Examinando por Autor "Solano, E."

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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, Enrique
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/).
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, E.; Rodrigo, C.; Solano, Enrique; 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-2017-0737
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/).
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-2017-0709
Surveys 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 Science
Acceso Abierto
CARMENES input catalogue of M dwarfs: V. Luminosities, colours, and spectral energy distributions
(EDP Sciences, 2020-10-12) Cifuentes, C.; Caballero, J. A.; Cortés Contreras, M.; Montes, D.; Abellán, F. J.; Dorda, R.; Holgado, G.; Zapatero Osorio, M. R.; Morales, J. C.; Amado, P. J.; Passegger, V. M.; Quirrenbach, A.; Reiners, A.; Ribas, I.; Sanz Forcada, J.; Schweitzer, A.; Seifert, W.; Solano, E.; Solano, Enrique; Agencia Estatal de Investigación (AEI); National Aeronautics and Space Administration (NASA); 0000-0003-1715-5087; 0000-0002-7349-1387; 0000-0003-3734-9866; 0000-0002-7779-238X; 0000-0001-5664-2852; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Context. The relevance of M dwarfs in the search for potentially habitable Earth-sized planets has grown significantly in the last years. Aims. In our on-going effort to comprehensively and accurately characterise confirmed and potential planet-hosting M dwarfs, in particular for the CARMENES survey, we have carried out a comprehensive multi-band photometric analysis involving spectral energy distributions, luminosities, absolute magnitudes, colours, and spectral types, from which we have derived basic astrophysical parameters. Methods. We have carefully compiled photometry in 20 passbands from the ultraviolet to the mid-infrared, and combined it with the latest parallactic distances and close-multiplicity information, mostly from Gaia DR2, of a sample of 2479 K5 V to L8 stars and ultracool dwarfs, including 2210 nearby, bright M dwarfs. For this, we made extensive use of Virtual Observatory tools. Results. We have homogeneously computed accurate bolometric luminosities and effective temperatures of 1843 single stars, derived their radii and masses, studied the impact of metallicity, and compared our results with the literature. The over 40 000 individually inspected magnitudes, together with the basic data and derived parameters of the stars, individual and averaged by spectral type, have been made public to the astronomical community. In addition, we have reported 40 new close multiple systems and candidates (ρ < 3.3 arcsec) and 36 overluminous stars that are assigned to young Galactic populations. Conclusions. In the new era of exoplanet searches around M dwarfs via transit (e.g. TESS, PLATO) and radial velocity (e.g. CARMENES, NIRPS+HARPS), this work is of fundamental importance for stellar and therefore planetary parameter determination. © ESO 2020.
Restringido
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, E.; Galadí Enríquez, D.; Jordi, C.; Jiménez Esteban, F. M.; Masana, E.; Carbajo Hijarrubia, J.; Paunzen, E.; Solano, Enrique; 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-2017-0737
Clusterix 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.
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; 0000-0003-0987-1593
Debido 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.x
Acceso Abierto
Exploring nine simultaneously occurring transients on April 12th 1950
(Nature Research Journals, 2021-06-17) Villarroel, B.; Marcy, G. W.; Geier, S.; Streblyanska, A.; Solano, E.; Andruk, V. N.; Shultz, M. E.; Gupta, A. C.; Mattsson, L.; Solano, Enrique; Agencia Estatal de Investigación (AEI)
Nine point sources appeared within half an hour on a region within ∼ 10 arcmin of a red-sensitive photographic plate taken in April 1950 as part of the historic Palomar Sky Survey. All nine sources are absent on both previous and later photographic images, and absent in modern surveys with CCD detectors which go several magnitudes deeper. We present deep CCD images with the 10.4-m Gran Telescopio Canarias, reaching brightness r∼26 mag, that reveal possible optical counterparts, although these counterparts could equally well be just chance projections. The incidence of transients in the investigated photographic plate is far higher than expected from known detection rates of optical counterparts to e.g. flaring dwarf stars, Fast Radio Bursts, Gamma Ray Bursts or microlensing events. One possible explanation is that the plates have been subjected to an unknown type of contamination producing mainly point sources with of varying intensities along with some mechanism of concentration within a radius of ∼ 10 arcmin on the plate. If contamination as an explanation can be fully excluded, another possibility is fast (t <0.5 s) solar reflections from objects near geosynchronous orbits. An alternative route to confirm the latter scenario is by looking for images from the First Palomar Sky Survey where multiple transients follow a line.
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, SEV2015-0493
Context. 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.
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-2014-0369
Context. 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.
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, E.; 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.; Manteiga, Minia; Solano, Enrique; 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), SEV2015-0493
Aims. 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.
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, E.; Meeus, G.; Marcos Arenal, P.; Solano, Enrique; 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.
Restringido
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, E.; Durech, J.; Barceló Forteza, S.; Rodrigo, C.; Velasco, A.; Carry, B.; Solano, Enrique; 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-2017-0737
The 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.
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-2017-0737
We 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.
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-2017-0737
Context. 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.
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-2017-0737
The 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.
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-2017-0737
Existing 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.
Acceso Abierto
The CARMENES search for exoplanets around M dwarfs Different roads to radii and masses of the target stars
(EDP Sciences, 2019-05-14) Schweitzer, A.; Passegger, V. M.; Cifuentes, C.; Béjar, V. J. S.; Cortés Contreras, M.; Caballero, J. A.; Del Burgo, C.; Czesla, S.; Kürster, M.; Montes, D.; Zapatero Osorio, M. R.; Ribas, I.; Reiners, A.; Quirrenbach, A.; Amado, P. J.; Aceituno, J.; Anglada Escudé, G.; Bauer, F. F.; Dreizler, S.; Jeffers, S. V.; Guenther, E. W.; Henning, T.; Kaminski, A.; Lafarga, M.; Marfil, E.; Morales, J. C.; Schmitt, J. H. M. M.; Seifert, W.; Solano, E.; Tabernero, H. M.; Zechmeister, M.; Solano, Enrique; Agencia Estatal de Investigación (AEI); Ministerio de Economía y Competitividad (MINECO); Deutsche Forschungsgemeinschaft (DFG); 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
Aims. We determine the radii and masses of 293 nearby, bright M dwarfs of the CARMENES survey. This is the first time that such a large and homogeneous high-resolution (R > 80 000) spectroscopic survey has been used to derive these fundamental stellar parameters. Methods. We derived the radii using Stefan–Boltzmann’s law. We obtained the required effective temperatures Teff from a spectral analysis and we obtained the required luminosities L from integrated broadband photometry together with the Gaia DR2 parallaxes. The mass was then determined using a mass-radius relation that we derived from eclipsing binaries known in the literature. We compared this method with three other methods: (1) We calculated the mass from the radius and the surface gravity log g, which was obtained from the same spectral analysis as Teff. (2) We used a widely used infrared mass-magnitude relation. (3) We used a Bayesian approach to infer stellar parameters from the comparison of the absolute magnitudes and colors of our targets with evolutionary models. Results. Between spectral types M0 V and M7 V our radii cover the range 0.1 R⊙ < R < 0.6 R⊙ with an error of 2–3% and our masses cover 0.09 ℳ⊙ < ℳ< 0.6ℳ⊙ with an error of 3–5%. We find good agreement between the masses determined with these different methods for most of our targets. Only the masses of very young objects show discrepancies. This can be well explained with the assumptions that we used for our methods.
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, E.; Barnes, R.; Solano, Enrique; 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-2017-0709
Context. 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.
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-2015-0548
The 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.
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-2017-0737
We 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.