for Astronomy. It is also partly based on observations made with the Jacobus Kapteyn 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 de Astrofísica de Canarias and the 1.52 m telescope of the EOCA/OAN 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. We have also use of the LEDA database, http://www-obs.univ-lyon1.fr. This research was also supported by the Spanish Programa Sectorial de Promoción General del Conocimiento under grants PB96-0610 and PB96-0645. We would like to thank C.E. García Dabó and S. Pascual for their help during part of the observing runs. We are grateful to Dr. M. Fukugita for his helpful remarks that have improved this paper., We present Johnson B CCD photometry for the whole sample of galaxies of the Universidad Complutense de Madrid (UCM) Survey Lists I and II. They constitute a well-defined and complete sample of galaxies in the Local Universe with active star formation. The data refer to 191 SO to Irr galaxies at an averaged redshift of 0.027, and complement the already published Gunn r, J and K photometries. In this paper the observational and reduction features are discussed in detail, and the new colour information is combined to search for clues on thee properties of the galaxies, mainly by comparing our sample with other surveys., National Aeronautics and Space Administration (NASA), 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

© 2013 The American Astronomical Society. All rights reserved. Artículo firmado por 37 autores. Support for Program number HST-GO-12060 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. G.B. acknowledges support from NSF grant AST-08-08133. P.G.P.-G. acknowledges support from grant AYA2009-07723-E., We combine high-resolution Hubble Space Telescope/WFC3 images with multi-wavelength photometry to track the evolution of structure and activity of massive (M_*> 10^10 M_☉) galaxies at redshifts z = 1.4-3 in two fields of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. We detect compact, star-forming galaxies (cSFGs) whose number densities, masses, sizes, and star formation rates (SFRs) qualify them as likely progenitors of compact, quiescent, massive galaxies (cQGs) at z = 1.5-3. At z≲2, cSFGs present SFR = 100-200 M_☉ yr^–1, yet their specific star formation rates (sSFR ~ 10^–9 yr^–1) are typically half that of other massive SFGs at the same epoch, and host X-ray luminous active galactic nuclei (AGNs) 30 times (~30%) more frequently. These properties suggest that cSFGs are formed by gas-rich processes (mergers or disk-instabilities) that induce a compact starburst and feed an AGN, which, in turn, quench the star formation on dynamical timescales (few 10^8 yr). The cSFGs are continuously being formed at z = 2-3 and fade to cQGs down to z ~ 1.5. After this epoch, cSFGs are rare, thereby truncating the formation of new cQGs. Meanwhile, down to z = 1, existing cQGs continue to enlarge to match local QGs in size, while less-gas-rich mergers and other secular mechanisms shepherd (larger) SFGs as later arrivals to the red sequence. In summary, we propose two evolutionary tracks of QG formation: an early (z≲2), formation path of rapidly quenched cSFGs fading into cQGs that later enlarge within the quiescent phase, and a late-arrival (z≳2) path in which larger SFGs form extended QGs without passing through a compact state., National Aeronautics and Space Administration (NASA), Space Telescope Science Institute (STSI), National Science Foundation (NSF), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2009. We thank the referee M. Bershady for his useful and constructive comments. We acknowledge support from the Spanish Programa Nacional de Astronomía y Astrofísica under grant AYA 2006-02358. Partially funded by the Spanish MEC under the Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC (http://www.iac.es/consolider-ingenio-gtc/). Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut fur Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). This article is based on observations made with the WHT operated on the island of La Palma by the Instituto Astrofísico de Canarias in the Spanish Observatorio del Roque de los Muchachos. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, Caltech under NASA contract 1407. GALEX is a NASA Small Explorer launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and scientific analysis of the GALEX mission. Based in part on data collected at Subaru Telescope and obtained from the SMOKA, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan. 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. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii., Context. The galaxy number counts has been traditionally used to test models of galaxy evolution. However, the origin of significant differences in the shape of number counts at different wavelengths is still unclear. By relating the most remarkable features in the number counts with the underlying galaxy population it is possible to introduce further constraints on galaxy evolution. Aims. We aim to investigate the causes of the different shape of the K-band number counts when compared to other bands, analyzing in detail the presence of a change in the slope around K similar to 17.5. Methods. We present a near-infrared imaging survey, conducted at the 3.5 m telescope of the Calar Alto Spanish-German Astronomical Center (CAHA), covering two separated fields centered on the HFDN and the Groth field, with a total combined area of similar to 0.27 deg(2) to a depth of K similar to 19 (3 sigma, Vega). By combining our data with public deep K-band images in the CDFS (GOODS/ISAAC) and high quality imaging in multiple bands, we extract K-selected catalogs characterized with highly reliable photometric redshift estimates. We derive redshift binned number counts, comparing the results in our three fields to sample the effects of cosmic variance. We derive luminosity functions from the observed K-band in the redshift range [0.25-1.25], that are combined with data from the references in multiple bands and redshifts, to build up the K-band number count distribution. Results. The overall shape of the number counts can be grouped into three regimes: the classic Euclidean slope regime (d log N/dm similar to 0.6) at bright magnitudes; a transition regime at intermediate magnitudes, dominated by M* galaxies at the redshift that maximizes the product phi*dVc/d Omega; and an alpha dominated regime at faint magnitudes, where the slope asymptotically approaches -0.4(alpha + 1) controlled by post-M* galaxies. The slope of the K-band number counts presents an averaged decrement of similar t, Spanish Programa Nacional de Astronomia y Astrofísica, Spanish MEC, NASA, National Astronomical Observatory of Japan, National Science Foundation, Canada-France-Hawaii Telescope (CFHT), National Research Council (NRC) of Canada, Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, University of Hawaii, 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

© 2012. The American Astronomical Society. All rights reserved. We thank the anonymous referee for reviewing the manuscript, and for the comments and suggestions that helped to improve the content of the paper. We also thank Carmen Eliche Moral, Fabián Rosales Ortega, Judit Bakos, and Sheila Kannappan for helpful discussions. R. A. Marino was also funded by the Spanish program International Campus of Excellence Moncloa (CEI). We thank the Calar Alto Observatory for the allocation of the director's discretionary time to this program. We acknowledge support from the Spanish Programa Nacional de Astronomía y Astrofísica under grant AYA 2009-10368. We are also partially funded by the Spanish MICINN under the Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC. J.C.M.M. receives financial support from NASA JPL/Spitzer grant RSA 1374189. He also acknowledges support from the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, Caltech under NASA contract 1407. GALEX is a NASA Small Explorer launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and scientific analysis of the GALEX mission. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, and the California Institute of Technology, under contract with the National Aeronautics and Space Administration. 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, We present an analysis of the full bidimensional optical spectral cube of the nearby spiral galaxy NGC 5668, observed with the Pmas fiber PAcK Integral Field Unit (IFU) at the Calar Alto observatory 3.5 m telescope. We make use of broadband imaging to provide further constraints on the evolutionary history of the galaxy. This data set will allow us to improve our understanding of the mechanisms that drive the evolution of disks. We investigated the properties of 62 H II regions and concentric rings in NGC 5668 and derived maps in ionized-gas attenuation and chemical (oxygen) abundances. We find that while inward of r similar to 36 '' similar to 4.4 kpc similar to 0.36 (D-25/2) the derived O/H ratio follows the radial gradient typical of spiral galaxies, the abundance gradient beyond r similar to 36 '' flattens out. The analysis of the multi-wavelength surface brightness profiles of NGC 5668 is performed by fitting these profiles with those predicted by chemo-spectrophotometric evolutionary models of galaxy disks. From this, we infer a spin and circular velocity of lambda = 0.053 and nu(c) = 167 km s(-1), respectively. The metallicity gradient and rotation curve predicted by this best-fitting galaxy model nicely match the values derived from the IFU observations, especially within r similar to 36 ''. The same is true for the colors despite some small offsets and a reddening in the bluest colors beyond that radius. On the other hand, deviations of some of these properties in the outer disk indicate that a secondary mechanism, possibly gas transfer induced by the presence of a young bar, must have played a role in shaping the recent chemical and star formation histories of NGC 5668., Spanish program International Campus of Excellence Moncloa (CEI), Spanish Programa Nacional de Astronomía y Astrofísica, Spanish MICINN, NASA JPL/Spitzer, National Radio Astronomy Observatory, NASA, Alfred P. Sloan Foundation, National Science Foundation, U.S. Department of Energy, National Aeronautics and Space Administration, Japanese Monbukagakusho, Max Planck Society, Higher Education Funding Council for England, Astrophysical Research Consortium, American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, Institute for Advanced Study, Japan Participation Group, Johns Hopkins University, Joint Institute for Nuclear Astrophysics, Kavli Institute for Particle Astrophysics and Cosmology, Korean Scientist Group, Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, Max-Planck-Institute for Astronomy (MPIA), Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, United States Naval Observatory, University of Washington, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. We are grateful with the anonymous referee for improving the manuscript contents. NEB and JZ acknowledge funding support from the Spanish Programa Nacional de Astronomía y Astrofísica under grant AYA2006-02358. NEB acknowledges support from Fac. CC. Físicas, Universidad Complutense de Madrid (UCM), and from Coordinación de Astrofísica, Instituto Nacional de Astrofísica ptica y Electrónica (INAOE). PGPG acknowledges funding support from the Spanish Government under grant PGC2018-093499-B-I00. LRM acknowledges support from grant PRIN MIUR 2017-20173ML3WW_001 and funding from the Universita degli studi di Padova - Dipartimento di Fisica e Astronomia 'G. Galilei'. This work has made use of the rainbow Cosmological Surveys Database, which is operated by the Centro de Astrobiología (CAB/CSIC-INTA)., We study in detail the properties of the stellar populations of 111 massive [log (M-*/M-circle dot) >= 10] dusty [far-infrared (FIR)-selected] starburst (SFR/SFRMS > 2) galaxies at 0.7 < z < 1.2. For that purpose, we use self-consistent methods that analyse the UV-to-FIR broad-band observations in terms of the stellar light and dust re-emission with energy-balance techniques. We find that the emission of our starburst galaxies can be interpreted as a recent star formation episode superimposed on a more evolved stellar population. On average, the burst age is similar to 80 Myr and its attenuation similar to 2.4 mag. Assuming our starburst galaxies at half their lifetimes, we infer a duration of the starburst phase of similar to 160 Myr. The median stellar mass and star formation rate (SFR) are log (M-*/M-circle dot) similar to 10.6 and similar to 220 M(circle dot)yr(-1). Assuming this SFR and the inferred duration of the starburst phase, the stellar mass added during this phase corresponds to similar to 40 per cent the median stellar mass of our sample. The young-population age determines the position of our galaxies in the M-*-SFR plane. Galaxies located at the largest distances of the MS present shorter young-population ages. The properties of the underlying stellar population cannot be constrained accurately with our broad-band data. We also discuss the impact of including the FIR data and energy-balance techniques in the analysis of the properties of the stellar populations in starburst galaxies., Ministerio de Ciencia e Innovación (MICINN), Universita degli studi di Padova - Dipartimento di Fisica e Astronomia 'G. Galilei', Facultad Ciencias Físicas, Universidad Complutense de Madrid (UCM), Coordinación de Astrofísica, Instituto Nacional de Astrofísica Óptica y Electrónica (INAOE), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. Artículo firmado por 24 autores. We are grateful to the anonymous referee for her/his constructive comments. 1,R -M thanks Casiana Mufoz Tuthill for useful suggestions on this manuscript. LR-M, GR, and AF acknowledge the support from grant PRIN MIUR 2017-20173ML3WW_001. LR-M also acknowledges funding support from the University degli Studi di Padova -Dipartimento di Fisica e Astronomia '(1. Gal ilei'. POP -G and LC acknowledge support from Spanish Ministerio de Ciencia, Innovación y Universidades through grant PGC2018-093499-13100. LC acknowledges also financial support from Comunidad de Madrid under Atraccian de Talents grant 2018-T2/TIC-11612. AVG acknowledges support from the European Research Council through the Advanced Grant MIST (H7/2017-2020, No. 742719). AP gratefully acknowledges financial support from STFC through grants ST/T000244/1 and ST/P000541/1. Analyses were performed in R 3.6.1 (R Core Team 2019)., We use a sample of 706 galaxies, selected as [O II]lambda 3727 ([O II]) emitters in the Survey for High-z Absorption Red and Dead Sources SHARDS) on the CANDELS/GOODS-N field, to study the differential attenuation of the nebular emission with respect to the stellar continuum. The sample includes only galaxies with a counterpart in the infrared and log(10) (M-*/M-circle dot) > 9, over the redshift interval 0.3 less than or similar to z less than or similar to 1.5. Our methodology consists in the comparison of the star formation rates inferred from [O II] and Haemission lines with a robust quantification of the total star-forming activity (SFR TOT) that is independently estimated based on both infrared and ultraviolet (UV) luminosities. We obtain f = E(B - V)(stellar)/E(B - V)(nebular) = 0.69(0.69)(0.71) and 0.55(0.53)(0.56) for [O II] and H alpha, respectively. Our resulting f-factors display a significant positive correlation with the UV attenuation and shallower or not-significant trends with the stellar mass, the SFR TOT, the distance to the main sequence, and the redshift. Finally, our results favour an average nebular attenuation curve similar in shape to the typical dust curve of local starbursts., Unión Europea. Horizonte 2020, Ministerio de Ciencia e Innovación (MICINN), PRIN MIUR, University degli Studi di Padova - Dipartimento di Fisica e Astronomia, Comunidad de Madrid under Atraccian de Talents, STFC, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2022. The Author(s). Published by the American Astronomical Society. We would like to thank the anonymous referee for improving the content of the manuscript. We are grateful to Ignacio Trujillo and Christopher J. Conselice for the useful discussions and comments. L.C. wishes to thank Cristina Cabello for the support provided while this project was devised and Michele Perna for the fruitful discussions. L.C. acknowledges financial support from Comunidad de Madrid under Atraccion de Talento grant 2018-T2/TIC-11612. L.C. and P.G.P.G. acknowledge support from the Spanish Ministerio de Ciencia, Innovación y Universidades through grant PGC2018-093499-B-I00. J.M.A. acknowledges the support of the Viera y Clavijo Senior program funded by ACIISI and ULL. D.C. is a Ramón-Cajal Researcher and supported by the Ministerio de Ciencia, Innovación y Universidades (MICIU/FEDER) under research grant PGC2018-094975-C21. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Centro de Astrobiología (CAB/INTA), partnered with the University of California Observatories at Santa Cruz (UCO/Lick, UCSC)., We investigate the assembly history of massive disk galaxies and describe how they shape their morphology through cosmic time. Using SHARDS and HST data, we modeled the surface brightness distribution of 91 massive galaxies at redshift 0.14 < z <= 1 in the wavelength range 0.5-1.6 mu m, deriving the uncontaminated spectral energy distributions of their bulges and disks separately. This spectrophotometric decomposition allows us to compare the stellar population properties of each component in individual galaxies. We find that the majority of massive galaxies (similar to 85%) build inside-out, growing their extended stellar disk around the central spheroid. Some bulges and disks could start forming at similar epochs, but these bulges grow more rapidly than their disks, assembling 80% of their mass in similar to 0.7 and similar to 3.5 Gyr, respectively. Moreover, we infer that both older bulges and older disks are more massive and compact than younger stellar structures. In particular, we find that bulges display a bimodal distribution of mass-weighted ages; i.e., they form in two waves. In contrast, our analysis of the disk components indicates that they form at z similar to 1 for both first- and second-wave bulges. This translates to first-wave bulges taking longer to acquire a stellar disk (5.2 Gyr) compared to second-wave, less compact spheroids (0.7 Gyr). We do not find distinct properties (e.g., mass, star formation timescale, and mass surface density) for the disks in both types of galaxies. We conclude that the bulge mass and compactness mainly regulate the timing of the stellar disk growth, driving the morphological evolution of massive disk galaxies., Ministerio de Ciencia e Innovación (MICINN)/FEDER, Comunidad de Madrid, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2020. We thank José Acosta Pulido for valuable scientific discussions and the anonymous referee for the thorough revision of the manuscript. Thanks also to Yue Shen for making his QSO1 near-infrared spectra available. Partly based on observations made with the GTC telescope and the EMIR instrument at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias (program GTC14-19A). We thank the GTC staff for their support with the observations. We thank Joel Vernet for providing the high z NLRG composite spectrum. M. V. M. acknowledges support from the Spanish Ministerio de Ciencia, Innovación y Universidades through the grants AYA2015- 64346-C2-2-P and PGC2018-094671-B-I00 (MCIU/AEI/FEDER,UE). M. P. is supported by the Programa Atracción de Talento de la Comunidad de Madrid via grant 2018-T2/TIC-11715. M. P. acknowledges support from the Spanish Ministerio de Economía y Competitividad through the grant ESP2017- 83197-P. AH acknowledges FCT Fellowship SFRH/BPD/107919/2015; Support from European Community Programme (FP7/2007-2013) under grant agreement No. PIRSES-GA-2013-612701 (SELGIFS); Support from FCT through national funds (PTDC/FIS-AST/3214/2012 and UID/FIS/04434/2013), and by FEDER through COMPETE (FCOMP-01-0124-FEDER-029170) and COMPETE2020 (POCI-01-0145-FEDER-007672). S. M. acknowledges financial support through grant AYA2016-76730-P (MINECO/FEDER). This research has made use of: (1) the VizieR catalogue access tool, CDS, Strasbourg, France. The original description of the VizieR service was published in Ochsenbein et al. A&AS, 143, 23; (2) data from Sloan Digital Sky Survey. 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, Context. Core extremely red quasars (core ERQ) have been proposed to represent an intermediate evolutionary phase in which a heavily obscured quasar blows out the circumnuclear interstellar medium with very energetic outflows before it becomes an optical quasar. Aims. We investigate whether the properties of core ERQ fit the AGN orientation-based unification scenario. Methods. We revised the general UV and optical emission line properties of core ERQ in the context of the orientation-based scenario. We used diagnostic diagrams based on UV emission line ratios and UV-to-optical line kinematic information to compare the physical and kinematic gas properties of core ERQ with those of other luminous narrow- and broad-line AGN. In particular, we provide a revised comparison of the [OIII] kinematics in 21 core ERQ (20 from Perrotta et al. 2019, MNRAS, 488, 4126 and SDSS J171420.38+414815.7, based on GTC EMIR near-infrared spectroscopy) with other samples of quasars with matching luminosity with the aim of evaluating whether core ERQ host the most extreme [OIII] outflows. Results. The UV line ratios suggest that the physical properties (e.g., density and metallicity) of the ionised gas in core ERQ are similar to those observed in the broad-line region of blue nitrogen-loud quasars. The [OIII] outflow velocities of core ERQ are on average consistent with those of very luminous blue type 1 quasars, although extreme outflows are much more frequent in core ERQ. These similarities can be explained in the context of the AGN unification model under the assumption that core ERQ are viewed with an intermediate orientation between type 2 (edge-on) and type 1 (face-on) quasars. Conclusions. We propose that core ERQ are very luminous but otherwise normal quasars viewed at an intermediate orientation. This orientation allows a direct view of the outer part of the large broad-line region from which core ERQ UV line emission originates; the extreme [OIII] outflow velocities are instead a, Unión Europea. FP7, Ministerio de Ciencia e Innovación (MICINN)/FEDER, Ministerio de Economía y Competitividad (MINECO)/FEDER, Comunidad de Madrid, Fondo Europeo de Desarrollo Regional (FEDER), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2019 RAS., A diverse range of dust attenuation laws is found in star-forming galaxies. In particular, Tress et al. (2018) studied the SHARDS survey to constrain the NUV bump strength (B) and the total-to-selective ratio (R_(V)) of 1,753 star-forming galaxies in the GOODS-N field at 1.5

The work of A.C., D.S., M.D.-Z.,L.M. and V.T. is supported by the STARFORM Sinergia Project funded by the Swiss National Science Foundation. J.R. acknowledges support from the European Research Council starting grant 336736-CALENDS. P.G. P.-P. acknowledges support from Spanish Government MINECO grants AYA2015-70815-ERC and AYA2015-63650-P. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM), partnered with the University of California Observatories at Santa Cruz (UCO/Lick, UCSC). Based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST- ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA)., Giant stellar clumps are ubiquitous in high-redshift galaxies(1,2). They are thought to play an important role in the build-up of galactic bulges(3) and as diagnostics of star formation feedback in galactic discs(4). Hubble Space Telescope (HST) blank field imaging surveys have estimated that these clumps have masses of up to 10(9.5) M-circle dot and linear sizes of greater than or similar to 1 kpc(5,6). Recently, gravitational lensing has also been used to get higher spatial resolution(7-9). However, both recent lensed observations(10,11) and models(12,13) suggest that the clumps' properties may be overestimated by the limited resolution of standard imaging techniques. A definitive proof of this observational bias is nevertheless still missing. Here we investigate directly the effect of resolution on clump properties by analysing multiple gravitationally lensed images of the same galaxy at different spatial resolutions, down to 30 pc. We show that the typical mass and size of giant clumps, generally observed at similar to 1 kpc resolution in high-redshift galaxies, are systematically overestimated. The high spatial resolution data, only enabled by strong gravitational lensing using currently available facilities, support smaller scales of clump formation by fragmentation of the galactic gas disk via gravitational instabilities., Unión Europea. FP7, Ministerio de Economía y Competitividad (MINECO), STARFORM Sinergia Project - Swiss National Science Foundation, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Artículo firmado por 45 autores. We thank the directors of the Space Telescope Science Institute, the Gemini Observatory, the GTC and the European Southern Observatory for granting us discretionary time. We thank B. Katz, D. Kushnir, B. Periello, I. Momcheva, T. Royale, L. Strolger, D. Coe, J. Lotz, M. L. Graham, R. Humphreys, R. Kurucz, A. Dolphin, M. Kriek, S. Rajendran, T. Davis, I. Hubeny, C. Leitherer, F. Nieva, D. Kasen, J. Mauerhan, D. Kelson, J. M. Silverman, A. Oscoz Abaz and Z. Levay for help with the observations and other assistance. The Keck Observatory was made possible with the support of the W. M. Keck Foundation. NASA/STScI grants 14041, 14199, 14208, 14528, 14872 and 14922 provided financial support. P.L.K., A.V.F. and W.Z. are grateful for assistance from the Christopher R. Redlich Fund, the TABASGO Foundation and the Miller Institute for Basic Research in Science (U. C. Berkeley). The work of A.V.F. was completed in part at the Aspen Center for Physics, which is supported by NSF grant PHY-1607611. J.M.D. acknowledges support of projects AYA2015-64508-P (MINECO/FEDER, UE) and AYA2012-39475-C02-01 and the consolider project CSD2010-00064 funded by the Ministerio de Economía y Competitividad. P.G.P.-G. acknowledges support from Spanish government MINECO grants AYA2015-70815-ERC and AYA2015-63650-P. M.O. is supported by JSPS KAKENHI grants 26800093 and 15H05892. M. J. acknowledges support by the Science and Technology Facilities Council (grant ST/L00075X/1). R.J.F. is supported by NSF grant AST-1518052 and Sloan and Packard Foundation fellowships. M.N. acknowledges support from PRIN-INAF-2014 1.05.01.94.02. O.G. was supported by NSF Fellowship under award AST-1602595. J.H. acknowledges support from a VILLUM FONDEN Investigator Grant (16599). HST imaging was obtained at https://archive.stsci.edu., Galaxy-cluster gravitational lenses can magnify background galaxies by a total factor of up to similar to 50. Here we report an image of an individual star at redshift z = 1.49 (dubbed MACS J1149 Lensed Star 1) magnified by more than x 2,000. A separate image, detected briefly 0.26 '' from Lensed Star 1, is probably a counterimage of the first star demagnified for multiple years by an object of greater than or similar to 3 solar masses in the cluster. For reasonable assumptions about the lensing system, microlensing fluctuations in the stars' light curves can yield evidence about the mass function of intracluster stars and compact objects, including binary fractions and specific stellar evolution and supernova models. Dark-matter subhaloes or massive compact objects may help to account for the two images' long-term brightness ratio., Ministerio de Economía y Competitividad (MINECO)/FEDER, Ministerio de Economía y Competitividad (MINECO), NASA/STScI, NSF, JSPS KAKENHI, Science and Technology Facilities Council, Sloan and Packard Foundation fellowships, PRIN-INAF, VILLUM FONDEN Investigator Grant, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2018. The American Astronomical Society. All rights reserved. Artículo firmado por 22 autores. We acknowledge the anonymous referee for constructive comments and suggestions that significantly improved this paper. We thank Steven Willner for helpful comments on the manuscript, and Shude Mao for useful discussion. We acknowledge support from the NSF grants of China (11573017,11733006) and the CANDELS program HST-GO-12060 by NASA through a grant from the STScI. Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This work is partly based on observations taken by the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. S.M.F., D.C.K., Y.G., and H.M.Y. acknowledge partial support from US NSF grant AST-16-15730. P.G.P.-G. acknowledges support from Spanish Government MINECO AYA2015-70815-ERC and AYA2015-63650-P Grants., We investigate the galaxy quenching process at intermediate redshift using a sample of similar to 4400 galaxies with M-* >10(9) M-circle dot between redshift 0.5 and 1.0 in all five CANDELS fields. We divide this sample, using the integrated specific star formation rate (sSFR), into four subgroups: star-forming galaxies (SFGs) above and below the ridge of the star-forming main sequence (SFMS), transition galaxies and quiescent galaxies. We study their UVI (U -V versus V-I) color gradients to infer their sSFR gradients out to twice effective radii. We show that on average both star-forming and transition galaxies at all masses are not fully quenched at any radii, whereas quiescent galaxies are fully quenched at all radii. We find that at low masses (M-* = 10(9) - 10(10) M-circle dot) SFGs both above and below the SFMS ridge generally have flat sSFR profiles, whereas the transition galaxies at the same masses generally have sSFRs that are more suppressed in their outskirts. In contrast, at high masses (M-* > 10(10.5) M-circle dot), SFGs above and below the SFMS ridge and transition galaxies generally have varying degrees of more centrally suppressed sSFRs relative to their outskirts. These findings indicate that at z similar to 0.5-1.0 the main galaxy quenching mode depends on its already formed stellar mass, exhibiting a transition from "the outside-in" at M*<= 10(10) M-circle dot to "the inside-out" at M-* > 10(10.5) M-circle dot. In other words, our findings support that internal processes dominate the quenching of massive galaxies, whereas external processes dominate the quenching of low-mass galaxies., Ministerio de Economía y Competitividad (MINECO), NSF grants of China, NASA through a grant from the STScI, NASA, 3D-HST Treasury Program, US NSF, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2017 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. Artículo firmado por 40 autores. This work is dedicated in memory of K. N. V. S. Kishore Babu, a dear friend who inspired KBM to pursue Astrophysics. We are grateful to Peter Behroozi, Mark Brodwin, Philip Hopkins, Kartheik Iyer, Allison Kirkpatrick, Viraj Pandya, Vicente Rodríguez Gómez, Brett Salmon, and Raymond Simons for helpful comments and discussions during different manifestations of this work. Special thanks to Daniel Shanaberger for carefully reading the manuscript, thanks to Gillen Brown, Cody Ciaschi, Bandon Decker, Benjamin Floyd, Ripon Saha, and Madalyn Weston for their valuable inputs during the University of Missouri Kansas City (UMKC) Galaxy Evolution Group discussions. DHM and KBM acknowledge support from the Missouri Consortium of National Aeronautics and Space Administration (NASA)'s National Space Grant College and Fellowship Program, and funding from the University of Missouri Research Board. RSS acknowledges support from the Downsbrough family, and from the Simons Foundation. SL acknowledges support from the National Research Foundation of Korea grant, no. 2017R1A3A3001362, funded by the Korea government. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for Program number HST-GO-12060 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This publication makes use of the SDSS. Funding for the creation and distribution of the SDSS Archive has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the NASA, the Japanese Monbuk, The rate of major galaxy-galaxy merging is theoretically predicted to steadily increase with redshift during the peak epoch of massive galaxy development (1 <= z <= 3). We use close-pair statistics to objectively study the incidence of massive galaxies (stellar M1 > 2 x 10(10)M(circle dot)) hosting major companions (1 <= M-1/M-2 <= 4; i.e. <4: 1) at six epochs spanning 0 < z < 3. We select companions from a nearly complete, mass-limited (>= 5 x 10(9)M(circle dot)) sample of 23 696 galaxies in the five Cosmic Assembly Near-Infrared Deep Extragalactic Legacy Survey fields and the Sloan Digital Sky Survey. Using 5-50 kpc projected separation and close redshift proximity criteria, we find that the major companion fraction f(mc)(z) based on stellar mass-ratio (MR) selection increases from 6 per cent (z similar to 0) to 16 per cent (z similar to 0.8), then turns over at z similar to 1 and decreases to 7 per cent (z similar to 3). Instead, if we use a major F160W flux-ratio (FR) selection, we find that f(mc)(z) increases steadily until z similar to 3 owing to increasing contamination from minor (MR > 4: 1) companions at z > 1. We show that these evolutionary trends are statistically robust to changes in companion proximity. We find disagreements between published results are resolved when selection criteria are closely matched. If we compute merger rates using constant fraction-to-rate conversion factors (C-merg,C-pair = 0.6 and T-obs,T-pair = 0.65 Gyr), we find that MR rates disagree with theoretical predictions at z > 1.5. Instead, if we use an evolving T-obs,T-pair(z) alpha (1 + z)- 2 from Snyder et al., our MR-based rates agree with theory at 0 < z < 3. Our analysis underscores the need for detailed calibration of C-merg,C-pair and T-obs,T-pair as a function of redshift, mass, and companion selection criteria to better constrain the empirical major merger history., Missouri Consortium of National Aeronautics and Space Administration (NASA)'s National Space Grant College and Fellowship Program, University of Missouri Research Board, Simons Foundation, National Research Foundation of Korea - Korea government, NASA, Alfred P. Sloan Foundation, National Science Foundation, US Department of Energy, Japanese Monbukagakusho, Max Planck Society, Higher Education Funding Council for England, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. Artículo firmado por 14 autores. We would like to thank Sandro Bressan for his comments and suggestions. MT acknowledges support from the Mexican 'Consejo Nacional de Ciencia y Tecnología' (CONACyT), with scholarship #329741, as well as the Royal Astronomical Society for travel funding related to this project. EMQ acknowledges the support of the European Research Council via the award of a Consolidator Grant (PI McLure). PGP wishes to acknowledge support from Spanish Government MINECO Grants AYA2015-63650-P and AYA201570815-ERC. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM), partnered with the University of California Observatories at Santa Cruz (UCO/Lick, UCSC). Based on observations made with the GTC, installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma., We make use of the Survey of High-z Absorption Red and Dead Sources, an ultradeep (<26.5AB) galaxy survey that provides optical photospectra at resolution R similar to 50, via medium-band filters (FWHM similar to 150 angstrom). This data set is combined with ancillary optical and NIR fluxes to constrain the dust attenuation law in the rest-frame NUV region of star-forming galaxies within the redshift window 1.5 < z < 3. We focus on the NUV bump strength (B) and the total-to-selective extinction ratio (R-V), targeting a sample of 1753 galaxies. By comparing the data with a set of population synthesis models coupled to a parametric dust attenuation law, we constrain R-V and B, as well as the colour excess, E(B - V). We find a correlation between R-V and B, which can be interpreted either as a result of the grain size distribution, or a variation of the dust geometry among galaxies. According to the former, small dust grains are associated with a stronger NUV bump. The latter would lead to a range of clumpiness in the distribution of dust within the interstellar medium of star-forming galaxies. The observed wide range of NUV bump strengths can lead to a systematic in the interpretation of the UV slope beta typically used to characterize the dust content. In this study, we quantify these variations, concluding that the effects are Delta beta similar to 0.4., Ministerio de Economía y Competitividad (MINECO), Consejo Nacional de Ciencia y Tecnología (CONACyT), Royal Astronomical Society, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Artículo firmado por 13 autores. We thank Seong-Kook Lee for helpful comments on the manuscript, and we thank Aldo Rodríguez Puebla and Andrey Kravtsov for useful discussions. We thank Kuang-Han Huang for providing his data in electronic format and for helpful discussions. We thank the anonymous referee for comments and suggestions that improved the paper. We acknowledge the Kavli Institute for Theoretical Physics at the University of Santa Barbara, where part of this work was performed. This research was supported in part by the National Science Foundation under Grant No. NSF PHY-1125915. RSS thanks the Downsbrough family for their generous support, and acknowledges support from the Simons Foundation through a Simons Investigator grant. PB was supported by program number HST-HF2-51353.001-A, provided by NASA through a Hubble Fellowship grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. PGP-G acknowledges support from Spanish MINECO Grants AYA2015-63650-P and AYA2015-70815-ERC. We acknowledge the contributions of hundreds of individuals to the planning and support of the CANDELS observations, and to the development and installation of new instruments on HST, without which this work would not have been possible. Support for HST Programs GO-12060 and GO-12099 was provided by NASA through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555., We explore empirical constraints on the statistical relationship between the radial size of galaxies and the radius of their host dark matter haloes from z similar to 0.1-3 using the Galaxy And Mass Assembly (GAMA) and Cosmic Assembly Near Infrared Deep Extragalactic Legacy Survey (CANDELS) surveys. We map dark matter halo mass to galaxy stellar mass using relationships from abundance matching, applied to the Bolshoi-Planck dissipationless N-body simulation. We define SRHR equivalent to r(e)/R-h as the ratio of galaxy radius to halo virial radius, and SRHR lambda equivalent to r(e)/(lambda R-h) as the ratio of galaxy radius to halo spin parameter times halo radius. At z similar to 0.1, we find an average value of SRHR similar or equal to 0.018 and SRHR. similar or equal to 0.5 with very little dependence on stellar mass. Stellar radius-halo radius (SRHR) and SRHR lambda have a weak dependence on cosmic time since z similar to 3. SRHR shows a mild decrease over cosmic time for low-mass galaxies, but increases slightly or does not evolve formoremassive galaxies. We find hints that at high redshift (z similar to 2-3), SRHR. is lower for more massive galaxies, while it shows no significant dependence on stellar mass at z less than or similar to 0.5. We find that for both the GAMA and CANDELS samples, at all redshifts from z similar to 0.1-3, the observed conditional size distribution in stellar mass bins is remarkably similar to the conditional distribution of lambda R-h. We discuss the physical interpretation and implications of these results., Ministerio de Economía y Competitividad (MINECO), National Science Foundation, Downsbrough family, Simons Foundation through a Simons Investigator grant, NASA, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2018. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM), partnered with the University of California Observatories at Santa Cruz (UCO/Lick, UCSC). We are very grateful to Tucker Jones and Nicha Leethochawalit for sharing their two-dimensional modeling codes. We also want to thank Mark Swinbank for advice on the data reduction and Nicolas Bouche for discussions on GalPaK3D. This work was supported by the Swiss National Science Foundation. MG is grateful to the Fonds de recherche du Quebec Nature et Technologies (FRQNT) for financial support. PGP-G acknowledges support from Spanish Government MINECO grants AYA2015-63650-P and AYA2015-70815-ERC., We present results from the KMOS LENsing Survey (KLENS), which is exploiting gravitational lensing to study the kinematics of 24 star -forming galaxies at 1.4 < z < 3.5 with a median mass of log(M-*/M-circle dot) = 9.6 and a median star formation rate (SFR) of 7.5 M-circle dot yr(-1). We find that 25% of these low mass/low SFR galaxies are rotation -dominated, while the majority of our sample shows no velocity gradient. When combining our data with other surveys, we find that the fraction of rotation -dominated galaxies increases with the stellar mass, and decreases for galaxies with a positive offset from the main sequence (higher specific star formation rate). We also investigate the evolution of the intrinsic velocity dispersion, sigma(0), as a function of the redshift, z, and stellar mass, M-*, assuming galaxies in quasi-equilibrium (Toomre Q parameter equal to 1). From the z -sigma(0) relation, we find that the redshift evolution of the velocity dispersion is mostly expected for massive galaxies (log(M-*/M-circle dot) > 10). We derive a M* - sigma(0) relation, using the Tully Fisher relation, which highlights that a different evolution of the velocity dispersion is expected depending on the stellar mass, with lower velocity dispersions for lower masses, and an increase for higher masses, stronger at higher redshift. The observed velocity dispersions from this work and from comparison samples spanning 0 < z < 3.5 appear to follow this relation, except at higher redshift (z > 2), where we observe higher velocity dispersions for low masses (log(M-*/M-circle dot) similar to 9.6) and lower velocity dispersions for high masses (log(M-*/M-circle dot) similar to 10.9) than expected. This discrepancy could, for instance, suggest that galaxies at high redshift do not satisfy the stability criterion, or that the adopted parametrization of the specific star formation rate and molecular properties fail at high redshift., Ministerio de Economía y Competitividad (MINECO), Swiss National Science Foundation, Fonds de recherche du Quebec Nature et Technologies (FRQNT), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2018. The American Astronomical Society. All rights reserved. Artículo firmado por 23 autores. We would like to thank the anonymous referee for carefully reviewing our paper and providing constructive comments, which truly improved the quality of the paper. Support for Program HST-GO-12060 and HST-GO-13309 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. PGP-G acknowledges support from Spanish Government MINECO AYA2015-70815-ERC and AYA2015-63650-P Grants., Studying giant star-forming clumps in distant galaxies is important to understand galaxy formation and evolution. At present, however, observers and theorists have not reached a consensus on whether the observed "clumps" in distant galaxies are the same phenomenon that is seen in simulations. In this paper, as a step to establish a benchmark of direct comparisons between observations and theories, we publish a sample of clumps constructed to represent the commonly observed "clumps" in the literature. This sample contains 3193 clumps detected from 1270 galaxies at 0.5 <= z < 3.0. The clumps are detected from rest-frame UV images, as described in our previous paper. Their physical properties (e.g., rest-frame color, stellar mass (M-*), star formation rate (SFR), age, and dust extinction) are measured by fitting the spectral energy distribution (SED) to synthetic stellar population models. We carefully test the procedures of measuring clump properties, especially the method of subtracting background fluxes from the diffuse component of galaxies. With our fiducial background subtraction, we find a radial clump U - V color variation, where clumps close to galactic centers are redder than those in outskirts. The slope of the color gradient (clump color as a function of their galactocentric distance scaled by the semimajor axis of galaxies) changes with redshift and M-* of the host galaxies: at a fixed M-*, the slope becomes steeper toward low redshift, and at a fixed redshift, it becomes slightly steeper with M-*. Based on our SED fitting, this observed color gradient can be explained by a combination of a negative age gradient, a negative E(B - V) gradient, and a positive specific SFR gradient of the clumps. We also find that the color gradients of clumps are steeper than those of intra-clump regions. Correspondingly, the radial gradients of the derived physical properties of clumps are different from those of the diffuse component or intra-clump regions., Ministerio de Economía y Competitividad (MINECO), NASA through a grant from the Space Telescope Science Institute, Association of Universities for Research in Astronomy, Inc., under NASA, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub