Examinando por Autor "Delisle, J. B."

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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
Six transiting planets and a chain of Laplace resonances in TOI-178
(EDP Sciences, 2021-05-06) Leleu, A.; Alibert, Y.; Hara, N. C.; Hooton, M. J.; Wilson, T. G.; Robutel, P.; Delisle, J. B.; Laskar, J.; Hoyer, S.; Lovis, C.; Bryant, E. M.; Ducrot, E.; Gillen, E.; Alonso, R.; Pepe, F. A.; Correia, A. C. M.; Alves, D.; Cooke, B. F.; Cristiani, S.; Damasso, M.; Simon, A. E.; Angerhausen, D.; Günther, M. N.; Beck, M.; Queloz, D.; Dumusque, X.; Beck, T.; Di Marcoantonio, P.; Ehrenreich, D.; Erikson, A.; Olofsson, G.; Bourrier, V.; Reimers, C.; Futyan, D.; Boué, G.; Fridlund, M.; Gandolfi, D.; García Muñoz, Antonio; Peter, G.; Burleigh, M. R.; Bárczy, T.; Guillon, M.; Goad, M. R.; Cabrera, J.; Chamberlain, S.; Moyaro, M.; Davies, M. B.; Thomas, N.; Isaak, K.; Deleuil, M.; Heng, K.; Jehin, E.; Jenkins, J. S.; Anglada Escudé, G.; Pedersen, P. P.; Figueira, P.; Verrecchia, F.; Lecavelier des Etangs, A.; Fortier, A.; Lam, K.; Lendl, M.; Lillo Box, J.; Sousa, S. G.; García, L. J.; Osborn, Hugh P.; Gill, S.; Maxted, P. F. L.; McCormac, J.; Mehner, A.; Tilbrook, R. H.; Guedel, M.; Nunes, N. J.; Oshagh, M.; Ottensamer, R.; Charnoz, S.; Haldemann, J.; Sebastian, D.; Jordán, A.; Bekkelien, A.; Piotto, G.; Kiss, L.; Persson, C. M.; Polenta, G.; Pollacco, D.; Acton, J. S.; Lo Curto, G.; Brandeker, A.; Rando, N.; Magrin, D.; Ragazzoni, R.; Ratti, F.; Rauer, H.; Barrado, D.; Micela, G.; Molaro, P.; Ribas, I.; Santos, N. C.; Scandariato, G.; Billot, N.; Murray, C. A.; Zapatero Osorio, M. R.; Pagano, I.; Demory, B. O.; Sozzetti, A.; Pallé, E.; Smith, A. M. S.; Steller, M.; Suárez Mascareño, A.; Henderson, B.; Anderson, D. R.; Poretti, E.; Fossati, L.; Triaud, A.; Pozuelos, F. J.; Thompson, S.; Turner, O.; Udry, S.; Corral Van Damme, C.; Raynard, L.; Adibekyan, V.; Rebolo, R.; Vines, J. I.; Walton, N. A.; West, R. G.; Di Persio, G.; Schneider, J.; Delrez, L.; Allart, R.; Allende Prieto, C.; Nascimbeni, V.; Sestovic, M.; Cameron, A. C.; Szabó, G. M.; Kristiansen, M. H.; Barros, S. C. C.; Ségransan, D.; Asquier, J.; Baumjohann, W.; Bayliss, D.; Demangeon, O. D. S.; Van Grootel, V.; Martins, C. J. A. P.; Bonfanti, A.; Venus, H.; Benz, W.; Bonfils, X.; Bouchy, F.; Hogan, A. E.; Wheatley, P. J.; Wolter, D.; Broeg, C.; Buder, M.; Burdanov, A.; Lavie, B.; González Hernández, Carmen; Alvarez, M. [0000-0002-6786-2620]; Carrasco Martínez, J. M. [0000-0002-3029-5853]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Determining the architecture of multi-planetary systems is one of the cornerstones of understanding planet formation and evolution. Resonant systems are especially important as the fragility of their orbital configuration ensures that no significant scattering or collisional event has taken place since the earliest formation phase when the parent protoplanetary disc was still present. In this context, TOI-178 has been the subject of particular attention since the first TESS observations hinted at the possible presence of a near 2:3:3 resonant chain. Here we report the results of observations from CHEOPS, ESPRESSO, NGTS, and SPECULOOS with the aim of deciphering the peculiar orbital architecture of the system. We show that TOI-178 harbours at least six planets in the super-Earth to mini-Neptune regimes, with radii ranging from 1.152−0.070+0.073 to 2.87−0.13+0.14 Earth radii and periods of 1.91, 3.24, 6.56, 9.96, 15.23, and 20.71 days. All planets but the innermost one form a 2:4:6:9:12 chain of Laplace resonances, and the planetary densities show important variations from planet to planet, jumping from 1.02−0.23+0.28 to 0.177−0.061+0.055 times the Earth’s density between planets c and d. Using Bayesian interior structure retrieval models, we show that the amount of gas in the planets does not vary in a monotonous way, contrary to what one would expect from simple formation and evolution models and unlike other known systems in a chain of Laplace resonances. The brightness of TOI-178 (H = 8.76 mag, J = 9.37 mag, V = 11.95 mag) allows for a precise characterisation of its orbital architecture as well as of the physical nature of the six presently known transiting planets it harbours. The peculiar orbital configuration and the diversity in average density among the planets in the system will enable the study of interior planetary structures and atmospheric evolution, providing important clues on the formation of super-Earths and mini-Neptunes.
Acceso Abierto
Two temperate earth-mass planets orbiting the nearby star GJ 1002
(EDP Sciences, 2023-01-27) Suárez Mascareño, A.; González Álvarez, E.; Zapatero Osorio, M. R.; Lillo Box, J.; Faria, J. P.; Passegger, V. M.; Figueira, P.; Sozzetti, A.; Rebolo López, R.; Pepe, F.; Santos, N. C.; Cristiani, S.; Lovis, C.; Silva, André; Ribas, I.; Amado, P. J.; Caballero, J. A.; Quirrenbach, A.; Reiners, A.; Zechmeister, M.; Adibekyan, V.; Alibert, Y.; Béjar, V. J. S.; Benatti, S.; D´Odorico, V.; Damasso, M.; Delisle, J. B.; Di Marcantonio, P.; Dreizler, S.; Ehrenreich, D.; Hatzes, A. P.; Hara, N. C.; Henning, T.; Kaminski, A.; López González, M. J.; Martins, C. J. A. P.; Micela, G.; Montes, D.; Pallé, E.; Pedraz, S.; Rodríguez Martínez, Eloy; Rodríguez López, C.; Tal Or, L.; Sousa, S. G.; Udry, S.; González Hernández, Carmen; European Commission (EC); Ministerio de Ciencia e Innovación (MICINN); Agencia Estatal de Investigación (AEI); Consejo Superior de Investigaciones Científicas (CSIC); Fundacao para a Ciencia e a Tecnologia (FCT); Junta de Andalucía; Swiss National Science Foundation (SNSF); Cabildo de Gran Canaria
We report the discovery and characterisation of two Earth-mass planets orbiting in the habitable zone of the nearby M-dwarf GJ 1002 based on the analysis of the radial-velocity (RV) time series from the ESPRESSO and CARMENES spectrographs. The host star is the quiet M5.5 V star GJ 1002 (relatively faint in the optical, V ~ 13.8 mag, but brighter in the infrared, J ~ 8.3 mag), located at 4.84 pc from the Sun. We analyse 139 spectroscopic observations taken between 2017 and 2021. We performed a joint analysis of the time series of the RV and full-width half maximum (FWHM) of the cross-correlation function (CCF) to model the planetary and stellar signals present in the data, applying Gaussian process regression to deal with the stellar activity. We detect the signal of two planets orbiting GJ 1002. GJ 1002 b is a planet with a minimum mass mp sin i of 1.08 ± 0.13 M⊕ with an orbital period of 10.3465 ± 0.0027 days at a distance of 0.0457 ± 0.0013 au from its parent star, receiving an estimated stellar flux of 0.67 F⊕. GJ 1002 c is a planet with a minimum mass mp sin i of 1.36 ± 0.17 M⊕ with an orbital period of 20.202 ± 0.013 days at a distance of 0.0738 ± 0.0021 au from its parent star, receiving an estimated stellar flux of 0.257 F⊕. We also detect the rotation signature of the star, with a period of 126 ± 15 days. We find that there is a correlation between the temperature of certain optical elements in the spectrographs and changes in the instrumental profile that can affect the scientific data, showing a seasonal behaviour that creates spurious signals at periods longer than ~200 days. GJ 1002 is one of the few known nearby systems with planets that could potentially host habitable environments. The closeness of the host star to the Sun makes the angular sizes of the orbits of both planets (~9.7 mas and ~15.7 mas, respectively) large enough for their atmosphere to be studied via high-contrast high-resolution spectroscopy with instruments such as the future spectrograph ANDES for the ELT or the LIFE mission.