Search

Aims. We take advantage of the capabilities of the OSIRIS Tunable Emission Line Object (OTELO) survey to select and study the AGN population in the field. In particular, we aim to perform an analysis of the properties of these objects, including their demography, morphology, and IR luminosity. Focusing on the population of H alpha emitters at z similar to 0.4, we also aim to study the environments of AGN and non-AGN galaxies at that redshift. methods. We make use of the multiwavelength catalogue of objects in the field compiled by the OTELO survey, unique in terms of minimum flux and equivalent width. We also take advantage of the pseudo-spectra built for each source, which allow the identification of emission lines and the discrimination of different types of objects. Results. We obtained a sample of 72 AGNs in the field of OTELO, selected with four different methods in the optical, X-rays, and mid-infrared bands. We find that using X-rays is the most efficient way to select AGNs. An analysis was performed on the AGN population of OTELO in order to characterise its members. At z similar to 0 .4, we find that up to 26% of our H alpha emitters are AGNs. At that redshift, AGNs are found in identical environments to non-AGNs, although they represent the most clustered group when compared to passive and star-forming galaxies. The majority of our AGNs at any redshift were classified as late-type galaxies, including a 16% proportion of irregulars. Another 16% of AGNs show signs of interactions or mergers. Regarding the infrared luminosity, we are able to recover all the luminous infrared galaxies (LIRGs) in the field of OTELO up to z similar to 1.6. We find that the proportion of LIRGs and ultra-luminous infraed galaxies (ULIRGs) is higher among the AGN population, and that ULIRGs show a higher fraction of AGNs than LIRGs., This work was supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under the grants AYA2013 - 46724 - P, AYA2013 - 42227 - P, AYA2014 -58861 -C3 - 1 - P, AYA2014 -58861 - C3 - 2 - P, AYA2014 -58861 - C3 - 3 - P, AYA2016 -75808 - R, AYA2016 - 75931 - C2 - 1 P, AYA2016 - 75931 - C2 - 2 - P, AYA2016 -76682C3 - 1 - P, AYA2017 -88007 C3 - 1 - P and AYA2017 -88007 - C3 - 2 - P. The authors thank the anonymous referee for her/his feedback and suggestions. Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma. MP acknowledges financial supports from the Ethiopian Space Science and Technology Institute (ESSTI) under the Ethiopian Ministry of Innovation and Technology (MInT), and from the State Agency for Research of the Spanish MCIU through the >Center of Excellence Severo Ochoa> award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). EJA acknowledges financial support from the State Agency for Research of the Spanish MCIU through the >Center of Excellence Severo Ochoa> award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709).

Context. The evolution of galaxies through cosmic time is studied observationally by means of extragalactic surveys. The usefulness of these surveys is greatly improved by increasing the cosmological volume, in either depth or area, and by observing the same targets in different wavelength ranges. A multi-wavelength approach using different observational techniques can compensate for observational biases. Aims. The OTELO survey aims to provide the deepest narrow-band survey to date in terms of minimum detectable flux and emission line equivalent width in order to detect the faintest extragalactic emission line systems. In this way, OTELO data will complements other broad-band, narrow-band, and spectroscopic surveys. Methods. The red tunable filter of the OSIRIS instrument on the 10.4m Gran Telescopio Canarias (GTC) is used to scan a spectral window centred at 9175 angstrom, which is free from strong sky emission lines, with a sampling interval of 6 angstrom and a bandwidth of 12 angstrom in the most deeply explored EGS region. Careful data reduction using improved techniques for sky ring subtraction, accurate astrometry, photometric calibration, and source extraction enables us to compile the OTELO catalogue. This catalogue is complemented with ancillary data ranging from deep X-ray to far-infrared, including high resolution HST images, which allow us to segregate the different types of targets, derive precise photometric redshifts, and obtain the morphological classification of the extragalactic objects detected. Results. The OTELO multi-wavelength catalogue contains 11 237 entries and is 50% complete at AB magnitude 26.38. Of these sources, 6600 have photometric redshifts with an uncertainty delta z(phot) better than 0.2 (1+z(phot)). A total of 4336 of these sources correspond to preliminary emission line candidates, which are complemented by 81 candidate stars and 483 sources that qualify as absorption line systems. The OTELO survey results will be released to the public on the second half of 2019.© ESO 2019, This work was supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under the grants AYA2013 - 46724 - P, AYA2014 - 58861 - C3 - 1 - P, AYA2014 - 58861 - C3 - 2 - P, AYA2014 - 58861 - C3 - 3 - P, AYA2016 - 75808 - R, AYA2016 -7 5931 - C2 - 2 - P, AYA2017 - 88007 - C3 - 1 - P and AYA2017 - 88007 - C3 - 2 - P. Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, on the island of La Palma. This study makes use of data from AEGIS, a multi-wavelength 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. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, 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. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of the NRC and CNRS. Based on observations obtained with WIRCam, a joint project of the CFHT, Taiwan, Korea, Canada, France, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX, the WIRDS (WIRcam Deep Survey) consortium, and the Canadian Astronomy Data Centre. This research was supported by a grant from the Agence Nationale de la Recherche ANR-07-BLAN-0228. Jose A. de Diego thanks the Instituto de Astrofisica de Canarias for it s support through the Programa de Excelencia Severo Ochoa and the Gobierno de Canarias for the Programa de Talento Tricontinental grant. A. Bongiovanni thanks the anonymous Referee for her/his feedback and suggestions, and Terry Mahoney (at the IAC's Scientific Editorial Service) for his subtantial improvements of the manuscript.

Context. The evolution of galaxies through cosmic time is studied observationally by means of extragalactic surveys. The usefulness of these surveys is greatly improved by increasing the cosmological volume, in either depth or area, and by observing the same targets in different wavelength ranges. A multi-wavelength approach using different observational techniques can compensate for observational biases. Aims. The OTELO survey aims to provide the deepest narrow-band survey to date in terms of minimum detectable flux and emission line equivalent width in order to detect the faintest extragalactic emission line systems. In this way, OTELO data will complements other broad-band, narrow-band, and spectroscopic surveys. Methods. The red tunable filter of the OSIRIS instrument on the 10.4m Gran Telescopio Canarias (GTC) is used to scan a spectral window centred at 9175 angstrom, which is free from strong sky emission lines, with a sampling interval of 6 angstrom and a bandwidth of 12 angstrom in the most deeply explored EGS region. Careful data reduction using improved techniques for sky ring subtraction, accurate astrometry, photometric calibration, and source extraction enables us to compile the OTELO catalogue. This catalogue is complemented with ancillary data ranging from deep X-ray to far-infrared, including high resolution HST images, which allow us to segregate the different types of targets, derive precise photometric redshifts, and obtain the morphological classification of the extragalactic objects detected. Results. The OTELO multi-wavelength catalogue contains 11 237 entries and is 50% complete at AB magnitude 26.38. Of these sources, 6600 have photometric redshifts with an uncertainty delta z(phot) better than 0.2 (1+z(phot)). A total of 4336 of these sources correspond to preliminary emission line candidates, which are complemented by 81 candidate stars and 483 sources that qualify as absorption line systems. The OTELO survey results will be released to the public on the second half of 2019.© ESO 2019 This work was supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under the grants AYA2013 - 46724 - P, AYA2014 - 58861 - C3 - 1 - P, AYA2014 - 58861 - C3 - 2 - P, AYA2014 - 58861 - C3 - 3 - P, AYA2016 - 75808 - R, AYA2016 -7 5931 - C2 - 2 - P, AYA2017 - 88007 - C3 - 1 - P and AYA2017 - 88007 - C3 - 2 - P. Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, on the island of La Palma. This study makes use of data from AEGIS, a multi-wavelength 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. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, 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. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of the NRC and CNRS. Based on observations obtained with WIRCam, a joint project of the CFHT, Taiwan, Korea, Canada, France, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX, the WIRDS (WIRcam Deep Survey) consortium, and the Canadian Astronomy Data Centre. This research was supported by a grant from the Agence Nationale de la Recherche ANR-07-BLAN-0228. Jose A. de Diego thanks the Instituto de Astrofisica de Canarias for it s support through the Programa de Excelencia Severo Ochoa and the Gobierno de Canarias for the Programa de Talento Tricontinental grant. A. Bongiovanni thanks the anonymous Referee for her/his feedback and suggestions, and Terry Mahoney (at the IAC's Scientific Editorial Service) for his subtantial improvements of the manuscript.

[Aims] We take advantage of the capability of the OTELO survey to obtain the H alpha luminosity function (LF) at z similar to 0.40. Because of the deepest coverage of OTELO, we are able to determine the faint end of the LF, and thus better constrain the star formation rate and the number of galaxies at low luminosities. The AGN contribution to this LF is estimated as well. [Methods] We make use of the multiwavelength catalogue of objects in the field compiled by the OTELO survey, which is unique in terms of minimum flux and equivalent width. We also take advantage of the pseudo-spectra built for each source, which allow the identification of emission lines and the discrimination of different types of objects. [Results] The H alpha luminosity function at z similar to 0.40 is obtained, which extends the current faint end by almost 1 dex, reaching minimal luminosities of log(10) L-lim = 38.5 erg s(-1) (or similar to 0.002 M-circle dot yr(-1)). The AGN contribution to the total H alpha luminosity is estimated. We find that no AGN should be expected below a luminosity of log(10) L = 38.6 erg s(-1). From the sample of non-AGN (presumably, pure SFG) at z similar to 0.40 we estimated a star formation rate density of rho(SFR) = 0.012 +/- 0.005 M-circle dot yr(-1) Mpc(-3)., This work was supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under the grants AYA2013- 46724- P, AYA2014 58861-C3-1- P, AYA2014-58861-C3-2-P, AYA2014-58861-C3-3- P, AYA2016 -75808-R, AYA2016-75931-C2-2-P, AYA2017-88007-C3-1-P, and AYA2017 -88007-C3-2- P. Based on observations made with the Gran Telescopio Canarias installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma. The authors thanks the anonymous referee for her/his feedback and suggestions.

The status of OTELO and Lockman SpReSO surveys, the two large guaranteed time programs currently under way using OSIRIS at the 10.4m GTC is presented. The OTELO project, designed to detect the main optical emission lines from Hα to Lyα at redshifts from 0.4 through 7, is the deepest emission line survey to date, with unprecedented sensitivity in the detection of small equivalent widths. Lockman SpReSO is aimed to obtaining optical spectra, up to 24.5 AB magnitudes, in the central 24×24 square arcminutes of the Lockman Hole field, which has been observed with ROSAT and XMM–Newton at the highest depth. Lockman SpReSO mainly targets Far Infrared sources detected with the Herschel Space Observatory This work was supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under the grants AYA2014–58861–C3–1–P, AYA2014–58861–C3–2–P, AYA2014–58861–C3–3–P and AYA2013–46724–P. Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof´ısica de Canarias, in the island of La Palma. 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. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Re[1]search 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. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on observations obtained with WIRCam, a joint project of CFHT,Taiwan, Korea, Canada, France, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l’Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX, the WIRDS (WIRcam Deep Survey) consortium, and the Canadian Astronomy Data Centre. This research was supported by a grant from the Agence Nationale de la Recherche ANR-07-BLAN-0228

arXiv:1510.03226v1, Broad absorption line quasars are among the objects presenting the fastest outflows. The launching mechanism itself is not completely understood. Models in which they could be launched from the accretion disk, and then curved and accelerated by the effect of the radiation pressure, have been presented. We conducted an extensive observational campaign, from radio to optical band, to collect information about their nature and test the models present in the literature, the main dichotomy being between a young scenario and an orientation one. We found a variety of possible orientations, morphologies, and radio ages, not converging to a particular explanation for the BAL phenomenon. From our latest observations in the m- and mm-band, we obtained an indication of a lower dust abundance with respect to normal quasars, thus suggesting a possible feedback process on the host galaxy. Also, in the low-frequency regime we confirmed the presence of CSS components, sometime in conjunction with a GPS one already detected at higher frequencies. Following this, about 70% of our sample turns out to be in a GPS or CSS+GPS phase. We conclude that fast outflows, responsible for the BAL features, can be more easily present among objects going through a restarting or just-started radio phase, where radiation pressure can substantially contribute to their acceleration., Part of this work was supported by a grant of the Italian Programme for Research of National Interest (PRIN No. 18/2007, PI: K.-H. Mack). The authors acknowledge financial support from the Spanish Ministerio de Ciencia e Innovacion under project AYA2008-06311-C02-02.

Sánchez-Portal, Miguel et. al., The cores of clusters at 0 ≲ z ≲ 1 are dominated by quiescent early-type galaxies, whereas the field is dominated by star-forming late-type galaxies. Clusters grow through the accretion of galaxies and groups from the surrounding field, which implies that galaxy properties, notably the star formation ability, are altered as they fall into overdense regions. The critical issues for understanding this evolution are how the truncation of star formation is connected to the morphological transformation and what physical mechanism is responsible for these changes. The GaLAxy Cluster Evolution Survey (GLACE) is conducting a thorough study of the variations in galaxy properties (star formation, AGN activity, and morphology) as a function of environment in a representative and well-studied sample of clusters. To address these questions, the GLACE survey is making a deep panoramic survey of emission line galaxies (ELG), mapping a set of optical lines ([O ii], [O iii], Hβ andHα/[N ii] when possible) in several galaxy clusters at z ~ 0.40, 0.63, and 0.86. Using the tunable filters (TF) of the OSIRIS instrument at the 10.4 m GTC telescope, the GLACE survey applies the technique of TF tomography: for each line, a set of images are taken through the OSIRIS TF, each image tuned at a different wavelength (equally spaced), to cover a rest frame velocity range of several thousand km s-1 centred on the mean cluster redshift, and scanned for the full TF field of view of an 8 arcmin diameter. Here we present the first results of the GLACE project, targeting the Hα/[N ii] lines in the intermediate-redshift cluster ZwCl 0024.0+1652 at z = 0.395. Two pointings have been performed that cover ~2 × rvir. We discuss the specific techniques devised to process the TF tomography observations in order to generate the catalogue of cluster Hα emitters, which contains more than 200 sources down to a star formation rate (SFR) ≲1 M⊙/yr. An ancillary broadband catalogue is constructed, allowing us to discriminate line interlopers by means of colour diagnostics. The final catalogue contains 174 unique cluster sources. The AGN population is distinguished using different diagnostics and found to be ~37% of the ELG population. The median SFR of the star-forming population is 1.4 M⊙/yr. We studied the spatial distribution of ELG and confirm the existence of two components in the redshift space. Finally, we exploited the outstanding spectral resolution of the TF, attempting to estimate the cluster mass from ELG dynamics, finding M200 = (4.1 ± 0.2) × 1014 M⊙ h-1, in agreement with previous weak-lensing estimates., We acknowledge financial support from Spanish MINECO under grant AYA2014-29517-C03-01, AYA2011-29517-C03-02 and AYA2014-58861-C03. E.J.A. acknowledges support from MINECO under grant AYA2013-40611-P. J.M.R.E. acknowledges support from MINECO under grant AYA2012-39168-C03-01. We acknowledge support from the Faculty of the European Space Astronomy Centre (ESAC). I.R.S. acknowledges support from STFC GT/I001573/1, a European Research Council Advanced Programme Dustygal (321334) and a Royal Society/Wolfson Research Merit Award. J.S.S. acknowledges funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 267251 "Astronomy Fellowships in Italy" (AstroFIt).

Sánchez-Portal, Miguel et. al. The cores of clusters at 0 ≲ z ≲ 1 are dominated by quiescent early-type galaxies, whereas the field is dominated by star-forming late-type galaxies. Clusters grow through the accretion of galaxies and groups from the surrounding field, which implies that galaxy properties, notably the star formation ability, are altered as they fall into overdense regions. The critical issues for understanding this evolution are how the truncation of star formation is connected to the morphological transformation and what physical mechanism is responsible for these changes. The GaLAxy Cluster Evolution Survey (GLACE) is conducting a thorough study of the variations in galaxy properties (star formation, AGN activity, and morphology) as a function of environment in a representative and well-studied sample of clusters. To address these questions, the GLACE survey is making a deep panoramic survey of emission line galaxies (ELG), mapping a set of optical lines ([O ii], [O iii], Hβ andHα/[N ii] when possible) in several galaxy clusters at z ~ 0.40, 0.63, and 0.86. Using the tunable filters (TF) of the OSIRIS instrument at the 10.4 m GTC telescope, the GLACE survey applies the technique of TF tomography: for each line, a set of images are taken through the OSIRIS TF, each image tuned at a different wavelength (equally spaced), to cover a rest frame velocity range of several thousand km s-1 centred on the mean cluster redshift, and scanned for the full TF field of view of an 8 arcmin diameter. Here we present the first results of the GLACE project, targeting the Hα/[N ii] lines in the intermediate-redshift cluster ZwCl 0024.0+1652 at z = 0.395. Two pointings have been performed that cover ~2 × rvir. We discuss the specific techniques devised to process the TF tomography observations in order to generate the catalogue of cluster Hα emitters, which contains more than 200 sources down to a star formation rate (SFR) ≲1 M⊙/yr. An ancillary broadband catalogue is constructed, allowing us to discriminate line interlopers by means of colour diagnostics. The final catalogue contains 174 unique cluster sources. The AGN population is distinguished using different diagnostics and found to be ~37% of the ELG population. The median SFR of the star-forming population is 1.4 M⊙/yr. We studied the spatial distribution of ELG and confirm the existence of two components in the redshift space. Finally, we exploited the outstanding spectral resolution of the TF, attempting to estimate the cluster mass from ELG dynamics, finding M200 = (4.1 ± 0.2) × 1014 M⊙ h-1, in agreement with previous weak-lensing estimates. We acknowledge financial support from Spanish MINECO under grant AYA2014-29517-C03-01, AYA2011-29517-C03-02 and AYA2014-58861-C03. E.J.A. acknowledges support from MINECO under grant AYA2013-40611-P. J.M.R.E. acknowledges support from MINECO under grant AYA2012-39168-C03-01. We acknowledge support from the Faculty of the European Space Astronomy Centre (ESAC). I.R.S. acknowledges support from STFC GT/I001573/1, a European Research Council Advanced Programme Dustygal (321334) and a Royal Society/Wolfson Research Merit Award. J.S.S. acknowledges funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 267251 "Astronomy Fellowships in Italy" (AstroFIt).

Observations of the location and kinematics of the atomic gas (HI) and the continuum radio emission from high redshift galaxies would mean a huge step forward in our understanding of galaxy evolution. We now have a secure global picture of the stellar content of massive galaxies and their precursors up to z~4. But we still have to understand why star formation in these systems started early and quenched some time after, a scenario known as downsizing which, at face value, conflicts with the predictions from the current hierarchical galaxy formation paradigm. SKA will provide the missing piece to solve the puzzle: information about the amounts of gas falling into galaxies to form stars, as well as data to measure when and how the star formation turns off as the gas stops cooling due to still to be understood feedback mechanisms, such as (radio mode) obscured nuclear activity., PGP-G acknowledges support from Spanish Government MINECO AYA2012-31277 Grant. JIGS acknowledges support from the Spanish Ministry for Economy and Competitiveness AYA2011-29517-C03-02. AFS acknowledges support from the Spanish Ministry for Economy and Competitiveness and FEDER funds through grants AYA2010-22111-C03-02 and AYA2013-48623-C2-2, and Generalitat Valenciana project PROMETEOII/2014/060.

The cores of clusters at 0 ? z ? 1 are dominated by quiescent early-type galaxies, whereas the field is dominated by star-forming late-type galaxies. Clusters grow through the accretion of galaxies and groups from the surrounding field, which implies that galaxy properties, notably the star formation ability, are altered as they fall into overdense regions. The critical issues for understanding this evolution are how the truncation of star formation is connected to the morphological transformation and what physical mechanism is responsible for these changes. The GaLAxy Cluster Evolution Survey (GLACE) is conducting a thorough study of the variations in galaxy properties (star formation, AGN activity, and morphology) as a function of environment in a representative and well-studied sample of clusters. To address these questions, the GLACE survey is making a deep panoramic survey of emission line galaxies (ELG), mapping a set of optical lines ([O?ii], [O?iii], Hß andHa/[N?ii] when possible) in several galaxy clusters at z ~ 0.40, 0.63, and 0.86. Using the tunable filters (TF) of the OSIRIS instrument at the 10.4 m GTC telescope, the GLACE survey applies the technique of TF tomography: for each line, a set of images are taken through the OSIRIS TF, each image tuned at a different wavelength (equally spaced), to cover a rest frame velocity range of several thousand km?s-1 centred on the mean cluster redshift, and scanned for the full TF field of view of an 8?arcmin diameter. Here we present the first results of the GLACE project, targeting the Ha/[N?ii] lines in the intermediate-redshift cluster ZwCl?0024.0+1652 at z = 0.395. Two pointings have been performed that cover ~2?×?rvir. We discuss the specific techniques devised to process the TF tomography observations in order to generate the catalogue of cluster Ha emitters, which contains more than 200 sources down to a star formation rate (SFR)??1?M?/yr. An ancillary broadband catalogue is constructed, allowing us to discriminate line interlopers by means of colour diagnostics. The final catalogue contains 174 unique cluster sources. The AGN population is distinguished using different diagnostics and found to be ~37% of the ELG population. The median SFR of the star-forming population is 1.4?M?/yr. We studied the spatial distribution of ELG and confirm the existence of two components in the redshift space. Finally, we exploited the outstanding spectral resolution of the TF, attempting to estimate the cluster mass from ELG dynamics, finding M200?=?(4.1?±?0.2)?×?1014?M? h-1, in agreement with previous weak-lensing estimates. Acknowledgements. We acknowledge the support provided by M. Balogh during the preparation of the GLACE proposal to ESO, as well as his useful suggestions for improving the quality of this paper. We also acknowledge the anonymous referee. We acknowledge financial support from Spanish MINECO under grant AYA2014-29517-C03-01, AYA2011-29517-C03-02 and AYA2014-58861-C03. E.J.A. acknowledges support from MINECO under grant AYA2013-40611-P. J.M.R.E. acknowledges support from MINECO under grant AYA2012-39168-C03-01. We acknowledge support from the Faculty of the European Space Astronomy Centre (ESAC). I.R.S. acknowledges support from STFCGT/I001573/1, a European Research Council Advanced Programme Dustygal (321334) and a Royal Society/Wolfson Research Merit Award. J.S.S. acknowledges funding from the European Union Seventh Framework Programme (FP7/2007−2013) under grant agreement No. 267251 “Astronomy Fellowshipsin Italy” (AstroFIt). Based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias, on the island of La Palma. 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, by the National Aeronautics and Space Administration and the National Science Foundation

arXiv:1302.6719v1, Luminosity functions are one of the most important observational clues when studying galaxy evolution over cosmic time. In this paper we present the X-ray luminosity functions for X-ray detected AGN in the SXDS and GWS fields. The limiting fluxes of our samples are 9.0 ×10-15 and 4.8 ×10-16 erg cm-2 s-1 in the 0.5-7.0 keV band in the two fields, respectively. We carried out analysis in three X-ray bands and in two redshift intervals up to z ≤ 1.4. Moreover, we derive the luminosity functions for different optical morphologies and X-ray types. We confirm strong luminosity evolution in all three bands, finding the most luminous objects at higher redshift. However, no signs of density evolution are found in any tested X-ray band. We obtain similar results for compact and early-type objects. Finally, we observe the >Steffen effect>, where X-ray type-1 sources are more numerous at higher luminosities in comparison with type-2 sources., This research has been supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under the grant AYA2011-29517-C03-01. MP, IM, and JM acknowledge Junta de Andalucía and MINECO through projects PO8-TIC-03531 and AYA2010-15169. We acknowledge support from the Faculty of the European Space Astronomy Centre (ESAC). JIGS acknowledge financial support from the MINECO under project AYA2008-06311-C02-02 and AYA2011-29517-C03-02. JG acknowledges support from the MINECO through AYA2009-10368 project. The CEFCA is funded by the Fondo de Inversiones de Teruel, supported by both the Government of Spain (50%) and the regional Government of Aragón (50%). This work has been partially funded by the Spanish Ministerio de Ciencia e Innovación through the PNAYA, under grants AYA2006-14056 and th-rough the ICTS 2009-14.

We present new far-infrared (70–500 μm) Herschel Photodetector Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) imaging observations as well as new mid-IR Gemini/Thermal-Region Camera Spectrograph imaging (8.7 and 18.3 μm) and spectroscopy of the inner Lindblad resonance (ILR) region (R < 2.5 kpc) of the spiral galaxy NGC 1365. We complemented these observations with archival Spitzer imaging and spectral mapping observations. The ILR region of NGC 1365 contains a Seyfert 1.5 nucleus and a ring of star formation with an approximate diameter of 2 kpc. The strong star formation activity in the ring is resolved by the Herschel/PACS imaging data, as well as by the Spitzer 24 μm continuum emission, [Ne ii] 12.81 μm line emission, and 6.2 and 11.3 μm PAH emission. The active galactic nucleus (AGN) is the brightest source in the central regions up to λ ∼ 24 μm, but it becomes increasingly fainter in the far-infrared when compared to the emission originating in the infrared clusters (or groups of them) located in the ring. We modelled the AGN unresolved infrared emission with the clumpy torus models and estimated that the AGN contributes only to a small fraction (∼5 per cent) of the infrared emission produced in the inner ∼5 kpc. We fitted the non-AGN 24–500 μm spectral energy distribution of the ILR region and found that the dust temperatures and mass are similar to those of other nuclear and circumnuclear starburst regions. Finally we showed that within the ILR region of NGC 1365, most of the ongoing star formation activity is taking place in dusty regions as probed by the 24 μm emission., This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).

Context. The Groth field is one of the sky regions that will be targeted by the OTELO (OSIRIS Tunable Filter Emission Line Object) survey in the optical 820 nm and 920 nm atmospheric windows. A complementary broad-band photometric catalogue of the field is essential for several purposes, in particular the inequivocal identification of sources, photometric redshift estimation, and population synthesis fitting.Aims. We aim to describe the OTELO survey and present deep BVRI imaging data of the Groth field. Galaxy number counts, colour distributions and galaxy clustering are analysed.Methods. BVRI deep images (?8 ks) were obtained with the Prime Focus Camera at the WHT (La Palma) and reduced with the IRAF package. The extraction and photometry of the sources was done with SExtractor software. We analysed the final catalogue to obtain galaxy number counts, as well as galaxy correlation functions as a function of I magnitude and V - I colour. It is also compared with estimations from mock catalogues of the Virgo-Millenium consortium.Results. We find excellent agreement between observed and mock data number counts. We also find evidence of galaxy clustering evolution and strong dependence of the angular correlation function on the V - I observed colour. Our data favour a flattening of the clustering amplitude with median apparent magnitude. The good general agreement between our clustering analysis and the estimates from the mock data is remarkable Acknowledgements. This work was supported by the Spanish Plan Nacional de Astronomía y Astrofísica under grants AYA2005–04149 and AYA2006–2358. We thank the referee for helpful comments that improved the clarity of this paper. The Millennium Simulation databases used in this paper and the web application providing online access to them were constructed as part of the activities of the German Astrophysical Virtual Observatory. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. 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.

15 pages. Accepted for publishing in A&A., We have conducted a NIR study of the environments of seven radio-loud quasars at redshifts 1, We have selected a sample of cluster candidates analyzing the R-K vs. K diagram. A ~25% of the candidates present red optical-NIR colours and an ultraviolet excess. This population has been also found in clusters around quasars at the same redshifts (Tanaka et al. 2000; Haines et al. 2001). These galaxies seem to follow a mixed evolution: a main passive evolution plus late starformation processes. The quasars do not inhabit the core of the clusters, being found in the outer regions. This result agrees with the hypothesis that the origin/feeding mechanism of the nuclear activity were merging processes. The quasars inhabit the region were a collision is most probably to produce a merger., J.I. González-Serrano wants to aknowledge financial support from DGESIC (Ministerio de Educacion y Cultura) under project PB98-0409-C02-02.

The broad range of optical?infrared colours of radio QSOs, 1 < B ? K < 6, has been cited as evidence for several mag of dust extinction (Webster et al., 1995). If such large extinctions are typical, the implications for our understanding of the space density of optically selected QSOs are profound. We have previously found that the host galaxies of several of the reddest B3 QSOs are readily detectable in K-band images. This suggests contamination of the K apparent magnitudes by starlight, i.e. the redness in B ? K may be due to excess light in K, rather than to dust extinction of the B light. We have now imaged the B3 QSOs in UBV R, and we use the range of observed optical and optical?IR colours to place an upper limit on the amount of dust extinction present, rest-frame AV < 1.5 mag

We have conducted an optical study of the environments of seven radio-loud quasars at redshifts 122.5 and R>22.0) galaxies on scales of r

We have carried out optical spectroscopic observations at intermediate spectral resolution of the massive high redshift radio galaxy 0902+34 at z ≈ 3.39. This source was first identified by Lilly (1988) (from hereafter L88). The study of high redshift radio galaxies is interesting to analyze the physical conditions of the early universe and the galaxy evolution at cosmological redshifts. It has been claimed that some of these systems may be protogalaxies in the process of formation. Indications for this are the flat spectrum and the absence of the 4000 Å break, features which have already been observed in many cases. In particular, observations in the spectral range from V to K suggest that 0902+34 is a young galaxy (Eisenhardt and Dickinson 1992). Recent radio observations of the 21 cm line of neutral hydrogen have detected (Uson et. al. 1991) an absorption against the radio continuum source. This absorption could also leave a track in the optical, redwards the Lyα line. Our observations were carried out with the ISIS spectrograph at the 4.2 m William Herschel Telescope (seeing ≈ 1.2–1.6 arcsec). A spectral dispersion of 0.78 Å/pixel (blue arm) and 1.38 Å/pixel (red arm) was obtained. A long slit of width 3″ was used providing a spectral resolution of ≈ 5.4 Å in the blue arm and of ≈ 9.5 Å in the red one. Both resolutions are a clear improvement over that achieved by L88 of 20 Å, allowing us to resolve the Lyα line (and its possible structure) and any other possible strong features appearing in the spectral range observed (e. g., C IV λ1549, He II λ1640,…). We acknowledge financia! support from the spanish DGICYT, project PB92-0741. Partial financia! support for this project was provided by the Comission ofthe European Union and their Human Capital and Mobility Contract CHRX CT92-0033. The William Herschel Telescope is operated by the Royal Greenwich Observatory at the spanish Observatorio del Roque de Los Muchachos of the Instituto de Astrofísica de Canarias, on behalf of the Science and Engineering Research Council of the United Kingdom and the Netherlands Organization for Scientific Research.

Background The Neurological Disorders in Central Spain, second survey (NEDICES-2) is a population-based, closed-cohort study that will include over 8000 subjects aged ≥55 years. It will also include a biobank. Objective The objective of this study was to evaluate all major aspects of the NEDICES-2 (methods, database, screening instruments, and questionnaires, as well as interexpert rating of the neurological diagnoses) in each one of the planned areas (all of them in central Spain) and to test the possibility of obtaining biological samples from each participant. Methods A selection of patients and participants of the planned NEDICES-2 underwent face-to-face interviews including a comprehensive questionnaire on demographics, current medications, medical conditions, and lifestyle habits. Biological samples (blood, saliva, urine, and hair) were also obtained. Furthermore, every participant was examined by a neurologist. Results In this pilot study, 567 study participants were enrolled (196 from hospitals and 371 from primary care physician lists). Of these 567, 310 completed all study procedures (questionnaires and the neurological evaluation). The study was time-consuming for several primary care physicians. Hence, a few primary care physicians from some areas refused to participate, which led to a reconfiguration of study areas. In addition, the central biobank needed to be supplemented by the biobanks of local Spanish National Health System hospitals. Conclusions Population-based epidemiological surveys, such as the NEDICES-2, require a pilot study to evaluate the feasibility of all aspects of a future field study (population selection, methods and instruments to be used, neurological diagnosis agreement, and data collection)., Our thanks to all collaborators in this feasibility pilot study, the Instituto de Salud Carlos III and the Biomedical Research Networking Center on Neurodegenerative Diseases (CIBERNED), and the two hospital computer experts (Victoria Garcia Baquero and Teresa Garcia Morales), who created the website (http://nedices2.ciberned.com/estudio-de-salud-nedices-2/). We would also like to thank Miss Jennifer Gates for the editing and proofreading of the manuscript.

Programa Oficial de Postgrado en Ciencias, Tecnología y Computación., [EN]: Around 8-13\% of the known population of quasars (QSOs) are powerful radio emitter and therefore classified as Radio-Loud (RL), while the remaining part is classified as Radio-Quiet (RQ). The reason of the radio emission is explained in terms of the presence of a radio-jet, responsible for the synchrotron emission and relativistic particles in intense magnetic fields. Nevertheless, the reason why only a minority of the quasars show strong radio-emission and which is the physical connection between these two major classes of objects, still lack a convincing explanation. Quasars are relatively rare, especially at high redshift, since their comoving density is a strong function of redshift that peaks at z~2-3 and declines exponentially at higher redshifts. The radio-loud quasar population at z > 3.5 is an even more elusive population, therefore does not allow exhaustive statistical studies and comparisons between radio-loud and radio-quiet populations in the early universe, where it might be possible to gather clues on the connection between radio and optical activity in QSOs. The quest to increase the number of known radio-loud quasars at high redshift require the use of large area surveys, advanced techniques of data mining to deal with the sheer volume of data of modern surveys, and the refinement of the candidate-selection techniques to select quasar-candidate of potential interest from broad-band photometric surveys. This thesis is focused on the selection and study of high-redshift RL QSOs at z>3.6. We combined modern data mining techniques and machine-learning algorithms for an efficient and complete exploitation of multi-wavelength data from large-area surveys in the optical (SDSS), in the near- and mid-infrared (UKIDSS, WISE) and in the radio (FIRST). We completed and tested our modern techniques of analysis and selection through follow-up optical spectroscopy and radio observations of the samples of RL quasars of our interest. We analyzed the results of our observations and drew conclusions both on the techniques used for the candidate-selection and on the physics of the studied objects., [ES]: Los cuásares (QSOs) son fuentes extragalácticas compactas, muy brillantes, originadas por material de acreción que cae en un agujero negro supermasivo y forman parte de la familia de los núcleos activos galácticos (AGN). Los cuásares tienen una distribución de energía espectral amplia y se encuentran entre los objetos más brillantes del cielo en todas las longitudes de onda en que han sido observados. Alrededor del 8-13% de la población conocida de cuásares son potentes emisores en radio y, por tanto, se clasifican como radio-intensos (RL), mientras que a la parte restante se le denomina radio-silenciosos (RQ). El motivo por el que sólo una minoría de los cuásares muestra una fuerte emisión en radio y cuál es la conexión física entre estas dos clases de objetos no cuenta aún con una explicación convincente. La densidad comóvil de los cuásares luminosos es una fuerte función del desplazamiento al rojo (z) que alcanza un máximo a z~2-3 y desciende exponencialmente hacia mayores (y menores) desplazamientos al rojo. Por tanto, la población de cuásares radio-intensos a alto z es bastante reducida y no permite llevar a cabo estudios estadísticos exhaustivos ni comparaciones entre poblaciones radio-intensas y radio-silenciosas en el universo temprano, donde podría ser posible recopilar pruebas sobre la conexión entre actividad radio y óptica en los cuásares. Los estudios para aumentar el número de cuásares radio-intensos y reducir los sesgos asociados a su selección requieren el uso de cartografiados de gran área de nueva generación, especialmente en el infrarrojo cercano y lejano, ya que la combinación de campo de visión y sensibilidad permite buscar cuásares débiles a mayor desplazamiento al rojo. Esto requiere del perfeccionamiento de técnicas de minería de datos, para procesar y combinar tal cantidad de datos multi-longitud de onda, y así aprovechar completamente su potencial. Por último, es necesaria la mejora en la determinación de los sesgos de selección, que deben ser corregidos minuciosamente para poder inferir las propiedades estadísticas de la población de cuásares. Esta tesis doctoral está centrada en la selección y estudio de los RL cuásares a alto desplazamiento al rojo z>3.6. Se combinaron las técnicas modernas de minería de datos y algoritmos de aprendizaje automático para explotar los datos multi-longitud de onda procedentes de cartografiados de gran área en el óptico, en el cercano y medio infrarrojo y en el radio. Completamos y evaluamos la eficiencia de nuestras técnicas de análisis y selección mediante espectroscopía óptica, y observamos en radio una submuestra de cuásares de especial interés. Analizamos los resultados de nuestras observaciones y obtuvimos conclusiones tanto en lo referente a las técnicas empleadas para la selección de candidatos como sobre la física de los objetos estudiados.

[EN]: The origin of Broad Absorption Line Quasars (BAL QSOs) is still an open issue. Accounting for ? 20% of the QSO population, these objects present broad absorption lines in their optical spectra generated from outflows with velocities up to 0.2 c. There is still no consensus about the origin of the absorbing gas in BAL QSOs, the mechanism which accelerates it, or the relationship between BAL QSOs and the quasar population as a whole. Nowadays, the hypotheses about their nature are principally related to orientation or evolutionary scenarios. In the first one, absorption lines are produced by outflows originated by the accretion disk, basically present in all QSOs, but seen only when they intercept the line of sight. In the second hypothesis, BAL QSOs would be young or recently re-fueled QSOs, still ejecting their dust cocoon. In this case orientation would not play a role, since the absorption features would be produced by spherically ejected matter. In this work we present the results of a multi-frequency study of a Radio- Loud BAL QSO sample, and a comparison sample of Radio-Loud non-BAL QSOs, both selected from the Sloan Digital Sky Survey (SDSS). We performed observations in the radio band, to sample the SED in the GHz range and study the characteristics of the synchrotron emission, aiming at collecting indications about the age and the orientation of the central radio source, as well as the polarization properties. The comparison with the non-BAL QSO sample allows us to conclude that no particular orientation is present in BAL QSOs. Nevertheless, similar fractions of GHz-peaked sources in the two sample (36±12% vs 23±8%) does not seem to suggest a young age for BAL QSOs, and this conclusion is favoured by the presence, in some cases, of low-frequency, presumably old components in the radio spectrum. Through the VLBI technique, it was possible to study the pc-scale radiomorphology of half the sample. About 80% of sources present a resolved structure, with projected linear sizes comprised between tens and hundreds of pc. This fraction is comparable with previous results from literature. The missing flux density with respect to observations at kpc-scale resolution suggests a low frequency, diffuse component in some cases. The variety of morphologies does not support a particular orientation. We also investigated the dust grey-body emission at mm-wavelengths, to verify whether BAL QSOs are dust-rich, physical condition requested by the evolutionary model. Only 7% of the sources present a clear dust contribution at 250 GHz. Not being dust rich, BAL QSOs should not present an high star-formation rate. Thus, again, they should not be a particularly young class of objects. Finally, using a sample of optically-bright Radio-Loud and Radio-Quiet QSOs, we collected spectra in the Near-Infrared band, to estimate the central black hole mass, the Eddington ratio, and the Broad Line Region radius, in order to underline dfferences induced by the Radio-Loud phase. From an analysis of the SDSS DR7 QSO catalogue, the Eddington ratio is the only physical quantity found to be significantly dfferent in Radio-Loud BAL QSOs, 26% of these objects being super-Eddington, while only 13% of Radio-Quiet BAL QSOs show the same property. Even a bigger difference has been found between BAL and non-BAL QSOs as a whole (13% vs 2%)., [ES]: El origen de los cuásares con líneas anchas de absorción (BAL QSOs, del acrónimo en inglés Broad Absorption Line Quasars) es un tema todavía en discusión. Representando aproximadamente un 20% de la población de QSOs, estos objetos muestran líneas de absorción muy anchas en su espectro óptico/UV que están generadas por flujos de material que emerge con velocidades de hasta 0.2c. No existe consenso sobre el origen de este gas causante de las absorciones, ni del mecanismo que lo acelera, o de la relación entre los cuásares BAL y el resto de la población de cuásares. Actualmente, las hipótesis sobre su naturaleza están relacionadas principalmente con la orientación o con escenarios evolutivos. En la primera, las líneas de absorción estarían producidas por flujos emergentes originados en el disco de acrecimiento asociado al agujero negro central del QSO, pero que se observarían solamente cuando interceptan la línea de visión. En un escenario evolutivo, sin embargo, los cuásares BAL serían objetos jóvenes o re-abastecidos que todavía estarían expeliendo su envoltura de gas y polvo. En este caso, la orientación no jugaría ningún papel y las absorciones estarían producidas por materia eyectada radialmente. En este trabajo se presentan los resultados de un estudio multifrecuencia de una muestra de cuásares BAL emisores en radio. Se ha seleccionado una muestra de comparación de cuásares no-BAL emisores en radio también. Ambas muestras se han seleccionado a partir del Sloan Digital Sky Survey (SDSS). Se han realizado observaciones en radio de ambas muestras, para estudiar su distribución espectral de energía (SED) en el rango del GHz y estudiar las características de la emisión sincrotrón. El objetivo es obtener estimaciones de la edad de la radiofuente, la orientación de la radiofuente central, y obtener medidas de polarización. La comparación con la muestra de objetos no-BAL nos permite concluir que no existe una orientación preferida o predominante en los cuásares BAL. Por otro lado, sin embargo, la fracción similar de fuentes con pico en 1 GHz (36±12% vs. 24±8%) no parece sugerir que los BALs sean más jóvenes. Esta conclusión está apoyada por la presencia, en algunos casos, de componentes de baja frecuencia, supuestamente viejas, en sus radio espectros. Utilizando técnicas VLBI (Very Large Baseline Interferometry) ha sido posible estudiar así mismo la morfología, a la escala del parsec, de la mitad de la muestra. Sobre un 80% de las fuentes observadas muestran estructura resuelta con tamaños proyectados de entre decenas y centenares de parsecs. Esta fracción es comparable con otros resultados de otros autores. La variedad de morfologías observada no parece apoyar la idea de orientaciones preferentes. Se investigó también en este trabajo la emisión de cuerpo gris a longitudes de onda milimétricas con el fin de determinar si los cuásares BAL pudieran ser ricos en polvo, requisito indispensable para apoyar un escenario evolutivo. Solamente un 7% de, las fuentes observadas presentan una clara contribución por polvo a 250 GHz. Al no ser ricos en polvo, los cuásares BAL no deberían presentar un alto ritmo de formación estelar, así pues, concluimos que no deben ser una clase de objetos particularmente jóvenes. Finalmente, se han estudiado dos muestras de BALs, brillantes en el rango óptico, la primera consistente en cuásares emisores en radio y la segunda, de comparación, en objetos no emisores en radio. Se obtuvieron espectros en el infrarrojo cercano para estimar la masa del agujero negro central, sus luminosidades, sus cocientes de Eddington, el tamaño de la Broad Line Region (BLR) con el fin de buscar diferencias que podrían estar inducidas en la fase de radioemisión. Después de este análisis y junto con un análisis del catálogo SDSS DR7 de cuásares, encontramos que el único parámetro que distingue a los radio cuásares BAL es el cociente de Eddington. Un 23% de los objetos emisores en radio son super-Eddington, mientras que sólo un 13% de los no emisores en radio lo son. Una diferencia aún mayor se encuentra entre cuásares BAL y no BAL (13% vs. 2%)., This thesis work has been done under the joint PhD program between the Università di Bologna and the Universidad de Cantabria.

Grado en Física