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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.

Los cartografiados celestes han sido, históricamente, el principal método de obtención de datos astronómicos para el estudio del Universo. Esta tesis se centra en uno de ellos, OTELO, un cartografiado en líneas de emisión que utiliza los filtros sintonizables del instrumento OSIRIS del Gran Telescopio CANARIAS, actualmente el mayor telescopio óptico reflector completamente orientable del mundo. El uso combinado de los filtros sintonizables, que permiten obtener espectroscopía de baja resolución en dos dimensiones de todas las fuentes del campo, y de un telescopio de gran diámetro, capaz de alcanzar magnitudes límite extremadamente profundas, es ideal para la búsqueda de objetos emisores débiles. En particular, nos hemos centrado en el estudio de los núcleos activos de galaxias (AGN, por sus siglas en inglés), uno de los objetos más brillantes y fascinantes del Universo. Las galaxias que albergan un AGN muestran una intensa emisión en su núcleo, fruto de la acreción de material por parte de un agujero negro super-masivo ubicado en su centro, según el modelo actualmente aceptado. Su estudio puede darnos información valiosa acerca de la formación y evolución de las galaxias en el Universo. Durante esta tesis, hemos llevado a cabo la reducción y la calibración de los datos de OTELO desde cero, un proceso que ha requerido múltiples iteraciones y el diseño de procedimientos específicos. A continuación se ha obtenido un catálogo profundo multi-rango de todas las fuentes del campo. El siguiente paso ha sido la selección de los objetos emisores usando, por un lado, la información contenida en el catálogo y, por otro, los pseudo-espectros previamente construidos para cada fuente, que constituyen una herramienta única fruto del uso de filtros sintonizables. Nos hemos centrado, específicamente, en la población de emisores Hα a z~0.40, una de las líneas de emisión más intensas del espectro óptico de las galaxias, directamente relacionada con su formación estelar y con la actividad nuclear cuando ésta está presente. A continuación, hemos seleccionado los AGN del campo utilizando cuatro métodos distintos, cada uno de ellos centrado en un rango espectral diferente. Finalmente hemos analizado la muestra de AGN, en un estudio que incluye su demografía y morfología, la búsqueda de galaxias infrarrojas luminosas y ultra-luminosas (LIRGs/ULIRGs), la obtención de la función de luminosidad (LF) de Hα a z~0.40 y un análisis del entorno a ese desplazamiento al rojo. El principal producto de esta tesis es el catálogo de objetos emisores de OTELO, un catálogo profundo y multi-rango que será la base de futuros trabajos. Además, hemos obtenido muestras fiables de emisores Hα y de AGN en el campo de OTELO. El análisis de la población de AGN nos ha permitido confirmar resultados previos, como el predominio de galaxias de tipo tardío, una mayor incidencia de AGN entre los ULIRGs que entre los LIRGs o la efectividad de los rayos-X a la hora de seleccionar los AGN, entre otras muchas cosas. La función de luminosidad Hα obtenida a z~0.40 nos ha permitido, además, extender el límite de anteriores LFs, llegando a luminosidades casi 1 dex más débiles que el resto de los trabajos publicados hasta la fecha. Conociendo los AGN a z~0.40, hemos podido estimar también la tasa de formación estelar de las galaxias con formación estelar a ese desplazamiento al rojo, así como la contribución de los AGN a la luminosidad total.

OTELO (Osiris Tunable Emission Line Object survey) has become the deepest emission-line survey to date using the Tunable Filters of the OSIRIS instrument at the GTC, which allow to obtain 2D low-resolution spectroscopy of all the objects in the field. More than 10k objects have been detected up to 3 sigma in the resulting deep image, with limiting flux of 1.8x10-20 erg/s/cm²/angstrom (mAB=27.18). A first multiwavelength catalogue of all the objects has been built using public archive data from X-Rays to Infrared. The emission-line objects have then been selected and their photometric redshifts derived. The confirmed emitters account for about 10% of the total number of objects, although another 20% of candidates is still awaiting confirmation. The next step has been to discriminate between Star-Forming Galaxies and AGN. To do that, we have used diagnostic and color-color diagrams, such as the ones in Cid-Fernandes et al. (2010) or Donley et al. (2012), as well as the complementary information in X-Rays and MIR. In this talk, we present the latest results obtained from the analysis of the population of Active Galactic Nuclei found in OTELO field of view, with special emphasis on the low-luminosity ones.