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 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 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 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/).Publicación Acceso Abierto Infrared-excess white dwarfs in the Gaia 100 pc sample(Oxford Academics: Oxford University Press, 2019-09-02) Rebassa Mansergas, A.; Solano, Enrique; Xu, S.; Rodrigo, C.; Jiménez Esteban, F. M.; Torres, S.; 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 The Gran Telescopio Canarias OSIRIS broad-band first data release(Oxford Academics: Oxford University Press, 2020-01-05) Cortés Contreras, M.; Bouy, H.; Solano, Enrique; Mahlke, M.; Jiménez Esteban, F. M.; Alacid, J. M.; Rodrigo, C.; 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 A deep learning approach to determine fundamental parameters of target stars(EDP Sciences, 2020-09-30) Passegger, V. M.; Bello García, A.; Ordieres Meré, J.; Caballero, J. A.; Schweitzer, A.; González Marcos, A.; Ribas, I.; Reiners, A.; Quirrenbach, A.; Amado, P. J.; Azzaro, M.; Bauer, F. F.; Béjar, V. J. S.; Cortés Contreras, M.; Dreizler, S.; Hatzes, Artie; Henning, T.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Lafarga, M.; Marfil, E.; Montes, D.; Morales, J. C.; Nagel, E.; Sarro, L. M.; Solano, E.; Tabernero, H. M.; Zechmeister, M.; Solano, Enrique; Agencia Estatal de Investigación (AEI); Fundacao para a Ciencia e a Tecnologia (FCT); National Aeronautics and Space Administration (NASA); Bello García, A. [0000-0001-8691-3342]; Ordieres Meré, J. [0000-0002-9677-6764]; Caballero, J. A. [0000-0002-7349-1387]; González Marcos, A. [0000-0003-4684-659X]; Ribas, I. [0000-0002-6689-0312]; Azzaro, M. [0000-0002-1317-0661]; Kürster, M. [0000-0002-1765-9907]; Marfil, E. [0000-0001-8907-4775]; Montes, D. [0000-0002-7779-238X]; Morales, J. C. [0000-0003-0061-518X]; Nagel, E. [0000-0002-4019-3631]; Sarro, L. M. [0000-0002-5622-5191]; Tabernero, H. [0000-0002-8087-4298]; Zechmesister, M. [0000-0002-6532-4378]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737Existing and upcoming instrumentation is collecting large amounts of astrophysical data, which require efficient and fast analysis techniques. We present a deep neural network architecture to analyze high-resolution stellar spectra and predict stellar parameters such as effective temperature, surface gravity, metallicity, and rotational velocity. With this study, we firstly demonstrate the capability of deep neural networks to precisely recover stellar parameters from a synthetic training set. Secondly, we analyze the application of this method to observed spectra and the impact of the synthetic gap (i.e., the difference between observed and synthetic spectra) on the estimation of stellar parameters, their errors, and their precision. Our convolutional network is trained on synthetic PHOENIX-ACES spectra in different optical and near-infrared wavelength regions. For each of the four stellar parameters, Teff, log g, [M/H], and v sin i, we constructed a neural network model to estimate each parameter independently. We then applied this method to 50 M dwarfs with high-resolution spectra taken with CARMENES (Calar Alto high-Resolution search for M dwarfs with Exo-earths with Near-infrared and optical Échelle Spectrographs), which operates in the visible (520–960 nm) and near-infrared wavelength range (960–1710 nm) simultaneously. Our results are compared with literature values for these stars. They show mostly good agreement within the errors, but also exhibit large deviations in some cases, especially for [M/H], pointing out the importance of a better understanding of the synthetic gap.Publicación Acceso Abierto Wide companions to M and L subdwarfs with Gaia and the Virtual Observatory(EDP Sciences, 2021-06-29) González Payo, J.; Cortés Contreras, M.; Lodieu, N.; Solano, Enrique; Zhang, Z. H.; Gálvez Ortiz, M. C.; Agencia Estatal de Investigación (AEI); European Research Council (ERC)Aims. The aim of the project is to identify wide common proper motion companions to a sample of spectroscopically confirmed M and L metal-poor dwarfs (also known as subdwarfs) to investigate the impact of metallicity on the binary fraction of low-mass metal-poor binaries and to improve the determination of their metallicity from the higher-mass binary. Methods. We made use of Virtual Observatory tools and large-scale public surveys to look in Gaia for common proper motion companions to a well-defined sample of ultracool subdwarfs with spectral types later than M5 and metallicities below or equal to −0.5 dex. We collected low-resolution optical spectroscopy for our best system, which is a binary composed of one sdM1.5 subdwarf and one sdM5.5 subdwarf located at ∼1360 au, and for another two likely systems separated by more than 115 000 au. Results. We confirm one wide companion to an M subdwarf, and infer a multiplicity for M subdwarfs (sdMs) of 1.0−1.0+2.0% for projected physical separations of up to 743 000 au. We also find four M–L systems, three of which are new detections. No colder companion was identified in any of the 219 M and L subdwarfs of the sample, mainly because of limitations on the detection of faint sources with Gaia. We infer a frequency of wide systems for sdM5–9.5 of 0.60−0.60+1.17% for projected physical separations larger than 1 360 au (up to 142 400 au). This study shows a multiplicity rate of 1.0−1.0+2.0% in sdMs, and 1.9−1.9+3.7% in extreme M subdwarfs. We did not find any companion for the ultra M subdwarfs of our sample, establishing an upper limit of 5.3% on binarity for these objects.Publicación Acceso Abierto Clusterix 2.0: a virtual observatory tool to estimate cluster membership probability.(Oxford Academics: Blackwell Publishing, 2020-02-11) Balaguer Núñez, L.; López del Fresno, M.; Solano, Enrique; Galadí Enríquez, D.; Jordi, C.; Jiménez Esteban, F. M.; Masana, E.; Carbajo Hijarrubia, J.; Paunzen, E.; Agencia Estatal de Investigación (AEI); European Commission (EC); European Research Council (ERC); 0000-0001-9789-7069; 0000-0002-3304-5200; 0000-0002-6985-9476; Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos (ICCUB), MDM-2014-0369; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737Clusterix 2.0 is a web-based, Virtual Observatory compliant, interactive tool for the determination of membership probabilities in stellar clusters based on proper-motion data using a fully non-parametric method. In an area occupied by a cluster, the frequency function is made up of two contributions: cluster and field stars. The tool performs an empirical determination of the frequency functions from the vector point diagram without relying on any previous assumption about their profiles. Clusterix 2.0 allows us to search the appropriate spatial areas in an interactive way until an optimal separation of the two populations is obtained. Several parameters can be adjusted to make the calculation computationally feasible without interfering with the quality of the results. The system offers the possibility to query different catalogues, such as Gaia, or upload a user’s own data. The results of the membership determination can be sent via Simple Application Messaging Protocol (SAMP) to Virtual Observatory (VO) tools such as Tool for OPerations on Catalogues And Tables (TOPCAT). We apply Clusterix 2.0 to several open clusters with different properties and environments to show the capabilities of the tool: an area of five degrees radius around NGC 2682 (M67), an old, well-known cluster; a young cluster NGC 2516 with a striking elongated structure extended up to four degrees; NGC 1750 and NGC 1758, a pair of partly overlapping clusters; the area of NGC 1817, where we confirm a little-known cluster, Juchert 23; and an area with many clusters, where we disentangle two overlapping clusters situated where only one was previously known: Ruprecht 26 and the new CLUSTERIX 1.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 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/).
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