Examinando por Autor "Sarro, L. M."

Mostrando 1 - 7 de 7

Acceso Abierto
Chamaeleon DANCe Revisiting the stellar populations of Chamaeleon I and Chamaeleon II with Gaia-DR2 data
(EDP Sciences, 2021-02-04) Galli, P. A. B.; Bouy, H.; Olivares, J.; Miret Roig, N.; Sarro, L. M.; Barrado, D.; Berihuete, A.; Bertín, E.; Cuillandre, J. C.; European Research Council (ERC); Berihuete, A. [0000-0002-8589-4423]; Galli, P. A. B. [0000-0003-2271-9297]; Olivares Romero, J. [0000-0003-0316-2956]
Context. Chamaeleon is the southernmost low-mass star-forming complex within 200 pc from the Sun. Its stellar population has been extensively studied in the past, but the current census of the stellar content is not complete yet and deserves further investigation. Aims. We take advantage of the second data release of the Gaia space mission to expand the census of stars in Chamaeleon and to revisit the properties of the stellar populations associated to the Chamaeleon I (Cha I) and Chamaeleon II (Cha II) dark clouds. Methods. We perform a membership analysis of the sources in the Gaia catalogue over a field of 100 deg2 encompassing the Chamaeleon clouds, and use this new census of cluster members to investigate the 6D structure of the complex. Results. We identify 188 and 41 high-probability members of the stellar populations in Cha I and Cha II, respectively, including 19 and 7 new members. Our sample covers the magnitude range from G = 6 to G = 20 mag in Cha I, and from G = 12 to G = 18 mag in Cha II. We confirm that the northern and southern subgroups of Cha I are located at different distances (191.4−0.8+0.8 pc and 186.7−1.0+1.0 pc), but they exhibit the same space motion within the reported uncertainties. Cha II is located at a distance of 197.5−0.9+1.0 pc and exhibits a space motion that is consistent with Cha I within the admittedly large uncertainties on the spatial velocities of the stars that come from radial velocity data. The median age of the stars derived from the Hertzsprung-Russell diagram and stellar models is about 1−2 Myr, suggesting that they are somewhat younger than previously thought. We do not detect significant age differences between the Chamaeleon subgroups, but we show that Cha II exhibits a higher fraction of disc-bearing stars compared to Cha I. Conclusions. This study provides the most complete sample of cluster members associated to the Chamaeleon clouds that can be produced with Gaia data alone. We use this new census of stars to revisit the 6D structure of this region with unprecedented precision.
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.; Pailler, F.; Carlucci, T.; Castellani, M.; Carrasco, J. M.; Wyrzykowski, L.; Barbato, D.; Smart, R. L.; Reylé, C.; Chemin, L.; Evans, D. W.; Siddiqui, H. I.; Caffau, E.; Thuillot, W.; Chiavassa, A.; Comoretto, G.; Sarasso, M.; Cornez, T.; Babusiaux, C.; Crifo, F.; Dapergolas, A.; Crowley, C.; Janßen, Katja; Altmann, M.; Lebzelter, T.; Millar, N. R.; Fouron, C.; Charlot, P.; Molinaro, R.; Bertone, S.; Marchal, O.; Bouquillon, S.; Salgado, J; Lanzafame, A. C.; De Teodoro, P.; García Torres, M.; Rybicki, K. A.; Liao, S.; Delgado, A.; Granvik, M.; Souchay, J.; Buzzi, R.; Cowell, S.; Tauran, G.; Jordan, S.; Siltala, L.; Dolding, C.; Zhao, H.; Jonker, P. G.; Enke, H.; Julbe, F.; Sciacca, E.; Fedorets, G.; Faigler, S.; Panahi, A.; Rixon, G.; Livanou, E.; Weiler, M.; Del Peloso, E. F.; Juaristi Campillo, J.; Marcos Santos, M. M. S.; Bakker, J.; Hilger, T.; Franke, F.; Unger, N.; Garabato, D.; Teyssier, D.; Fouesneau, M.; Souami, D.; Nienartowicz, K.; Gavras, P.; Eyer, L.; Zurbach, C.; Gilmore, G.; Szegedi Elek, E.; Gómez, A.; Romero Gómez, M.; Musella, I.; Royer, F.; Licata, E.; Katz, D.; Fabre, C.; Szabados, L.; Hutton, A.; Viala, Y.; Haywood, M.; Mints, A.; Mowlavi, N.; Lindstrom, H. E. P.; Anglada Varela, E.; Holland, G.; Jansen, F.; Jasniewicz, G.; Haigron, R.; Seabroke, G. M.; Figueras, F.; Voutsinas, S.; Khanna, S.; Hauser, M.; Moitinho, A.; Busso, G.; Kochoska, A.; Kordopatis, G.; Guiraud, J.; Le Fustec, Y.; Gerlach, E.; Lecoeur Taibi, I.; Jordi, C.; Leccia, S.; Raiteri, C. M.; Barros, M.; Sanna, N.; Pourbaix, D.; Kervella, P.; Schultheis, M.; Garofalo, A.; Prusti, T.; Girona, S.; Madrero Pardo, P.; Ducourant, C.; Zwitter, T.; Morris, D.; Walton, N. A.; Marchant, J. M.; Pagani, C.; Gracia Abril, G.; Guy, L. P.; Lebreton, Y.; Blomme, R.; Riclet, F.; Plachy, E.; Panem, C.; Harrison, D. L.; Masip, A.; Poggio, E.; Masana, E.; Michalik, D.; Messina, S.; Süveges, M.; Riva, A.; González Núñez, J.; Managau, S.; Utrilla, E.; Plum, G.; Arenou, F.; Jevardat de Fombelle, G.; Montegriffo, P.; Damerdji, Y.; Morbidelli, R.; Abreu Aramburu, A.; Thévenin, F.; Anderson, R. I.; Muñoz, D.; Hestroffer, D.; Mora, A.; Benson, K.; Randich, S.; Ordénovic, C.; Noval, L.; Zucker, S.; Van Leeuwen, F.; Regibo, S.; Smith, M.; Mastrobuono Battisti, A.; Bellas Velidis, I.; Muinonen, K.; Galluccio, L.; Santoveña, R.; Sartoretti, P.; Álvarez Cid Fuentes, J.; Eappachen, D.; Penttilä, A.; Osborne, Paul; Pineau, F. X.; Busonero, D.; Baker, S. G.; Molina, D.; García Reinaldos, M.; Poujoulet, E.; Bellazzini, M.; Palicio, P. A.; Prsa, A.; Pulone, L.; Ajaj, M.; Ragaini, S.; Holl, B.; Re Fiorentin, P.; Pancino, E.; Rambaux, N.; Vanel, O.; Guerra, R.; Soubiran, C.; Richards, P. J.; Jean Antonie Piccolo, A.; Mulone, A. F.; Murphy, C. P.; Robichon, N.; Van Reeven, W.; Hodgkin, S. T.; Robin, A. C.; Rohrbasser, L.; Spagna, A.; Palaversa, L.; Balog, Z.; Rainer, M.; Baudesson-Stella, A.; Audard, M.; Teixeira, R.; Recio Blanco, A.; Sahlmann, J.; Tonello, N.; Álvarez, M. A.; Bailer Jones, C. A. L.; Sánchez Giménez, V.; Wevers, T.; Andrae, R.; Bucciarelli, B.; Robin, C.; De Souza, R.; Roegiers, T.; Carnerero, M. I.; Segol, M.; Boch, T.; Ségransan, D.; Del Pozo, E.; Steidelmüller, H.; Siebert, A.; Creevey, O. L.; Vallenari, A.; Bassilana, J. L.; Riello, M.; Solitro, F.; Heiter, U.; Ulla, A.; Lattanzi, M. G.; De Luise, F.; Salguero, E.; Brown, A. G. A.; Bartolomé, S.; Guerrier, A.; Geyer, R.; Di Stefano, E.; Martín Fleitas, J. M.; Taris, F.; Cooper, W. J.; Taylor, M. B.; Gutiérrez Sánchez, R.; Fabrizio, M.; Brouillet, N.; García Gutierrez, A.; Torra, F.; Steele, I. A.; Torra, J.; Turon, C.; Di Matteo, P.; Vaillant, M.; Carballo, R.; Vicente, D.; Vecchiato, A.; Dell´Oro, A.; Aerts, C.; Altavilla, G.; Crosta, M.; Rimoldini, L.; Cropper, M.; Chaoul, L.; Slezak, E.; Yoldas, A.; Cantat Gaudin, T.; Dafonte, C.; Zorec, J.; Portell, J.; Drimmel, R.; Fernique, P.; Gai, M.; Van Dillen, E.; Esquej, P.; Burgess, P. W.; De Angeli, F.; Carry, B.; Diener, C.; Rybizki, J.; Frémat, Y.; Gosset, E.; Barstow, M. A.; González Vidal, J. J.; Yvard, P.; Luri, X.; Huckle, H. E.; Messineo, M.; Giacobbe, P.; Nicolas, C.; Mann, R. G.; Krone Martins, A.; Panuzzo, P.; Marrese, P. M.; Lorca, A.; Fraile, E.; Tanga, P.; Sordo, R.; Cánovas, H.; De Ridder, J.; Sozzetti, A.; Lister, T. A.; Fabricius, C.; Löffler, W.; Fragkoudi, F.; Aguado, J. J.; Martin Polo, L.; Sagristà Sellés, A.; Berthier, J.; Le Campion, J. F.; Brugaletta, E.; Pagano, I.; Mazeh, T.; González Santamaría, I.; Morel, T.; Cellino, A.; Cheek, N.; Clementini, G.; Marinoni, S.; Davidson, M.; Hladczuk, N.; García Lario, P.; Fernández Hernández, J.; Bramante, L.; Delgado, H. E.; Diakite, S.; De Bruijne, J. H. J.; Sarro, L. M.; Karbevska, L.; Roux, W.; Halbwachs, J. L.; Hidalgo, S. L.; Leclerc, N.; Hatzidimitriou, D.; Barache, C.; Siopis, C.; Mor, R.; Delchambre, L.; Massari, D.; Stephenson, C. A.; Van Leeuwen, M.; Bernet, M.; Marshall, D. J.; David, M.; Accart, S.; Burlacu, A.; Osinde, J.; Hambly, N. C.; Pauwels, T.; Piersimoni, A. M.; Lammers, U.; Muraveva, T.; Alves, J.; Roelens, M.; Casamiquela, L.; Antoja, T.; Castro Sampol, P.; Molnár, L.; Balbinot, E.; Balaguer Núñez, L.; Helmi, A.; Lobel, A.; De March, R.; Ripepi, V.; Abbas, U.; Castro Ginard, A.; Delisle, J. B.; Sadowski, G.; Castañeda, J.; Bauchet, N.; Racero, E.; Becciani, U.; Spoto, F.; Samaras, N.; Orrù, G.; Semeux, D.; Bianchi, L.; Blanco Cuaresma, S.; Rowell, N.; Bossini, D.; Peñalosa Ester, X.; Bressan, A.; Breedt, E.; Giuffrida, G.; Marconi, M.; Marocco, F.; David, P.; Poretti, E.; Baines, D.; Butkevich, A. G.; Pawlak, M.; Ramos, P.; Cancelliere, R.; Fienga, A.; De Laverny, P.; Segovia, J. C.; 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.; Mulone, A. F.; Siebert, A.; Le Fustec, Y.; Helmi, A.; Pourbaix, D.; Brown, A. G. A.; Vallenari, A.; Guerrier, A.; Utrilla, E.; Samaras, N.; González Santamaría, I.; Piersimoni, A. M.; Evans, D. W.; Busso, G.; Garofalo, A.; Jansen, F.; Fernández Hernández, J.; Klioner, S. A.; Liao, S.; Muñoz, D.; González Núñez, J.; Morris, D.; Fragkoudi, F.; Pineau, F. X.; Hutton, A.; Leclerc, N.; Delgado, A.; Hilger, T.; Girona, S.; Torra, F.; Drimmel, R.; De Laverny, P.; Lattanzi, M. G.; García Lario, P.; Zwitter, T.; Castañeda, J.; Jordi, C.; Musella, I.; Halbwachs, J. L.; Fabricius, C.; Randich, S.; Siopis, C.; Guiraud, J.; Zurbach, C.; De Angeli, F.; Charlot, P.; Palicio, P. A.; Kostrzewa Rutkowska, Z.; Lindegren, L.; Ducourant, C.; Buzzi, R.; Rambaux, N.; Roelens, M.; Julbe, F.; Molinaro, R.; Tanga, P.; Castellani, M.; Gracia Abril, G.; García Reinaldos, M.; Teyssier, D.; Aerts, C.; Sordo, R.; Bellas Velidis, I.; Álvarez, M. A.; Berthier, J.; Rohrbasser, L.; Anglada Varela, E.; Sánchez Giménez, V.; Zorec, J.; Pulone, L.; Marocco, F.; Madrero Pardo, P.; Robin, A. C.; Davidson, M.; Riclet, F.; Dell´Oro, A.; Benson, K.; Turron, C.; Seabroke, G. M.; Boch, T.; Pawlak, M.; Salgado, J.; Millar, N. R.; Blomme, R.; Galluccio, L.; Fabre, C.; Segovia, J. C.; Rixon, G.; Siltala, L.; Messineo, R.; Rainer, M.; Holl, B.; Recio Blanco, A.; Jevardat de Fombelle, G.; Jordan, S.; Ajaj, M.; Biermann, M.; Van Leeuwen, F.; Szegedi Elek, E.; Bertone, S.; Hodgkin, S. T.; Moitinho, A.; Bragaglia, A.; Muinonen, K.; Regibo, S.; Slezak, E.; Brouillet, N.; Massari, D.; Taris, F.; Pailler, F.; Marrese, P. M.; Ramos Lerate, M.; Lindstrom, H. E. P.; Osinde, J.; Morbidelli, R.; Burgess, P. W.; Sozzetti, A.; Ulla, A.; Breedt, E.; Heiter, U.; Van Reeven, W.; Mora, A.; Arenou, F.; Busonero, D.; Destroffer, D.; Richards, P. J.; De Luise, F.; Hatzidimitriou, D.; Abbas, U.; Kervella, P.; Steidelmüller, H.; Poujoulet, E.; Pancino, E.; Abreu Aramburu, A.; Haywood, M.; Van Dillen, E.; Yoldas, A.; Segol, M.; Balog, Z.; Juaristi Campillo, J.; Barbato, D.; Bressan, A.; Barstow, M. A.; Delisle, J. B.; Balaguer Núñez, L.; Bauchet, N.; Di Stefano, E.; Yvard, P.; Enke, H.; Bakker, J.; Hambly, N. C.; Torra, J.; Soubiran, C.; Robin, C.; David, M.; Bossini, D.; Baines, D.; Baudesson Stella, A.; Carry, B.; Muraveva, T.; Geyer, R.; Süveges, M.; Katz, D.; Schultheis, M.; Becciani, U.; Bramante, S.; Marcos Santos, M. M. S.; Cropper, M.; Mowlavi, N.; Álvarez Cid Fuentes, J.; Unger, C.; Carballo, R.; Babusiaux, C.; Carnerero, M. I.; Carrasco, J. M.; Diakite, S.; Cioni, M. R. L.; Altmann, M.; Chaoul, L.; Gavras, P.; Cantat Gaudin, T.; Comoretto, G.; Giuffrida, G.; Cornez, T.; Vicente, D.; Nicolas, C.; Granvik, M.; Andrae, R.; Antoja, T.; Chiavassa, A.; Vecchiato, A.; Sartoretti, P.; Souchay, J.; Semeux, D.; Bernet, M.; De Ridder, J.; De Souza, R.; Caffau, E.; De Torres, A.; Cooper, W. J.; Roegiers, T.; Guy, L. P.; Cánovas, H.; Crowley, C.; Lebreton, Y.; Prusti, T.; Del Peloso, E. F.; Thévenin, F.; Tonello, N.; Crifo, F.; Del Pozo, E.; Ordénovic, C.; Damerdji, Y.; Gosset, E.; Guerra, R.; Fernique, P.; Peñalosa Esteller, X.; González Vidal, J. J.; Fouron, C.; Lister, T. A.; Fedorets, G.; Franke, F.; Lammers, U.; Haigron, R.; Marchant, J. M.; Van Leeuwen, M.; Butkevich, A. G.; Rimoldini, L.; Wyrzykowski, L.; Lasne, Y.; Gilmore, G.; Fabrizio, M.; Gai, M.; Bianchi, L.; Janßen, Katja; Mignard, F.; Portell, J.; Fouesneau, M.; Garabato, D.; Gómez, A.; Rybicki, K. A.; Smith, M.; Alves, J.; Creevey, O. L.; Cellino, A.; Holland, G.; Löffler, W.; Jasniewicz, G.; Lobel, A.; Hernández, J.; Bartolomé, S.; Karbevska, L.; Molina, D.; Hobbs, D.; Kochoska, A.; Morel, T.; Kordopatis, G.; Anderson, R. I.; Murphy, C. P.; Bassilana, J. L.; Esquej, P.; Khanna, S.; Delchambre, L.; Riello, M.; Roux, W.; Jean Antonie Piccolo, A.; García Torres, M.; Leccia, S.; Hidalgo, S. L.; Lecoeur Taibi, I.; Kontizas, M.; David, P.; Noval, L.; Hladczuk, N.; Kruszynska, K.; Raiteri, C. M.; Krone Martins, A.; Barache, C.; Brugaletta, E.; Korn, A. J.; Licata, E.; Solitro, F.; Bombrun, A.; Brucciarelli, B.; Aguado, J. J.; Martín Polo, L.; Bailer Jones, C. A. L.; Masip, A.; Riva, A.; Marshall, D. J.; Mazeh, T.; Osborne, Paul; Burlacu, A.; Rowell, N.; De Teodoro, P.; Hauser, M.; Dapergolas, A.; Racero, E.; Montegriffo, P.; Marinoni, S.; Messina, S.; Eyer, L.; Carlucci, T.; Pauwels, T.; Barros, M.; Accart, S.; Michalik, D.; Zucker, S.; De March, R.; Dolding, C.; Lorca, A.; Blanco Cuaresma, S.; Palaversa, L.; De Bruijne, J. H. J.; Panahi, A.; Robichon, N.; Cancelliere, R.; Penttilä, A.; Sciacca, E.; Pagano, I.; Plachy, E.; Siddiqui, H. I.; Poggio, E.; Eappachen, D.; Smart, R. L.; Fraile, E.; Marconi, M.; Bouquillon, S.; Dafonte, C.; Baker, S. G.; Altavilla, G.; Mints, A.; Ramos, P.; Orrù, G.; Re Fiorentin, P.; Plum, G.; Le Campion, J. F.; Pagani, C.; Prsa, A.; Vaillant, M.; Casamiquela, L.; Fienga, A.; Bellazzini, M.; Poretti, E.; Reylé, C.; Panuzzo, P.; Giacobbe, P.; Di Matteo, P.; Sahlmann, J.; Rybizki, J.; Salguero, E.; Weiler, M.; Sagristà Sellés, A.; Sanna, N.; Cowell, S.; Gutierrez Sánchez, R.; Zhao, H.; Panem, C.; Lanza, A. F.; Bastian, U.; Ségransan, D.; Sadowski, G.; Santoveña, R.; Marchal, O.; Huckle, H. E.; Crosta, M.; Figueras, F.; Sarasso, M.; Harrison, D. L.; Lebzelter, T.; Managau, S.; Castro Sampol, P.; Gerlach, E.; Steele, I. A.; Lanzafame, A. C.; Stephenson, C. A.; Wevers, T.; Szabados, L.; Frémat, Y.; Spoto, F.; Tauran, G.; Masana, E.; Teixeira, R.; Mann, R. G.; Nienartowicz, K.; Mastrobuono Battisti, A.; Royer, F.; Lambert, S.; Faigler, S.; Diener, C.; Walton, N. A.; Vanel, O.; Souami, D.; Viala, Y.; Taylor, M. B.; Ragaini, S.; Spagna, A.; Cheek, N.; Jonker, P. G.; Martín Fleitas, J. M.; García Gutierrez, A.; Thuillot, W.; Voutsinas, S.; Audard, M.; Molnár, L.; Livanou, E.; Solano, Enrique; Manteiga, Minia; 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.; Riclet, F.; Seabroke, G. M.; De Ridder, J.; Lammers, U.; Boch, T.; Hauser, M.; Del Pozo, E.; Fedorets, G.; De Bruijne, J. H. J.; Tanga, P.; Rybicki, K. A.; Samaras, N.; Marchant, J. M.; Klioner, S. A.; Jordan, S.; Luri, X.; Mignard, F.; Teyssier, D.; Bellas Velidis, I.; Randich, S.; Tauron, C.; Sánchez Giménez, V.; Masip, A.; Cropper, M.; Garofalo, A.; Harrison, D. L.; Riello, M.; Drimmel, R.; Giacobbe, P.; Muinonen, K.; Franke, F.; Sozzetti, A.; De Angeli, F.; Prsa, A.; Segovia, J. C.; Palaversa, L.; Frémat, Y.; Santoveña, R.; Mulone, A. F.; Guiraud, J.; Cioni, M. R. L.; Masana, E.; Butkevich, A. G.; Mowlavi, N.; Nicolas, C.; Fraile, E.; García Torres, M.; Giuffrida, G.; Hladczuk, N.; Van Reeven, W.; Smith, M.; Brouillet, N.; Clementini, G.; Walton, N. A.; Casamiquela, L.; Gosset, E.; Guerrier, A.; Fabrizio, M.; Anderson, R. I.; Managau, S.; Krone Martins, A.; Fouesneau, M.; Faigler, S.; Busso, G.; Anglada Varela, E.; Livanou, E.; Delchambre, L.; Fouron, C.; Damerdji, Y.; Van Leeuwen, F.; Chaoul, L.; Caffau, E.; Fernández Hernández, J.; Audard, M.; Abreu Aramburu, A.; Licarta, E.; Haztdimitriou, D.; Gai, M.; Haigron, R.; Arenou, F.; Racero, E.; Halbwachs, J. L.; Poretti, E.; Heiter, U.; Hernández, J.; Barache, C.; Diener, C.; Baines, D.; Janßen, Katja; Leclerc, N.; Murphy, C. P.; Gerlach, E.; Lanzafame, A. C.; Löffler, W.; Martín Fleitas, J. M.; Martín Polo, L.; Balog, Z.; Portell, J.; Lobel, A.; Lorca, A.; De Teodoro, P.; Osborne, Paul; Pancino, E.; Barros, M.; Recio Blanco, A.; Richards, P. J.; Siopis, C.; Sahlmann, J.; Sarro, L. M.; Lasne, Y.; Blanco Cuaresma, S.; Dafonte, C.; Davidson, M.; Marshall, D. J.; Van Leeuwen, M.; Brown, A. G. A.; Messina, S.; Accart, S.; Marocco, F.; Brugaletta, E.; Steele, I. A.; Eyer, L.; Andrae, R.; Siebert, A.; Ajaj, M.; Kervella, P.; Álvarez, M. A.; Álvarez Cid Fuentes, J.; Alves, J.; Kruszynska, K.; Molina, D.; Morris, D.; Pagani, C.; De March, R.; Charlot, P.; Rimoldini, L.; González Santamaría, I.; Hutton, A.; Huckle, H. E.; Bucciarelli, B.; Aguado, J. J.; Bassilana, J. L.; Eappachen, D.; Robichon, N.; Castellani, M.; Hodgkin, S. T.; Bernet, M.; Enke, H.; Riva, A.; Bouquillon, S.; Mastrobuono Battisti, A.; Bombrun, A.; Ulla, A.; Juaristi Campillo, J.; Bagaglia, A.; Bramante, L.; Regibo, S.; Michalik, D.; Bellazzini, M.; Esquej, P.; Burlacu, A.; Robin, A. C.; Bakker, J.; Buzzi, R.; Zurbach, C.; Cancelliere, R.; Cánovas, H.; Mann, R. G.; Rambaux, N.; Carnerero, M. I.; Montegriffo, P.; Cooper, W. J.; Bastian, U.; Castro Ginard, A.; Castro Sampol, P.; Cowell, S.; Sagristà Sellés, A.; Barbato, D.; Bailer Jones, C. A. L.; Comoretto, G.; Panem, C.; Cornez, T.; Fabre, C.; Fienga, A.; Crosta, M.; Crowley, C.; Busonero, D.; De Laverny, P.; Pulone, L.; Gavras, P.; Lanza, A. F.; De Luise, F.; Sadowski, G.; Bossini, D.; Jevardat de Fombelle, G.; Delisle, J. B.; De Torres, A.; Salguero, E.; Garía Reinaldos, M.; Delgado, A.; Bartolomé, S.; Cellino, A.; Di Matteo, P.; Piersimoni, A. M.; Bressan, A.; Distefano, E.; Dolding, C.; Schultheis, M.; Siddiqui, H. I.; Spagna, A.; Romero Gómez, M.; Leccia, S.; Julbe, F.; Muñoz, D.; Evans, D. W.; Palicio, P. A.; González Vidal, J. J.; Fragkoudi, F.; Marrese, P. M.; Messineo, R.; Jasniewicz, G.; Carballo, R.; García Gutierrez, A.; Marconi, M.; Jean Antonie Piccolo, A.; Jansen, F.; Korn, A. J.; De Souza, R.; Peñalosa Esteller, X.; Gilmore, G.; Girona, S.; Marcos Santos, M. M. S.; Guerra, R.; Garabato, D.; Sanna, V.; Granvik, M.; Dapergolas, A.; Guy, L. P.; Destroffer, D.; Haywood, M.; Hidalgo, S. L.; Hilger, T.; Marinoni, S.; Hobbs, D.; Fabricius, C.; Kontizas, M.; Segol, M.; Jonker, P. G.; Rybizki, J.; Sordo, R.; Fernique, P.; Roegiers, T.; Kochoska, A.; Pauwels, T.; Molinero, R.; Kostrzewa Rutkowska, Z.; Massari, D.; Lambert, S.; Gutiérrez Sánchez, R.; Lebreton, Y.; Berthier, J.; Molnár, L.; Muraveva, T.; Lebzelter, T.; Roux, W.; Geyer, R.; Carrasco, J. M.; Liao, S.; Gracia Abril, G.; Souami, D.; Lister, T. A.; Panahi, A.; Bianchi, L.; Madrero Pardo, P.; Unger, N.; Gómez, A.; Burgess, P. W.; Benson, K.; Carry, B.; Galluccio, L.; Holl, B.; Raiteri, C. M.; Penttilä, A.; Siltala, L.; Marchal, O.; Taris, F.; Salgado, J.; Chiavassa, A.; Vallenari, A.; Soubiran, C.; Lindstrom, H. E. P.; Mints, A.; Rohrbasser, L.; Altavilla, G.; Sartoretti, P.; Plum, G.; Lecoeur Taibi, I.; Morbidelli, R.; Morel, T.; Rowell, N.; Aerts, C.; Ordénovic, C.; Altmann, M.; Mazeh, T.; García Lario, P.; Noval, L.; Biermann, M.; Orrù, G.; Osinde, J.; Royer, F.; Pagano, I.; Abbas, U.; Plachy, E.; Blomme, R.; Pawlak, M.; David, P.; Balaguer Núñez, L.; David, M.; Pineau, F. X.; Crifo, F.; Sciacca, E.; Poggio, E.; Pourbaix, D.; Pojoulet, E.; Musella, I.; Ragaini, S.; Baudesson Stella, A.; Lattanzi, M. G.; Rainer, M.; Baker, S. G.; Mor, R.; Holland, G.; Re Fiorentin, P.; Millar, N. R.; Dell´Oro, A.; Ripepi, V.; Moitinho, A.; Rixon, G.; Hambly, N. C.; Robin, C.; Roelens, M.; Bauchet, N.; Bertone, S.; Breedt, E.; Carlucci, T.; Ducourant, C.; Katz, D.; Creevey, O. L.; Mora, A.; Slezak, E.; Karbevska, L.; Castañeda, J.; Tauran, G.; Creylé, C.; Sarasso, M.; Nienartowicz, K.; Diakite, S.; Prusti, T.; Ramos Lerate, M.; Ségransan, D.; Semeux, D.; Pailler, F.; Delgado, H. E.; Solitro, F.; Barstow, M. A.; Smart, R. L.; Babusiaux, C.; Cheek, N.; Utrilla, E.; Souchay, J.; Panuzzo, P.; Spoto, F.; Del Peloso, E. F.; Vicente, D.; Becciani, U.; Teixeira, R.; Le Fustec, Y.; Le Campion, J. F.; Viala, Y.; González Núñez, J.; Weiler, M.; Zucker, S.; Thévenin, F.; Zwitter, T.; Solano, Enrique; Manteiga, Minia; 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
Lupus DANCe Census of stars and 6D structure with Gaia-DR2 data
(EDP Sciences, 2020-11-16) Galli, P. A. B.; Bouy, H.; Olivares, J.; Miret Roig, N.; Vieira, R. G.; Sarro, L. M.; Barrado, D.; Berihuete, A.; Bertout, C.; Bertín, E.; Cuillandre, J. C.; European Research Council (ERC); Agencia Estatal de Investigación (AEI); Agence Nationale de la Recherche (ANR); Berihuete, A. [0000-0002-8589-4423]; Georgetti Vieira, R. [0000-0002-3607-3979]; Galli, P. [0000-0003-2271-9297]; Olivares Romero, J. [0000-0003-0316-2956]; Sarro, L. M. [0000-0002-5622-5191]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Context. Lupus is recognised as one of the closest star-forming regions, but the lack of trigonometric parallaxes in the pre-Gaia era hampered many studies on the kinematic properties of this region and led to incomplete censuses of its stellar population. Aims. We use the second data release of the Gaia space mission combined with published ancillary radial velocity data to revise the census of stars and investigate the 6D structure of the Lupus complex. Methods. We performed a new membership analysis of the Lupus association based on astrometric and photometric data over a field of 160 deg2 around the main molecular clouds of the complex and compared the properties of the various subgroups in this region. Results. We identified 137 high-probability members of the Lupus association of young stars, including 47 stars that had never been reported as members before. Many of the historically known stars associated with the Lupus region identified in previous studies are more likely to be field stars or members of the adjacent Scorpius-Centaurus association. Our new sample of members covers the magnitude and mass range from G ≃ 8 to G ≃ 18 mag and from 0.03 to 2.4 M⊙, respectively. We compared the kinematic properties of the stars projected towards the molecular clouds Lupus 1–6 and showed that these subgroups are located at roughly the same distance (about 160 pc) and move with the same spatial velocity. Our age estimates inferred from stellar models show that the Lupus subgroups are coeval (with median ages ranging from about 1 to 3 Myr). The Lupus association appears to be younger than the population of young stars in the Corona-Australis star-forming region recently investigated by our team using a similar methodology. The initial mass function of the Lupus association inferred from the distribution of spectral types shows little variation compared to other star-forming regions. Conclusions. In this paper, we provide an updated sample of cluster members based on Gaia data and construct the most complete picture of the 3D structure and 3D space motion of the Lupus complex.
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, A. P.; Henning, T.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Lafarga, M.; Marfil, E.; Montes, D.; Morales, J. C.; Nagel, E.; Sarro, L. M.; 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 Gaia Ultra-Cool Dwarf Sample – III: seven new multiple systems containing at least one Gaia DR2 ultracool dwarf
(Oxford Academics: Oxford University Press, 2020-04-15) Marocco, F.; Smart, R. L.; Mamajek, E. E.; Sarro, L. M.; Burgasser, A. J.; Caballero, J. A.; Rees, J. M.; Caselden, D.; Cruz, K. L.; Van Linge, R.; Pinfield, D. J.; National Aeronautics and Space Administration (NASA); Agencia Estatal de Investigación (AEI); 0000-0002-5622-5191; 0000-0002-4424-4766; 0000-0002-6523-9536; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
We present 10 new ultracool dwarfs in seven wide binary systems discovered using Gaia second data release data, identified as part of our Gaia Ultra-Cool Dwarf Sample project. The seven systems presented here include an L1 companion to the G5 IV star HD 164507, an L1: companion to the V478 Lyr AB system, an L2 companion to the metal-poor K5 V star CD-28 8692, an M9 V companion to the young variable K0 V star LT UMa, and three low-mass binaries consisting of late Ms and early Ls. The HD 164507, CD-28 8692, V478 Lyr, and LT UMa systems are particularly important benchmarks, because the primaries are well characterized and offer excellent constraints on the atmospheric parameters and ages of the companions. We find that the M8 V star 2MASS J23253550+4608163 is ∼2.5 mag overluminous compared to M dwarfs of similar spectral type, but at the same time it does not exhibit obvious peculiarities in its near-infrared spectrum. Its overluminosity cannot be explained by unresolved binarity alone. Finally, we present an L1+L2 system with a projected physical separation of 959 au, making this the widest L + L binary currently known.