Persona: Solano, Enrique
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Centro de Astrobiologia
El Centro de Astrobiología (CAB) es un centro mixto de investigación en astrobiología, dependiente tanto del Instituto Nacional de Técnica Aeroespacial (INTA) como del Consejo Superior de Investigaciones Científicas (CSIC).
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Publicación Restringido A Catalog of Wide Binary and Multiple Systems of Bright Stars from Gaia-DR2 and the Virtual Observatory(The Institute of Physics (IOP), 2019-01-28) Jiménez Esteban, F. M.; Solano, Enrique; Rodrigo, C.; Ministerio de Economía y Competitividad (MINECO); Agencia Estatal de Investigación (AEI); European Research Council (ERC); Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737Binary 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 Acceso Abierto The CARMENES search for exoplanets around M dwarfs: Dynamical characterization of the multiple planet system GJ 1148 and prospects of habitable exomoons around GJ 1148 b(EDP Sciences, 2020-06-03) Trifonov, T.; Lee, M. H.; Kürster, M.; Henning, T.; Grishin, E.; Stock, S.; Tjoa, J.; Caballero, J. A.; Wong, K. H.; Bauer, F. F.; Quirrenbach, A.; Zechmeister, M.; Ribas, I.; Reffert, S.; Reiners, A.; Amado, P. J.; Kossakowski, D.; Azzaro, M.; Béjar, V. J. S.; Cortés Contreras, M.; Dreizler, S.; Hatzes, Artie; Jeffers, S. V.; Kaminski, A.; Lafarga, M.; Montes, D.; Morales, J. C.; Pavlov, Alexander; Rodríguez López, C.; Schmitt, H. M. M.; Solano, Enrique; Barnes, R.; Deutsche Forschungsgemeinschaft (DFG); Ministerio de Economía y Competitividad (MINECO); Junta de Andalucía; European Research Council (ERC); Agencia Estatal de Investigación (AEI); Trifonov, T. https://orcid.org/0000-0002-0236-775X; 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 ASTROFÍSICA DE CANARIAS (IAC), SEV-2015-0548; Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709Context. GJ 1148 is an M-dwarf star hosting a planetary system composed of two Saturn-mass planets in eccentric orbits with periods of 41.38 and 532.02 days. Aims. We reanalyze the orbital configuration and dynamics of the GJ 1148 multi-planetary system based on new precise radial velocity measurements taken with CARMENES. Methods. We combined new and archival precise Doppler measurements from CARMENES with those available from HIRES for GJ 1148 and modeled these data with a self-consistent dynamical model. We studied the orbital dynamics of the system using the secular theory and direct N-body integrations. The prospects of potentially habitable moons around GJ 1148 b were examined. Results. The refined dynamical analyses show that the GJ 1148 system is long-term stable in a large phase-space of orbital parameters with an orbital configuration suggesting apsidal alignment, but not in any particular high-order mean-motion resonant commensurability. GJ 1148 b orbits inside the optimistic habitable zone (HZ). We find only a narrow stability region around the planet where exomoons can exist. However, in this stable region exomoons exhibit quick orbital decay due to tidal interaction with the planet. Conclusions. The GJ 1148 planetary system is a very rare M-dwarf planetary system consisting of a pair of gas giants, the inner of which resides in the HZ. We conclude that habitable exomoons around GJ 1148 b are very unlikely to exist. © 2020 T. Trifonov et al.Publicación Acceso Abierto The miniJPAS survey: star-galaxy classification using machine learning(EDP Sciences, 2021-01-18) Baqui, P. O.; Marra, V.; Casarini, L.; Angulo, R.; Díaz García, L. A.; Hernández Monteagudo, C.; Lopes, P. A. A.; López Sanjuan, C.; Muniesa, D. J.; Placco, V. M.; Quartin, M.; Queiroz, C.; Sobral, D.; Solano, Enrique; Tempel, E.; Varela, J.; Vílchez, J. M.; Abramo, L. R.; Alcaniz, J. S.; Benítez, N.; Bonoli, S.; Carneiro, S.; Cenarro, A. J.; Cristóbal Hornillos, D.; De Amorim, A. L.; De Oliveira, C. M.; Dupke, R. A.; Ederoclite, A.; González Delgado, R. M.; Marín Franch, A.; Moles, M.; Vázquez Ramió, H.; Sodré, L.; Taylor, K.; European Commission (EC); Agencia Estatal de Investigación (AEI); Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES); Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq); Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP); Gobierno de Aragón; Ministerio de Ciencia e Innovación (MICINN); Ministerio de Economía y Competitividad (MINECO); Ministry of Education, Culture, Sports, Science and Technology (MEXT); 0000-0002-7773-1579Context. Future astrophysical surveys such as J-PAS will produce very large datasets, the so-called “big data”, which will require the deployment of accurate and efficient machine-learning (ML) methods. In this work, we analyze the miniJPAS survey, which observed about ∼1 deg2 of the AEGIS field with 56 narrow-band filters and 4 ugri broad-band filters. The miniJPAS primary catalog contains approximately 64 000 objects in the r detection band (magAB ≲ 24), with forced-photometry in all other filters. Aims. We discuss the classification of miniJPAS sources into extended (galaxies) and point-like (e.g., stars) objects, which is a step required for the subsequent scientific analyses. We aim at developing an ML classifier that is complementary to traditional tools that are based on explicit modeling. In particular, our goal is to release a value-added catalog with our best classification. Methods. In order to train and test our classifiers, we cross-matched the miniJPAS dataset with SDSS and HSC-SSP data, whose classification is trustworthy within the intervals 15 ≤ r ≤ 20 and 18.5 ≤ r ≤ 23.5, respectively. We trained and tested six different ML algorithms on the two cross-matched catalogs: K-nearest neighbors, decision trees, random forest (RF), artificial neural networks, extremely randomized trees (ERT), and an ensemble classifier. This last is a hybrid algorithm that combines artificial neural networks and RF with the J-PAS stellar and galactic loci classifier. As input for the ML algorithms we used the magnitudes from the 60 filters together with their errors, with and without the morphological parameters. We also used the mean point spread function in the r detection band for each pointing. Results. We find that the RF and ERT algorithms perform best in all scenarios. When the full magnitude range of 15 ≤ r ≤ 23.5 is analyzed, we find an area under the curve AUC = 0.957 with RF when photometric information alone is used, and AUC = 0.986 with ERT when photometric and morphological information is used together. When morphological parameters are used, the full width at half maximum is the most important feature. When photometric information is used alone, we observe that broad bands are not necessarily more important than narrow bands, and errors (the width of the distribution) are as important as the measurements (central value of the distribution). In other words, it is apparently important to fully characterize the measurement. Conclusions. ML algorithms can compete with traditional star and galaxy classifiers; they outperform the latter at fainter magnitudes (r ≳ 21). We use our best classifiers, with and without morphology, in order to produce a value-added catalog.Publicación Acceso Abierto Homogeneous study of Herbig Ae/Be stars from spectral energy distributions and Gaia EDR3(EDP Sciences, 2021-06-25) Guzmán Díaz, J.; Mendigutía, I.; Montesinos Comino, B.; Oudmaijer, R. D.; Vioque, M.; Rodrigo, C.; Solano, Enrique; Meeus, G.; Marcos Arenal, P.; Comunidad de Madrid; Agencia Estatal de Investigación (AEI); European Research Council (ERC)Context. Herbig Ae/Be stars (HAeBes) have so far been studied based on relatively small samples that are scattered throughout the sky. Their fundamental stellar and circumstellar parameters and statistical properties were derived with heterogeneous approaches before Gaia. Aims. Our main goal is to contribute to the study of HAeBes from the largest sample of such sources to date, for which stellar and circumstellar properties have been determined homogeneously from the analysis of the spectral energy distributions (SEDs) and Gaia EDR3 parallaxes and photometry. Methods. Multiwavelength photometry was compiled for 209 bona fide HAeBes for which Gaia EDR3 distances were estimated. Using the Virtual Observatory SED Analyser (VOSA), photospheric models were fit to the optical SEDs to derive stellar parameters, and the excesses at infrared (IR) and longer wavelengths were characterized to derive several circumstellar properties. A statistical analysis was carried out to show the potential use of such a large dataset. Results. The stellar temperature, luminosity, radius, mass, and age were derived for each star based on optical photometry. In addition, their IR SEDs were classified according to two different schemes, and their mass accretion rates, disk masses, and the sizes of the inner dust holes were also estimated uniformly. The initial mass function fits the stellar mass distribution of the sample within 2 < M*∕M⊙ < 12. In this aspect, the sample is therefore representative of the HAeBe regime and can be used for statistical purposes when it is taken into account that the boundaries are not well probed. Our statistical study does not reveal any connection between the SED shape from the Meeus et al. (2001, A&A, 365, 476) classification and the presence of transitional disks, which are identified here based on the SEDs that show an IR excess starting at the K band or longer wavelengths. In contrast, only ~28% of the HAeBes have transitional disks, and the related dust disk holes are more frequent in HBes than in HAes (~34% vs. 15%). The relatively small inner disk holes and old stellar ages estimated for most transitional HAes indicate that photoevaporation cannot be the main mechanism driving disk dissipation in these sources. In contrast, the inner disk holes and ages of most transitional HBes are consistent with the photoevaporation scenario, although these results alone do not unambiguously discard other disk dissipation mechanisms.Conclusions. The complete dataset is available online through a Virtual Observatory-compliant archive, representing the most recent reference for statistical studies on the HAeBe regime. VOSA is a complementary tool for the future characterization of newly identified HAeBes.Publicación Acceso Abierto Gaia Early Data Release 3 The Galactic anticentre(EDP Sciences, 2021-04-28) Antoja, T.; McMillan, P. J.; Kordopatis, G.; Ramos, P.; Helmi, A.; Balbinot, E.; Cantat Gaudin, T.; Chemin, L.; Figueras, F.; Jordi, C.; Khanna, S.; Marchal, O.; Pineau, F. X.; Taris, F.; Fabricius, C.; Salgado, J.; Pawlak, M.; Davidson, M.; Lobel, A.; Anglada Varela, E.; Rowell, N.; Evans, D. W.; Marinoni, S.; Busonero, D.; Ripepi, V.; Segovia, J. C.; Burlacu, A.; Randich, S.; Hodgkin, S. T.; Fabrizio, M.; Sciacca, E.; Hambly, N. C.; Kochoska, A.; Regibo, S.; Franke, F.; García Lario, P.; Lasne, Y.; Messineo, R.; Robin, C.; Anderson, R. I.; Kontizas, M.; Fienga, A.; Lecoeur Taibi, I.; Palicio, P. A.; Roelens, M.; Walton, N. A.; Garabato, D.; Fedorets, G.; Recio Blanco, A.; Jansen, F.; Le Fustec, Y.; Kostrzewa Rutkowska, Z.; Muraveva, T.; Hidalgo, S. L.; Montegriffo, P.; Gilmore, G.; García Gutierrez, A.; Baines, D.; Baker, S. G.; Balaguer Núñez, L.; Balog, Z.; Barbato, D.; Bauchet, N.; Bertone, S.; Siebert, A.; González Vidal, J. J.; Breedt, E.; Steele, I. A.; Jasniewicz, G.; Tauron, C.; Osborne, Paul; Carlucci, T.; Brown, A. G. A.; Korn, A. J.; Biermann, M.; Busso, G.; Jonker, P. G.; Ducourant, C.; Sarro, L. M.; Altavilla, G.; Sanna, V.; Delgado, A.; Crifo, F.; Kervella, P.; Fernández Hernández, J.; Spoto, F.; Katz, D.; Drimmel, R.; Harrison, D. L.; Aerts, C.; Segol, M.; De Torres, A.; Bakker, J.; Geyer, R.; Masana, E.; Andrae, R.; Klioner, S. A.; Diener, C.; Marchant, J. M.; Seabroke, G. M.; Creevey, O. L.; Viala, Y.; Mora, A.; Abbas, U.; Slezak, E.; Teixeira, R.; De Luise, F.; Bailer Jones, C. A. L.; Enke, H.; Pailler, F.; Royer, F.; Gutiérrez Sánchez, R.; Guiraud, J.; Brugaletta, E.; Granvik, M.; Richards, P. J.; Carballo, R.; Bassilana, J. L.; Weiler, M.; Butkevich, A. G.; Marcos Santos, M. M. S.; Messina, S.; Babusiaux, C.; Pulone, L.; Vallenari, A.; Mowlavi, N.; Eappachen, D.; Plachy, E.; Massari, D.; Ramos Lerate, M.; Nicolas, C.; Hutton, A.; Ordénovic, C.; Martín Fleitas, J. M.; Crosta, M.; Sartoretti, P.; Arenou, F.; Poggio, E.; Lattanzi, M. G.; Orrù, G.; Morbidelli, R.; Mints, A.; Rambaux, N.; Prsa, A.; Giacobbe, P.; De Bruijne, J. H. J.; Fernique, P.; Fraile, E.; García Torres, M.; Cellino, A.; Giuffrida, G.; Garía Reinaldos, M.; Soubiran, C.; Siopis, C.; Cornez, T.; Hladczuk, N.; Jevardat de Fombelle, G.; Plum, G.; Cheek, N.; Hauser, M.; Van Reeven, W.; De Laverny, P.; Diakite, S.; Altmann, M.; Lister, T. A.; González Núñez, J.; Piersimoni, A. M.; Bramante, L.; Abreu Aramburu, A.; Smith, M.; Blanco Cuaresma, S.; Delgado, H. E.; Blomme, R.; Liao, S.; Jordan, S.; Mor, R.; Álvarez, M. A.; Bartolomé, S.; Lorca, A.; Mann, R. G.; Janßen, Katja; Manteiga, M.; Halbwachs, J. L.; Brouillet, N.; Del Peloso, E. F.; Clementini, G.; Haigron, R.; Lebzelter, T.; Roegiers, T.; Marconi, M.; Panuzzo, P.; Musella, I.; Ajaj, M.; Salguero, E.; Mazeh, T.; Crowley, C.; Lindstrom, H. E. P.; Fragkoudi, F.; Heiter, U.; Lammers, U.; Delisle, J. B.; Van Leeuwen, F.; Berthier, J.; Castañeda, J.; Álvarez Cid Fuentes, J.; Marrese, P. M.; Vicente, D.; Pourbaix, D.; Fouesneau, M.; Alves, J.; Solitro, F.; Cowell, S.; Mignard, F.; Riello, M.; Robin, A. C.; Zucker, S.; Sozzetti, A.; Utrilla, E.; Ségransan, D.; Sarasso, M.; Marocco, F.; Marshall, D. J.; Martín Polo, L.; Masip, A.; Kruszynska, K.; Molina, D.; Bianchi, L.; Morris, D.; Souami, D.; Tauran, G.; Molinero, R.; Pagani, C.; Carrasco, J. M.; Prusti, T.; Chaoul, Laurence; Lanzafame, A. C.; De March, R.; Lebreton, Y.; Managau, S.; Barstow, M. A.; Poretti, E.; Unger, N.; Girona, S.; Del Pozo, E.; Charlot, P.; Gavras, P.; Livanou, E.; Becciani, U.; Re Fiorentin, P.; De Teodoro, P.; Bressan, A.; Panahi, A.; Comoretto, G.; Hilger, T.; Carnerero, M. I.; Rimoldini, L.; Buzzi, R.; González Santamaría, I.; Licata, E.; Boch, T.; Rainer, M.; David, M.; Rohrbasser, L.; Audard, Marc; Solano, Enrique; Di Matteo, P.; Gracia Abril, G.; Smart, R. L.; Lambert, S.; Creylé, C.; Cancelliere, R.; Murphy, C. P.; Teyssier, D.; Ulla, A.; Baudesson Stella, A.; Casamiquela, L.; Distefano, E.; Chiavassa, A.; Haztdimitriou, D.; Thévenin, F.; Dolding, C.; Delchambre, L.; Rybizki, J.; Pancino, E.; Dafonte, C.; Dapergolas, A.; Hernández, J.; De Ridder, J.; Caffau, E.; Faigler, S.; Rybicki, K. A.; Sadowski, G.; Sagristà Sellés, A.; Sahlmann, J.; Samaras, N.; Schultheis, M.; Garofalo, A.; Siddiqui, H. I.; Dell´Oro, A.; Gosset, E.; Spagna, A.; Holland, G.; Krone Martins, A.; Juaristi Campillo, J.; Castro Ginard, A.; Romero Gómez, M.; Ragaini, S.; Robichon, N.; Fouron, C.; Zurbach, C.; Morel, T.; Löffler, W.; Leccia, S.; Molnár, L.; Riva, A.; Gai, M.; Frémat, Y.; Panem, C.; Gómez, A.; Moitinho, A.; Osinde, J.; Hobbs, D.; Julbe, F.; Guy, L. P.; Muñoz, D.; Michalik, D.; Gerlach, E.; De Angeli, F.; Le Campion, J. F.; Nienartowicz, K.; Van Leeuwen, M.; Madrero Pardo, P.; Millar, N. R.; Damerdji, Y.; Pojoulet, E.; Guerrier, A.; Haywood, M.; Cooper, W. J.; Barros, M.; De Souza, R.; Huckle, H. E.; Burgess, P. W.; Karbevska, L.; Bellazzini, M.; Barache, C.; Bellas Velidis, I.; Bouquillon, S.; David, P.; Fabre, C.; Lanza, A. F.; Cánovas, H.; Leclerc, N.; Bagaglia, A.; Bernet, M.; Riclet, F.; Roux, W.; Sordo, R.; Tanga, P.; Portell, J.; Benson, K.; Carry, B.; Mulone, A. F.; Bucciarelli, B.; Galluccio, L.; Palaversa, L.; Castellani, M.; Peñalosa Esteller, X.; Luri, X.; Holl, B.; Muinonen, K.; Mastrobuono Battisti, A.; Destroffer, D.; Semeux, D.; Castro Sampol, P.; Raiteri, C. M.; Cropper, M.; Jean Antonie Piccolo, A.; Esquej, P.; Eyer, L.; Pauwels, T.; Cioni, M. R. L.; Souchay, J.; Pagano, I.; Penttilä, A.; Noval, L.; Siltala, L.; Guerra, R.; Bastian, U.; Accart, S.; Racero, E.; Bossini, D.; Rixon, G.; Santoveña, R.; Bombrun, A.; Zwitter, T.; Aguado, J. J.; Sánchez Giménez, V.; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MINECO/ICTI2013-2016/MDM-2014-0369; Centrode Excelencia Científica Instituto de Ciencias del Cosmos Universidad de Barcelona, MINECO/ICTI2013-2016/SEV2015-0493; Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP); Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES); National Natural Science Foundation of China (NSFC); Estonian Ministry of Education and Research; Centre National D'Etudes Spatiales (CNES); Agence Nationale de la Recherche (ANR); Centre National de la Recherche Scientifique (CNRS); European Commission (EC); European Research Council (ERC); Institut des Sciences de l'Univers (INSU); Institut National Polytechnique (INP); Institut National de Physique nucleaire et de Physique des Particules (IN2P3); Deutsches Zentrum für Luft- und Raumfahrt (DLR); Hungarian Academy of Sciences; Hungarian National Research, Development, and Innovation Office (NKFIH); Science Foundation Ireland (SFI); Israel Science Foundation (ISF); Agenzia Spaziale Italiana (ASI); Italian Istituto Nazionale di Astrofisica (INAF); Netherlands Organisation for Scientific Research (NWO); Polish National Science Centre; Ministry of Science and Higher Education (MNiSW); Fundacao para a Ciencia e a Tecnologia (FCT); Slovenian Research Agency; Xunta de Galicia; Agencia Estatal de Investigación (AEI); Generalitat de Catalunya; United Kingdom Science and Technology Facilities Council (STFC); United Kingdom Space Agency (UKSA); Krone Martins, A. [0000-0002-2308-6623]; McMillan, P. [0000-0002-8861-2620]; Carrasco Martínez, J. P. [0000-0002-3029-5853]; Sozzetti, A. [0000-0002-7504-365X]; Centros de Excelencia Severo Ochoa, BARCELONA SUPERCOMPUTING CENTER (BSC), SEV2015-0493Aims. We aim to demonstrate the scientific potential of the Gaia Early Data Release 3 (EDR3) for the study of different aspects of the Milky Way structure and evolution and we provide, at the same time, a description of several practical aspects of the data and examples of their usage. Methods. We used astrometric positions, proper motions, parallaxes, and photometry from EDR3 to select different populations and components and to calculate the distances and velocities in the direction of the anticentre. In this direction, the Gaia astrometric data alone enable the calculation of the vertical and azimuthal velocities; also, the extinction is relatively low compared to other directions in the Galactic plane. We then explore the disturbances of the current disc, the spatial and kinematical distributions of early accreted versus in situ stars, the structures in the outer parts of the disc, and the orbits of open clusters Berkeley 29 and Saurer 1. Results. With the improved astrometry and photometry of EDR3, we find that: (i) the dynamics of the Galactic disc are very complex with oscillations in the median rotation and vertical velocities as a function of radius, vertical asymmetries, and new correlations, including a bimodality with disc stars with large angular momentum moving vertically upwards from below the plane, and disc stars with slightly lower angular momentum moving preferentially downwards; (ii) we resolve the kinematic substructure (diagonal ridges) in the outer parts of the disc for the first time; (iii) the red sequence that has been associated with the proto-Galactic disc that was present at the time of the merger with Gaia-Enceladus-Sausage is currently radially concentrated up to around 14 kpc, while the blue sequence that has been associated with debris of the satellite extends beyond that; (iv) there are density structures in the outer disc, both above and below the plane, most probably related to Monoceros, the Anticentre Stream, and TriAnd, for which the Gaia data allow an exhaustive selection of candidate member stars and dynamical study; and (v) the open clusters Berkeley 29 and Saurer 1, despite being located at large distances from the Galactic centre, are on nearly circular disc-like orbits. Conclusions. Even with our simple preliminary exploration of the Gaia EDR3, we demonstrate how, once again, these data from the European Space Agency are crucial for our understanding of the different pieces of our Galaxy and their connection to its global structure and history.Publicación Acceso Abierto Ultracool dwarfs in deep extragalactic surveys using the virtual observatory: ALHAMBRA and COSMOS(Oxford Academics: Oxford University Press, 2021-02-01) Solano, Enrique; Gálvez Ortiz, M. C.; Martín, Eduardo L.; Gómez Muñoz, I. M.; Rodrigo, C.; Burgasser, A. J.; Lodieu, N.; Béjar, V. J. S.; Huélamo, N.; Morales Calderón, M.; Bouy, H.; Agencia Estatal de Investigación (AEI); Ministerio de Economía y Competitividad (MINECO); Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737Ultracool dwarfs (UCDs) encompass a wide variety of compact stellar-like objects with spectra classified as late-M, L, T, and Y. Most of them have been discovered using wide-field imaging surveys. The Virtual Observatory (VO) has proven to be of great utility to efficiently exploit these astronomical resources. We aim to validate a VO methodology designed to discover and characterize UCDs in deep extragalactic surveys like Advance Large Homogeneous Area Medium-Band Redshift Astronomical (ALHAMBRA) and Cosmological Evolution Survey (COSMOS). Three complimentary searches based on parallaxes, proper motions and colours, respectively, were carried out. A total of 897 candidate UCDs were found, with only 16 previously reported in SIMBAD. Most of the new UCDs reported here are likely late-M and L dwarfs because of the limitations imposed by the utilization of optical (Gaia DR2 and r-band) data. We complement ALHAMBRA and COSMOS photometry with other catalogues in the optical and infrared using VOSA, a VO tool that estimates effective temperatures from the spectral energy distribution fitting to collections of theoretical models. The agreement between the number of UCDs found in the COSMOS field and theoretical estimations together with the low false-negative rate (known UCDs not discovered in our search) validates the methodology proposed in this work, which will be used in the forthcoming wide and deep surveys provided by the Euclid space mission. Simulations of Euclid number counts for UCDs detectable in different photometric passbands are presented for a wide survey area of 15 000 deg2, and the limitations of applicability of Euclid data to detect UCDs using the methods employed in this paper are discussed.Publicación Acceso Abierto Identification of asteroids using the Virtual Observatory: the WFCAM Transit Survey(Oxford Academics: Oxford University Press, 2019-10-26) Cortés Contreras, M.; Jiménez Esteban, F. M.; Mahlke, M.; Solano, Enrique; Durech, J.; Barceló Forteza, S.; Rodrigo, C.; Velasco, A.; Carry, B.; Agencia Estatal de Investigación (AEI); European Space Agency (ESA); Contreras, M. [0000-0003-3734-9866]; Rodrigo Blanco, C. [0000-0001-6068-0077]; Jiménez Esteban, F. M. [0000-0002-6985-9476]; Carry, B. [0000-0001-5242-3089]; 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-2017-0737The nature and physical properties of asteroids, in particular those orbiting in the near-Earth space, are of scientific interest and practical importance. Exoplanet surveys can be excellent resources to detect asteroids, both already known and new objects. This is due to their similar observing requirements: large fields of view, long sequences, and short cadence. If the targeted fields are not located far from the ecliptic, many asteroids will cross the field of view occasionally. We present two complementary methodologies to identify asteroids serendipitously observed in large-area astronomical surveys. One methodology focuses on detecting already known asteroids using the Virtual Observatory tool SkyBoT, which predicts their positions and motions in the sky at a specific epoch. The other methodology applies the ssos pipeline, which is able to identify known and new asteroids based on their apparent motion. The application of these methods to the 6.4 deg2 of the sky covered by the Wide-Field CAMera Transit Survey in the J-band is described. We identified 15 661 positions of 1821 different asteroids. Of them, 182 are potential new discoveries. A publicly accessible online, Virtual Observatory compliant catalogue was created. We obtained the shapes and periods for five of our asteroids from their light curves built with additional photometry taken from external archives. We demonstrated that our methodologies are robust and reliable approaches to find, at zero cost of observing time, asteroids observed by chance in astronomical surveys. Our future goal is to apply them to other surveys with adequate temporal coverage.Publicación 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, Enrique; 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.; 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 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, 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.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, Enrique; Rodrigo, C.Binary 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/).
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