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© 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

© 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

Studying the resolved stellar populations of the different structural components that build massive galaxies directly unveils their assembly history. We aim at characterizing the stellar population properties of a representative sample of bulges and pure spheroids in massive galaxies (M ∗ > 1010 M o˙) in the GOODS-N field. We take advantage of the spectral and spatial information provided by SHARDS and Hubble Space Telescope data to perform the multi-image spectrophotometric decoupling of the galaxy light. We derive the spectral energy distribution separately for bulges and disks in the redshift range 0.14 < z ≤ 1 with spectral resolution R ∼ 50. Analyzing these spectral energy distributions, we find evidence of a bimodal distribution of bulge formation redshifts. We find that 33% of them present old mass-weighted ages, implying a median formation redshift form=6.2_-1.7+1.5. They are relics of the early universe embedded in disk galaxies. A second wave, dominant in number, accounts for bulges formed at median redshift form=1.3_-0.6+0.6. The oldest (first-wave) bulges are more compact than the youngest. Virtually all pure spheroids (i.e., those without any disk) are coetaneous with the second-wave bulges, presenting a median redshift of formation form=1.1_-0.3+0.3 The two waves of bulge formation are distinguishable not only in terms of stellar ages but also in star formation mode. All first-wave bulges formed fast at z ∼ 6, with typical timescales around 200 Myr. A significant fraction of the second-wave bulges assembled more slowly, with star formation timescales as long as 1 Gyr. The results of this work suggest that the centers of massive disk-like galaxies actually harbor the oldest spheroids formed in the universe.

The ultimate goal in galaxy studies is having a complete picture of galaxy formation and evolution across the history of the Universe. A robust determination of the abundance of massive (an even quiescent) galaxies at high redshift is essential to constrain current models of galaxy formation and alleviate the tension between existing models and observations. In this context, this Ph.D. Thesis addresses the challenge of studying the build-up of massive galaxies adding a new population of optically faint Balmer Break Galaxies (BBGs), which are bright at longer wave lengths, to the general population of massive galaxies at z È 3..., El objetivo último de los estudios de galaxias es lograr una visión completa de la formación y evolución de las galaxias a lo largo de la historia del Universo. Determinar de forma robusta la abundancia de galaxias masivas (e incluso quiescentes) a alto desplazamiento al rojo es esencial para acotar los modelos existentes de formación de galaxias y mitigar la tensión existente entre los modelos y las observaciones. En este sentido, esta tesis doctoral aborda el reto de estudiar el ensamblado de las galaxias masivas añadiendo una nueva población de galaxias con discontinuidad de Balmer (BBG),débiles en longitudes ópticas y brillantes en longitudes de onda más largas, a la población general de galaxias masivas a z>3...

© 2020 The American Astronomical Society. Artículo firmado por 34 autores.We thank the anonymous reviewer for their critical reading of the manuscript and providing detailed and insightful comments, which greatly enhanced the quality and clarity of the paper. Support for this work was provided by NASA through grants HST-GO-13657.010-A and HST-AR-14298.004-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Support was also provided by NASA through grant NNX16AB36G as part of the Astrophysics Data Analysis Program. This work was also supported by start-up funds and the Dean’s Research Initiation Grant fund from the Rochester Institute of Technology’s College of Science. ES would like to thank Athis Osathapan, Krystal Tyler, and Kevin Cooke for intriguing discussions and assistance with spectral energy distribution fitting, which was performed using the computational resources and support from Research Computing Services at the Rochester Institute of Technology (Rochester Institute of Technology 2019). ES thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant #1829740, the Brinson Foundation, and the Moore Foundation; her participation in the program has benefited this work. HI acknowledges support from JSPS KAKENHI Grant Number JP19K23462. ET acknowledges support from FONDECYT Regular 1190818, ANID PIA ACT172033 and Basal-CATA AFB170002. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Based in part on observations obtained at the international Gemini Observatory and processed using the Gemini IRAF package (, Galaxy interactions and mergers are thought to play an important role in the evolution of galaxies. Studies in the nearby universe show a higher AGN fraction in interacting and merging galaxies than their isolated counterparts, indicating that such interactions are important contributors to black hole growth. To investigate the evolution of this role at higher redshifts, we have compiled the largest known sample of major spectroscopic galaxy pairs (2381 with ∆V < 5000 km s^(−1) ) at 0.5 < z < 3.0 from observations in the COSMOS and CANDELS surveys. We identify X-ray and IR AGN among this kinematic pair sample, a visually identified sample of mergers and interactions, and a mass-, redshift- and environment-matched control sample for each in order to calculate AGN fractions and the level of AGN enhancement as a function of relative velocity, redshift, and X-ray luminosity. While we see a slight increase in AGN fraction with decreasing projected separation, overall, we find no significant enhancement relative to the control sample at any separation. In the closest projected separation bin (< 25 kpc, ∆V < 1000 km s^(−1)), we find enhancements of a factor of 0.94^(+0.21)_(−0.16) and 1.00^(+0.58)_(−0.31) for X-ray and IR-selected AGN, respectively. While we conclude that galaxy interactions do not significantly enhance AGN activity on average over 0.5 < z < 3.0 at these separations, given the errors and the small sample size at the closest projected separations, our results would be consistent with the presence of low-level AGN enhancement., NASA, LSSTC, NSF Cybertraining, Brinson Foundation, Moore Foundation, JSPS KAKENHI, FONDECYT Regula, ANID PIA, Basal-CATA, W. M. Keck Foundation, National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), Korea Astronomy and Space Science Institute (Republic of Korea), the Association of Universities for Research in Astronomy, Inc., under NASA contract, the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA, 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 American Astronomical Society. All rights reserved. Artículo firmado por 23 autores. We thank the anonymous referee for thoughtful comments and suggestions that helped improve this work. A.H.-C. and P.G.P.-G. acknowledge funding by the Spanish Ministry of Economy and Competitiveness (MINECO) under grants AYA2012-31277, AYA2015-70815-ERC, and AYA2015-63650-P. J.M.D. acknowledges support of the projects AYA2015-64508-P (MINECO/FEDER, UE), AYA2012-39475-C02-01, and the consolider project CSD2010-00064 funded by MINECO. D.J.L. and J.R. acknowledge support from the ERC starting grant 336736-CALENDS. R.A.M. acknowledges support by the Swiss National Science Foundation. A.A.-H. acknowledges funding by the MINECO grant AYA2015-64346-C2-1-P, which is partly funded by the FEDER program. H.D.S. acknowledges funding from the program ANR-T-ERC ASTROBRAIN. P.S. acknowledges funding from the Swiss National Science Foundation under grant P2GEP2_165426. J.M.R.E. acknowledges funding by the MINECO grant AYA2015-70498-C2-1-R. H.D. acknowledges financial support from the Spanish 2014 Ramón y Cajal program MINECO RYC-2014-15686., We analyze the properties of a multiply imaged Ly alpha (Ly alpha) emitter at z = 5.75 identified through SHARDS Frontier Fields intermediate-band imaging of the Hubble Frontier Fields (HFF) cluster Abell 370. The source, A370-L57, has low intrinsic luminosity (M-UV similar to -16.5), steep UV spectral index (beta = -2.4 +/- 0.1), and extreme rest-frame equivalent width of Ly alpha (EW0 (Ly alpha) = 420(-120)(+180) angstrom). Two different gravitational lens models predict high magnification (mu similar to 10-16) for the two detected counterimages, separated by 7 '', while a predicted third counterimage (mu similar to 3-4) is undetected. We find differences of similar to 50% in magnification between the two lens models, quantifying our current systematic uncertainties. Integral field spectroscopy of A370-L57 with MUSE shows a narrow (FWHM = 204 +/- 10 km s(-1)) and asymmetric Ly alpha profile with an integrated luminosity L(Ly alpha) similar to 10(42) erg s(-1). The morphology in the Hubble Space Telescope bands comprises a compact clump (r(e) < 100 pc) that dominates the Ly alpha and continuum emission and several fainter clumps at projected distances. 1 kpc that coincide with an extension of the Ly alpha emission in the SHARDS F823W17 and MUSE observations. The latter could be part of the same galaxy or an interacting companion. We find no evidence of a contribution from active galactic nuclei to the Ly alpha emission. Fitting of the spectral energy distribution with stellar population models favors a very young (t < 10 Myr), low-mass (M-* 10(6.5) M circle dot), and metal-poor (Z less than or similar to 4 x 10(-3)) stellar population. Its modest star formation rate (SFR similar to 1.0 M circle dot yr(-1)) implies high specific SFR (sSFR similar to 2.5 x 10(-7) yr(-1)) and SFR density (SSFR similar to 7-35 M circle dot yr(-1) kpc(-2)). The properties of A370-L57 make it a good representative of the population of galaxies responsible for cosmic reionization., Unión Europea. FP7, Ministerio de Economía y Competitividad (MINECO), Swiss National Science Foundation, Program ANR-T-ERC ASTROBRAIN, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub