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Artículo firmado por 369 autores., Aims. Large-Sized Telescope 1 (LST-1), the prototype for the Large-Sized Telescope at the upcoming Cherenkov Telescope Array Observatory, is concluding its commissioning phase at the Observatorio del Roque de los Muchachos on the island of La Palma. The proximity of LST-1 to the two MAGIC (Major Atmospheric Gamma Imaging Cherenkov) telescopes makes it possible to carry out observations of the same gamma-ray events with both systems. Methods. We describe the joint LST-1+MAGIC analysis pipeline and used simultaneous Crab Nebula observations and Monte Carlo simulations to assess the performance of the three-telescope system. The addition of the LST-1 telescope allows for the recovery of events in which one of the MAGIC images is too dim to survive analysis quality cuts. Results. Thanks to the resulting increase in the collection area and stronger background rejection, we found a significant improvement in sensitivity, allowing for the detection of 30% weaker fluxes in the energy range between 200 GeV and 3 TeV. The spectrum of the Crab Nebula, reconstructed in the energy range between ∼60 GeV and ∼10 TeV, is in agreement with previous measurements., Spanish Ministry of Science and Innovation, Spanish Research State Agency (AEI), Centro de Excelencia Severo Ochoa program, Unidad de Excelencia María de Maeztu program, Juan de la Cierva Incorporación program, Programa Operativo FEDER 2014-2020, Consejería de Economía y Conocimiento de la Junta de Andalucía, PAIDI 2020, Universidad de Jaén, Programa Operativo de Crecimiento Inteligente FEDER 2014-2020, Consejería de Economía, Industria, Comercio y Conocimiento del Gobierno de Canarias, Generalitat de Catalunya-CERCA, European Union’s-Horizon 2020, Ramon y Cajal program, Next Generation EU, Spanish MCIN by State Secretariat for Education, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, Instituto de Física de Partículas y del Cosmos (IPARCOS), TRUE, pub

Firmado por 966 autores (MAGIC Collaboration), Neutrino emission from a flaring blazar Neutrinos interact only very weakly with matter, but giant detectors have succeeded in detecting small numbers of astrophysical neutrinos. Aside from a diffuse background, only two individual sources have been identified: the Sun and a nearby supernova in 1987. A multiteam collaboration detected a high-energy neutrino event whose arrival direction was consistent with a known blazar—a type of quasar with a relativistic jet oriented directly along our line of sight. The blazar, TXS 0506+056, was found to be undergoing a gamma-ray flare, prompting an extensive multiwavelength campaign. Motivated by this discovery, the IceCube collaboration examined lower-energy neutrinos detected over the previous several years, finding an excess emission at the location of the blazar. Thus, blazars are a source of astrophysical neutrinos., USA-U.S. National Science Foundation-Office of Polar Programs, National Science Foundation (NSF), Wisconsin Alumni Research Foundation, Center for High Throughput Computing (CHTC) at the University of Wisconsin-Madison, Open Science Grid (OSG), Extreme Science and Engineering Discovery Environment (XSEDE), United States Department of Energy (DOE), Particle astrophysics research computing center at the University of Maryland, Institute for Cyber-Enabled Research at Michigan State University, Astroparticle physics computational facility at Marquette University, Fonds de la Recherche Scientifique - FNRS, Belgium-Fund for Scientific Research (FWO), FWO Odysseus programme, Big Science programme, Belgian Federal Science Policy Office, Federal Ministry of Education & Research (BMBF), German Research Foundation (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Helmholtz Association, High Performance Computing cluster of the RWTH Aachen, Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), Knut & Alice Wallenberg Foundation, Australia-Australian Research Council, Natural Sciences and Engineering Research Council of Canada (NSERC), Calcul Quebec, Compute Ontario, Canada Foundation for Innovation CGIAR, Spanish Government, WestGrid, Compute Canada, Villum Fonden, Danmarks Grundforskningsfond, Royal Society of New Zealand Marsden Fund (NZ), Japan-Japan Society for Promotion of Science (JSPS), Institute for Global Prominent Research (IGPR) of Chiba University, National Research Foundation of Korea, Swiss National Science Foundation (SNSF), Istituto Nazionale Astrofisica (INAF), Centre National D'etudes Spatiales, United States Department of Energy (DOE), Federal Ministry of Education & Research (BMBF), Max Planck Society, Istituto Nazionale di Fisica Nucleare (INFN), Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT), Japan Society for the Promotion of Science, Unidad de Excelencia "Mara de Maeztu", Croatian Science Foundation (HrZZ) Project, University of Rijeka Project, German Research Foundation (DFG), Polish National Research Centre, Brazilian MCTIC, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ), Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio De Janeiro (FAPERJ), Agenzia Spaziale Italiana (ASI), Gordon and Betty Moore Foundation, National Science Foundation (NSF), Mt. Cuba Astronomical Foundation, Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, Chinese Academy of Sciences South America Center for Astronomy (CASSACA), National Natural Science Foundation of China (NSFC), Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT), Ministry of Economy, Development, and Tourism's Millennium Science Initiative, Robert Martin Ayers Sciences Fund, Laboratory Directed Research and Development (LDRD) program of Los Alamos National Laboratory, Consejo Nacional de Ciencia y Tecnologia (CONACyT), Laboratorio Nacional HAWC de rayos gamma, L'Oreal Group, Red HAWC, Mexico, Universidad Nacional Autonoma de Mexico, VIEP-BUAP, PIFI, PROFOCIE, Royal Society, University of Wisconsin Alumni Research Foundation, Institute of Geophysics, Planetary Physics, and Signatures at Los Alamos National Laboratory, Polish Science Centre grant, Coordinacion de la Investigacion Cientfica de la Universidad Michoacana, Federal Ministry of Education & Research (BMBF), Max Planck Society Foundation CELLEX, German Research Foundation (DFG), Helmholtz Association, Alexander von Humboldt Foundation, French Ministry of Higher Education, Research and Innovation, Centre National de la Recherche Scientifique (CNRS/IN2P3), Centre National de la Recherche Scientifique (CNRS), French Atomic Energy Commission, UK Research & Innovation (UKRI) Science & Technology Facilities Council (STFC), National Science Centre, Poland, South African Department of Science and Technology, National Research Foundation, University of Namibia, National Commission on Research, Science AMP; Technology of Namibia (NCRST), Austrian Federal Ministry of Education, Science and Research, Austrian Science Fund (FWF), Australian Research Council, Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT), Japan Society for the Promotion of Science, University of Amsterdam, European Space Agency, French Atomic Energy Commission, Centre National D'etudes Spatiales, Helmholtz Association German Aerospace Centre (DLR), INTA, National Aeronautics & Space Administration (NASA), OSTC, European Union's Horizon 2020 Programme under the AHEAD project, German INTEGRAL, Optical and Near-infrared Astronomy Inter-University Cooperation Program, National Aeronautics and Space Administration Swift Guest Investigator Program, University of Leicester by the UK Space Agency, Smithsonian Institution, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

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

©The Authors 2023. Artículo firmado por 48 autores. Funding for the WEAVE facility has been provided by UKRI STFC, the University of Oxford, NOVA, NWO, Instituto de Astrofisica de Canarias (IAC), the Isaac Newton Group partners (STFC, NWO, and Spain, led by the IAC), INAF, CNRS-INSU, the Observatoire de Paris, Region Ile-de-France, CONCYT through INAOE, Konkoly Observatory (CSFK), Max-Planck-Institut fuer Astronomie (MPIA Heidelberg), Lund University, the Leibniz Institute for Astrophysics Potsdam (AIP), the Swedish Research Council, the European Commission, and the University of Pennsylvania. The WEAVE Survey Consortium consists of the ING, its three partners, represented by UKRI STFC, NWO, and the IAC, NOVA, INAF, GEPI, INAOE, and individual WEAVE Participants. Please see the relevant footnotes for the WEAVE website (https://ingconfluence.ing.iac.es/confluence//display/WEAV/The+WEAVE+Project) and for the full list of granting agencies and grants supporting WEAVE (https://ingconfluence.ing.iac.es/confluence/display/WEAV/WEAVE+Acknowledgements). This work makes use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular, the institutions participating in the Gaia Multilateral Agreement. This work makes use of data from the VIMOS VLT Deep Survey, the VIPERS-MLS database and the HST-COSMOS database, operated by CeSAM/Laboratoire d'Astrophysique de Marseille, France. This work makes use of observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This wo, The upcoming new generation of optical spectrographs on four-meter-class telescopes will provide valuable opportunities for forthcoming galaxy surveys through their huge multiplexing capabilities, excellent spectral resolution, and unprecedented wavelength coverage.Aims. WEAVE is a new wide-field spectroscopic facility mounted on the 4.2 m William Herschel Telescope in La Palma. WEAVE-StePS is one of the five extragalactic surveys that will use WEAVE during its first five years of operations. It will observe galaxies using WEAVE MOS (similar to 950 fibres distributed across a field of view of similar to 3 square degrees on the sky) in low-resolution mode (R similar to 5000, spanning the wavelength range 3660 - 9590 angstrom).Methods. WEAVE-StePS will obtain high-quality spectra (S/N similar to 10 angstrom(-1) at R similar to 5000) for a magnitude-limited (I-AB=20.5) sample of similar to 25000 galaxies, the majority selected at z >= 0.3. The survey goal is to provide precise spectral measurements in the crucial interval that bridges the gap between LEGA-C and SDSS data. The wide area coverage of similar to 25 square degrees will enable us to observe galaxies in a variety of environments. The ancillary data available in each of the observed fields (including X-ray coverage, multi-narrow-band photometry and spectroscopic redshift information) will provide an environmental characterisation for each observed galaxy.Results. This paper presents the science case of WEAVE-StePS, the fields to be observed, the parent catalogues used to define the target sample, and the observing strategy that was chosen after a forecast of the expected performance of the instrument for our typical targets.Conclusions. WEAVE-StePS will go back further in cosmic time than SDSS, extending its reach to encompass more than similar to 6 Gyr. This is nearly half of the age of the Universe. The spectral and redshift range covered by WEAVE-StePS will open a new observational window by continuously tr, UK Research & Innovation (UKRI), Science & Technology Facilities Council (STFC), University of Oxford, NOVA, Netherlands Organization for Scientific Research (NWO), Instituto de Astrofisica de Canarias (IAC), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 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

© ESO 2016. Artículo firmado por 22 autores. This study makes uses of the data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey (http://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 at 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. E.P.M., J.M.V., C.K., S.P., and J.I.P. acknowledge support from the Spanish MICINN through grants AYA2010-21887-C04-01 and AYA2013-47742-C4-1-P and the Junta de Andalucía for grant EXC/2011 FQM-7058. R.G.B., R.G.D., and E.P. acknowledge support from grants AYA2014-57490-P and JA-FQM-2828. Support for L.G. 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. L.G. acknowledges support by CONICYT through FONDECYT grant 3140566. This research made use of python (http://www.python.org), of Matplotlib (Hunter 2007), a suite of open-source python modules that provides a framework for creating scientific plots. We also thank Dr. Christophe Morisset for many discussions and constructive comments that have helped to improve the original manuscript., Context. The study of the integrated properties of star-forming galaxies is central to understand their formation and evolution. Some of these properties are extensive and therefore their analysis require totally covering and spatially resolved observations. Among these properties, metallicity can be defined in spiral discs by means of integral field spectroscopy (IFS) of individual H II regions. The simultaneous analysis of the abundances of primary elements, as oxygen, and secondary, as nitrogen, also provides clues about the star formation history and the processes that shape the build-up of spiral discs. Aims. Our main aim is to analyse simultaneously O/H and N/O abundance ratios in H II regions in different radial positions of the discs in a large sample of spiral galaxies to obtain the slopes and the characteristic abundance ratios that can be related to their integrated properties. Methods. We analysed the optical spectra of individual selected H II regions extracted from a sample of 350 spiral galaxies of the CALIFA survey. We calculated total O/H abundances and, for the first time, N/O ratios using the semi-empirical routine H II-C HI-MISTRY, which, according to Perez-Montero (2014, MNRAS, 441, 2663), is consistent with the direct method and reduces the uncertainty in the O/H derivation using [N II] lines owing to the dispersion in the O/H-N/O relation. Then we performed linear fittings to the abundances as a function of the de-projected galactocentric distances. Results. The analysis of the radial distribution both for O/H and N/O in the non-interacting galaxies reveals that both average slopes are negative, but a non-negligible fraction of objects have a flat or even a positive gradient (at least 10% for O/H and 4% for N/O). The slopes normalised to the effective radius appear to have a slight dependence on the total stellar mass and the morphological type, as late low-mass objects tend to have flatter slopes. No clear relation is found, however, to expla, Ministerio de Ciencia e Innovación (MICINN), Junta de Andalucía, Millennium Science Initiative (MSI) - Ministerio de Economía, Fomento y Turismo (Chile), Comisión Nacional de Investigación Científica y Tecnológica (CONICYT), Chile), Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT), Chile, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Artículo firmado por 38 autores. ©Elsevier Science BV. The authors wish to thank Bill Pence and Rob Seaman for many insightful discussions. We thank Bob Hanisch and Michael Wise for providing helpful comments that improved the contents of this paper. This research has made use of NASA’s Astrophysics Data System., The Flexible Image Transport System (FITS) standard has been a great boon to astronomy, allowing observatories, scientists and the public to exchange astronomical information easily. The FITS standard, however, is showing its age. Developed in the late 1970s, the FITS authors made a number of implementation choices that, while common at the time, are now seen to limit its utility with modern data. The authors of the FITS standard could not anticipate the challenges which we are facing today in astronomical computing. Difficulties we now face include, but are not limited to, addressing the need to handle an expanded range of specialized data product types (data models), being more conducive to the networked exchange and storage of data, handling very large datasets, and capturing significantly more complex metadata and data relationships. There are members of the community today who find some or all of these limitations unworkable, and have decided to move ahead with storing data in other formats. If this fragmentation continues, we risk abandoning the advantages of broad interoperability, and ready archivability, that the FITS format provides for astronomy. In this paper we detail some selected important problems which exist within the FITS standard today. These problems may provide insight into deeper underlying issues which reside in the format and we provide a discussion of some lessons learned. It is not our intention here to prescribe specific remedies to these issues; rather, it is to call attention of the FITS and greater astronomical computing communities to these problems in the hope that it will spur action to address them. (C) 2015 Elsevier B.V. All rights reserved., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2015. Artículo firmado por 18 autores. The authors thank the referee for the useful comments and suggestions. This study made use of the data provided by the Calar Alto Legacy Field Area (CALIFA) survey (http://www.califa.caha.es). It was 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 performed at the 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 the telescope time and support in manpower and infrastructures. The CALIFA collaboration also thanks the CAHA staff for their dedication to this project. J.B.-B. and B.G-L acknowledge support from the Plan Nacional de I+D+i (PNAYA) funding programs (AYA-2012-39408-C02-1 and AYA-2013-41656-P) of the Spanish Ministry of Economy and Competitiveness (MINECO). J.F.B. acknowledges support from the Plan Nacional de I+D+i (PNAYA) funding programs from MINECO (AYA2013-48226-03-1-P, RAVET). J.I.P. acknowledges financial support from the Spanish MINECO through grant AYA2010-21887-C04-01 and from the Junta de Andalucía Excellence Project PEX2011-FQM7058. R.A.M. is funded by the Spanish program of International Campus of Excellence Moncloa (CEI). Support for L.G. 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. L.G. acknowledges support by CONICYT through FONDECYT grant 3140566. C.J.W. acknowledges support through the Marie Curie Career Integration Grant 303912., We use optical integral-field spectroscopic (IFS) data from 103 nearby galaxies at different stages of the merging event, from close pairs to merger remnants provided by the CALIFA survey, to study the impact of the interaction in the specific star formation and oxygen abundance on different galactic scales. To disentangle the effect of the interaction and merger from internal processes, we compared our results with a control sample of 80 non-interacting galaxies. We confirm the moderate enhancement (x 2-3 times) of specific star formation for interacting galaxies in central regions as reported by previous studies; however, the specific star formation is comparable when observed in extended regions. We find that control and interacting star-forming galaxies have similar oxygen abundances in their central regions, when normalized to their stellar masses. Oxygen abundances of these interacting galaxies seem to decrease compared to the control objects at the large aperture sizes measured in effective radius. Although the enhancement in central star formation and lower metallicities for interacting galaxies have been attributed to tidally induced inflows, our results suggest that other processes such as stellar feedback can contribute to the metal enrichment in interacting galaxies., Unión Europea. FP7, Ministerio de Economía y Competitividad (MINECO), España, Instituto Milenio de Astrofísica (Millennium Institute of Astrophysics, MAS), Chile, Junta de Andalucia, Campus de Excelencia Internacional Moncloa (CEI), Ministry of Economy, Development, and Tourism's Millennium Science Initiative, Millennium Science Initiative (SIG), Comisión Nacional de Investigación Científica y Tecnológica (CONICYT), Chile, Fondo Nacional de Desarrollo Científico y Tecnológico (CONDECYT), Chile, Marie Skłodowska-Curie actions (UE), Marie Curie Career Integration Grants (CIG), UE, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

We thank Dan Duriscoe for discussion of the the maximum naturally occuring night sky brightness, Liz Perkin for hosting the SQM at the Hackescher Markt site, Tine Weinzierl for hosting the SQM at the Seebergen site, and Veneto Stellato for sharing their data. This work was partially supported by MILIEU (FU Berlin), the Federal Ministry of Education and Research, Germany (PT-Julich under grant BMBF-033L038A), EU COST Action ES1204 (Loss of the Night Network), the European Research Council (ERC) under the EU's Seventh Framework Program (FP7/2007-2013)/ERC grant agreement No 268504 to K.J.G., Spanish grant AYA2012-31277, AYA-2012-30717 and the Spanish Network for Light Pollution Studies (AYA2011-15808-E). Data collected at Winer Observatory funded in part by the National Aeronautics and Space Administration (Goddard Space Flight Center), the Ohio State University, University of Iowa, and The Adam Mickiewicz University., Despite constituting a widespread and significant environmental change, understanding of artificial nighttime skyglow is extremely limited. Until now, published monitoring studies have been local or regional in scope, and typically of short duration. In this first major international compilation of monitoring data we answer several key questions about skyglow properties. Skyglow is observed to vary over four orders of magnitude, a range hundreds of times larger than was the case before artificial light. Nearly all of the study sites were polluted by artificial light. A non-linear relationship is observed between the sky brightness on clear and overcast nights, with a change in behavior near the rural to urban landuse transition. Overcast skies ranged from a third darker to almost 18 times brighter than clear. Clear sky radiances estimated by the World Atlas of Artificial Night Sky Brightness were found to be overestimated by similar to 25%; our dataset will play an important role in the calibration and ground truthing of future skyglow models. Most of the brightly lit sites darkened as the night progressed, typically by similar to 5% per hour. The great variation in skyglow radiance observed from site-to-site and with changing meteorological conditions underlines the need for a long-term international monitoring program., Unión Europea. FP7, MILIEU (FU Berlin), Federal Ministry of Education and Research, Germany, EU COST Action (Loss of the Night Network), Spanish Network for Light Pollution Studies, National Aeronautics and Space Administration (Goddard Space Flight Center), Ohio State University, University of Iowa, Adam Mickiewicz University, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© Author(s) 2015. Artículo firmado por 24 autores. This work is distributed under the Creative Commons Attribution 3.0 License. This study is based on discussions held during the joint workshop of the PAGES 2k network and PAST2k-PMIP Integrated analyses of reconstructions and multimodel simulations for the past two millennia, Madrid, Spain, 4-6 November 2013. PAGES and FECYT (FCT-13-6276) are greatly thanked for supporting this workshop. We acknowledge the World Climate Research Programme's Working Group on Coupled Modelling, which is responsible for CMIP. The US Department of Energy's Program for Climate Model Diagnosis and Intercomparison provides coordinating support for CMIP and led the development of software infrastructure in partnership with the Global Organization for Earth System Science Portals. H. Goosse is Research Director with the Fonds National de la Recherche Scientifique (F.R.S.-FNRS, Belgium). This work is supported by the F.R.S.-FNRS and by the Belgian Federal Science Policy Office (Research Programme on Science for a Sustainable Development). C. C. Raible and F. Lehner are supported by the Swiss National Science foundation. P. Yiou is supported by the MILEX project of the Swedish Research Council. J. Gergis is funded by Australian Research Council project DE130100668. O. Bothe was supported by LOCHMES (Leibniz Society), PRIME-II (within DFG INTERDYNAMIK), and CliSAP. L. Fernández Donado was funded by a FPU grant: AP2009-4061. A. Moberg and A. Hind are supported by the Swedish Research Council grants B0334901 and C0592401. G. Hegerl and A. Schurer are supported by the ERC advanced grant TITAN (320691). L. Fernández Donado, E. García Bustamente, and J. F. González Rouco were supported by grants CGL2011-29677-CO2-02 and CGL2014-59644-R. Gabi Hegerl was also supported by a Royal Society Wolfson Research Merit Award and by NCAS. This is LDEO contribution number 7956. N. McKay was funded through the US National Science Foundation (ARC-1107869)., Estimated external radiative forcings, model results, and proxy-based climate reconstructions have been used over the past several decades to improve our understanding of the mechanisms underlying observed climate variability and change over the past millennium. Here, the recent set of temperature reconstructions at the continental-scale generated by the PAGES 2k project and a collection of state-of-the-art model simulations driven by realistic external forcings are jointly analysed. The first aim is to estimate the consistency between model results and reconstructions for each continental-scale region over the time and frequency domains. Secondly, the links between regions are investigated to determine whether reconstructed global-scale covariability patterns are similar to those identified in model simulations. The third aim is to assess the role of external forcings in the observed temperature variations. From a large set of analyses, we conclude that models are in relatively good agreement with temperature reconstructions for Northern Hemisphere regions, particularly in the Arctic. This is likely due to the relatively large amplitude of the externally forced response across northern and high-latitude regions, which results in a clearly detectable signature in both reconstructions and simulations. Conversely, models disagree strongly with the reconstructions in the Southern Hemisphere. Furthermore, the simulations are more regionally coherent than the reconstructions, perhaps due to an underestimation of the magnitude of internal variability in models or to an overestimation of the response to the external forcing in the Southern Hemisphere. Part of the disagreement might also reflect large uncertainties in the reconstructions, specifically in some Southern Hemisphere regions, which are based on fewer palaeoclimate records than in the Northern Hemisphere., Unión Europea. FP7, Fonds de la Recherche Scientifique (F.R.S.-FNRS), Francia, Belgian Federal Science Policy Office (Research Programme on Science for a Sustainable Development), Swiss National Science foundation, MILEX project of the Swedish Research Council, Australian Research Council, LOCHMES (Leibniz Society), Precipitation in the past millennium in Europe (PRIME-II), Cluster of Excellence Integrated Climate System Analysis and Prediction (CliSAP), Formación del Profesorado Universitario (FPU) MECD, España, Swedish Research Council, Royal Society of London for Improving Natural Knowledge, National Centre for Atmospheric Science (NCAS), Reino Unido, US National Science Foundation, Integrated Analysis of Interglacial Climate Dynamics (INTERDYNAMIC), Deutsche Forschungsgemeinschaft (DFG), Alemania, Ministerio de Educación, Cultura y Deporte (MECD), España, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© EDP Sciences, Springer-Verlag 2012. Artículo firmado por 26 autores. We wish to thank several past members of the Janus Collaboration, F. Belletti, M. Cotallo, D. Sciretti and J.L. Velasco, for their important contributions to the project. Over the years, the Janus project has been supported by the EU (FEDER funds, No. UNZA05-33-003, MEC-DGA, Spain), by the MICINN (Spain) (contracts FIS2006- 08533, FIS2009-12648, FIS2007-60977, FIS2010-16587, FPA2004-02602, TEC2010- 19207), by CAM(Spain), by the Junta de Extremadura (GR10158), by UCM-Banco Santander (GR32/10-A/910383), by the Universidad de Extremadura (ACCVII-08) and by the Microsoft Prize 2007. We thank ETHlab for their technical help. E.M. was supported by the DREAM SEED project and by the Computational Platform of IIT (Italy). M.B.-J. and B.S. were supported by the FPU program (Ministerio de Educación, Spain); R.A.B. and J.M.-G. were supported by the FPI program (Diputación de Aragón, Spain); finally J.M.G.-N. was supported by the FPI program (Ministerio de Ciencia e Innovación, Spain)., We describe Janus, a massively parallel FPGA-based computer optimized for the simulation of spin glasses, theoretical models for the behavior of glassy materials. FPGAs (as compared to GPUs or many-core processors) provide a complementary approach to massively parallel computing. In particular, our model problem is formulated in terms of binary variables, and floating-point operations can be (almost) completely avoided. The FPGA architecture allows us to run many independent threads with almost no latencies in memory access, thus updating up to 1024 spins per cycle. We describe Janus in detail and we summarize the physics results obtained in four years of operation of this machine; we discuss two types of physics applications: long simulations on very large systems (which try to mimic and provide understanding about the experimental non equilibrium dynamics), and low-temperature equilibrium simulations using an artificial parallel tempering dynamics. The time scale of our non-equilibrium simulations spans eleven orders of magnitude (from picoseconds to a tenth of a second). On the other hand, our equilibrium simulations are unprecedented both because of the low temperatures reached and for the large systems that we have brought to equilibrium. A finite-time scaling ansatz emerges from the detailed comparison of the two sets of simulations. Janus has made it possible to perform spin glass simulations that would take several decades on more conventional architectures. The paper ends with an assessment of the potential of possible future versions of the Janus architecture, based on state-of-the-art technology., EU (FEDER funds), Ministerio de Economía y Competitividad (MINECO), Ministerio de Ciencia e Innovación (MICINN), Comunidad de Madrid, Junta de Extremadura (Spain), UCM-Banco Santander (Spain), Universidad de Extremadura (Spain), Microsoft Prize 2007, Computational Platform of IIT (Italy), FPU program (Ministerio de Educación, Spain), FPI program (Diputación de Aragón, Spain), FPI program (Ministerio de Ciencia e Innovación, Spain), Depto. de Física Teórica, 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

© 2015 Elsevier B.V. Artículo firmado por 167 autores. We would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO, and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Centro de Excelencia Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. We thank the two anonymous referees for thorough reading and helpful comments on the manuscript., The MAGIC telescopes are two Imaging Atmospheric Cherenkov Telescopes (IACTs) located on the Canary island of La Palma. The telescopes are designed to measure Cherenkov light from air showers initiated by gamma rays in the energy regime from around 50 GeV to more than 50 TeV. The two telescopes were built in 2004 and 2009, respectively, with different cameras, triggers and readout systems. In the years 2011-2012 the MAGIC collaboration undertook a major upgrade to make the stereoscopic system uniform, improving its overall performance and easing its maintenance. In particular, the camera, the receivers and the trigger of the first telescope were replaced and the readout of the two telescopes was upgraded. This paper (Part I) describes the details of the upgrade as well as the basic performance parameters of MAGIC such as raw data treatment, linearity in the electronic chain and sources of noise. In Part II, we describe the physics performance of the upgraded system., German BMBF and MPG, Italian INFN and INAF, Swiss National Fund SNF, ERDF under the Spanish MINECO, Japanese JSPS, MEXT, Centro de Excelencia Severo Ochoa, Spanish Consolider-Ingenio 2010 programme, Academy of Finland, Croatian Science Foundation (HrZZ), University of Rijeka, the DFG Collaborative Research Centers, Polish MNiSzW, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

© 2005 by the American Geophysical Union. Artículo firmado por 18 autores. We are grateful to Cathy Johnson, Bill Hurlin and Mike Spelman for comments on the manuscript, to Frank Koesters for discussion, to Jianjun Yin for his help in preparing the paper, to Oleg Saenko and an anonymous referee for their reviews, and to our respective funding agencies for support., As part of the Coupled Model Intercomparison Project, integrations with a common design have been undertaken with eleven different climate models to compare the response of the Atlantic thermohaline circulation ( THC) to time-dependent climate change caused by increasing atmospheric CO2 concentration. Over 140 years, during which the CO2 concentration quadruples, the circulation strength declines gradually in all models, by between 10 and 50%. No model shows a rapid or complete collapse, despite the fairly rapid increase and high final concentration of CO2. The models having the strongest overturning in the control climate tend to show the largest THC reductions. In all models, the THC weakening is caused more by changes in surface heat flux than by changes in surface water flux. No model shows a cooling anywhere, because the greenhouse warming is dominant., Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2016 IOP Publishing Ltd. Artículo firmado por 45 autores. Support for PAGES 2k activities is provided by the US and Swiss National Science Foundations, US National Oceanographic and Atmospheric Administration and by the International Geosphere-Biosphere Programme. JPW acknowledges support from the Centre of Climate Dynamics (SKD), Bergen. The work of OB, SW and EZ is part of CLISAP. JL, SW, EZ, JPW, JGN, OB also acknowledge support by the German Science Foundation Project 'Precipitation in the past millennia in Europe-Extension back to Roman times'. MB acknowledges the Catalan Meteorological Survey (SMC), National Programme I + D, Project CGL2011-28255. PD and RB acknowledge support from the Czech Science Foundation project no. GA13-04291S. VK was supported by Russian Science Foundation (grant 14-19-00765) and the Russian Foundation for Humanities (grants 15-07-00012, 15-37-11129). GH and AS are supported by the ERC funded project TITAN (EC-320691). GH was further funded by the Wolfson Foundation and the Royal Society as a Royal Society Wolfson Research Merit Award (WM130060) holder. NY is funded by the LOEWE excellence cluster FACE2-FACE of the Hessen State Ministry of Higher Education, Research and the Arts; HZ acknowledge support from the DFG project AFICHE. Lamont contribution #7961. The reconstructions can be downloaded from the NOAA paleoclimate homepage: www.ncdc.noaa.gov/paleo/study/19600. LFD, EGB and JFGR were supported by grants CGL2011-29677-c02-02 and CGL2014-599644-R. All authors are part of the Euro-Med 2k Consortium., The spatial context is criticalwhen assessing present-day climate anomalies, attributing them to potential forcings and making statements regarding their frequency and severity in a long-term perspective. Recent international initiatives have expanded the number of high-quality proxy-records and developed new statistical reconstruction methods. These advances allow more rigorous regional past temperature reconstructions and, in turn, the possibility of evaluating climate models on policy-relevant, spatiotemporal scales. Here we provide a new proxy-based, annually-resolved, spatial reconstruction of the European summer (June-August) temperature fields back to 755 CE based on Bayesian hierarchical modelling (BHM), together with estimates of the European mean temperature variation since 138 BCE based on BHM and composite-plus-scaling (CPS). Our reconstructions compare well with independent instrumental and proxy-based temperature estimates, but suggest a larger amplitude in summer temperature variability than previously reported. Both CPS and BHM reconstructions indicate that the mean 20th century European summer temperature was not significantly different from some earlier centuries, including the 1st, 2nd, 8th and 10th centuries CE. The 1st century (in BHM also the 10th century) may even have been slightly warmer than the 20th century, but the difference is not statistically significant. Comparing each 50 yr period with the 1951-2000 period reveals a similar pattern. Recent summers, however, have been unusually warm in the context of the last two millennia and there are no 30 yr periods in either reconstruction that exceed the mean average European summer temperature of the last 3 decades (1986-2015 CE). A comparison with an ensemble of climate model simulations suggests that the reconstructed European summer temperature variability over the period 850-2000 CE reflects changes in both internal variability and external forcing on multi-decadal time-scales. For pan-Eur, Unión Europea. FP7, Deutsche Forschungsgemeinschaf = German Science Foundation(DFG), Alemania, Servei de Meteorologia de Catalunya (SMC), Russian Science Foundation, Czech Science Foundation, Russian Foundation for Humanities, Wolfson Foundation, Royal Society, LOEWE excellence cluster FACE2-FACE, Ministerio de Economía y Competitividad (MINECO), España, Centre of Climate Dynamics (SKD), Bergen, National Science Foundation (NSF), EE.UU., Swiss National Science Foundation (SNSF) - SNF, Suiza, US National Oceanographic and Atmospheric Administration, International Geosphere-Biosphere Programme (IGBP), Cluster of Excellence Integrated Climate System Analysis and Prediction (CliSAP), Universidad de Hamburgo, Comisión Interministerial de Ciencia y Tecnología (CICYT), Hessen State Ministry of Higher Education, Research and the Arts, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Artículo firmado por 355 autores. We would like to thank all the National Space Agencies who supported the EChO phase-A study. We also thank Nick Cowan for useful comments., The discovery of almost two thousand exoplanets has revealed an unexpectedly diverse planet population. We see gas giants in few-day orbits, whole multi-planet systems within the orbit of Mercury, and new populations of planets with masses between that of the Earth and Neptune—all unknown in the Solar System. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? How do planetary systems work and what causes the exceptional diversity observed as compared to the Solar System? The EChO (Exoplanet Characterisation Observatory) space mission was conceived to take up the challenge to explain this diversity in terms of formation, evolution, internal structure and planet and atmospheric composition. This requires in-depth spectroscopic knowledge of the atmospheres of a large and well-defined planet sample for which precise physical, chemical and dynamical information can be obtained. In order to fulfil this ambitious scientific program, EChO was designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large, diverse and well-defined planet sample within its 4-year mission lifetime. The transit and eclipse spectroscopy method, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allows us to measure atmospheric signals from the planet at levels of at least 10^-4 relative to the star. This can only be achieved in conjunction with a carefully designed stable payload and satellite platform. It is also necessary to provide broad instantaneous wavelength coverage to detect as many molecular species as possible, to probe the thermal structure of the planetary atmospheres and to correct for the contaminating effects of the stellar photosphere. This requires wavelength cover, European Space Agency (ESA), Exoplanet Characterisation Observatory (EChO), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© Springer International Publishing AG. Artículo firmado por 135 autores. We thank Florence Henry, Silvain Cnudde, CNES/PASO, Astrium GmbH Germany, AIM Infrarot-Module GmbH and Astrium UK for their support in preparing this paper., A dedicated mission to investigate exoplanetary atmospheres represents a major milestone in our quest to understand our place in the universe by placing our Solar System in context and by addressing the suitability of planets for the presence of life. EChO—the Exoplanet Characterisation Observatory—is a mission concept specifically geared for this purpose. EChO will provide simultaneous, multi-wavelength spectroscopic observations on a stable platform that will allow very long exposures. The use of passive cooling, few moving parts and well established technology gives a low-risk and potentially long-lived mission. EChO will build on observations by Hubble, Spitzer and ground-based telescopes, which discovered the first molecules and atoms in exoplanetary atmospheres. However, EChO’s configuration and specifications are designed to study a number of systems in a consistent manner that will eliminate the ambiguities affecting prior observations. EChO will simultaneously observe a broad enough spectral region—from the visible to the mid-infrared—to constrain from one single spectrum the temperature structure of the atmosphere, the abundances of the major carbon and oxygen bearing species, the expected photochemically-produced species and magnetospheric signatures. The spectral range and resolution are tailored to separate bands belonging to up to 30 molecules and retrieve the composition and temperature structure of planetary atmospheres. The target list for EChO includes planets ranging from Jupiter-sized with equilibrium temperatures T_ eq up to 2,000 K, to those of a few Earth masses, with T _eq \u223c 300 K. The list will include planets with no Solar System analog, such as the recently discovered planets GJ1214b, whose density lies between that of terrestrial and gaseous planets, or the rocky-iron planet 55 Cnc e, with day-side temperature close to 3,000 K. As the number of detected exoplanets is growing rapidly each year, and the mass and radius of those detecte, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© Wiley-Blackwell. All rights reserved. Artículo firmado por 24 autores. We acknowledge the WCRP/CLIVAR Working Group on Seasonal to Interannual Prediction (WGSIP) for establishing the Climate-system Historical Forecast Project (CHFP: Kirtman and Pirani, 2009) and the Centro de Investigaciones del Mar y la Atmósfera (CIMA) for providing the model output. We also thank the data providers for making the model output available through CHFP. We have no potential sources of conflict of interest. The contribution of AYK is funded by the Academy of Finland, project no. 286298., Using an international, multi-model suite of historical forecasts from the World Climate Research Programme (WCRP) Climate-system Historical Forecast Project (CHFP), we compare the seasonal prediction skill in boreal wintertime between models that resolve the stratosphere and its dynamics (high-top') and models that do not (low-top'). We evaluate hindcasts that are initialized in November, and examine the model biases in the stratosphere and how they relate to boreal wintertime (December-March) seasonal forecast skill. We are unable to detect more skill in the high-top ensemble-mean than the low-top ensemble-mean in forecasting the wintertime North Atlantic Oscillation, but model performance varies widely. Increasing the ensemble size clearly increases the skill for a given model. We then examine two major processes involving stratosphere-troposphere interactions (the El Niño/Southern Oscillation (ENSO) and the Quasi-Biennial Oscillation (QBO)) and how they relate to predictive skill on intraseasonal to seasonal time-scales, particularly over the North Atlantic and Eurasia regions. High-top models tend to have a more realistic stratospheric response to El Niño and the QBO compared to low-top models. Enhanced conditional wintertime skill over high latitudes and the North Atlantic region during winters with El Niño conditions suggests a possible role for a stratospheric pathway., Academy of Finland, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© ESO, 2013. Artículo firmado por 21 autores. The authors would like to thank all of the CALIFA collaboration for their input, Brent Groves for very useful discussions on ionisation properties, and Remco van den Bosch for his technical and scientific advises. R. S. acknowledges support by the IMPRS for Astronomy & Cosmic Physics at the University of Heidelberg. K. J. is supported by the Emmy NoetherProgramme of the German Science Foundation DFG under grant Ja 1114/3-2 and the German Space Agency DLR. G. v. d. V. and J. F.-B. acknowledge 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. J. F.-B. further acknowledges financial support from the Ramón y Cajal Program and grant AYA2010-21322-C03-02 from the Spanish Ministry of Economy and Competitiveness (MINECO). V. W. acknowledges support from the ERC Starting Grant SEDmorph. R. A. Marino was also funded by the spanish programme 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://califa.caha.es/) and 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 Astrofísica de Andalucía (CSIC)., Context. Galaxies, which often contain ionised gas, sometimes also exhibit a so-called low-ionisation nuclear emission line region (LINER). For 30 years, this was attributed to a central mass-accreting supermassive black hole (more commonly known as active galactic nucleus, AGN) of low luminosity, making LINER galaxies the largest AGN sub-population, which dominate in numbers over higher luminosity Seyfert galaxies and quasars. This, however, poses a serious problem. While the inferred energy balance is plausible, many LINERs clearly do not contain any other independent signatures of an AGN. Aims. Using integral field spectroscopic data from the CALIFA survey, we compare the observed radial surface brightness profiles with what is expected from illumination by an AGN. Methods. Essential for this analysis is a proper extraction of emission lines, especially weak lines, such as Balmer H beta lines, which are superposed on an absorption trough. To accomplish this, we use the GANDALF code, which simultaneously fits the underlying stellar continuum and emission lines. Results. For 48 galaxies with LINER-like emission, we show that the radial emission-line surface brightness profiles are inconsistent with ionisation by a central point-source and hence cannot be due to an AGN alone. Conclusions. The most probable explanation for the excess LINER-like emission is ionisation by evolved stars during the short but very hot and energetic phase known as post-AGB. This leads us to an entirely new interpretation. Post-AGB stars are ubiquitous and their ionising effect should be potentially observable in every galaxy with the gas present and with stars older than ~1 Gyr unless a stronger radiation field from young hot stars or an AGN outshines them. This means that galaxies with LINER-like emission are not a class defined by a property but rather by the absence of a property. It also explains why LINER emission is observed mostly in massive galaxies with old stars and little star f, Unión Europea. FP7, Ministerio de Economía y Competitividad (MINECO), Emmy NoetherProgramme of the German Science Foundation DFG, German Space Agency, Programa Ramón y Cajal, European Research Council (ERC), Campus de Excelencia Internacional (CEI) Moncloa, Acciones Marie Curie (UE), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2011 American Physical Society. Artículo firmado por 23 autores. Janus has been funded by European Union (Fondo Europeo de Desarrollo Regional) funds, by Diputación General de Aragón (Spain), by a Microsoft Award-Sapienza-Italy, and by Eurotech. We acknowledge partial financial support from Ministerio de Ciencia e Innovación, Spain (Contracts No. FIS2009-12648-C03, No. FIS2010-16587, and No. TEC2010- 19207), Junta de Extremadura (GR10158), UEx (ACCVII-08), and from UCM-Banco de Santander (GR32/10-A/910383). D. Íñiguez is supported by the Government of Aragon through a Fundación ARAID contract. B. Seoane and D. Yllanes are supported by the Formación del Profesorado Universitario program (Ministerio de Educación, Spain)., We study the sample-to-sample fluctuations of the overlap probability densities from large-scale equilibrium simulations of the three-dimensional Edwards-Anderson spin glass below the critical temperature. Ultrametricity, stochastic stability, and overlap equivalence impose constraints on the moments of the overlap probability densities that can be tested against numerical data. We found small deviations from the Ghirlanda Guerra predictions, which get smaller as system size increases. We also focus on the shape of the overlap distribution, comparing the numerical data to a mean-field-like prediction in which finite-size effects are taken into account by substituting delta functions with broad peaks., Ministerio de Ciencia e Innovación (MICINN), Junta de Extremadura, Spain, UEx, UCM-Banco de Santander, Government of Aragon through a Fundación ARAID, Formación del Profesorado Universitario program (Ministerio de Educación, Spain), Depto. de Física Teórica, Fac. de Ciencias Físicas, TRUE, pub

© 2013 Elsevier B.V. Artículo firmado por 24 autores. We warmly acknowledge the excellent work done by the Janus II team at Link Engineering. In particular we thank Pietro Lazzeri, Pamela Pedrini, Roberto Preatoni, Luigi Trombetta and Alessandro Zambardi for their professional and enthusiastic work. The Janus II project was supported by the European Regional Development Fund (ERDF/2007-2013, FEDER project UNZA08-4E-020); by the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013, ERC grant agreement no. 247328); by the MICINN (Spain) (contracts FIS2012-35719-C02, FIS2010-16587); by Junta de Extremadura (contract GR101583); by the Italian Ministry of Education and Research (PRIN Grant 2010HXAW77 007)., This paper describes the architecture, the development and the implementation of Janus II, a new generation application-driven number cruncher optimized for Monte Carlo simulations of spin systems (mainly spin glasses). This domain of computational physics is a recognized grand challenge of high-performance computing: the resources necessary to study in detail theoretical models that can make contact with experimental data are by far beyond those available using commodity computer systems. On the other hand, several specific features of the associated algorithms suggest that unconventional computer architectures – that can be implemented with available electronics technologies – may lead to order of magnitude increases in performance, reducing to acceptable values on human scales the time needed to carry out simulation campaigns that would take centuries on commercially available machines. Janus II is one such machine, recently developed and commissioned, that builds upon and improves on the successful JANUS machine, which has been used for physics since 2008 and is still in operation today. This paper describes in detail the motivations behind the project, the computational requirements, the architecture and the implementation of this new machine and compares its expected performances with those of currently available commercial systems., Unión Europea. FP7, Ministerio de Ciencia e Innovación (MICINN), European Regional Development Fund, Junta de Extremadura (Spain), Italian Ministry of Education and Research, Depto. de Física Teórica, Fac. de Ciencias Físicas, TRUE, pub

© 2006. The American Astronomical Society. Artículo firmado por 20 autores. We are grateful to Stuart Shaklan, Michael Shao, Chas Beichman, Richard Green, Skip Andree, Daryl Wilmarth, and the KPNO staff for their generous support and advice and to Larry Molnar for his help in the early photometric data acquisition. The HET observations, whose timings were critical, were made possible by the dedicated efforts of the HET staff. We are indebted to Sara Seager and Eric Agol for a number of stimulating discussions. We thank Aldo Martínez Fiorenzano for helping the line bisector analysis of HD 102195. We appreciate many valuable comments made by the referee, which helped to improve the paper quality. This work is supported by the National Science Foundation grant AST 02-43090, JPL, Pennsylvania State University, and the University of Florida. S. M. and J. v. E. acknowledge the JPL Michelson Fellowship funded by NASA. G. W. H. is grateful for the efforts of Lou Boyd at Fairborn Observatory and acknowledges support from NASA grant NCC5-511 and NSF grant HRD 97-06268. E. B. F. acknowledges the support of the Miller Institute for Basic Research. W. D. C., M. E., and R. A. W. were supported by NASA grants NNG04G141G and NNG05G107G to the University of Texas at Austin. The Hobby-Eberly Telescope (HET) is a joint project of the University of Texas at Austin, Pennsylvania State University, Stanford University, Ludwig-MaximilliansUniversität München, and Georg-August-Universität Göttingen. The HET is named in honor of its principal benefactors,William P. Hobby and Robert E. Eberly. D. M. was supported by the Universidad Complutense de Madrid and the Spanish Ministerio de Educación y Ciencia (MEC), Programa Nacional de Astronomía y Astrofísica under grant AYA2005-02750. D. M. is grateful to Raquel M. Martínez, Jesús Maldonado, and Benjamín Montesinos for their help during the observations. FOCES high-resolution optical spectra were based on observations collected at the Centro Astr, We report the detection of the first extrasolar planet, ET-1 (HD 102195b), using the Exoplanet Tracker (ET), a new-generation Doppler instrument. The planet orbits HD 102195, a young star with solar metallicity that may be part of the local association. The planet imparts radial velocity variability to the star with a semiamplitude of 63.4 ± 2.0 m s^-1 and a period of 4.11 days. The planetary minimum mass (m sin i) is 0.488MJ ± 0.015M_J. The planet was initially detected in the spring of 2005 with the Kitt Peak National Observatory (KPNO) 0.9 m coudé feed telescope. The detection was confirmed by radial velocity observations with the ET at the KPNO 2.1 m telescope and also at the 9 m Hobby-Eberly Telescope (HET) with its High Resolution Spectrograph. This planetary discovery with a 0.9 m telescope around a V = 8.05 magnitude star was made possible by the high throughput of the instrument: 49% measured from the fiber output to the detector. The ET's interferometer-based approach is an effective method for planet detection. In addition, the ET concept is adaptable to multiple-object Doppler observations or very high precision observations with a cross-dispersed echelle spectrograph to separate stellar fringes over a broad wavelength band. In addition to spectroscopic observations of HD 102195, we obtained brightness measurements with one of the automated photometric telescopes at Fairborn Observatory. Those observations reveal that HD 102195 is a spotted variable star with an amplitude of ~0.015 mag and a 12.3 ± 0.3 day period. This is consistent with spectroscopically observed Ca II H and K emission levels and line-broadening measurements but inconsistent with rotational modulation of surface activity as the cause of the radial velocity variability. Our photometric observations rule out transits of the planetary companion., National Science Foundation (NSF), EE.UU., NASA Jet Propulsion Laboratory (JPL), Pennsylvania State University, University of Florida, National Aeronautics and Space Administration (NASA), Miller Institute for Basic Research., University of Texas, Universidad Complutense de Madrid (UCM), Ministerio de Educación y Ciencia (MEC), España, Programa Nacional de Astronomía y Astrofísica (PNAyA), 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

© 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

© ESO, 2014. Artículo firmado por 46 autores. This study makes use 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 thanks also the CAR staff for the dedication to this project, The authors would like to thank the anonymous referee for comments that significantly improved the paper, Dimitri Gadotti for providing extersive help and advice with the image decomposition; Mike Dopita and Tim Heckman for their patience explaining the effects of shocks in superwinds; Daria Dubinoyska for creating undistorted ACS PSF images from the Tiny Tim images and Carotin Villforth for further help with the ACS PSF; Lia Athanassoula for help interpeting the kinematic maps: Daniel Pomarede for help getting SDvision running; Jeremy Sanders and Roderik Johnstone for help interpreting( the X-ray observations: Eva Schinnerer for pointing out the effect of beam smearing; all other interested researchers who have contributed with questions and comments following discussions and presentations of this work over the last 2 years. The numerical simulations were performed on facilities hosted by the CSC-IT Center for Science in Espoo. Finland, which are financed by the Finnish ministry of education. Funding and financial support acknowledgements.: V. W. from the European Research Council Starting Grant (RI, Wild SEDmorph), European Research Council Advanced Grant (RI. J. Dunlop) and Marie Curie Career Reintegration Grant (RI. Wild Phiz-e, We present optical integral field spectroscopy (IFS) observations of the Mice, a major merger between two massive (≳10^11 M_⊙) gas-rich spirals NGC 4676A and B, observed between first passage and final coalescence. The spectra provide stellar and gas kinematics, ionised gas properties, and stellar population diagnostics, over the full optical extent of both galaxies with ~1.6 kpc spatial resolution. The Mice galaxies provide a perfect case study that highlights the importance of IFS data for improving our understanding of local galaxies. The impact of first passage on the kinematics of the stars and gas has been significant, with strong bars most likely induced in both galaxies. The barred spiral NGC 4676B exhibits a strong twist in both its stellar and ionised gas disk. The edge-on disk galaxy NGC 4676A appears to be bulge free, with a strong bar causing its “boxy” light profile. On the other hand, the impact of the merger on the stellar populations has been minimal thus far. By combining the IFS data with archival multiwavelength observations we show that star formation induced by the recent close passage has not contributed significantly to the total star formation rate or stellar mass of the galaxies. Both galaxies show bicones of high ionisation gas extending along their minor axes. In NGC 4676A the high gas velocity dispersion and Seyfert-like line ratios at large scaleheight indicate a powerful outflow. Fast shocks (vs ~ 350 km s^-1) extend to ~6.6 kpc above the disk plane. The measured ram pressure (P/k = 4.8 × 10^6 K cm^-3) and mass outflow rate (~8−20 M_⊙ yr^-1) are similar to superwinds from local ultra-luminous infrared galaxies, although NGC 4676A only has a moderate infrared luminosity of 3 × 10^10 L_⊙. Energy beyond what is provided by the mechanical energy of the starburst appears to be required to drive the outflow. Finally, we compare the observations to mock kinematic and stellar population maps extracted from a hydrodynamical merger simulation. T, Unión Europea. FP7, Ministerio de Economía y Competitividad (MINECO), European Research Council, Marie Curie Career Reintegration, Consejo Nacional de Ciencia y Tecnología (CONACYT), México, Danish National Research Foundation, University of Helsinki, Programa Ramón y Cajal, Agence Nationale de la Recherche (ANR), Francia, Ministerio de Educación e Investigación = Bundesministeriums für Bildung und Forschung (BMBF), Alemania, Campus de Excelencia Internacional (CEI) Moncloa, España, Emmy Noether-Programme (GSF), Fundacao para a Ciencia e a Tecnologia (FCT), Portugal, FCT-MEC, Junta de Andalucía, Marie Curie Career Integration, Junta de Andalucia, National Science Foundation (NSF), Aspen Center for Physics, German Science Foundation (GSF), Alemania, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

© 2008 The American Physical Society. Artículo firmado por 21 autores. We corresponded with M. Hasenbusch, A. Pelissetto, and E. Vicari. Janus was supported by EU FEDER funds (UNZA05-33-003, MEC-DGA, Spain), and developed in collaboration with ETHlab. We were partially supported by MEC (Spain), through Contracts No. FIS2006-08533, FIS2007-60977, FPA2004-02602, TEC2007-64188; by CAM (Spain), and by Microsoft, We study numerically the nonequilibrium dynamics of the Ising spin glass, for a time spanning 11 orders of magnitude, thus approaching the experimentally relevant scale (i.e., seconds). We introduce novel analysis techniques to compute the coherence length in a model-independent way. We present strong evidence for a replicon correlator and for overlap equivalence. The emerging picture is compatible with noncoarsening behavior., EU FEDER funds, MEC (Spain), CAM (Spain), Microsoft, Depto. de Física Teórica, Fac. de Ciencias Físicas, TRUE, pub

© 2016 American Physical Society. Artículo firmado por 17 autores. The work at UniFr was supported by the Schweizer Nationalfonds (SNF) through Grants No. 200020-153660 and No. CRSII2-154410/1. The work at Muni was supported by the projects CEITEC(CZ.1.05/1.1.00/02.0068) and MUNI/A/1496/2014. The XAS measurements were performed at the EPFL/PSI XTreme beamline of the Swiss Light Source at the Paul Scherrer Institut, Villigen, Switzerland. The neutron experiment was done at the NREX instrument operated by the Max-Planck Society at the Heinz MaierLeibnitz Zentrum (MLZ), Garching, Germany, and was supported by the European Commission under the 7th Framework Programme through the “Research Infrastructures” action of the Capacities Programme, NMI3-II, Grant No. 283883., With x-ray absorption spectroscopy and polarized neutron reflectometry we studied how the magnetic proximity effect at the interface between the cuprate high-TC superconductor YBa_(2)Cu_(3)O_(7) (YBCO) and the ferromagnet La_(2/3)Ca_(1/3)MnO_(3) (LCMO) is related to the electronic and magnetic properties of the LCMO layers. In particular, we explored how the magnitude of the ferromagnetic Cu moment on the YBCO side depends on the strength of the antiferromagnetic (AF) exchange coupling with the Mn moment on the LCMO side. We found that the Cu moment remains sizable if the AF coupling with the Mn moments is strongly reduced or even entirely suppressed. The ferromagnetic order of the Cu moments thus seems to be intrinsic to the interfacial CuO_(2) planes and related to a weakly ferromagnetic intraplanar exchange interaction. The latter is discussed in terms of the partial occupation of the Cu 3d_(3z^(2)−r^(2)) orbitals, which occurs in the context of the so-called orbital reconstruction of the interfacial Cu ions., Unión Europea. FP7, Schweizer Nationalfonds (SNF), Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

© 2010 IOP Publishing Ltd and SISSA. Artículo firmado por 21 autores. Janus has been funded by European Union (FEDER) funds, Diputación General de Aragón (Spain), by a Microsoft Award - Sapienza - Italy, and by Eurotech. We were partially supported by MICINN (Spain), through contracts No. TEC2007-64188, FIS2006-08533-C03, FIS2007-60977, FIS2009-12648-C03 and UCM-Banco de Santander. D. Yllanes and B. Seoane are FPU Fellow (Spain). S.P.-G. was supported by FECYT (Spain). The authors would like to thank the Arénaire team, especially J. Detrey and F. de Dinechin for the VHDL code of the logarithm function 19., We study the 3D Disordered Potts Model with p = 5 and p = 6. Our numerical simulations (that severely slow down for increasing p) detect a very clear spin glass phase transition. We evaluate the critical exponents and the critical value of the temperature, and we use known results at lower p values to discuss how they evolve for increasing p. We do not find any sign of the presence of a transition to a ferromagnetic regime., Ministerio de Ciencia e Innovación (MICINN), European Union (FEDER), Diputación General de Aragón (Spain), Microsoft Award - Sapienza - Italy, Eurotech, UCM-Banco de Santander, FPU Fellow (Spain), FECYT (Spain), Depto. de Física Teórica, Fac. de Ciencias Físicas, TRUE, pub

© ESO, 2014. Artículo firmado por 23 autores. We thank the referee for a thorough reading of this work and for the comments and suggestions. We also thank Lindsay Holmes for allowing us to use her DiskFit kinematic modelling for comparison with our results. This study makes use of the data provided by the Calar Alto Legacy FieldArea (CALIFA) survey (http://www.califa.caha.es). and is based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calor Alto, operated jointly by the Max-Planck-Institut fur Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). CALIFA is the first legacy survey performed at Calar Alto. The CALIFA collaboration would like to thanks the IAA-CSIC and MPIA-MPG as major partners of the observatory, and CAHA itself for the unique access to telescope time and for support in manpower and infrastructures. The CALIFA collaboration also thanks the CAHA staff for their dedication to this project. J.B.-B. and B.G.-L. acknowledge the support from the Plan Nacional de I+D+i (PNAYA) funding programme (AYA2012-39408-C02-02) of the Spanish Ministry of Economy and Competitiveness (MINECO). J.F.-B. acknowledges support from the Ramón y Cajal Program, grants AYA2010-21322-C03-02 from MINECO. We also acknowledge support from the FP7 Marie Curie Actions of the European Commission, via the Initial Training Network DAGAL under REA grant agreement number 289313. R.A.M is funded by the Spanish programme of International Campus of Excellence Moncloa (CEI). L.V.M. acknowledges support from the grant AYA2011-30491-C02-01 co-financed by MICINN and FEDER funds and the Junta de Andalucía (Spain) grants P08-FQM-4205 and TIC-114. 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. J.M.A. acknowledges support from the European Research Council Starting Grant (SEDmorphi P.I. V. Wild)., We present 80 stellar and ionised gas velocity maps from the Calar Alto Legacy Integral Field Area (CALIFA) survey in order to characterise the kinematic orientation of non interacting galaxies. The study of galaxies in isolation is a key step towards understanding how fast external processes, such as major mergers. affect kinematic properties in galaxies. We derived the global and individual (projected approaching and receding sides) kinematic position angles (PAs) for both the stellar and ionised gas line-of-sight velocity distributions. When compared to the photometric PA, we find that morpho-kinematic differences are smaller than 22 degrees in 90% of the sample for both stellar and nebular components and that internal kinematic misalignments are generally smaller than 16 degrees. We find a tight relation between the global stellar and ionised gas kinematic PA consistent with circular-flow pattern motions in both components (~90% of the sample has differences smaller than 16 degrees). This relation also holds, generally in barred galaxies across the bar and galaxy disc scales. Our findings suggest that even in the presence of strong bars, both the stellar and the gaseous components tend to follow the gravitational potential of the disc. As a result, kinematic orientation can be used to assess the degree of external distortions in interacting galaxies., Unión Europea. FP7, Ministerio de Economía y Competitividad (MINECO), Programa Ramón y Cajal Program (MINECO), Spanish programme of International Campus of Excellence Moncloa (CEI), Ministerio de Ciencia e Innovacion (MICINN), FEDER funds, Junta de Andalucía, Plan Nacional de Investigación Científica, Desarrollo e Innovación Tecnológica (Plan Nacional de I+D+i) (PNAYA), European Research Council, 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

© 2016 IOP Publishing Ltd. Artículo firmado por 157 autores. The MAGIC Collaboration thanks the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2012-39502), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Centro de Excelencia Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucl´eaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France., We present the first joint analysis of gamma-ray data from the MAGIC Cherenkov telescopes and the Fermi Large Area Telescope (LAT) to search for gamma-ray signals from dark matter annihilation in dwarf satellite galaxies. We combine 158 hours of Segue 1 observations with MAGIC with 6-year observations of 15 dwarf satellite galaxies by the Fermi-LAT. We obtain limits on the annihilation cross-section for dark matter particle masses between 10 GeV and 100 TeV – the widest mass range ever explored by a single gamma-ray analysis. These limits improve on previously published Fermi-LAT and MAGIC results by up to a factor of two at certain masses. Our new inclusive analysis approach is completely generic and can be used to perform a global, sensitivity-optimized dark matter search by combining data from present and future gamma-ray and neutrino detectors., Ministerio de Economía y Competitividad (MINECO), German BMBF and MPG, Italian INFN and INAF, Swiss National Fund SNF, Japanese JSPS and MEXT, Centro de Excelencia Severo Ochoa, Spanish Consolider-Ingenio 2010 programme, Academy of Finland, Croatian Science Foundation (HrZZ, University of Rijeka Project, DFG Collaborative Research Centers, Polish MNiSzW, National Aeronautics and Space Administration, Department of Energy in the United States, Commissariat à l’Energie Atomique, Centre National de la Recherche Scientifique / Institut National de Physique Nucl´eaire et de Physique des Particules in France, Agenzia Spaziale Italiana, Istituto Nazionale di Fisica Nucleare in Italy, Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK), Japan Aerospace Exploration Agency (JAXA), K. A. Wallenberg Foundation, Swedish Research Council, Swedish National Space Board, Istituto Nazionale di Astrofisica in Italy, Centre National d’Études Spatiales in France, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

© 2007 Elsevier B.V. Artículo firmado por 18 autores. The help of G. Poli in the development of the IANUS Ethernet interface is warmly acknowledged., We describe the hardwired implementation of algorithms for Monte Carlo simulations of a large class of spin models. We have implemented these algorithms as VHDL codes and we have mapped them onto a dedicated processor based on a large FPGA device. The measured performance on one such processor is comparable to O(100) carefully programmed high-end PCs: it turns out to be even better for some selected spin models. We describe here codes that we are currently executing on the IANUS massively parallel FPGA-based system., Depto. de Física Teórica, Fac. de Ciencias Físicas, TRUE, pub

© 2010 The American Physical Society. Artículo firmado por 21 autores. The Janus computer was funded by EU FEDER (UNZA05 33-003, MEC-DGA, Spain) and developed in collaboration with ETHlab. We were partially supported by MICINN (Spain), through Contracts No. TEC2007- 64188, No. FIS2007-60977, No. FIS2009-12648-C03, by Junta de Extremadura (GRU09038), and by UCM-Banco de Santander. B. S. and D. Y. were supported by the FPU program (Spain) and SPG by FECYT (Spain)., We numerically study the aging properties of the dynamical heterogeneities in the Ising spin glass. We find that a phase transition takes place during the aging process. Statics-dynamics correspondence implies that systems of finite size in equilibrium have static heterogeneities that obey finite-size scaling, thus signaling an analogous phase transition in the thermodynamical limit. We compute the critical exponents and the transition point in the equilibrium setting, and use them to show that aging in dynamic heterogeneities can be described by a finite-time scaling ansatz, with potential implications for experimental work., Ministerio de Ciencia e Innovación (MICINN), EU FEDER, MEC-DGA, Spain, Junta de Extremadura, Spain, UCM-Banco de Santander, FPU program (Spain), SPG by FECYT (Spain), Depto. de Física Teórica, 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

© 2016. The American Astronomical Society. All rights reserved. Artículo firmado por 19 autores. S.B. acknowledges support from BMBF through the Erasmus-F project (grant number 05 A12BA1) and is grateful to Leibniz-Institut fur Astrophysik Potsdam for its hospitality during her guest stay there in 2016. J.F.B. acknowledges support from grant AYA2013-48226-C3-1-P from the Spanish Ministry of Economy and Competitiveness (MINECO). C.J.W. acknowledges support through the Marie Curie Career Integration Grant 303912. S.F.S. thanks the CONACYT-125180 and DGAPA-IA100815 projects for providing support during this study. D.O. thanks the University of Western Australia for its support via a Research Collaboration Award. K.S. acknowledges funding from the Natural Sciences and Engineering Research Council of Canada., The velocity function (VF) is a fundamental observable statistic of the galaxy population that is similar to the luminosity function in importance, but much more difficult to measure. In this work we present the first directly measured circular VF that is representative between 60 < v_circ < 320 km s^-1 for galaxies of all morphological types at a given rotation velocity. For the low-mass galaxy population (60 < v_circ < 170 km s^-1), we use the HI Parkes All Sky Survey VF. For the massive galaxy population (170 < v_circ < 320 km s^-1), we use stellar circular velocities from the Calar Alto Legacy Integral Field Area Survey (CALIFA). In earlier work we obtained the measurements of circular velocity at the 80% light radius for 226 galaxies and demonstrated that the CALIFA sample can produce volume-corrected galaxy distribution functions. The CALIFA VF includes homogeneous velocity measurements of both late and early-type rotation-supported galaxies and has the crucial advantage of not missing gas-poor massive ellipticals that HI surveys are blind to. We show that both VFs can be combined in a seamless manner, as their ranges of validity overlap. The resulting observed VF is compared to VFs derived from cosmological simulations of the z = 0 galaxy population. We find that dark-matter-only simulations show a strong mismatch with the observed VF. Hydrodynamic simulations fare better, but still do not fully reproduce observations., Unión Europea. FP7, Ministerio de Economía y Competitividad (MINECO), Bundesministerium für Bildung und Forschung (BMBF), Alemania, Ayudas a la integración profesional (CIG) - Acciones Marie Skłodowska-Curie (UE), University of Western Australia, Natural Sciences and Engineering Research Council of Canada, Consejo Nacional de Ciencia y Tecnología (CONACYT), México, Dirección General Asuntos del Personal Académico - Universidad Autónoma de México (UNAM), 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

© 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

© 2014 American Physical Society. Artículo firmado por 24 autores. The Janus project has been partially supported by the EU (FEDER funds, Grant No. UNZA05-33-003, MEC-DGA, Spain); by the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013, ERC Grant agreement N. 247328); by the MICINN (Spain) (Contracts No. FIS2006-08533, No. FIS2012-35719-C02, No. FIS2010-16587, and No. TEC2010-19207); by the SUMA project of INFN (Italy); by CAM (Spain); by the Junta de Extremadura (GR10158); by the Microsoft Prize 2007 and by the European Union (PIRSES-GA-2011-295302). F.R.-T. was supported by the Italian Research Ministry through the FIRB Project No. RBFR086NN1; M.B.-J. was supported by the FPU program (Ministerio de Educación, Spain); R.A.B. and J.M.-G. were supported by the FPI program (Diputación de Aragón, Spain); S.P.-G. was supported by the ARAID foundation; finally, J.M.G.-N. was supported by the FPI program (Ministerio de Ciencia e Innovación, Spain)., We study the off-equilibrium dynamics of the three dimensional Ising spin glass in the presence of an external magnetic field. We have performed simulations both at fixed temperature and with an annealing protocol. Thanks to the Janus special-purpose computer, based on field-programmable gate array (FPGAs), we have been able to reach times equivalent to 0.01 s in experiments. We have studied the system relaxation both for high and for low temperatures, clearly identifying a dynamical transition point. This dynamical temperature is strictly positive and depends on the external applied magnetic field. We discuss different possibilities for the underlying physics, which include a thermodynamical spin-glass transition, a mode-coupling crossover, or an interpretation reminiscent of the random first-order picture of structural glasses., Unión Europea. FP7, EU (FEDER funds), Ministerio de Ciencia e Innovación (MICINN), INFN (Italy), CAM (Spain), Junta de Extremadura, Microsoft Prize 2007, European Union, Italian Research Ministry, Ministerio de Educación (Spain) under FPU program, Diputación de Aragón (Spain) under FPI program, ARAID foundation, Ministerio de Ciencia e Innovación (Spain) under FPI program, Depto. de Física Teórica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2016. Artículo firmado por 147 autores. We would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2012-39502), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Centro de Excelencia Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESSMAGIC/2010/0., Aims. We investigate the extension of the very high-energy spectral tail of the Crab Pulsar at energies above 400 GeV. Methods. We analyzed ~320 h of good-quality Crab data obtained with the MAGIC telescope from February 2007 to April 2014. Results. We report the most energetic pulsed emission ever detected from the Crab Pulsar reaching up to 1.5 TeV. The pulse profile shows two narrow peaks synchronized with those measured in the GeV energy range. The spectra of the two peaks follow two different power-law functions from 70 GeV up to 1.5 TeV and connect smoothly with the spectra measured above 10 GeV by the Large Area Telescope (LAT) on board the Fermi satellite. When making a joint fit of the LAT and MAGIC data above 10 GeV the photon indices of the spectra differ by 0.5 ± 0.1. Conclusions. Using data from the MAGIC telescopes we measured the most energetic pulsed photons from a pulsar to date. Such TeV pulsed photons require a parent population of electrons with a Lorentz factor of at least 5 × 106. These results strongly suggest IC scattering off low-energy photons as the emission mechanism and a gamma-ray production region in the vicinity of the light cylinder., Ministerio de Economía y Competitividad (MINECO), German BMBF, German MPG, Italian INFN, Italian INAF, Swiss National Fund SNF, Japanese JSPS, Japanese MEXT, Centro de Excelencia Severo Ochoa, Spanish Consolider-Ingenio 2010 programme, Academy of Finland, Croatian Science Foundation (HrZZ), University of Rijeka, DFG Collaborative Research Centers, Polish MNiSzW, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

© 2011. The American Astronomical Society. All rights reserved. Artículo firmado por 24 autores. The authors thank the entire S^4G team for their efforts in this project. 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 S^(4)G project.K.S., J.-C.M.M., T. Kim and T. Mizusawa acknowledge support from the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. E. A. and A. B. thank the Centre National d'Etudes Spatiales for financial support. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. 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., Most, if not all, disk galaxies have a thin (classical) disk and a thick disk. In most models thick disks are thought to be a necessary consequence of the disk formation and/or evolution of the galaxy. We present the results of a study of the thick disk properties in a sample of carefully selected edge-on galaxies with types ranging from T = 3 to T = 8. We fitted one-dimensional luminosity profiles with physically motivated functions—the solutions of two stellar and one gaseous isothermal coupled disks in equilibrium—which are likely to yield more accurate results than other functions used in previous studies. The images used for the fits come from the Spitzer Survey of Stellar Structure in Galaxies (S^4G). We found that thick disks are on average more massive than previously reported, mostly due to the selected fitting function. Typically, the thin and thick disks have similar masses. We also found that thick disks do not flare significantly within the observed range in galactocentric radii and that the ratio of thick-to-thin disk scale heights is higher for galaxies of earlier types. Our results tend to favor an in situ origin for most of the stars in the thick disk. In addition, the thick disk may contain a significant amount of stars coming from satellites accreted after the initial buildup of the galaxy and an extra fraction of stars coming from the secular heating of the thin disk by its own overdensities. Assigning thick disk light to the thin disk component may lead to an underestimate of the overall stellar mass in galaxies because of different mass-to-light ratios in the two disk components. On the basis of our new results, we estimate that disk stellar masses are between 10% and 50% higher than previously thought and we suggest that thick disks are a reservoir of "local missing baryons.", National Radio Astronomy Observatory, Centre National d'Etudes Spatiales, Alfred P. Sloan Foundation, National Science Foundation (NFS), EE.UU., U.S. Department of Energy, National Aeronautics and Space Administration (NASA), Japanese Monbukagakusho, Max Planck Society, Higher Education Funding Council for England, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub