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La evolución de las galaxias es el resultado de una gran cantidad de interacciones muy complejas que tienen lugar entre los distintos componentes que las conforman. Esto hace que desentrañar los misterios que aún permanecen desconocidos necesite de una cantidad ingente de datos que abarquen la mayor cantidad posible de observables. El objetivo de esta tesis es profundizar en el conocimiento que tenemos sobre las características que presentan las poblaciones estelares y el medio interestelar en las galaxias cercanas ayudándonos de las últimas herramientas desarrolladas en el campo de la astrofísica..., The evolution of galaxies is the result of a large number of very complex interactions that take place between the different components that make them up. This means that unravelling the mysteries that remain unknown requires a huge amount of data covering as many observables as possible. The aim of this thesis is to deepen our knowledge of the characteristics of stellar populations and the interstellar medium in nearby galaxies with the help of the latest tools developed in the field of astrophysics...

We use high-resolution HST imaging and e-MERLIN 1.5-GHz observations of galaxy cores from the LeMMINGs survey to investigate the relation between optical structural properties and nuclear radio emission for a large sample of galaxies. We perform accurate, multi-component decompositions of new surface brightness profiles extracted from HST images for 163 LeMMINGs galaxies and fit up to six galaxy components (e.g., bulges, discs, AGN, bars, rings, spiral arms, and nuclear star clusters) simultaneously with Sérsic and/or core-Sérsic models. By adding such decomposition data for 10 LeMMINGs galaxies from our past work, the final sample of 173 nearby galaxies (102 Ss, 42 S0s, 23 Es plus 6 Irr) with bulge stellar mass (typically) M_*, bulge ~ 10^6-10^12.5 M_sun, encompasses all optical spectral classes (LINER, Seyfert, ALG and H II). We show that the bulge mass can be significantly overestimated in many galaxies when components such as bars, rings and spirals are not included in the fits. We additionally implement a Monte Carlo method to determine errors on bulge, disc and other fitted structural parameters. Moving (in the opposite direction) across the Hubble sequence, i.e., from the irregular to elliptical galaxies, we confirm that bulges become larger, more prominent and round. Such bulge dominance is associated with a brighter radio core luminosity. We also find that the radio detection fraction increases with bulge mass. At M_*,bulge > 10^11 M_sun, the radio detection fraction is 77%, declining to 24% for M_bulge < 10^10 M_sun. Furthermore, we observe core-Sérsic bulges tend to be systematically round and to possess high radio core luminosities and boxy-distorted or pure elliptical isophotes.

Multiwavelength studies indicate that nuclear activity and bulge properties are closely related, but the details remain unclear. To study this further, we combine Hubble Space Telescope bulge structural and photometric properties with 1.5 GHz, e-MERLIN nuclear radio continuum data from the LeMMINGs survey for a large sample of 173 `active' galaxies (LINERs and Seyferts) and `inactive' galaxies (H IIs and absorption line galaxies, ALGs). Dividing our sample into active and inactive, they define distinct (radio core luminosity)−(bulge mass), L_R,core-M_*,bulge, relations, with a mass turnover at M_*, bulge ~ 10^(9.8 +- 0.3) M_sun (supermassive black hole mass M_BH ~ 10^(6.8 +- 0.3) M_sun), which marks the transition from AGN-dominated nuclear radio emission in more massive bulges to that mainly driven by stellar processes in low-mass bulges. None of our 10/173 bulgeless galaxies host an AGN. The AGN fraction increases with increasing M_*, bulge such that f_optical_AGN ∝ M_*,bulge^(0.24 +- 0.06) and f_radio_AGN ∝ M_*,bulge^(0.24 +- 0.05). Between M_*,bulge ~ 10^8.5 and 10^11.3 M_sun, f_optical_AGN steadily rises from 15 +- 4 to 80 +- 5 per cent. We find that at fixed bulge mass, the radio loudness, nuclear radio activity and the (optical and radio) AGN fraction exhibit no dependence on environment. Radio-loud hosts preferentially possess an early-type morphology than radio-quiet hosts, the two types are however indistinguishable in terms of bulge Sérsic index and ellipticity, while results on the bulge inner logarithmic profile slope are inconclusive. We finally discuss the importance of bulge mass in determining the AGN triggering processes, including potential implications for the nuclear radio emission in nearby galaxies.

© 2007. The American Astronomical Society. All rights reserved. Artículo firmado por 29 autores. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA’s support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d’Etudes Spatiales of France and the Korean Ministry of Science and Technology. A. G. d. P. is financed by the MAGPOP EU Marie Curie Research Training Network and partially by the Spanish Programma Nacional de Astronomía y Astrofísica under grants AYA2003-01676 and AYA2006-02358. This research has made use of the NASA/IPAC Extragalactic Database (NED). We acknowledge the use of the HyperLeda database (http://leda.univ-lyon1.fr). The Digitized Sky Surveys were produced at the Space Telescope Science Institute under US Government grant NAG W-2166. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. Some images presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST ). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5- 26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NAG5-7584 and by other grants and contracts. This research has made use of the NASA/ IPAC Infrared Science Archive. This publication makes use of data products from the Two Micron All Sky Survey., We have initiated a search for extended ultraviolet disk (XUV-disk) galaxies in the local universe. Here we compare GALEX UV and visible-NIR images of 189 nearby (D < 40 Mpc) S0-Sm galaxies included in the GALEX Atlas of Nearby Galaxies and present the first catalog of XUV-disk galaxies. We find that XUV-disk galaxies are surprisingly common but have varied relative (UV/optical) extent and morphology. Type 1 objects (≳20% incidence) have structured, UV-bright/optically faint emission features in the outer disk, beyond the traditional star formation threshold. Type 2 XUV-disk galaxies (~10% incidence) exhibit an exceptionally large, UV-bright/optically low surface brightness (LSB) zone having blue UV-K_s outside the effective extent of the inner, older stellar population, but not reaching extreme galactocentric distance. If the activity occurring in XUV-disks is episodic, a higher fraction of present-day spirals could be influenced by such outer disk star formation. Type 1 disks are associated with spirals of all types, whereas Type 2 XUV-disks are predominantly found in late-type spirals. Type 2 XUV-disks are forming stars quickly enough to double their (currently low) stellar mass in the next Gyr (assuming a constant star formation rate). XUV-disk galaxies of both types are systematically more gas-rich than the general galaxy population. Minor external perturbation may stimulate XUV-disk incidence, at least for Type 1 objects. XUV-disks are the most actively evolving galaxies growing via inside-out disk formation in the current epoch, and may constitute a segment of the galaxy population experiencing significant, continued gas accretion from the intergalactic medium or neighboring objects., Programa Nacional de Astronomía y Astrofísica (PNAyA), España, US Government, Alfred P. Sloan Foundation, National Science Foundation (NSF), US Department of Energy, National Aeronautics and Space Administration, Japanese Monbukagakusho, Max Planck Society, Higher Education Funding Council for England, National Aeronautics and Space Administration (NASA), Office of Space Science (NASA), Unión Europea. FP6, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2016. The American Astronomical Society. All rights reserved. Artículo firmado por 28 autores., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2001. This paper is based on observations obtained at the German-Spanish Astronomical Centre, Calar Alto, Spain, operated by the Max-Planck Institute für Astronomie (MPIE), Heidelberg, jointly with the Spanish Commission for Astronomy. It is also partly based on observations made with the Jacobus Kapteyn Telescope operated on the island of La Palma by the Royal Greenwich Observatory in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias and the 1.52 m telescope of the EOCA/OAN Observatory. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We have also use of the LEDA database, http://www-obs.univ-lyon1.fr. This research was also supported by the Spanish Programa Sectorial de Promoción General del Conocimiento under grants PB96-0610 and PB96- 0645. P. G. Pérez González acknowledges the receipt of a “Formación de Profesorado Universitario” fellowship from the Spanish “Ministerio de Educación y Cultura”. We would like to thank C. E. García Dabó and S. Pascual for their help during part of the observing runs and stimulating conversations. We thank M. N. Estévez for carefully reading the manuscript and making some useful remarks. We are also grateful to Dr. E. Emsellem for his helpful comments and suggestions., We present Johnson B surface photometry for the UCM Survey galaxies. One-dimensional bulge-disk decomposition is attempted, discussing on fitting functions and computational procedures. The results from this decomposition, jointly with concentration indices and an asymmetry coefficient, are employed to study the morphological properties of these galaxies. We also compare our results with the previous morphological classification established using Gunn r imaging data and with other samples of galaxies. No major statistical differences in morphology are found between red and blue data, although some characteristics such as size and luminosity concentration vary. We find a correlation between luminosity and size. Several parameters are used to segregate the objects according to their morphological type., National Aeronautics and Space Administration (NASA), Programa Sectorial de Promoción General del Conocimiento (MEC), España, Ministerio de Educación y Cultura (MEC), España, Programa Formación de Profesorado Universitario (MEC), España, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2014. This study makes uses of the data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey (http://califs.caha.es). CALIFA is the first legacy survey being performed at Calar Alto. The CALIFA collaboration would like to thank the IAA-CSIC and MPIA-MPG as major partners of the observatory, and CAHA itself, for the unique access to telescope time and support in manpower and infrastructures. The CALIFA collaboration thanks also the CAHA staff for the dedication to this project. We thank Mike Blanton for helpful discussions on the SDSS survey footprint and for providing the NYU low-z catalogue to the community. CJW acknowledges useful discussion with Nick Scott, Davor Krajnovic and Remco van den Bosch as well as support through the Marie Curie Career Integration Grant 303912. We thank the anonymous referee for a careful reading of the paper and several suggestions that improved its presentation. IM acknowledges the financial support from the Spanish grant AYA2010-15169 and from the Junta de Andalucía through TIC-114 and the Excellence Project P08-TIC-03531. R.G.D., E.P. and R.G.B. acknowledge support from the Spanish Ministerio de Economía y Competitividad, through projects AYA2010-15081. RAM is funded by the Spanish programme of International Campus of Excellence Moncloa (CEI). J.I.P. acknowledges financial support from the Spanish MINECO under grant AYA2010-21887-C04-01 and from Junta de Andalucía Excellence Project PEX2011-FQM7058. Support for L.G. is provided by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC12009, awarded to The Millennium Institute of Astrophysics, MAS. L.G. acknowledges support by CONICYT through FONDECYT grant 3140566. AM.-I. acknowledges support from Agence Nationale de la Recherche through the STILISM project (ANR-12-BS05-0016-02). AM.-I. and S.B. acknowledge support from BMBF through the Erasmus-F project (grant number 05 A12BA1). JMA acknowledges support from the Eur, We describe and discuss the selection procedure and statistical properties of the galaxy sample used by the Calar Alto Legacy Integral Field Area (CALIFA) survey, a public legacy survey of 600 galaxies using integral field spectroscopy. The CALIFA "mother sample" was selected from the Sloan Digital Sky Survey (SDSS) DR7 photometric catalogue to include all galaxies with an r-band isophotal major axis between 45 '' and 79 : 2 '' and with a redshift 0 : 005 < z < 0 : 03. The mother sample contains 939 objects, 600 of which will be observed in the course of the CALIFA survey. The selection of targets for observations is based solely on visibility and thus keeps the statistical properties of the mother sample. By comparison with a large set of SDSS galaxies, we find that the CALIFA sample is representative of galaxies over a luminosity range of -19 > M-r > -23 : 1 and over a stellar mass range between 10(9.7) and 10(11.4) M-circle dot. In particular, within these ranges, the diameter selection does not lead to any significant bias against - or in favour of - intrinsically large or small galaxies. Only below luminosities of M-r = -19 (or stellar masses < 10(9.7) M-circle dot) is there a prevalence of galaxies with larger isophotal sizes, especially of nearly edge-on late-type galaxies, but such galaxies form < 10% of the full sample. We estimate volume-corrected distribution functions in luminosities and sizes and show that these are statistically fully compatible with estimates from the full SDSS when accounting for large-scale structure. For full characterization of the sample, we also present a number of value-added quantities determined for the galaxies in the CALIFA sample. These include consistent multi-band photometry based on growth curve analyses; stellar masses; distances and quantities derived from these; morphological classifications; and an overview of available multi-wavelength photometric measurements. We also explore different ways of characterizing the e, Marie Curie Career Integration Grant, Junta de Andalucía, Ministerio de Economia y Competitividad (MINECO), Spanish programme of International Campus of Excellence Moncloa (CEI), Unión Europea. FP7, Ministry of Economy, Development, and Tourism's Millennium Science Initiative, CONICYT through FONDECYT, Agence Nationale de la Recherche through the STILISM project, BMBF through the Erasmus-F project, European Research Council, European Union, Natural Sciences and Engineering Research Council of Canada (NSERC), Academy of Sciences of the Czech Republic, National Aeronautics and Space Administration, Alfred P. Sloan Foundation, National Science Foundation, US Department of Energy, Japanese Monbukagakusho, Max Planck Society, Astrophysical Research Consortium (ARC), University of Chicago, Fermilab, Institute for Advanced Study, Japan Participation Group, Johns Hopkins University, Los Alamos National Laboratory, Max-Planck-Institute for Astronomy (MPIA), Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, Princeton University, United States Naval Observatory, University of Washington, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2013. Artículo firmado por 75 autores. CALIFA is the first legacy survey being performed at Calar Alto. The CALIFA collaboration would like to thank the IAA-CSIC and MPIAMPG as major partners of the observatory, and CAHA itself, for the unique access to telescope time and support in manpower and infrastructures. The CALIFA collaboration thanks also the CAHA staff for the dedication to this project. We thank the Viabilidad Diseño Acceso y Mejora funding program, ICTS-2009-10, for funding the data acquisition of this project. We thank the referee Mark Westmoquette for a prompt report with many valuable comments that improved the clarity of the article. B.H. gratefully acknowledges the support by the DFG via grant Wi 1369/29-1. K.J. was supported by the Emmy Noether Programme of the german DFG under grant Ja 1114/3-1. S.F.S., F.F.R.O., and D.M. thank the Plan Nacional de Investigación y Desarrollo funding programs, AYA2010-22111-C03-03 and AYA2010-10904E, of the Spanish Ministerio de Ciencia e Innovación, for the support given to this project. S.F.S. also thanks the the Ramón y Cajal project RyC-2011-07590 of the spanish Ministerio de Economia y Competitividad, for the support giving to this project. R.C.F. acknowledges the support of the brazilian agencies CAPES and CNPq. J.F.-B. acknowledges support from the Ramón y Cajal Program financed by the Spanish Ministry of Economy and Competitiveness (MINECO). This research has been supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under grants AYA2010-21322-C03-02 and AIB-2010-DE-00227. R.G.-B. has been supported by the Spanish Ministerio de Ciencia e Innovación under grant AYA2010-15081. R.A.M. was also funded by the spanish programme of International Campus of Excellence Moncloa (CEI). D.M. and A.M.I. are supported by the Spanish Research Council within the program JAE-Doc, Junta para la Ampliación de Estudios, co-funded by the FSE. F.F.R.-O. acknowledge fi- nancial support for the ESTALLIDOS, We present the first public data release (DR1) of the Calar Alto Legacy Integral Field Area (CALIFA) survey. It consists of science-grade optical datacubes for the first 100 of eventually 600 nearby (0.005 < z < 0.03) galaxies, obtained with the integral-field spectrograph PMAS/PPak mounted on the 3.5 m telescope at the Calar Alto observatory. The galaxies in DR1 already cover a wide range of properties in color-magnitude space, morphological type, stellar mass, and gas ionization conditions. This offers the potential to tackle a variety of open questions in galaxy evolution using spatially resolved spectroscopy. Two different spectral setups are available for each galaxy, (i) a low-resolution V500 setup covering the nominal wavelength range 3745-7500 angstrom with a spectral resolution of 6.0 angstrom (FWHM), and (ii) a medium-resolution V1200 setup covering the nominal wavelength range 3650-4840 angstrom with a spectral resolution of 2.3 angstrom (FWHM). We present the characteristics and data structure of the CALIFA datasets that should be taken into account for scientific exploitation of the data, in particular the effects of vignetting, bad pixels and spatially correlated noise. The data quality test for all 100 galaxies showed that we reach a median limiting continuum sensitivity of 1.0 x 10(-18) erg s(-1) cm(-2) angstrom(-1) arcsec(-2) at 5635 angstrom and 2.2 x 10(-18) erg s(-1) cm(-2) angstrom(-1) arcsec(-2) at 4500 angstrom for the V500 and V1200 setup respectively, which corresponds to limiting r and g band surface brightnesses of 23.6 mag arcsec(-2) and 23.4 mag arcsec(-2), or an unresolved emission-line flux detection limit of roughly 1 x 10(-17) erg s(-1) cm(-2) arcsec(-2) and 0.6 x 10(-17) erg s(-1) cm(-2) arcsec(-2), respectively. The median spatial resolution is 3 ''.7, and the absolute spectrophotometric calibration is better than 15% (1 sigma). We also describe the available interfaces and tools that allow easy access to this first public CALIFA d, Viabilidad Diseño Acceso y Mejora, DFG, Emmy Noether Programme of the german DFG, Plan Nacional de Investigación y Desarrollo of the Spanish Ministerio de Ciencia e Innovación, Ramón y Cajal of the spanish Ministerio de Economia y Competitividad, Spanish Ministry of Economy and Competitiveness (MINECO), Ministerio de Ciencia e Innovación, Spanish programme of International Campus of Excellence Moncloa (CEI), Spanish Research Council within the program JAE-Doc, FSE, FCT, Czech program for the long-term development of the research institution, Czech Academy of Sciences, Junta de Andalucía, Ramón y Cajal programme, MICINN, FCT/MCTES (Portugal), POPH/FSE (EC), Marie Curie IntraEuropean Reintegration grant, Plan Nacional del Espacio del Ministerio de Educación y Ciencia, European Research Council, PNAYA, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2011. The American Astronomical Society. All rights reserved. We thank the staff of the Arizona Radio Observatory for granting us observing time. We thank Noam Soker and Joel Kastner for their valuable comments on an earlier version of this Letter. R.S.'s contribution to the research described here was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Financial support was provided by NASA through a Long Term Space Astrophysics and GALEX GO award., Binarity is believed to dramatically affect the history and geometry of mass loss in asymptotic giant branch (AGB) and post-AGB stars, but observational evidence of binarity is sorely lacking. As part of a project to look for hot binary companions to cool AGB stars using the Galaxy Evolution Explorer archive, we have discovered a late-M star, Y Gem, to be a source of strong and variable UV emission. Y Gem is a prime example of the success of our technique of UV imaging of AGB stars in order to search for binary companions. Y Gem's large and variable UV flux makes it one of the most prominent examples of a late-AGB star with a mass accreting binary companion. The UV emission is most likely due to emission associated with accretion activity and a disk around a main-sequence companion star. The physical mechanism generating the UV emission is extremely energetic, with an integrated luminosity of a few × L_☉ at its peak. We also find weak CO J = 2-1 emission from Y Gem with a very narrow line profile (FWHM of 3.4 km s^–1). Such a narrow line is unlikely to arise in an outflow and is consistent with emission from an orbiting, molecular reservoir of radius 300 AU. Y Gem may be the progenitor of the class of post-AGB stars which are binaries and possess disks but no outflows., National Aeronautics and Space Administration (NASA), Galaxy Evolution Explorer (GALEX), NASA, Long Term Space Astrophysics Project (NASA), Arizona Radio Observatory, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2012 SPIE. Conference on High Energy, Optical, and Infrared Detectors for Astronomy V (2012. Amsterdam, Netherlands), A CCD test-bench has been built at the Universidad Complutense's LICA laboratory. It is initially intended for commissioning of the MEGARA(1) (Multi-Espectrografo en GTC de Alta Resolucion para Astronomia) instrument but can be considered as a general purpose scientific CCD test-bench. The test-bench uses an incandescent broad-band light source in combination with a monochromator and two filter wheels to provide programmable narrow-band illumination across the visible band. Light from the monochromator can be directed to an integrating sphere for flat-field measurements or sent via a small aperture directly onto the CCD under test for high accuracy diode-mode quantum efficiency measurements. Point spread function measurements can also be performed by interposing additional optics between sphere and the CCD under test. The whole system is under LabView control via a clickable GUI. Automated measurement scans of quantum efficiency can be performed requiring only that the user replace the CCD under test with a calibrated photodiode after each measurement run. A 20cm diameter cryostat with a 10cm window and Brooks Polycold PCC closed-cycle cooler also form part of the test-bench. This cryostat is large enough to accommodate almost all scientific CCD formats has initially been used to house an E2V CCD230 in order to fully prove the test-bench functionality. This device is read-out using an Astronomical Research Camera controller connected to the UKATC's UCAM data acquisition system., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

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

© 2007. The American Astronomical Society. All rights reserved. We thank Harold Corwin for his comments on early descriptions of these galaxies. This research made use of the NASA/ IPAC Extragalactic Database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration., The object NGC 6908 was once thought to simply be a surface brightness enhancement in the eastern spiral arm of the nearby spiral galaxy NGC 6907. Based on an examination of near-infrared imaging, the object is shown to in fact be a lenticular S0(6/7) galaxy hidden in the optical glare of the disk and spiral structure of the larger galaxy. New radial velocities of NGC 6908 [3060 ± 16 km s^-1 (emission); 3113 ± 73 km s^-1 (absorption)] have been obtained at the Baade 6.5 m and the du Pont 2.5 m telescopes at Las Campanas, Chile, placing NGC 6908 at the same expansion velocity distance as NGC 6907 (3190 ± 5 km s^-1), eliminating the possibility of a purely chance line-of-sight coincidence. The once-enigmatic asymmetries in the disk and outer spiral structure of NGC 6907 are now explained as being due to an advanced merger event. Newly discovered tails and debris in the outer reaches of this galaxy further support the merger scenario for this system. This pair of galaxies is a rather striking example of two objects discovered over 100 years ago, whose true nature was lost until modern detectors operating at infrared wavelengths gave us a new (high-contrast) look. Other examples of embedded merger remnants may also reveal themselves in the growing samples of near-infrared imaging of nearby galaxies, and a pilot study does reveal several other promising candidates for follow-up observations., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2012 SPIE. Conference on Optical Systems Design (2012. Barcelona, Spain). MEGARA is being funded by GRANTECAN, public entity responsible for the management and operation of GTC. The sliced-pupil grating design efforts are part of a collaborative project between the SME FRACTAL and the UCM. The first prototype received funds from the Madrid Regional Government (CAM) through grant 22/2009 for Aero-spatial Innovation. The development of this concept for large telescopes (VIENTOS project) has been co-funded by CDTI (Development and Industrial Transfer Center; Ministry of Economy and Competiveness, Spain) under the Industry for Science program IdC-20101106. The authors thank also the support received from the Consolider-Ingenio 2010 Program grant CSD2006-00070 "First Science with the GTC" and the Spanish National Plan for Astronomy & Astrophysics grant AyA2009-10368. The LICA-UCM laboratory is funded by the Moncloa "Campus de Excelencia Internacional"., We describe the optical design of MEGARA, the future optical Integral Field Unit (IFU) and Multi-Object Spectrograph (MOS) for the 10.4-m Gran Telescopio CANARIAS (GTC). MEGARA is being built by a Consortium of public research institutions led by the Universidad Complutense de Madrid (UCM, Spain) that also includes INAOE (Mexico), IAA-CSIC (Spain) and UPM (Spain)., Gran Telescopio Canarias, GRANTECAN (GTC), Comunidad de Madrid, Consolider-Ingenio 2010 Program (MICINN), Programa Nacional de Astronomía y Astrofísica (PNAyA), España, Campus de Excelencia Internacional, Moncloa, SME FRACTAL, Universidad Complutense de Madrid, Fondo Europeo de Desarrollo Regional para el Fomento de la Innovación en el Sector Aeroespacial de la Comunidad de Madrid, Centro para el Desarrollo Tecnológico Industrial (CDTI), MINECO, Ministerio de Economía y Competitividad (MINECO), España, Ministerio de Ciencia e Innovación (MICINN), España, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

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

© 2013 American Physical Society. We acknowledge financial support from Conseil Regional d'Ile-de-France and from Ministere de l'Enseignement Superieur et de la Recherche within IFRAF and CPER. L. S. acknowledges support from the Deutsche Forschungsgemeinschaft (SA1031/6) and the Cluster of Excellence QUEST., We report on the realization of quantum magnetism using a degenerate dipolar gas in an optical lattice. Our system implements a lattice model resembling the celebrated t-J model. It is characterized by a nonequilibrium spinor dynamics resulting from intersite Heisenberg-like spin-spin interactions provided by nonlocal dipole-dipole interactions. Moreover, due to its large spin, our chromium lattice gases constitute an excellent environment for the study of quantum magnetism of high-spin systems, as illustrated by the complex spin dynamics observed for doubly occupied sites., Conseil Regional d'Ile-de-France, Ministere de l'Enseignement Superieur et de la Recherche within IFRAF and CPER, Francia, Deutsche Forschungsgemeinschaft, Cluster of Excellence QUEST, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO, 2015. Artículo firmado por 29 autores. We are grateful to the anonymous referee for constructive comments and suggestions. R. A. Marino is funded by the Spanish program of International Campus of Excellence Moncloa (CEI). This study makes uses of the data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey (http://www.califa.caha.es). CALIFA is the first legacy survey being performed at Calar Alto. The CALIFA collaboration would like to thank the IAA-CSIC and MPIA-MPG as major partners of the observatory, and CAHA itself, for the unique access to telescope time and support in manpower and infrastructures. The CALIFA collaboration thanks also the CAHA staff for their dedication to this project. We thank Carmen Eliche Moral and Antonio Cava for stimulating discussions at several points in the developments of this work. We acknowledge support from the Plan Nacional de Investigación y Desarrollo funding programs, AyA2010-15081, AyA2012-30717 and AyA2013-46724P, of Spanish Ministerio de Economía y Competitividad (MINECO). A.G.d.P. acknowledges the support from the FP7 Marie Curie Actions of the European Commission, via the Initial Training Network DAGAL under REA grant agreement PITN-GA-2011-289313. C.C.-T. thanks the support of the Spanish Ministerio de Educación, Cultura y Deporte by means of the FPU fellowship program. C.J.W. acknowledges support through the Marie Curie Career Integration Grant 303912. Support for L.G. is provided by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC 120009, awarded to The Millennium Institute of Astrophysics, MAS. L.G. acknowledges support by CONIC YT through FONDECYT grant 3140566. S.F.S. thanks the CONACYT-125180 and DGAPA-IA100815 projects for providing him support in this study. J.M.A. acknowledges support from the European Research Council Starting Grant (SEDmorph; P.I. V. Wild). P.P. is supported by FCT through the Investigador FCT Contract No. IF/01220/20, We study, for the first time in a statistically significant and well-defined sample, the relation between the outer-disk ionized-gas metallicity gradients and the presence of breaks in the surface brightness profiles of disk galaxies. Sloan Digital Sky Survey (SDSS) g′- and r′-band surface brightness, (g′ – r′) color, and ionized-gasoxygen abundance profiles for 324 galaxies within the Calar Alto Legacy Integral Field Area (CALIFA) survey are used for this purpose. We perform a detailed light-profile classification, finding that 84% of our disks show down- or up-bending profiles (Type II and Type III, respectively), while the remaining 16% are well fitted by one single exponential (Type I). The analysis of the color gradients at both sides of this break shows a U-shaped profile for most Type II galaxies with an average minimum (g′ − r′) color of ~0.5 mag and an ionized-gas metallicity flattening associated with it only in the case of low-mass galaxies. Comparatively, more massive systems show a rather uniform negative metallicity gradient. The correlation between metallicity flattening and stellar mass for these systems results in p-values as low as 0.01. Independent of the mechanism having shaped the outer light profiles of these galaxies, stellar migration or a previous episode of star formation in a shrinking star-forming disk, it is clear that the imprint in their ionized-gas metallicity was different for low- and high-mass Type II galaxies. In the case of Type III disks, a positive correlation between the change in color and abundance gradient is found (the null hypothesis is ruled out with a p-value of 0.02), with the outer disks of Type III galaxies with masses ≤10^10 M_⊙ showing a weak color reddening or even a bluing. This is interpreted as primarily due to a mass downsizing effect on the population of Type III galaxies that recently experienced an enhanced inside-out growth., Unión Europea. FP7, Ministerio de Economía y Competitividad (MINECO), España, Campus de Excelencia Internacional Moncloa (CEI), Acciones Marie Curie (UE), Ministerio de Educación, Cultura y Deporte (MECD), España, Ministry of Economy, Development, and Tourism's Millennium Science Initiative, Fondo Nacional de Desarrollo Científico, Tecnológico y de Innovación Tecnológica (FONDECYT), Chile, Iniciativa Científica Milenio (ICM), Chile, FCT Investigator Programme, Portugal, Ministerio de Educación y Ciencia (MEC), Portugal, Dirección General Asuntos del Personal Académico-UNAM, México, Fondos FEDER (UE), Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016 I+D+i (MINECO), España, Ministerio Economía, Fomento y Turismo (MEFT), Chile, Millennium Institute of Astrophysics (MAS), Comisión Nacional de Investigación Científica y Tecnológica (CONICYT), Chile, Universidad Nacional Autónoma de México (UNAM), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2014 SPIE. Conference on Modeling, Systems Engineering, and Project Management for Astronomy (VI. 2014. Montreal, Canada)., MEGARA (Multi-Espectrografo en GTC de Alta Resolucion para Astronomia) is a facility instrument of the 10.4m GTC (La Palma, Spain) working at optical wavelengths that provides both Integral-Field Unit (IFU) and Multi-Object Spectrograph (MOS) capabilities at resolutions in the range R= 6,000-20,000. The MEGARA focal plane subsystems are located at one of the GTC focal stations, while the MEGARA refractive VPH based spectrograph is located at one of the Nasmyth platforms. The fiber bundles conduct the light from the focal plane subsystems to the pseudo-slits at the entrance of the spectrograph. The project is an initiative led by Universidad Complutense de Madrid (Spain) in collaboration with INAOE (Mexico), IAA-CSIC (Spain) and Universidad Politecnica de Madrid (Spain) and is developed under contract with GRANTECAN. The project is carried out by a multidisciplinary and geographically distributed team, which includes the in-kind contributions of the project partners and personnel from several private companies. The MEGARA system-engineering plan has been tailored to the project and is being applied to ensure the technical control of the project in order to finally meet the science high-level requirements and GTC constrains., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2002. The American Astronomical Society. All rights reserved. We would like to thank the referee for the useful comments and suggestions that have significantly improved the quality of this paper. We are also very grateful to A. G. Bruzual for providing the GISSEL99 evolutionary synthesis models, P.G. Pérez González, N. Cardiel, and O. Pevunova for stimulating conversations, and C. Sánchez Contreras for carefully reading the manuscript and making some useful remarks. A. G. de P. acknowledges financial support from NASA through a Long Term Space Astrophysics grant to B. F. M., We have derived the uncertainties to be expected in the derivation of galaxy physical properties (star formation history, age, metallicity, and reddening) when comparing broadband photometry to the predictions of evolutionary synthesis models. We have obtained synthetic colors for a large sample (~9000) of artificial galaxies by assuming different star formation histories, ages, metallicities, reddening values, and redshifts. The colors derived have been perturbed by adopting different observing errors and compared against the evolutionary synthesis models grouped in different sets. The comparison has been performed using a combination of Monte Carlo simulations, a maximum likelihood estimator, and principal component analysis. After comparing the input and derived output values we have been able to compute the uncertainties and covariant degeneracies between the galaxy physical properties as a function of (1) the set of observables available, (2) the observing errors, and (3) the galaxy properties themselves. In this work we have considered different sets of observables, some of them including the standard Johnson-Cousins (UBVR_CI_C) and Sloan Digital Sky Survey (SDSS) bands in the optical, the Two Micron All-Sky Survey (2MASS) bands in the near-infrared, and the Galaxy Evolution Explorer (GALEX) bands in the UV, at three different redshifts, z = 0.0, 0.7, and 1.4. This study is intended to represent a basic tool for the design of future projects on galaxy evolution, allowing an estimate of the optimal bandpass combinations and signal-to-noise ratios required for a given scientific objective., National Aeronautics and Space Administration (NASA), Long Term Space Astrophysics Program (NASA), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2014. We wish to thank Brad Gibson and Pierre Ocvirk for their constant advice. P.S.-B. acknowledges support from the Ramón y Cajal program, grant ATA2010-21322-C03-02 from the Spanish Ministry of Economy and Competitiveness (MINECO). F.F.R.O. acknowledges the Mexican National Council for Science and Technology (CONACYT) for financial support under the programme Estancias Posdoctorales y Sabáticas al Extranjero para la Consolidación de Grupos de Investigación, 2010-2012. We acknowledge financial support from the research projects under grants AYA2010-21887-C04-03, AYA2010-21322-C03-03 and AYA2010-15081 by the Spanish Ministerio de Ciencia e Innovación. J.F.-B. acknowledges support from the Ramón y Cajal Program, grants AYA2010-21322-C03-02 from the Spanish Ministry of Economy and Competitiveness (MINECO). R. A. M. is funded by the Spanish program of International Campues of Excellence Moncloa (CEI). C.J.W. acknowledges support through the Marie Curie Career Integration Grant 303912. I.M. acknowledges financial support from the Junta de Andalucía through projects PO8-TIC-03531 and TIC114, and the Spanish Ministry of Economy and Competitiveness (MINECO) through the project AYA2010-15169. We acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr). Based on observations collected at the Centro Astronómico Hispano-Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut ur Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). FCT/MCTES (Portugal) and POPH/FSE (EC). He acknowledges support by the Fundacao para a Ciencia e a Tecnologia (FCT) under project FCOMP-01-0124-FEDER-029170 (Reference FCT PTDC/FIS-AST/3214/2012), funded by FCT-MEC (PIDDAC) and FEDER (COMPETE). We also thanks the referee por his/her suggestions that have improved the final version of this paper., While studies of gasphase metallicity gradients in disc galaxies are common, very little has been done towards the acquisition of stellar abundance gradients in the same regions. We present here a comparative study of the stellar metallicity and age distributions in a sample of 62 nearly face-on, spiral galaxies with and without bars, using data from the CALIFA survey. We measure the slopes of the gradients and study their relation with other properties of the galaxies. We find that the mean stellar age and metallicity gradients in the disc are shallow and negative. Furthermore, when normalized to the effective radius of the disc, the slope of the stellar population gradients does not correlate with the mass or with the morphological type of the galaxies. In contrast to this, the values of both age and metallicity at similar to 2.5 scale lengths correlate with the central velocity dispersion in a similar manner to the central values of the bulges, although bulges show, on average, older ages and higher metallicities than the discs. One of the goals of the present paper is to test the theoretical prediction that non-linear coupling between the bar and the spiral arms is an efficient mechanism for producing radial migrations across significant distances within discs. The process of radial migration should flatten the stellar metallicity gradient with time and, therefore, we would expect flatter stellar metallicity gradients in barred galaxies. However, we do not find any difference in the metallicity or age gradients between galaxies with and without bars. We discuss possible scenarios that can lead to this lack of difference., Ramón y Cajal program from the Spanish Ministry of Economy and Competitiveness (MINECO), Mexican National Council for Science and Technology (CONACYT), Spanish Ministerio de Ciencia e Innovación, Spanish program of International Campus of Excellence Moncloa (CEI), Marie Curie Career Integration Grant, Junta de Andalucía, Spanish Ministry of Economy and Competitiveness (MINECO), Fundacao para a Ciencia e a Tecnologia (FCT), FCT-MEC (PIDDAC), FEDER (COMPETE), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

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

© 2015. The American Astronomical Society. All rights reserved. Artículo firmado por 25 autores. We thank the anonymous referee for many helpful comments that greatly improved this paper. R.B. acknowledges the support of a grant from the Research Grants Committee of the University of Alabama. K.S. acknowledges the support of the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. J.H.K. acknowledges financial support from the Spanish MINECO under grant No. AYA2013-41243-P. E.A. and A.B. acknowledge financial support to the DAGAL network from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme FP7/2007-2013/under REA grant agreement number PITN-GA-2011-289313. E.A. and A.B. also acknowledge financial support from the CNES (Centre National d'Etudes Spatiales-France). L.C.H. acknowledges support from the Kavli Foundation, Peking University, and the Chinese Academy of Science through grant No. XDB09030100 (Emergence of Cosmological Structures) from the Strategic Priority Research Program. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration., The Spitzer Survey of Stellar Structure in Galaxies (S(4)G) is the largest available database of deep, homogeneous middle-infrared (mid-IR) images of galaxies of all types. The survey, which includes 2352 nearby galaxies, reveals galaxy morphology only minimally affected by interstellar extinction. This paper presents an atlas and classifications of S(4)G galaxies in the Comprehensive de Vaucouleurs revised Hubble-Sandage (CVRHS) system. The CVRHS system follows the precepts of classical de Vaucouleurs morphology, modified to include recognition of other features such as inner, outer, and nuclear lenses, nuclear rings, bars, and disks, spheroidal galaxies, X patterns and box/peanut structures, OLR subclass outer rings and pseudorings, bar ansae and barlenses, parallel sequence latetypes, thick disks, and embedded disks in 3D early-type systems. We show that our CVRHS classifications are internally consistent, and that nearly half of the S(4)G sample consists of extreme late-type systems (mostly bulgeless, pure disk galaxies) in the range Scd-Im. The most common family classification for mid-IR types S0/a to Sc is SA while that for types Scd to Sm is SB. The bars in these two type domains are very different in mid-IR structure and morphology. This paper examines the bar, ring, and type classification fractions in the sample, and also includes several montages of images highlighting the various kinds of "stellar structures" seen in mid-IR galaxy morphology., Unión Europea. FP7, Research Grants Committee of the University of Alabama, National Radio Astronomy Observatory, Spanish MINECO, CNES (Centre National d'Etudes Spatiales-France, Kavli Foundation, Peking University, Chinese Academy of Science, National Aeronautics and Space Administration, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO, 2010. This research was supported by the Spanish Ministry of Science and Innovation (MICINN) under the grant AYA2007-65090. We thank the anonymous referee for his/her useful comments and suggestions. We are grateful to Ignacio Trujillo, Michele Bellazzini, Julianne Dalcanton, and Juan Carlos Muñoz Mateos for helpful discussions. We also thank Steve Mandel for providing us their wide field deep images of the M81 sky area., Context. The optical ring-like structure detected by Arp (1965) around M81 (commonly referenced as "Arp's loop") represents one of thethe most spectacular features observed in nearby galaxies. Arp's loop is commonly interpreted as a tail resulting from the tidal interaction between M81 and M82. However, since its discovery the nature of this feature has remained controversial. Aims. Our primary purpose was to identify the sources of optical and infrared emission observed in Arp's loop. Methods. The morphology of Arp's loop has been investigated with deep wide-field optical images. We also measured its colors using IRAS and Spitzer-MIPS infrared images and compared them with those of the disk of M81 and Galactic dust cirrus that fills the area where M81 is located. Results. Optical images reveal that this peculiar object has a filamentary structure characterized by many dust features overlapping M81's field. The ratios of far-infrared fluxes and the estimated dust-to-gas ratios indicate the infrared emission of Arp's loop is dominated by the contribution of cold dust that is most likely from Galactic cirrus. Conclusions. The above results suggest that the light observed at optical wavelengths is a combination of emission from i) a few recent star-forming regions located close to M81, where both bright UV complexes and peaks in the HI distribution are found, ii) the extended disk of M81 and iii) scattered light from the same Galactic cirrus that is responsible for the bulk of the far-infrared emission., Ministerio de Ciencia e Innovación (MICINN), España, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO, 2013. Artículo firmado por 33 autores. We would like to thank the anonymous referee for the review of our manuscript. The comments and suggestions helped to improve the content of the paper. R. A. Marino is funded by the Spanish program of International Campus of Excellence Moncloa (CEI). This study makes uses of the data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey (http://www.califa.caha.es). Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck-Institut fur Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). CALIFA is the first legacy survey being performed at Calar Alto. The CALIFA collaboration would like to thank the IAA-CSIC and MPIA-MPG, as major partners of the observatory, and CAHA itself, for the unique access to telescope time and support in manpower and infrastructures. The CALIFA collaboration also thanks the CAHA staff for their dedication to this project. We thank the Viabilidad, Diseño, Acceso y Mejora funding program, ICTS-2009-10, for supporting the initial developement of this project. S.F.S., F.F.R.O., and D. Mast thank the Plan Nacional de Investigación y Desarrollo funding programs, AYA2012-31935 of the Spanish Ministerio de Economía y Competitividad, for the support given to this project. S. F. S thanks the the Ramón y Cajal project RyC-2011-07590 of the spanish Ministerio de Economía y Competitividad, for the support giving to this project. F. F. R. O. acknowledges the Mexican National Council for Science and Technology (CONACYT) for financial support under the program Estancias Postdoctorales y Sabáticas al Extranjero para la Consolidación de Grupos de Investigación, 2010-2012. We acknowledge financial support for the ESTALLIDOS collaboration by the Spanish Ministerio de Ciencia e Innovación under grant AYA2010-21887-C04-03. BG-L also acknowledges support from the Spanish Ministerio de Economía y Competitividad (MINECO) u, The use of integral field spectroscopy is since recently allowing to measure the emission line fluxes of an increasingly large number of star-forming galaxies, both locally and at high redshift. Many studies have used these fluxes to derive the gas-phase metallicity of the galaxies by applying the so-called strong-line methods. However, the metallicity indicators that these datasets use were empirically calibrated using few direct abundance data points (T_e-based measurements). Furthermore, a precise determination of the prediction intervals of these indicators is commonly lacking in these calibrations. Such limitations might lead to systematic errors in determining the gas-phase metallicity, especially at high redshift, which might have a strong impact on our understanding of the chemical evolution of the Universe. The main goal of this study is to review the most widely used empirical oxygen calibrations, O3N2 and N2, by using new direct abundance measurements. We pay special attention to (1) the expected uncertainty of these calibrations as a function of the index value or abundance derived and (2) the presence of possible systematic offsets. This is possible thanks to the analysis of the most ambitious compilation of T_e-based H II regions to date. This new dataset compiles the Te-based abundances of 603 H II regions extracted from the literature but also includes new measurements from the CALIFA survey. Besides providing new and improved empirical calibrations for the gas abundance, we also present a comparison between our revisited calibrations with a total of 3423 additional CALIFA H II complexes with abundances derived using the ONS calibration from the literature. The combined analysis of T_e-based and ONS abundances allows us to derive their most accurate calibration to date for both the O3N2 and N2 single-ratio indicators, in terms of all statistical significance, quality, and coverage of the parameters space. In particular, we infer that these indicators, Unión Europea. FP7, Ministerio de Economía y Competitividad (MINECO), Campus de Excelencia internacional (CEI) Moncloa, Subprograma de diseño, viabilidad, acceso y mejora de Instalaciones Científicas y Técnicas Singulares (ICTS) (MINECO), Proyecto Ramón y Cajal (MINECO), Consejo Nacional de Ciencia y Tecnología (CONACYT), México, ESTALLIDOS Collaboration (MICINN), Acciones marie Curie (EU), People´s Program, DAGAL network, Programa PNAYA, Fundacao para a Ciencia e a Tecnologia (FCT), Portugal, FCT-MEC (PIDDAC), Portugal, FONDOS FEDER (COMPETE), UE, Proyecto Estancias Postdoctorales y Sabáticas al Extranjero para la Consolidación de Grupos de Investigación (CONACYT), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2013. The American Astronomical Society. All rights reserved. Artículo firmado por 26 autores. D.Z. acknowledges financial support from NASA ADAP NNX12AE27G and thanks the Max Planck Institute for Astronomy and NYU CCPP for their hospitality during long-term visits. E. A. and A. B. acknowledge the CNES (Centre National d'Etudes Spatiales-France) for financial support. We acknowledge the support from the FP7 Marie Curie Actions of the European Commission, via the Initial Training Network DAGAL under REA grant agreement PITN-GA-2011-289313. The authors thank the entire S^(4)G team for the efforts in making this program possible. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This research is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Taehyun Kim is a student at the National Radio Astronomy Observatory., We study the m = 1 distortions (lopsidedness) in the stellar components of 167 nearby galaxies that span a wide range of morphologies and luminosities. We confirm the previous findings of (1) a high incidence of lopsidedness in the stellar distributions, (2) increasing lopsidedness as a function of radius out to at least 3.5 exponential scale lengths, and (3) greater lopsidedness, over these radii, for galaxies of later type and lower surface brightness. Additionally, the magnitude of the lopsidedness (1) correlates with the character of the spiral arms (stronger arm patterns occur in galaxies with less lopsidedness), (2) is not correlated with the presence or absence of a bar, or the strength of the bar when one is present, (3) is inversely correlated to the stellar mass fraction, f_*, within one radial scale length, and (4) correlates directly with f_* measured within the radial range over which we measure lopsidedness. We interpret these findings to mean that lopsidedness is a generic feature of galaxies and does not, generally, depend on a rare event, such as a direct accretion of a satellite galaxy onto the disk of the parent galaxy. While lopsidedness may be caused by several phenomena, moderate lopsidedness (< A_1 >_i + < A_1>_o)/2 < 0.3) is likely to reflect halo asymmetries to which the disk responds or a gravitationally self-generated mode. We hypothesize that the magnitude of the stellar response depends both on how centrally concentrated the stars are with respect to the dark matter and whether there are enough stars in the region of the lopsidedness that self-gravity is dynamically important., NASA ADAP, CNES (Centre National d'Etudes Spatiales-France), FP7 Marie Curie Actions of the European Commission, via the Initial Training Network DAGAL under REA grant, National Aeronautics and Space Administration (NASA), Unión Europea (UE), Séptimo Programa Marco de Investigación y Desarrollo Tecnológico (FP7), UE, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2014 SPIE. Conference on Ground-Based and Airborne Instrumentation for Astronomy (5th. 2014. Montreal, Canada)., MEGARA is the future integral-field and multi-object spectrograph for the GTC 10.4m telescope located in the Observatorio del Roque de los Muchachos in La Palma. INAOE is a member of the MEGARA Consortium and it is in charge of the Optics Manufacturing work package. In addition to the manufacturing of 73 elements, the work package includes the opto-mechanics i.e. the opto-mechanical design, manufacture, tests and integration of the complete assembly of the main optics composed by the collimator and camera subsystems. MEGARA passed the Optics Detailed Design Review in May 2013 and will have the Detailed Design Review of the complete instrument early 2014. Here we describe the detailed design of the collimator and camera barrels. We also present the finite elements models developed to simulate the behavior of the barrel, sub-cells and other mechanical elements. These models verify that the expected stress fields and the gravitational displacements on the lenses are compatible with the optical quality tolerances. The design is finished and ready for fabrication., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2008. The American Astronomical Society. All rights reserved. We would like to thank an anonymous referee for his/ her thoughtful review of our paper. We acknowledge discussions with Patrick Morrissey related to the possibility of red leaks in the GALEX FUV and NUV bands. R. S.' s contribution to the research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. R. S. thanks NASA for financial support via a GALEX award and an LTSA award. K. F. was partially funded by a SURF scholarship and through the Cornell Presidential Research Scholars (CPRS) program. A. G. d. P. is partially financed by the Spanish Ramón y Cajal program and the Programa Nacional de Astronomía y Astrofísica under grant AYA 2006-02358. C. S. C. is partially funded for this work by the Spanish MCyT under project AYA 2006-14876 and the Spanish MEC under project PIE 200750I028., The search for binarity in AGB stars is of critical importance for our understanding of how planetary nebulae acquire the dazzling variety of aspherical shapes which characterizes this class. However, detecting binary companions in such stars has been severely hampered due to their extreme luminosities and pulsations. We have carried out a small imaging survey of AGB stars in ultraviolet light (using GALEX), where these cool objects are very faint, in order to search for hotter companions. We report the discovery of significant far-ultraviolet excesses toward nine of these stars. The far-ultraviolet excess most likely results either directly from the presence of a hot binary companion or indirectly from a hot accretion disk around the companion., Programa Ramón y Cajal, Programa Nacional de Astronomía y Astrofísica (PNAyA), España, (National Aeronautics and Space Administration (NASA), Ministerio de Ciencia y Tecnología (MCYT), España, Ministerio de Educación y Ciencia (MEC), España, Cornell Presidential Research Scholars (CPRS) program, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2011. The American Astronomical Society. All rights reserved. Artículo firmado por 19 autores. The authors thank the entire S^(4)G team for their efforts in this project. We thank our anonymous referee for giving useful advice which improved the quality of this paper. We thank Inma Martínez Valpuesta for her useful comments. We are grateful to the dedicated staff at the Spitzer Science Center for their help and support in planning and execution of this Exploration Science program. We also gratefully acknowledge support from NASA JPL/Spitzer grant RSA 1374189 provided for the S^(4)G project. K. M. D. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0802399. E. A. and A. B. thank the Centre National d'Etudes Spatiales for financial support., If thick disks are ubiquitous and a natural product of disk galaxy formation and/or evolution processes, all undisturbed galaxies that have evolved during a significant fraction of a Hubble time should have a thick disk. The late-type spiral galaxy NGC 4244 has been reported as the only nearby edge-on galaxy without a confirmed thick disk. Using data from the Spitzer Survey of Stellar Structure in Galaxies (S^(4)G) we have identified signs of two disk components in this galaxy. The asymmetries between the light profiles on both sides of the mid-plane of NGC 4244 can be explained by a combination of the galaxy not being perfectly edge-on and a certain degree of opacity of the thin disk. We argue that the subtlety of the thick disk is a consequence of either a limited secular evolution in NGC 4244, a small fraction of stellar material in the fragments which built the galaxy, or a high amount of gaseous accretion after the formation of the galaxy., NASA JPL/Spitzer, NSF, Centre National d'Etudes Spatiales, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

©Wiley & Sons. This paper is partially based on data from CAHA, the German-Spanish Astronomical Centre, Calar Alto, operated by the Max-Planck-Institute for Astronomy, Heidelberg, jointly with the Spanish National Commission for Astronomy. Also partially based on data obtained with the 2.3m Bok Telescope of the University of Arizona on Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. Also partially based on observations made with the Isaac Newton and Jacobus Kapteyn Telescopes, operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. This research has made use of the NASA/IPAC Extragalactic Database (NED) and the NASA/IPAC Infrared Science Archive which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. PGPG wishes to acknowledge the Spanish Ministry of Education and Culture for the reception of a Formación de Profesorado Universitario fellowship. AGdP acknowledges financial support from NASA through a Long Term Space Astrophysics grant to B.F. Madore. During the course of this work AAH has been supported by the National Aeronautics and Space Administration grant NAG 5-3042 through the University of Arizona and Contract 960785 through the Jet Propulsion Laboratory. AAS acknowledges generous financial support from the Royal Society. We also would like to thank George and, We present an analysis of the integrated properties of the stellar populations in the Universidad Complutense de Madrid (UCM) Survey of Halpha-selected galaxies. In this paper, the first of a series, we describe in detail the techniques developed to model star-forming galaxies using a mixture of stellar populations, and taking into account the observational uncertainties. We assume a recent burst of star formation superimposed on a more evolved population. The effects of the nebular continuum, line emission and dust attenuation are taken into account. We also test different model assumptions, including the choice of specific evolutionary synthesis model, initial mass function, star formation scenario and the treatment of dust extinction. Quantitative tests are applied to determine how well these models fit our multiwavelength observations for the UCM sample. Our observations span the optical and near-infrared, including both photometric and spectroscopic data. Our results indicate that extinction plays a key role in this kind of study, revealing that low- and high-obscured objects may require very different extinction laws and must be treated differently. We also demonstrate that the UCM Survey galaxies are best described by a short burst of star formation occurring within a quiescent galaxy, rather than by continuous star formation. A detailed discussion on the inferred parameters, such as the age, burst strength, metallicity, star formation rate, extinction and total stellar mass for individual objects, is presented in Paper II of this series., National Aeronautics and Space Administration (NASA), National Science Foundation (NSF), EE.UU., Ministerio de Educación, Cultura y Deporte (MECD), España, University of Arizona, Jet Propulsion Laboratory, EE.UU., Royal Society, RU, Plan Nacional de Astronomía y Astrofísica (MICINN), España, Ministerio de ciencia e Innovación (MICINN), España, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2005. The American Astronomical Society. All rights reserved. Artículo firmado por 27 autores. GALEX is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA’s support for construction, operation, and science analysis of the GALEX mission, developed in cooperation with the Centre National d’Etudes Spatiales of France and the Korean Ministry of Science and Technology. We are very grateful to R. Chandar for helpful discussions and to the referee for many useful suggestions., The Galaxy Evolution Explorer (GALEX) Nearby Galaxies Survey is providing deep far-UV and near-UV imaging for a representative sample of galaxies in the local universe. We present early results for M51 and M101, from GALEX UV imaging and Sloan Digital Sky Survey optical data in five bands. The multiband photometry of compact stellar complexes in M101 is compared to population synthesis models, to derive ages, reddening, reddening-corrected luminosities, and current/initial masses. The GALEX UV photometry provides a complete census of young compact complexes on a ≈160 pc scale. A galactocentric gradient of the far-UV/near-UV color indicates younger stellar populations toward the outer parts of the galaxy disks, the effect being more pronounced in M101 than in M51., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2015. Artículo firmado por 75 autores. CALIFA is the first legacy survey being performed at Calar Alto. The CALIFA collaboration would like to thank the IAA-CSIC and MPIA-MPG as major partners of the observatory, and CAHA itself, for the unique access to telescope time and support in manpower and infrastructures. The CALIFA collaboration thanks also the CAHA staff for the dedication to this project. R.G.B., R.G.D., and E.P. are supported by the Spanish Ministerio de Ciencia e Innovación under grant AYA2010-15081. S.Z. is supported by the EU Marie Curie Integration Grant "SteMaGE" Nr. PCIG12-GA-2012-326466 (Call Identifier: FP7-PEOPLE-2012 CIG). J.F.B. acknowledges support from grants AYA2010-21322-C03-02 and AIB-2010-DE-00227 from the Spanish Ministry of Economy and Competitiveness (MINECO), as well as from the FP7 Marie Curie Actions of the European Commission, via the Initial Training Network DAGAL under REA grant agreement number 289313. Support for L.G. is provided by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC12009, awarded to The Millennium Institute of Astrophysics, M.A.S.L.G. also acknowledges support by CONICYT through FONDECYT grant 3140566. A.G. acknowledges support from the FP7/2007-2013 under grant agreement n. 267251 (AstroFIt). J.M.G. acknowledges support from the Fundacao para a Ciencia e a Tecnologia (FCT) through the Fellowship SFRH/BPD/66958/2009 from FCT (Portugal) and research grant PTDC/FIS-AST/3214/2012. RAM was funded by the Spanish programme of International Campus of Excellence Moncloa (CEI). J.M.A. acknowledges support from the European Research Council Starting Grant (SEDmorph; P.I. V. Wild). I.M., J.M. and A.d.O. acknowledge the support by the projects AYA2010-15196 from the Spanish Ministerio de Ciencia e Innovación and TIC 114 and PO08-TIC-3531 from Junta de Andalucía. AMI acknowledges support from Agence Nationale de la Recherche through the STILISM project (ANR-12-BS05-0016, This paper describes the Second Public Data Release (DR2) of the Calar Alto Legacy Integral Field Area (CALIFA) survey. The data for 200 objects are made public, including the 100 galaxies of the First Public Data Release (DR1). Data were obtained with the integral-field spectrograph PMAS /PPak mounted on the 3.5 m telescope at the Calar Alto observatory. Two different spectral setups are available for each galaxy, (i) a low-resolution V500 setup covering the wavelength range 3745-7500 Å with a spectral resolution of 6.0 Å (FWHM); and (ii) a medium-resolution V1200 setup covering the wavelength range 3650-4840 Å with a spectral resolution of 2.3 Å (FWHM). The sample covers a redshift range between 0.005 and 0.03, with a wide range of properties in the color-magnitude diagram, stellar mass, ionization conditions, and morphological types. All the cubes in the data release were reduced with the latest pipeline, which includes improved spectrophotometric calibration, spatial registration, and spatial resolution. The spectrophotometric calibration is better than 6% and the median spatial resolution is 2´´ 4. In total, the second data release contains over 1.5 million spectra., Unión Europea. FP7, Ministerio de Ciencia e Innovación (MCINN), Ministerio de Economía y Competitividad (MINECO), Programa SteMaGE, Unión Europea (UE), Initial Training Network DAGAL, Millennium Science Initiative (MSI), Comisión Nacional de Investigación Científica y Tecnológica CONICYT (Chile), Fundacao para a Ciencia e a Tecnologia (FCT), Portugal, Campus de Excelencia Internacional (CEI) Moncloa, European Research Council (ERC), UE, Projcte STructuring by Inversion the Local InterStellar Medium (STILISM), Francia, Junta de Andalucía, Agence Nationale de la Recherche, Francia, Fundação para a Ciência e a Tecnologia (FCT), Portugal, Programa Operacional Potencial Humano (POPH), Portugal, FCT - FCT-MEC (PIDDAC), Fondos Feder, UE, Ministerio de Educación, Cultura y Deporte (MECD), España, Programa Ramón y Cajal, Marie Curie Career Integration Grant, European Research Council Starting Grant, Career Re-integration Grant (UE), Fondo Nacionalde Desarrollo Científico y Tecnológico (FONDECYT), Chile, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2012 SPIE. Conference on Ground-Based and Airborne Telescopes IV (2012.Amsterdam, Netherlands), MEGARA (Multi-Espectrografo en GTC de Alta Resolucion para Astronomia) is the new integral field unit (IFU) and multi-object spectrograph (MOS) instrument for the GTC. The spectrograph subsystems include the pseudo-slit, the shutter, the collimator with a focusing mechanism, pupil elements on a volume phase holographic grating (VPH) wheel and the camera joined to the cryostat through the last lens, with a CCD detector inside. In this paper we describe the full preliminary design of the cryostat which will harbor the CCD detector for the spectrograph. The selected cryogenic device is an LN2 open-cycle cryostat which has been designed by the "Astronomical Instrumentation Lab for Millimeter Wavelengths" at INAOE. A complete description of the cryostat main body and CCD head is presented as well as all the vacuum and temperature sub-systems to operate it. The CCD is surrounded by a radiation shield to improve its performance and is placed in a custom made mechanical mounting which will allow physical adjustments for alignment with the spectrograph camera. The 4k x 4k pixel CCD231 is our selection for the cryogenically cooled detector of MEGARA. The characteristics of this CCD, the internal cryostat cabling and CCD controller hardware are discussed. Finally, static structural finite element modeling and thermal analysis results are shown to validate the cryostat model., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2012 SPIE. Conference on Ground-Based and Airborne Telescopes IV (2012, Amsterdam, Netherlands). VIENTOS project is being co-funded by CDTI, FRACTAL and UCM. This work has been done also in the framework of the Moncloa Campus of International Excellence initiative (UCM-UPM), The goal of VIENTOS project is to analyze pupil innovative systems that could be used in the new generation of instruments for the large telescopes. This study tries to identify the current scientific needs, to understand why some of them have not been fulfilled yet (due to pre-conceived technical ideas or to managerial reasons) and to propose opto-mechanical solutions for these pupil elements that could produce a qualitative leap in the performance of the instruments to operate in the large telescopes. VIENTOS is currently on-going as a collaborative project between FRACTAL and the University Complutense of Madrid (UCM) and is being partially funded by a CDTI grant under the program Industry for Science. CDTI is the Development and Industrial Transfer Center from the Minister of Science and Innovation (Spain). Among the different innovative systems that we have carried out, our team has explored potential solutions for narrow band Imaging with tunable filters in the near-IR and a novel pupil system called sliced-pupil grating, a device designed for increasing the spectral resolution in astronomical spectrographs, without changing the geometry of the main optics. Nanotechnology customized filters to be applicable to astronomical systems are under study., Centro para el Desarrollo Tecnológico Industrial (CDTI), MINECO, FRACTAL, Universidad Complutense de Madrid, Ministerio de Economía y Competitividad (MINECO), España, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© UNAM - INSTITUTO DE ASTRONOMÍA. Artículo firmado por 13 autores. We acknowledge the referee for his/her comments and suggestions that helped to improve the manuscript. SFS thanks the director of CEFCA, M. Moles, for his sincere support to this project. We thanks C.J. Walcher and R. González Delgado for their valuables comments and suggestions that improved this manuscripts in many senses. SFS thanks the CONACYT-125180 and DGAPA-IA100815 projects for providing support in this study. We acknowledge support from the Spanish Ministerio de Economía y Competitividad, through projects AYA2010-15081 and AYA2010-10904E, and Junta de Andalucía FQ1580. EP acknowledges support from the IA-UNAM and from the Guillermo Haro program at INAOE. This study used data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey (http://califa.caha.es/). CALIFA is the first legacy survey performed at Calar Alto. The CALIFA collaboration would like to thank the IAA-CSIC and MPIA-MPG as major partners of the observatory, and CAHA itself, for the unique access to telescope time and support in manpower and infrastructure. The CALIFA collaboration also thanks the CAHA staff for the dedication to this project. This research is based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck-Institut fur Astronomie and the Instituto de Astrofisica de Andalucía (CSIC)., We present an improved version of FIT3D, a fitting tool for the analysis of the spectroscopic properties of the stellar populations and the ionized gas derived from moderate resolution spectra of galaxies. This tool was developed to analyze integral field spectroscopy data and it is the basis of PIPE3D, a pipeline used in the analysis of CALIFA, MaNGA, and SAMI data. We describe the philosophy and each step of the fitting procedure. We present an extensive set of simulations in order to estimate the precision and accuracy of the derived parameters for the stellar populations and the ionized gas. We report on the results of those simulations. Finally, we compare the results of the analysis using FIT3D with those provided by other widely used packages, and we find that the parameters derived by FIT3D are fully compatible with those derived using these other tools., Presentamos una versión mejorada de FIT3D, una herramienta de ajuste para el análisis de las poblaciones estelares y el gas ionizado en espectros de galaxias de resolución intermedia. La misma se desarrolló para el análisis de datos de espectroscopía de campo integral y es la base de Pipe3D, un dataducto usado en el análisis de datos de los muestreos CALIFA, MaNGA y SAMI. Describimos la filosofía y los pasos seguidos en el ajuste, presentando un conjunto amplio de simulaciones con el fin de estimar la precisión de los parámetros derivados, mostrando el resultado de dichas simulaciones. Finalmente, comparamos el resultado del análisis con FIT3D y el obtenido mediante otros paquetes de uso frecuente, encontrando que los parámetros derivados son totalmente compatibles., Ministerio de Economía y Competitividad (MINECO), Junta de Andalucía, Universidad Nacional Autónoma de México (UNAM), Instituto Nacional de Astrofísica, Óptica y Electrónica (INAOE), México, Programa Guillermo Haro (INAOE), Consejo Nacional de Ciencia y Tecnología (CONACYT), México, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2005. The American Astronomical Society. All rights reserved. Artículo firmado por 25 autores. GALEX is a NASA small explorer launched in 2003 April. We gratefully acknowledge NASA’s support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d’Etudes Spatiales of France and the Korean Ministry of Science and Technology., New Galaxy Evolution Explorer (GALEX) observations have detected significant far-UV (FUV; 1530 Å) and near-UV (NUV; 2310 Å) emission from stellar substructures within the tidal tails of four ongoing galaxy mergers. The UV-bright regions are optically faint and are coincident with H I density enhancements. FUV emission is detected at any location where the H I surface density exceeds ~2 M_☉ pc^-2, and it is often detected in the absence of visible wavelength emission. UV luminosities of the brighter regions of the tidal tails imply masses of 10^6 to ~10^9 M_☉ in young stars in the tails, and H I luminosities imply similar H I masses. UV-optical colors of the tidal tails indicate stellar populations as young as a few megayears, and in all cases ages under 400 Myr. Most of the young stars in the tails formed in single bursts, rather than resulting from continuous star formation, and they formed in situ as the tails evolved. Star formation appears to be older near the parent galaxies and younger at increasing distances from the parent galaxy. This could be because the star formation occurs progressively along the tails, or because the star formation has been inhibited near the galaxy/tail interface. The youngest stellar concentrations, usually near the ends of long tidal tails, have masses comparable to confirmed tidal dwarf galaxies and may be newly forming galaxies undergoing their first burst of star formation., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© SPIE-Int Soc Optical Engineering. Congress of the International Commission for Optics: Light for the Development of the World (22. 2011.Puebla, Mexico), MEGARA is a multi-object spectrograph project for the 10.4m Gran Telescopio Canarias with medium to high resolution: R ~ 5600 - 17000. The instrument operates in three modes that cover different sky areas and that can run simultaneously: (1) the compact mode through a large central Integral Field Unit with minimum fiber pitch, covering a field of view on sky of 12 arcsec × 14 arcsec, (2) the sparse mode with fibers covering 1 arcmin × 1arcmin in three pointings and (3) the dispersed mode with a grid of nearly 100 robotics positioners able to place 7-fiber minibundles over a large field of view of 3.5 arcmin × 3.5 arcmin. The spectrograph is composed by a pseudo-slit, where the fibers are placed simulating a long slit; a slit shutter is placed just behind the pseudo-slit, a collimator, a 162mm pupil where the volume phase holographic gratings are placed, and the camera with the detector. Here we describe the spectrograph optical rationale, the conceptual optical design and the expected system performance., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

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

© UNAM-IA. Artículo firmado por 21 autores. SFS thanks the director of CEFCA, M. Moles, for his sincere support to this project. SFS thanks the CONACYT-125180 and DGAPA-IA100815 projects for providing support for this study.; We acknowledge support from the Spanish Ministerio de Economía y Competitividad, through projects AYA2010-15081 and AYA2010-10904E, and Junta de Andalucía FQ1580. EP acknowledges support from the IA-UNAM and from the Guillermo Haro program at INAOE.; Support for LG is provided by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. LG acknowledges support by CONICYT through FONDECYT grant 3140566.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Institute de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University., We present PIPE3D, an analysis pipeline based on the FIT3D fitting tool, developed to explore the properties of the stellar populations and ionized gas of integral field spectroscopy (IFS) data. PIPE3D was created to provide coherent, simple to distribute, and comparable dataproducts, independently of the origin of the data, focused on the data of the most recent IFU surveys (e.g., CALIFA, MaNGA, and SAMI), and the last generation IFS instruments (e.g., MUSE). In this article we describe the different steps involved in the analysis of the data, illustrating them by showing the dataproducts derived for NGC 2916, observed by CALIFA and P-MaNGA. As a practical example of the pipeline we present the complete set of dataproducts derived for the 200 datacubes that comprises the V500 setup of the CALIFA Data Release 2 (DR2), making them freely available through the network. Finally, we explore the hypothesis that the properties of the stellar populations and ionized gas of galaxies at the effective radius are representative of the overall average ones, finding that this is indeed the case., Presentamos Pipe3D, un dataducto de analisis basado en el paquete de ajustes FIT3D, desarrollado para explorar las propiedades de las poblaciones estelares y el gas ionizado en datos de espectroscopía de campo integral. Pipe3D se desarrolló para obtener productos derivados de una forma coherente, fácil de distribuir y de comparar independientemente del origen de los datos, enfocado al análisis de datos de muestreos recientes de espectroscopía 3D (por ej., CALIFA, MaNGA y SAMI), y la nueva generación de estos instrumentos (por ej., MUSE). A lo largo de este articulo describimos los diferentes pasos incluidos dentro del análisis d elos datos, ilustrandolos mediante los productos derivados para NGC 2916, observada por CALIFA y P-MaNGA. Como un ejemplo práctico del uso de este dataducto se presentan los datos completos obtenidos para 200 cubos que conforman la segunda distribución de datos CALIFA para la configuración de V500, distribuyéndolos de forma libre a través de la red. Finalmente, exploramos la hipótesis según la cual las propiedades de las poblaciones estelares y el gas ionizado en las galaxias al radio efectivo son representativas del promedio a lo largo de toda la galaxia, encontrando que de hecho este es el caso., Ministerio de Economía y Competitividad (MINECO), Junta de Andalucia, Universidad Nacional Autónoma de México (UNAM), Instituto Nacional de Astrofísica, Óptica y Electrónica (INAOE), México, Ministry of Economy, Development, and Tourism's Millennium Science Initiative, Comisión Nacional de Investigación Científica y Tecnológica (CONICYT), Chile, Alfred P. Sloan Foundation, National Science Foundation (NFS), U.S. Department of Energy Office of Science, Instituto de Astronomía (IA-UNAM), México, Programa Guillermo Haro (INAOE), Consejo Nacional de Ciencia y Tecnología (CONACYT), México, Fondo Nacional de Desarrollo Científico, Tecnológico y de Innovación Tecnológica (FONDECYT), Chile, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2006. The American Astronomical Society. All rights reserved. We wish to thank Professor M. Bershady for the WIYN R-band image of NGC 7673. Research by D. C. K. and K. G. N. was partly funded by NSF grants AST 00-71198 and AST 05-07483 and HST grants GO-09126.02-A and AR- 10321.02-A. We thank the referees for their valuable comments on this Letter, and B. Holden for helpful advice on ACS PSF peculiarities., We analyze 26 luminous compact blue galaxies (LCBGs) in the Hubble Space Telescope ACS Ultra Deep Field (UDF) at z ~ 0.2-1.3, to determine whether these truly are small galaxies or, rather, bright central starbursts within existing or forming large disk galaxies. Surface brightness profiles from UDF images reach fainter than rest-frame 26.5 B mag arcsec^-2 even for compact objects at z ~ 1. Most LCBGs show a smaller, brighter component that is likely star-forming, and an extended, roughly exponential component with colors suggesting stellar ages from ≳100 Myr to a few gigayears. Scale lengths of the extended components are mostly ≲2 kpc, more than 1.5-2 times smaller than those of nearby large disk galaxies like the Milky Way. Larger, very low surface brightness disks can be excluded down to faint rest-frame surface brightnesses (≳26 B mag arcsec^-2). However, one or two of the LCBGs are large, disklike galaxies that meet LCBG selection criteria because of a bright central nucleus, possibly a forming bulge. These results indicate that ≳90% of high-z LCBGs are small galaxies that will evolve into small disk galaxies, or low-mass spheroidal or irregular galaxies in the local universe, assuming passive evolution and no significant disk growth. The data do not reveal signs of disk formation around small, H II galaxy-like LCBGs, nor do they suggest a simple inside-out growth scenario for larger LCBGs with a disklike morphology. Irregular blue emission in distant LCBGs is relatively extended, suggesting that nebular emission lines from star-forming regions sample a major fraction of an LCBG's velocity field., National Science Foundation (NSF), The Hubble Space Telescope Observing Program (HTS), NASA, National Aeronautics and Space Administration (NASA), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub