Persona: Solano, Enrique
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Solano
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Publicación Acceso Abierto Gaia Early Data Release 3 Acceleration of the Solar System from Gaia astrometry(EDP Sciences, 2021-04-28) Klioner, S. A.; Mignard, F.; Lindegren, L.; Bastian, U.; McMillan, P. J.; Hernández, J.; Hobbs, D.; Ramos Lerate, M.; Biermann, M.; Bombrun, A.; De Torres, A.; Becciani, U.; Peñalosa Esteller, X.; Hauser, M.; Dell´Oro, A.; Viala, Y.; Brouillet, N.; Taris, F.; Bellas Velidis, I.; Blomme, R.; Pauwels, T.; Brugaletta, E.; Fabricius, C.; Haywood, M.; Eyer, L.; Mints, A.; Souami, D.; Mowlavi, N.; Lindstrom, H. E. P.; Portell, J.; Aerts, C.; Bernet, M.; Hladczuk, N.; De Souza, R.; Casamiquela, L.; Soubiran, C.; Fouesneau, M.; Cheek, N.; Anglada Varela, E.; Madrero Pardo, P.; Lorca, A.; Rybizki, J.; Drimmel, R.; Chemin, L.; Managau, S.; Pineau, F. X.; Heiter, U.; Panem, C.; Ducourant, C.; Marchal, O.; Balog, Z.; Spoto, F.; Fraile, E.; Gosset, E.; Vanel, O.; Steele, I. A.; Delgado, A.; Mastrobuono Battisti, A.; Smith, M.; Burgess, P. W.; Vecchiato, A.; Morbidelli, R.; Riclet, F.; Charlot, P.; Baker, S. G.; Pawlak, M.; Bucciarelli, B.; Carrasco, J. M.; Marinoni, S.; Leclerc, N.; Lebzelter, T.; Sordo, R.; Gilmore, G.; Zhao, H.; Fedorets, G.; Manteiga, M.; García Reinaldos, M.; Mulone, A. F.; Giacobbe, P.; Thuillot, W.; Arenou, F.; Clementini, G.; Osborne, Paul; Poggio, E.; Jevardat de Fombelle, G.; Semeux, D.; De Ridder, J.; Penttilä, A.; De Teodoro, P.; Lattanzi, M. G.; Montegriffo, P.; Muinonen, K.; Marshall, D. J.; Hatzidimitriou, D.; Rainer, M.; Barstow, M. A.; Gerlach, E.; García Lario, P.; Szabados, L.; Le Fustec, Y.; Garabato, D.; Szegedi Elek, E.; Bellazzini, M.; Bramante, L.; Galluccio, L.; González Santamaría, I.; Berthier, J.; Brown, A. G. A.; Baudesson Stella, A.; Cowell, S.; Abbas, U.; Santoveña, R.; Mora, A.; Sartoretti, P.; Anderson, R. I.; Álvarez Cid Fuentes, J.; Reylé, C.; Barache, C.; Delgado, H. E.; García Torres, M.; Luri, X.; Jonker, P. G.; Altavilla, G.; Thévenin, F.; Bianchi, L.; Eappachen, D.; Robichon, N.; Castro Sampol, P.; David, M.; Siopis, C.; Robin, C.; Taylor, M. B.; Cánovas, H.; Recio Blanco, A.; Van Reeven, W.; Girona, S.; Fernique, P.; Teyssier, D.; Molnár, L.; Burlacu, A.; Altmann, M.; Pagani, C.; Salguero, E.; De Luise, F.; Stephenson, C. A.; Fernández Hernández, J.; Ségransan, D.; Audard, Marc; Schultheis, M.; Fabrizio, M.; González Vidal, J. J.; Haigron, R.; Rowell, N.; Ramos, P.; Sanna, N.; Balaguer Núñez, L.; Randich, S.; Harrison, D. L.; Messina, S.; Chaoul, Laurence; Cropper, M.; Muraveva, T.; Kochoska, A.; Roegiers, T.; Blanco Cuaresma, S.; Cooper, W. J.; Tonello, N.; Carnerero, M. I.; Nienartowicz, K.; Lobel, A.; Zwitter, T.; Sozzetti, A.; Segol, M.; Comoretto, G.; Rybicki, K. A.; Cancelliere, R.; Gai, M.; Fouron, C.; Holl, B.; Bressan, A.; Ragaini, S.; Abreu Aramburu, A.; Ordénovic, C.; Torra, F.; Giuffrida, G.; Bartolomé, S.; Orrù, G.; Bauchet, N.; Löffler, W.; Van Dillen, E.; Del Peloso, E. F.; Guerrier, A.; Chiavassa, A.; Geyer, R.; Siebert, A.; Di Stefano, E.; Khanna, S.; Fienga, A.; Marconi, M.; Morris, D.; Masip, A.; Diakite, S.; Steidelmüller, H.; Gavras, P.; Martín Fleitas, J. M.; Yoldas, A.; Julbe, F.; Liao, S.; De Laverny, P.; Yvard, P.; Helmi, A.; Crifo, F.; Babusiaux, C.; Murphy, C. P.; Millar, N. R.; Barbato, D.; Sciacca, E.; Granvik, M.; Barros, M.; Spagna, A.; Lister, T. A.; Lanzafame, A. C.; Breedt, E.; Nicolas, C.; Esquej, P.; Jean Antonie Piccolo, A.; Mazeh, T.; Osinde, J.; Busonero, D.; Zurbach, C.; Guerra, R.; Faigler, S.; Riello, M.; Caffau, E.; Sánchez Giménez, V.; Karbevska, L.; Sarro, L. M.; Siltala, L.; Prsa, A.; Dapergolas, A.; Le Campion, J. F.; Carry, B.; Huckle, H. E.; Muñoz, D.; Rixon, G.; Hodgkin, S. T.; De March, R.; Messineo, M.; Guiraud, J.; Walton, N. A.; Mor, R.; Kervella, P.; Carballo, R.; Gómez, A.; Vaillant, M.; Del Pozo, E.; Solitro, F.; Cellino, A.; Musella, I.; Fragkoudi, F.; Franke, F.; Castro Ginard, A.; Delchambre, L.; Utrilla, E.; Aguado, J. J.; Kordopatis, G.; Janßen, Katja; Panuzzo, P.; Martin Polo, L.; Poujoulet, E.; Royer, F.; Siddiqui, H. I.; Sahlmann, J.; Marocco, F.; Krone Martins, A.; Hestroffer, D.; Sagristà Sellés, A.; Halbwachs, J. L.; Masana, E.; Marchant, J. M.; Hambly, N. C.; Panahi, A.; Jordi, C.; Lecoeur Taibi, I.; Slezak, E.; Pourbaix, D.; Figueras, F.; Michalik, D.; Gracia Abril, G.; Evans, D. W.; Ripepi, V.; Castellani, M.; Romero Gómez, M.; Alves, J.; Massari, D.; Rimoldini, L.; Samaras, N.; Souchay, J.; Gutiérrez Sánchez, R.; Benson, K.; Süveges, M.; Crowley, C.; Busso, G.; Frémat, Y.; Poretti, E.; David, P.; Plachy, E.; Torra, J.; Leccia, S.; Racero, E.; Piersimoni, A. M.; Creevey, O. L.; Wyrzykowski, L.; Cantat Gaudin, T.; Livanou, E.; Lammers, U.; Ajaj, M.; Robin, A. C.; Segovia, J. C.; Richards, P. J.; Noval, L.; Davidson, M.; Mann, R. G.; Tanga, P.; Bertone, S.; Smart, R. L.; Molinaro, R.; Damerdji, Y.; Juaristi Campillo, J.; Bouquillon, S.; Delisle, J. B.; Pulone, L.; Carlucci, T.; Antoja, T.; Sadowski, G.; García Gutierrez, A.; Van Leeuwen, F.; Pailler, F.; De Angeli, F.; Licata, E.; Vallenari, A.; Castañeda, J.; Butkevich, A. G.; Álvarez, M. A.; Rohrbasser, L.; Buzzi, R.; Riva, A.; Pancino, E.; Re Fiorentin, P.; Roux, W.; Molina, D.; Bailer Jones, C. A. L.; Palaversa, L.; Moitinho, A.; Weiler, M.; Jasniewicz, G.; Zucker, S.; Dolding, C.; Salgado, J.; De Bruijne, J. H. J.; Guy, L. P.; Pagano, I.; Bassilana, J. L.; Wevers, T.; Raiteri, C. M.; Palicio, P. A.; Accart, S.; Fabre, C.; Katz, D.; Teixeira, R.; Rambaux, N.; Unger, N.; Tauran, G.; Marrese, P. M.; Seabroke, G. M.; Hidalgo, S. L.; González Núñez, J.; Jordan, S.; Di Matteo, P.; Dafonte, C.; Crosta, M.; Solano, E.; Bossini, D.; Roelens, M.; Balbinot, E.; Prusti, T.; Voutsinas, S.; Garofalo, A.; Boch, T.; Plum, G.; Marcos Santos, M. M. S.; Turon, C.; Jansen, F.; Enke, H.; Bakker, J.; Morel, T.; Ulla, A.; Holland, G.; Van Leeuwen, M.; Regibo, S.; Hilger, T.; Hutton, A.; Diener, C.; Zorec, J.; Lebreton, Y.; Andrae, R.; Cornez, T.; Vicente, D.; Baines, D.; Sarasso, M.; Manteiga, Minia; Solano, Enrique; Forderung der wissenschaftlichen Forschung (FWF); Belgian federal Science Policy Office (BELSPO); Hertha Firnberg Programme; Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP); Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES); Comite Francais d'Evaluation de la Cooperation Universitaire et Scientifique avec le Bresil (COFECUB); National Natural Science Foundation of China (NSFC); China Scholarship Council (CSC); European Commission (EC); European Research Council (ERC); Hungarian National Research, Development, and Innovation Office (NKFIH); Science Foundation Ireland (SFI); Israel Science Foundation (ISF); Agenzia Spaziale Italiana (ASI); Istituto Nazionale di Astrofisica (INAF); Netherlands Research School for Astronomy (NOVA); Fundacao para a Ciencia e a Tecnologia (FCT); Agencia Estatal de Investigación (AEI); European Space Agency (ESA); Centre National D'Etudes Spatiales (CNES); Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR); Narodowe Centrum Nauki (NCN); Slovenian Research Agency; Swedish National Space Agency (SNSA); United Kingdom Science and Technology Facilities Council (STFC); Universitat de Barcelona (UB); Generalitat de Catalunya; Xunta de Galicia; Deliste, J. B. [0000-0001-5844-9888]; Sozzeti, A. [0000-0002-7504-365X]; Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos Universidad de Barcelona, MDM-2014-0369; Centro de Excelencia Científica Severo Ochoa, Instituto de Ciencias del Cosmos de la Universidad de Barcelona, SEV2015-0493Context. Gaia Early Data Release 3 (Gaia EDR3) provides accurate astrometry for about 1.6 million compact (QSO-like) extragalactic sources, 1.2 million of which have the best-quality five-parameter astrometric solutions. Aims. The proper motions of QSO-like sources are used to reveal a systematic pattern due to the acceleration of the solar systembarycentre with respect to the rest frame of the Universe. Apart from being an important scientific result by itself, the acceleration measured in this way is a good quality indicator of the Gaia astrometric solution. Methods. Theeffect of the acceleration was obtained as a part of the general expansion of the vector field of proper motions in vector spherical harmonics (VSH). Various versions of the VSH fit and various subsets of the sources were tried and compared to get the most consistent result and a realistic estimate of its uncertainty. Additional tests with the Gaia astrometric solution were used to get a better idea of the possible systematic errors in the estimate. Results. Our best estimate of the acceleration based on Gaia EDR3 is (2.32 ± 0.16) × 10−10 m s−2 (or 7.33 ±0.51 km s−1 Myr−1) towards α = 269.1° ± 5.4°, δ = −31.6° ± 4.1°, corresponding to a proper motion amplitude of 5.05 ±0.35 μas yr−1. This is in good agreement with the acceleration expected from current models of the Galactic gravitational potential. We expect that future Gaia data releases will provide estimates of the acceleration with uncertainties substantially below 0.1 μas yr−1.Publicación Restringido Infrared-excess white dwarfs in the Gaia 100 pc sample(Oxford Academics: Oxford University Press, 2019-09-02) Rebassa Mansergas, A.; Solano, E.; Xu, S.; Rodrigo, C.; Jiménez Esteban, F. M.; Torres, S.; Solano, Enrique; Agencia Estatal de Investigación (AEI); Rodrigo, C. [0000-0001-6068-0077]; Xu, S. [0000-0002-8808-4282]; Jiménez Esteban, F. M. [0000-0002-6985-9476]; Solano, E. [0000-0003-1885-5130]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737We analyse the 100 pc Gaia white dwarf volume-limited sample by means of VOSA (Virtual Observatory SED Analyser) with the aim of identifying candidates for displaying infrared excesses. Our search focuses on the study of the spectral energy distribution (SED) of 3733 white dwarfs with reliable infrared photometry and GBP − GRP colours below 0.8 mag, a sample that seems to be nearly representative of the overall white dwarf population. Our search results in 77 selected candidates, 52 of which are new identifications. For each target, we apply a two-component SED fitting implemented in VOSA to derive the effective temperatures of both the white dwarf and the object causing the excess. We calculate a fraction of infrared-excess white dwarfs due to the presence of a circumstellar disc of 1.6 ± 0.2 per cent, a value that increases to 2.6 ± 0.3 per cent if we take into account incompleteness issues. Our results are in agreement with the drop in the percentage of infrared excess detections for cool (<8000 K) and hot (>20 000 K) white dwarfs obtained in previous analyses. The fraction of white dwarfs with brown dwarf companions we derive is ≃0.1–0.2 per cent.Publicación Acceso Abierto A giant exoplanet orbiting a very-low-mass star challenges planet formation models(American Association for the Advancement of Science, 2019-09-27) Morales, J. C.; Mustill, A. J.; Ribas, I.; Davies, M. B.; Reiners, A.; Bauer, F. F.; Kossakowski, D.; Herrero, Enrique; Rodríguez, E.; López González, M. J.; Rodríguez López, C.; Stock, S.; Zechmeister, M.; Luque, R.; Gesa, L.; Pedraz, S.; Baroch, D.; Sarkis, P.; Lafarga, M.; Johnson, E. N.; Anglada Escudé, G.; González Álvarez, E.; Perryman, M. A. C.; Dreizler, S.; Sarmiento, L. F.; Tal Or, L.; Labarga, F.; Reffert, S.; Rebolo, R.; Schweitzer, A.; Schäfer, S.; Hagen, H. J.; Lázaro, F. J.; Quirrenbach, A.; Perger, M.; Guenther, E. W.; Schlecker, M.; Montes, D.; Jeffers, S. V.; Cortés Contreras, M.; Kürster, M.; Schmitt, J. H. M. M.; Aceituno, Francisco José; Abellán, F. J.; Rosich, A.; Aceituno, J.; Schöfer, P.; Arroyo Torres, B.; Amado, P. J.; Antona, R.; Solano, E.; Benítez, D.; Kaminski, A.; Becerril Jarque, S.; Sota, A.; Kehr, M.; Abril, M.; Brinkmöller, M.; Béjar, V. J. S.; Ammler von Eiff, M.; Calvo Ortega, R.; Zapatero Osorio, M. R.; Barrado, D.; Cardona Guillén, C.; Yan, F.; Bergond, G.; Casanova, V.; Klahr, H.; Chaturvedi, P.; Nagel, E.; Claret, A.; Trifonov, T.; Czesla, S.; Henning, T.; Dorda, R.; Seifert, W.; Fernández Hernández, Maite; Alonso Floriano, F. J.; Azzaro, M.; Berdiñas, Z. M.; Del Burgo, C.; Cano, J.; Carro, J.; Casasayas Barris, N.; Cifuentes, C.; Colomé, J.; Díez Alonso, E.; Emsenhuber, A.; Guàrdia, J.; Guijarro, A.; De Guindos, E.; Hatzes, Artie; Hauschildt, P. H.; Hedrosa, R. P.; Hermelo, I.; Hernández Arabi, R.; Hernández Otero, F.; Hintz, D.; Klüter, J.; González Peinado, R.; González Hernández, J. I.; González Cuesta, L.; De Juan, E.; Stahl, O.; Burn, R.; Kim, M.; Fernández Martín, A.; Lara, L. M.; Mordasini, C.; Labiche, N.; Cárdenas, M. C.; Lampón, M.; Ferro, I. M.; López del Fresno, M.; Passegger, V. M.; Lizon, Jean Louis; Casal, E.; Lodieu, N.; Fuhrmeister, B.; Mancini, L.; López Santiago, J.; Kemmer, J.; Mall, U.; Galadí Enríquez, D.; Martín Fernández, P.; Marfil, E.; Lalitha, S.; Martín, Eduardo L.; Gallardo Cava, I.; Mirabet, E.; Llamas, M.; Marvin, E. L.; García Vargas, M. L.; Nortmann, L.; Magán Madinabeitia, H.; Nelson, Richard; García Piquer, A.; Pallé, E.; Marín Molina, J. A.; Pascual Granado, J.; Caballero, J. A.; Martínez Rodríguez, H.; Pérez Medialdea, D.; Huke, P.; Naranjo, V.; Rabaza, O.; Huber, A.; Ofir, A.; Redondo, P.; Holgado, G.; Rodler, F.; Klutsch, A.; Sabotta, S.; Launhardt, R.; Salz, M.; López Salas, F. J.; Sánchez Carrasco, M. A.; Mandel, H.; Sanz Forcada, J.; Martín Ruiz, S.; Moya, A.; Nowak, G.; Pavlov, Alexander; Pérez Calpena, A.; Ramón Ballesta, A.; Rix, H. W.; Rodríguez Trinidad, A.; Sadegi, S.; Sánchez Blanco, E.; Sánchez López, A.; Stürmer, J.; Suárez, J. C.; Tabernero, H. M.; Tulloch, S. M.; Veredas, G.; Vico Linares, J. I.; Vilardell, F.; Wagner, K.; Winkler, J.; Wolthoff, V.; Johansen, A.; Stuber, T.; Solano, Enrique; González Hernández, Carmen; Israel Science Foundation (ISF); Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT); Swiss National Science Foundation (SNSF); Deutsches Zentrum für Luft- und Raumfahrt (DLR); Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR); European Research Council (ERC); Generalitat de Catalunya; Deutsche Forschungsgemeinschaft (DFG); Queen Mary University of London; Consejo Nacional de Ciencia y Tecnología (CONACYT); Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737; Morales, J. C. [0000-0003-0061-518X]; Mustill, A. J. [0000-0002-2086-3642]; Ribas, I. [0000-0002-6689-0312]; Davies, M. B. [0000-0001-6080-1190]; Bauer, F. F. [0000-0003-1212-5225]; Herrrero, E. [0000-0001-8602-6639]; Rodríguez, E. [0000-0001-6827-9077]; López González, M. J. [0000-0001-8104-5128]; Rodríguez López, C. [0000-0001-5559-7850]; López González, M. J. [0000-0001-8104-5128]; Rodríguez López, C. [0000-0001-5559-7850]; Sarkis, P. [0000-0001-8128-3126]; López Santiago, J. [0000-0003-2402-8166]; Vilardell, F. [0000-0003-0441-1504]; Winkler, J. [0000-0003-0568-8820]; Nowak, G. [0000-0002-7031-7754]; Béjar, V. J. S. [0000-0002-5086-4232]; Luque, R. [0000-0002-4671-2957]; Pérez Calpena, A. [0000-0001-7361-9240]; Sota, A. [https://orcid.org/0000-0002-9404-6952]; Klahr, H. [0000-0002-8227-5467]; Mordasini, C. [0000-0002-1013-2811]; Rodler, F. [0000-0003-0650-5723]; Tabernero, H. [0000-0002-8087-4298]; Cortés Contreras, M. [0000-0003-3734-9866]; Lafarga, M. [0000-0002-8815-9416]; Sánchez López, A. [0000-0002-0516-7956]; Yan, F. [0000-0001-9585-9034]; Reffert, S. [0000-0002-0460-8289]; Rosich, A. [0000-0002-9141-3067]; Sarmiento, L. F. [0000-0002-8475-9705]; Perger, M. [0000-0001-7098-0372]; Sabotta, S. [0000-0001-9078-5574]; Guenther, E. W. [0000-0002-9130-6747]; Kaminski, A. [0000-0003-0203-8208]; Schmitt, J. H. M. M. [0000-0003-2554-9916]; Aceituno, J. [0000-0003-0487-1105]; Alonso Floriano, F. J. [0000-0003-1202-5734]; Stock, S. [0000-0002-1166-9338]; Nagel, E. [0000-0002-4019-3631]; Barrado, D. [0000-0002-5971-9242]; Tulloch, S. [0000-0003-0840-8521]; Trifonov, T. [0000-0002-0236-775X]; Bergond, G. [0000-0003-3132-9215]; Burn, R. [0000-0002-9020-7309]; Zapatero Osorio, M. R. [0000-0001-5664-2852]; Montes, D. [0000-0002-7779-238X]; Cano, J. [0000-0003-1984-5401]; Cardona Guillén, C. [0000-0002-2198-4200]; Baroch, D. [0000-0001-7568-5161]; Ammler-von Eiff, M. [0000-0001-9565-1698]; Chaturvedi, P. [0000-0002-1887-1192]; Cifuentes, C. [0000-0003-1715-5087]; Anglada Escudé, G. [0000-0002-3645-5977]; Becerril Jarque, S. [0000-0001-9009-1150]; González Cuesta, L. [0000-0002-1241-5508]; Díez Alonso, E. [0000-0002-5826-9892]; Emsenhuber, A. [0000-0002-8811-1914]; Passegger, V. M. [0000-0002-8569-7243]; García Vargas, M. L. [0000-0002-2058-3528]; González Álvarez, E. [0000-0002-4820-2053]; Amado, P. J. [0000-0002-8388-6040]; Carro, J. [0000-0002-0838-3603]; Guàrdia, J. [0000-0002-7191-9001]; Abellán, F. J. [0000-0002-5724-1636]; Colomé, J. [0000-0002-1678-2241]; Hermelo, I. [0000-0001-9178-694X]; Hintz, D. [0000-0002-5274-2589]; Arroyo Torres, B. [0000-0002-3392-4694]; Fuhrmeister, B. [0000-0001-8321-5514]; Johnson, E. [0000-0003-2260-5134]; De Juan Fernández, E. [0000-0002-9382-4505]; Berdiñas, Z. M. [0000-0002-6057-6461]; González Hernández, J. I. [0000-0002-0264-7356]; Klüter, J. [0000-0002-3469-5133]; Klutsch, A. [0000-0001-7869-3888]; Calvo Ortega, R. [0000-0003-3693-6030]; Guijarro, A. [0000-0001-5518-1759]; Aceituno, F. J. [0000-0001-8074-4760]; Lara, L. M. [0000-0002-7184-920X]; Launhardt, R. [0000-0002-8298-2663]; Casasayas Barris, N. [0000-0002-2891-8222]; López del Fresno, M. [0000-0002-9479-7780]; Magan Madinabeitia, H. [0000-0003-1243-4597]; Czesla, S. [0000-0002-4203-4773]; Kehr, M. [0000-0002-7420-7368]; Marín Molina, J. A. [0000-0002-3525-0806]; Galadí Enríquez, D. [0000-0003-4946-5653]; Labarga, F. [0000-0002-7143-0206]; Martínez Rodríguez, H. [0000-0002-1919-228X]; Marvin, C. J. [0000-0002-2249-2611]; González Peinado, R. [0000-0002-6658-8930]; Lizon, J. L. [0000-0001-8928-2566]; Naranjo, V. [0000-0003-0097-1061]; Nelson, R. [0000-0002-9687-8779]; De Guindos, E. [0000-0002-8124-9101]; Manici, L. [0000-0002-9428-8732]; Ofir, A. [0000-0002-9152-5042]; Pascual Granado, J. [0000-0003-0139-6951]; Huke, P. [0000-0001-5913-2743]; Martín, E. [0000-0002-1208-4833]; García Piquer, A. [0000-0002-6872-4262]; Rabaza, O. [0000-0003-2766-2103]; Ramón Ballesta, A. [0000-0002-4323-0610]; Kim, M. [0000-0001-6218-2004]; Rodríguez Trinidad, A. [0000-0002-3356-8634]; Sadegi, S. [0000-0001-9897-6121]; Lampón, M. [0000-0002-0183-7158]; Nortmann, L. [0000-0001-8419-8760]; Sanz Forcada, J. [0000-0002-1600-7835]; Lodieu, N. [0000-0002-3612-8968]; Pedraz, S. [0000-0003-1346-208X]; Schäfer, S. [0000-0001-8597-8048]; Schlecker, M. [0000-0001-8355-2107]; Marfil, E. [0000-0001-8907-4775]; Redondo, P. G. [0000-0001-5992-5778]; Schöfer, P. [0000-0002-5969-3708]; Solano, E. [0000-0003-1885-5130]; Martín Ruiz, S. [0000-0002-9006-7182]; Sánchez Carrasco, M. A. [0000-0001-5533-3660]; Stuber, T. [0000-0003-2185-0525]; Suárez, J. C. [0000-0003-3649-8384]; Moya, A. [0000-0003-1665-5389]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737; Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709Surveys have shown that super-Earth and Neptune-mass exoplanets are more frequent than gas giants around low-mass stars, as predicted by the core accretion theory of planet formation. We report the discovery of a giant planet around the very-low-mass star GJ 3512, as determined by optical and near-infrared radial-velocity observations. The planet has a minimum mass of 0.46 Jupiter masses, very high for such a small host star, and an eccentric 204-day orbit. Dynamical models show that the high eccentricity is most likely due to planet-planet interactions. We use simulations to demonstrate that the GJ 3512 planetary system challenges generally accepted formation theories, and that it puts constraints on the planet accretion and migration rates. Disk instabilities may be more efficient in forming planets than previously thought.Copyright © 2019 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of SciencePublicación Acceso Abierto J-PLUS: Discovery and characterisation of ultracool dwarfs using Virtual Observatory tools(EDP Sciences, 2019-06-27) Solano, E.; Martín, Eduardo L.; Caballero, J. A.; Rodrigo, C.; Angulo, R. E.; Alcaniz, J. S.; Borges Fernandes, M.; Cenarro, A. J.; Cristóbal Hornillos, D.; Dupke, R. A.; Alfaro, Emilio J.; Ederoclite, A.; Jiménez Esteban, F. M.; Hernández Jiménez, J. A.; Hernández Monteagudo, C.; Lopes de Oliveira, R.; López Sanjuan, C.; Marín Franch, A.; Mendes de Oliveira, Claudia L.; Moles, M.; Orsi, Álvaro A.; Schmidtobreick, L.; Sobral, D.; Sodré, L.; Varela, J.; Vázquez Ramió, H.; Solano, Enrique; Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq); Ministerio de Economía y Competitividad (MINECO); Agencia Estatal de Investigación (AEI); Comisión Nacional de Investigación Científica y Tecnológica (CONICYT); European Research Council (ERC); Caballero, J. A. [https://orcid.org/0000-0002-7349-1387]; Jailson Souza de Alcaniz. [https://orcid.org/0000-0003-2441-1413]; Alfaro, Emilio J. [https://orcid.org/0000-0002-2234-7035]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737Context. Ultracool dwarfs are objects with spectral types equal to or later than M7. Most of them have been discovered using wide-field imaging surveys. The Virtual Observatory has proven to be very useful for efficiently exploiting these astronomical resources. Aims. We aim to validate a Virtual Observatory methodology designed to discover and characterise ultracool dwarfs in the J-PLUS photometric survey. J-PLUS is a multiband survey carried out with the wide-angle T80Cam optical camera mounted on the 0.83 m telescope JAST/T80 in the Observatorio Astrofísico de Javalambre. We make use of the Internal Data Release covering 528 deg2. Methods. We complemented J-PLUS photometry with other catalogues in the optical and infrared using VOSA, a Virtual Observatory tool that estimates physical parameters from the spectral energy distribution fitting to collections of theoretical models. Objects identified as ultracool dwarfs were distinguished from background M giants and highly reddened stars using parallaxes and proper motions from Gaia DR2. Results. We identify 559 ultracool dwarfs, ranging from i = 16.2 mag to i = 22.4 mag, of which 187 are candidate ultracool dwarfs not previously reported in the literature. This represents an increase in the number of known ultracool dwarfs of about 50% in the region of the sky we studied, particularly at the faint end of our sensitivity, which is interesting as reference for future wide and deep surveys such as Euclid. Three candidates are interesting targets for exoplanet surveys because of their proximity (distances less than 40 pc). We also analysed the kinematics of ultracool dwarfs in our catalogue and found evidence that it is consistent with a Galactic thin-disc population, except for six objects that might be members of the thick disc. Conclusion. The results we obtained validate the proposed methodology, which will be used in future J-PLUS and J-PAS releases. Considering the region of the sky covered by the Internal Data Release used in this work, we estimate that 3000–3500 new ultracool dwarfs will be discovered at the end of the J-PLUS project.Publicación Acceso Abierto Erratum: The first planet detected in the WTS: an inflated hot-Jupiter in a 3.35 day orbit around a late F-star(Oxford Academics: Blackwell Publishing, 2020-07-28) Cappetta, M.; Saglia, R. P.; Birkby, J. L.; Koppenhoefer, J.; Pinfield, David J.; Hodgkin, S. T.; Cruz, P.; Kovács, G.; Sipocz, B.; Barrado, D.; Nefs, B.; Pavlenko, Y. V.; Fossati, L.; Del Burgo, C.; Martín, Eduardo L.; Snellen, J.; Barnes, J.; Campbell, D.; Catalan, S.; Gálvez Ortiz, M. C.; Goulding, N.; Haswell, C. A.; Ivanyuk, O.; Jones, H.; Kuznetsov, M.; Lodieu, N.; Marocco, F.; Mislis, D.; Murgas Alcaino, F.; Napiwotzki, R.; Pallé, E.; Pollacco, D.; Sarro Baro, L.; Solano, E.; Steele, P.; Stoev, H.; Tata, R.; Zendejas, J.; Solano, Enrique; 0000-0003-0987-1593Debido a su tipología(Corrección), carece de Abstract. Due to its typology, it has no Abstract. This is a correction to: Monthly Notices of the Royal Astronomical Society, Volume 427, Issue 3, December 2012, Pages 1877–1890, https://doi.org/10.1111/j.1365-2966.2012.21937.xPublicación Acceso Abierto Gaia Early Data Release 3 Structure and properties of the Magellanic Clouds(EDP Sciences, 2021-04-28) Luri, X.; Chemin, L.; Clementini, G.; Delgado, H. E.; McMillan, P. J.; Romero Gómez, M.; Balbinot, E.; Castro Ginard, A.; Mor, R.; Ripepi, V.; Sarro, L. M.; Delchambre, L.; Guerra, R.; Lobel, A.; Kochoska, A.; De March, R.; Gracia Abril, G.; Gilmore, G.; Carry, B.; Robin, A. C.; Mints, A.; Vecchiato, A.; Kruszynska, K.; Palaversa, L.; Khanna, S.; Jonker, P. G.; Manteiga, M.; Vicente, D.; Dell´Oro, A.; Del Peloso, E. F.; Bartolomé, S.; Destroffer, D.; Segol, M.; Bernet, M.; Murphy, C. P.; Martín Fleitas, J. M.; Wyrzykowski, L.; Guy, L. P.; Managau, S.; Siopis, C.; Esquej, P.; García Gutierrez, A.; Lecoeur Taibi, I.; Diakite, S.; Muinonen, K.; Leclerc, N.; Thuillot, W.; Ulla, A.; Cowell, S.; Osinde, J.; Steidelmüller, H.; Fedorets, G.; Kostrzewa Rutkowska, Z.; Pulone, L.; Comoretto, G.; Voutsinas, S.; Santoveña, R.; Richards, P. J.; Fabrizio, M.; Riva, A.; Julbe, F.; Rybizki, J.; Audard, Marc; Musella, I.; Altavilla, G.; Smith, M.; Muñoz, D.; Mazeh, T.; Giacobbe, P.; Carballo, R.; Piersimoni, A. M.; Sahlmann, J.; Mastrobuono Battisti, A.; Lindegren, L.; Barstow, M. A.; Masana, E.; Stephenson, C. A.; Biermann, M.; Muraveva, T.; Rowell, N.; Hobbs, D.; Marrese, P. M.; Boch, T.; Hauser, M.; Lindstrom, H. E. P.; Brown, A. G. A.; Ducourant, C.; Bossini, D.; Taylor, M. B.; Soubiran, C.; Hidalgo, S. L.; Sciacca, E.; Messineo, R.; Krone Martins, A.; Siltala, L.; Lanzafame, A. C.; Blanco Cuaresma, S.; Buzzi, R.; Turron, C.; Rohrbasser, L.; Bouquillon, S.; Aguado, J. J.; Robichon, N.; Plachy, E.; Lebzelter, T.; Barbato, D.; Montegriffo, P.; Bianchi, L.; David, M.; Walton, N. A.; Prsa, A.; Steele, I. A.; Pineau, F. X.; Pawlak, M.; Chaoul, Laurence; Fernández Hernández, J.; Vallenari, A.; Liao, S.; Fragkoudi, F.; Cánovas, H.; García Torres, M.; Smart, R. L.; Salgado, J.; González Núñez, J.; Noval, L.; Roelens, M.; De Luise, F.; Marconi, M.; Millar, N. R.; Re Fiorentin, P.; Cornez, T.; Ramos Lerate, M.; Blomme, R.; De Souza, R.; Jordi, C.; Souchay, J.; Thévenin, F.; Marshall, D. J.; Poujoulet, E.; Torra, J.; Galluccio, L.; De Angeli, F.; Crowley, C.; Marinoni, S.; Weiler, M.; Pourbaix, D.; De Laverny, P.; Fabre, C.; Arenou, F.; Diener, C.; Slezak, E.; Sanna, N.; Molnár, L.; Holland, G.; Szegedi Elek, E.; Drimmel, R.; Sánchez Giménez, V.; Pancino, E.; Fouron, C.; Álvarez, M. A.; Cioni, M. R. L.; Janßen, Katja; Zhao, H.; Pagano, I.; Chiavassa, A.; Geyer, R.; Panem, C.; Sartoretti, P.; Jevardat de Fombelle, G.; Abreu Aramburu, A.; Benson, K.; Rimoldini, L.; Orrù, G.; Frémat, Y.; Álvarez Cid Fuentes, J.; Casamiquela, L.; Mowlavi, N.; Castellani, M.; Gerlach, E.; Haywood, M.; Yvard, P.; Girona, S.; Di Matteo, P.; Wevers, T.; Tauran, G.; Rambaux, N.; Evans, D. W.; Ségransan, D.; Eyer, L.; Lasne, Y.; Torra, F.; Tanga, P.; Taris, F.; Süveges, M.; Karbevska, L.; Bragaglia, A.; Jordan, S.; Regibo, S.; Massari, D.; Hladczuk, N.; Nienartowicz, K.; Katz, D.; Brouillet, N.; Solano, E.; Yoldas, A.; Lebreton, Y.; Royer, F.; Schultheis, M.; Viala, Y.; Kordopatis, G.; Becciani, U.; Leccia, S.; Mora, A.; Roux, W.; Barache, C.; Sagristà Sellés, A.; Tonello, N.; Busso, G.; Bramante, S.; Abbas, U.; Sadowski, G.; García Lario, P.; Recio Blanco, A.; Le Fustec, Y.; Marcos Santos, M. M. S.; Roegiers, T.; Madrero Pardo, P.; Nicolas, C.; Castañeda, J.; Segovia, J. C.; Altmann, M.; Sozzetti, A.; Bakker, J.; Crifo, F.; Masip, A.; Di Stefano, E.; Hernández, J.; Carlucci, T.; Halbwachs, J. L.; Spoto, F.; Mignard, F.; Fabricius, C.; Riello, M.; Carnerero, M. I.; Del Pozo, E.; Baudesson Stella, A.; Dapergolas, A.; Souami, D.; Aerts, C.; Creevey, O. L.; Alves, J.; Juaristi Campillo, J.; Molinaro, R.; Ordénovic, C.; Haigron, R.; Morbidelli, R.; Livanou, E.; García Reinaldos, M.; Bellas Velidis, I.; Van Dillen, E.; Guiraud, J.; Marchal, O.; Racero, E.; Burgess, P. W.; Balog, Z.; Andrae, R.; Portell, J.; Penttilä, A.; Giuffrida, G.; Carrasco, J. M.; Samaras, N.; Pagani, C.; Anglada Varela, E.; Garofalo, A.; Granvik, M.; Pailler, F.; Gosset, E.; Raiteri, C. M.; Zorec, J.; Fouesneau, M.; Poggio, E.; Garabato, D.; Ramos, P.; Cooper, W. J.; Baker, S. G.; Fienga, A.; Zwitter, T.; Brugaletta, E.; Bertone, S.; Gómez, A.; Zurbach, C.; Breedt, E.; Babusiaux, C.; Rainer, M.; Rybicki, K. A.; David, P.; Robin, C.; Anderson, R. I.; Van Reeven, W.; Guerrier, A.; De Ridder, J.; Van Leeuwen, M.; Korn, A. J.; Salguero, E.; Lammers, U.; Cancelliere, R.; Huckle, H. E.; Busonero, D.; Sordo, R.; Pauwels, T.; Dafonte, C.; Jansen, F.; Licata, E.; Gai, M.; Lanza, A. F.; Riclet, F.; Delisle, J. B.; Lorca, A.; Dolding, C.; Peñalosa Esteller, X.; Solitro, F.; Burlacu, A.; Semeux, D.; Rixon, G.; Bressan, A.; Bauchet, N.; Damerdji, Y.; Helmi, A.; Charlot, P.; Bastian, U.; Fernique, P.; Bassilana, J. L.; Barros, M.; Szabados, L.; Morel, T.; Jasniewicz, G.; Van Leeuwen, F.; Spagna, A.; Enke, H.; Hodgkin, S. T.; Antoja, T.; Brucciarelli, B.; Vaillant, M.; Hambly, N. C.; Accart, S.; Teixeira, R.; Michalik, D.; Vanel, O.; Kontizas, M.; Faigler, S.; Heiter, U.; Bellazzini, M.; Gavras, P.; Morris, D.; Hatzidimitriou, D.; González Santamaría, I.; Löffler, W.; Unger, C.; Zucker, S.; Le Campion, J. F.; Eappachen, D.; De Torres, A.; Ajaj, M.; Klioner, S. A.; De Teodoro, P.; Poretti, E.; Lattanzi, M. G.; Osborne, Paul; Hilger, T.; Palicio, P. A.; Balaguer Núñez, L.; Crosta, M.; Lambert, S.; Moitinho, A.; Reylé, C.; Messina, S.; Randich, S.; Baines, D.; Lister, T. A.; Castro Sampol, P.; Bailer Jones, C. A. L.; Panuzzo, P.; Gutierrez Sánchez, R.; Jean Antonie Piccolo, A.; Cropper, M.; González Vidal, J. J.; Franke, F.; Bombrun, A.; Holl, B.; Kervella, P.; Martín Polo, L.; Fraile, E.; Figueras, F.; Teyssier, D.; Siddiqui, H. I.; Panahi, A.; Utrilla, E.; Seabroke, G. M.; Marchant, J. M.; Cantat Gaudin, T.; Hutton, A.; Cheek, N.; Butkevich, A. G.; Delgado, A.; Berthier, J.; Sarasso, M.; Davidson, M.; Plum, G.; Marocco, F.; Caffau, E.; Molina, D.; Siebert, A.; Prusti, T.; Mulone, A. F.; De Bruijne, J. H. J.; Cellino, A.; Harrison, D. L.; Ragaini, S.; Mann, R. G.; Manteiga, Minia; Solano, Enrique; Forderung der wissenschaftlichen Forschung (FWF); Belgian federal Science Policy Office (BELSPO); Hertha Firnberg Programme; Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP); Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES); Comite Francais d'Evaluation de la Cooperation Universitaire et Scientifique avec le Bresil (COFECUB); National Natural Science Foundation of China (NSFC); China Scholarship Council (CSC); European Commission (EC); European Research Council (ERC); Agence Nationale de la Recherche (ANR); European Space Agency (ESA); Centre National D'Etudes Spatiales (CNES); Istituto Nazionale di Astrofisica (INAF); Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR); Narodowe Centrum Nauki (NCN); Fundacao para a Ciencia e a Tecnologia (FCT); Slovenian Research Agency; Agencia Estatal de Investigación (AEI); Xunta de Galicia; Universitat de Barcelona (UB); Generalitat de Catalunya; Swedish National Space Agency (SNSA); United Kingdom Science and Technology Facilities Council (STFC); Krone Martins, A. [0000-0002-2308-6623]; Seabroke, G. [0000-0003-4072-9536]; Chiavassa, A. [0000-0003-3891-7554]; Castro Ginard, A. [0000-0002-9419-3725]; McMillan, P. [0000-0002-8861-2620]; Siltala, L. [0000-0002-6938-794X]; Delise, J. B. [0000-0001-5844-9888]; Aerts, C. [0000-0003-1822-7126]; Fedorets, G. [0000-0002-8418-4809]; Centro de Excelencia Científica Severo Ochoa, Instituto de Ciencias del Cosmos de la Universidad de Barcelona, SEV2015-0493; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2014-0369Context. This work is part of the Gaia Data Processing and Analysis Consortium papers published with the Gaia Early Data Release 3 (EDR3). It is one of the demonstration papers aiming to highlight the improvements and quality of the newly published data by applying them to a scientific case. Aims. We use the Gaia EDR3 data to study the structure and kinematics of the Magellanic Clouds. The large distance to the Clouds is a challenge for the Gaia astrometry. The Clouds lie at the very limits of the usability of the Gaia data, which makes the Clouds an excellent case study for evaluating the quality and properties of the Gaia data. Methods. The basis of our work are two samples selected to provide a representation as clean as possible of the stars of the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC). The selection used criteria based on position, parallax, and proper motions to remove foreground contamination from the Milky Way, and allowed the separation of the stars of both Clouds. From these two samples we defined a series of subsamples based on cuts in the colour-magnitude diagram; these subsamples were used to select stars in a common evolutionary phase and can also be used as approximate proxies of a selection by age. Results. We compared the Gaia Data Release 2 and Gaia EDR3 performances in the study of the Magellanic Clouds and show the clear improvements in precision and accuracy in the new release. We also show that the systematics still present in the data make the determination of the 3D geometry of the LMC a difficult endeavour; this is at the very limit of the usefulness of the Gaia EDR3 astrometry, but it may become feasible with the use of additional external data. We derive radial and tangential velocity maps and global profiles for the LMC for the several subsamples we defined. To our knowledge, this is the first time that the two planar components of the ordered and random motions are derived for multiple stellar evolutionary phases in a galactic disc outside the Milky Way, showing the differences between younger and older phases. We also analyse the spatial structure and motions in the central region, the bar, and the disc, providing new insightsinto features and kinematics. Finally, we show that the Gaia EDR3 data allows clearly resolving the Magellanic Bridge, and we trace the density and velocity flow of the stars from the SMC towards the LMC not only globally, but also separately for young and evolved populations. This allows us to confirm an evolved population in the Bridge that is slightly shift from the younger population. Additionally, we were able to study the outskirts of both Magellanic Clouds, in which we detected some well-known features and indications of new ones.Publicación Acceso Abierto J-PLUS: The Javalambre Photometric Local Universe Survey(EDP Sciences, 2019-02-21) Cenarro, A. J.; Moles, M.; Cristóbal Hornillos, D.; Marín Franch, A.; Ederoclite, A.; Varela, J.; López Sanjuan, C.; Hernández Monteagudo, C.; Angulo, R. E.; Vázquez Ramió, H.; Viironen, K.; Díaz Martín, M. C.; Beers, T. C.; Domínguez Martínez, M.; Rueda Teruel, F.; Garzarán Calderaro, J.; Iñiguez, C.; Tilve, V.; Jiménez Ruiz, J. M.; Lasso Cabrera, N.; Alcaniz, J. S.; Mendes de Oliveira, Claudia L.; López Alegre, G.; Muniesa, D. J.; Lopes de Oliveira, R.; Tamm, A.; Rodríguez Llano, S.; Rueda Teruel, S.; Akras, S.; Alfaro, Emilio J.; Soriano Laguía, I.; Valdivielso, L.; Lyman, J. D.; Beasley, M. A.; Borges Fernandes, M.; Yanes Díaz, A.; Sodré, L.; Carrasco, J. M.; Coelho, P. R. T.; Xavier, H. S.; Costa Duarte, M. V.; Abramo, L. R.; Álvarez Candal, A.; Galarza, A.; Galbany, L.; Ascaso, B.; Bruzual, G.; González Serrano, J. I.; Gutiérrez Soto, L. A.; Buzzo, M. L.; Cepa, J.; Kuncarayakti, H.; Landim, R. C. G.; Cortesi, A.; De Prá, M.; Orsi, Álvaro A.; Lima Neto, G. B.; Maíz Apellániz, J.; Favole, G.; García, K.; Nogueira Cavalcante, J. P.; González Delgado, R. M.; Hernández Jiménez, J. A.; Oteo Gómez, I.; Kanaan, A.; Laur, J.; Rebassa-Mansergas, A.; Reis, R. R. R.; Lincandro, J.; Miralda Escudé, J.; Salvador Rusiñol, N.; Sampedro, L.; Morate, D.; Novais, P. M.; Schmidtobreick, L.; Siffert, B. B.; Oncins, M.; Overzier, R. A.; Molino, A.; Bonoli, S.; Hurier, G.; Pereira, C. B.; Roig, F.; Vilella-Rojo, G.; Sako, M.; Sánchez Blázquez, Patricia; Gurung López, S.; Santos, W. A.; Telles, E.; Allende Prieto, C.; Bonatto, C.; Vilchez, J. M.; San Roman, I.; Daflon, S.; Dupke, R. A.; Greisel, N.; Díaz García, L. A.; Jiménez Teja, Y.; Placco, V. M.; Logroño García, R.; Spinoso, D.; Maícas, N.; Izquierdo Villalba, D.; Abril, J.; Aguerri, J. A. L.; Carvano, J. M.; Bielsa de Toledo, S.; Chies Santos, A. L.; Falcón Barroso, J.; Civera, T.; Gonçalves, D. R.; Solano, E.; Hernández Fuertes, J.; Iglesias Marzoa, R.; Whitten, D. D.; Antón, J. L.; Kruuse, K.; Lamadrid, J. L.; Bello, R.; Castillo Ramírez, J.; López Sainz, A.; Moreno Signes, A.; Chueca, S.; Díaz García, Pedro; Solano, Enrique; Gobierno de Aragón; European Commission (EC); Conselho Nacional de Desenvolvimento Científico e Tecnológico; Financiadora de Estudos e Projetos (FINEP); Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP); Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ); Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES); National Science Foundation (NSF); Ministerio de Economía y Competitividad (MINECO); 0000-0002-2573-2342; Jailson Souza de Alcaniz. [https://orcid.org/0000-0003-2441-1413]; Coelho, P. R. T. [0000-0003-1846-4826]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737The Javalambre Photometric Local Universe Survey (J-PLUS ) is an ongoing 12-band photometric optical survey, observing thousands of square degrees of the Northern Hemisphere from the dedicated JAST/T80 telescope at the Observatorio Astrofísico de Javalambre (OAJ). The T80Cam is a camera with a field of view of 2 deg2 mounted on a telescope with a diameter of 83 cm, and is equipped with a unique system of filters spanning the entire optical range (3500–10 000 Å). This filter system is a combination of broad-, medium-, and narrow-band filters, optimally designed to extract the rest-frame spectral features (the 3700–4000 Å Balmer break region, Hδ, Ca H+K, the G band, and the Mg b and Ca triplets) that are key to characterizing stellar types and delivering a low-resolution photospectrum for each pixel of the observed sky. With a typical depth of AB ∼21.25 mag per band, this filter set thus allows for an unbiased and accurate characterization of the stellar population in our Galaxy, it provides an unprecedented 2D photospectral information for all resolved galaxies in the local Universe, as well as accurate photo-z estimates (at the δ z/(1 + z)∼0.005–0.03 precision level) for moderately bright (up to r ∼ 20 mag) extragalactic sources. While some narrow-band filters are designed for the study of particular emission features ([O II]/λ3727, Hα/λ6563) up to z < 0.017, they also provide well-defined windows for the analysis of other emission lines at higher redshifts. As a result, J-PLUS has the potential to contribute to a wide range of fields in Astrophysics, both in the nearby Universe (Milky Way structure, globular clusters, 2D IFU-like studies, stellar populations of nearby and moderate-redshift galaxies, clusters of galaxies) and at high redshifts (emission-line galaxies at z ≈ 0.77, 2.2, and 4.4, quasi-stellar objects, etc.). With this paper, we release the first ∼1000 deg2 of J-PLUS data, containing about 4.3 million stars and 3.0 million galaxies at r < 21 mag. With a goal of 8500 deg2 for the total J-PLUS footprint, these numbers are expected to rise to about 35 million stars and 24 million galaxies by the end of the survey.Publicación Acceso Abierto A Catalog of Wide Binary and Multiple Systems of Bright Stars from Gaia-DR2 and the Virtual Observatory(American Astronomical Society, 2019) Jiménez Esteban, F. M.; Solano, E.; Rodrigo, C.; Solano, EnriqueBinary and multiple stars have long provided an effective empirical method of testing stellar formation and evolution theories. In particular, the existence of wide binary systems (separations >20,000 au) is particularly challenging to binary formation models as their physical separations are beyond the typical size of a collapsing cloud core (∼5000-10,000 au). We mined the recently published Gaia-DR2 catalog to identify bright comoving systems in the five-dimensional space (sky position, parallax, and proper motion). We identified 3741 comoving binary and multiple stellar candidate systems, out of which 575 have compatible radial velocities for all the members of the system. The candidate systems have separations between ∼400 and 500,000 au. We used the analysis tools of the Virtual Observatory to characterize the comoving system members and to assess their reliability. The comparison with previous comoving systems catalogs obtained from TGAS showed that these catalogs contain a large number of false systems. In addition, we were not able to confirm the ultra-wide binary population presented in these catalogs. The robustness of our methodology is demonstrated by the identification of well known comoving star clusters and by the low contamination rate for comoving binary systems with projected physical separations <50,000 au. These last constitute a reliable sample for further studies. The catalog is available online at the Spanish Virtual Observatory portal (http://svo2.cab.inta-csic.es/vocats/v2/comovingGaiaDR2/).Publicación Restringido The Gran Telescopio Canarias OSIRIS broad-band first data release(Oxford Academics: Oxford University Press, 2020-01-05) Cortés Contreras, M.; Bouy, H.; Solano, E.; Mahlke, M.; Jiménez Esteban, F. M.; Alacid, J. M.; Rodrigo, C.; Solano, Enrique; European Space Agency (ESA); Agencia Estatal de Investigación (AEI); European Research Council (ERC); Cortés Contreras, M. [0000-0003-3734-9866]; Rodrigo, C. [0000-0001-6068-0077]; Solano, E. [0000-0003-1885-5130]; Jiménez Esteban, F. M. [0000-0002-6985-9476]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737We present the first release of GTC OSIRIS broad-band data archive. This is an effort conducted in the framework of the Spanish Virtual Observatory to help optimize science from the Gran Telescopio Canarias Archive. Data Release 1 includes 6788 broad-band images in the Sloan griz filters obtained between 2009 April and 2014 January and the associated catalogue with roughly 6.23 million detections of more than 630 000 unique sources. The catalogue contains standard PSF and Kron aperture photometry with a mean accuracy better than 0.09 and 0.15 mag, respectively. The relative astrometric residuals are always better than 30 mas and better than 15 mas in most cases. The absolute astrometric uncertainty of the catalogue is of 0.12 arcsec. In this paper we describe the procedure followed to build the image archive and the associated catalogue, as well as the quality tests carried out for validation. To illustrate some of the scientific potential of the catalogue, we also provide two examples of its scientific exploitation: discovery and identification of asteroids and cool dwarfs.Publicación Acceso Abierto The CARMENES search for exoplanets around M dwarfs: Measuring precise radial velocities in the near infrared: The example of the super-Earth CD Cet b(EDP Sciences, 2020-08-10) Bauer, F. F.; Zechmeister, M.; Kaminski, A.; Rodríguez López, C.; Caballero, J. A.; Azzaro, M.; Stahl, S.; Kossakowski, D.; Quirrenbach, A.; Becerril Jarque, S.; Rodríguez, E.; Amado, P. J.; Seifert, W.; Reiners, A.; Schäfer, S.; Ribas, I.; Béjar, V. J. S.; Cortés Contreras, M.; Dreizler, S.; Hatzes, Artie; Henning, T.; Jeffers, S. V.; Kürster, M.; Lafarga, M.; Montes, D.; Morales, J. C.; Schmitt, H. M. M.; Schweitzer, A.; Solano, E.; Solano, Enrique; European Research Council (ERC); Agencia Estatal de Investigación (AEI); Ministerio de Economía y Competitividad (MINECO); Deutsche Forschungsgemeinschaft (DFG); 0000-0003-1212-5225; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737; Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709; Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFÍSICA DE CANARIAS (IAC), SEV-2015-0548The high-resolution, dual channel, visible and near-infrared spectrograph CARMENES offers exciting opportunities for stellar and exoplanetary research on M dwarfs. In this work we address the challenge of reaching the highest radial velocity precision possible with a complex, actively cooled, cryogenic instrument, such as the near-infrared channel. We describe the performance of the instrument and the work flow used to derive precise Doppler measurements from the spectra. The capability of both CARMENES channels to detect small exoplanets is demonstrated with the example of the nearby M5.0 V star CD Cet (GJ 1057), around which we announce a super-Earth (4.0 ± 0.4 M· ) companion on a 2.29 d orbit. © 2020 ESO.
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