Examinando por Autor "Mora, A."

Mostrando 1 - 5 de 5

Acceso Abierto
Exocomets: A spectroscopic survey
(EDP Sciences, 2020-07-01) Rebollido, I.; Eiroa, C.; Montesinos Comino, B.; Maldonado, J.; Villaver, E.; Absil, O.; Bayo, A.; Canovas, H.; Carmona, A.; Chen, Ch.; Ertel, E.; Henning, T.; Iglesias, D. P.; Launhardt, R.; Liseau, R.; Meeus, G.; Moór, A.; Mora, A.; Olofsson, J.; Rauw, Gregor; Rivière Marichalar, P.; Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT); Ministerio de Economía y Competitividad (MINECO); 0000-0002-4388-6417; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Context. While exoplanets are now routinely detected, the detection of small bodies in extrasolar systems remains challenging. Since the discovery of sporadic events, which are interpreted to be exocomets (falling evaporating bodies) around β Pic in the early 1980s, only ∼20 stars have been reported to host exocomet-like events. Aims. We aim to expand the sample of known exocomet-host stars, as well as to monitor the hot-gas environment around stars with previously known exocometary activity. Methods. We have obtained high-resolution optical spectra of a heterogeneous sample of 117 main-sequence stars in the spectral type range from B8 to G8. The data were collected in 14 observing campaigns over the course of two years from both hemispheres. We analysed the Ca II K&H and Na I D lines in order to search for non-photospheric absorptions that originated in the circumstellar environment and for variable events that could be caused by the outgassing of exocomet-like bodies. Results. We detected non-photospheric absorptions towards 50% of the sample, thus attributing a circumstellar origin to half of the detections (i.e. 26% of the sample). Hot circumstellar gas was detected in the metallic lines inspected via narrow stable absorptions and/or variable blue- and red-shifted absorption events. Such variable events were found in 18 stars in the Ca II and/or Na I lines; six of them are reported in the context of this work for the first time. In some cases, the variations we report in the Ca II K line are similar to those observed in β Pic. While we do not find a significant trend in the age or location of the stars, we do find that the probability of finding CS gas in stars with larger v sin i is higher. We also find a weak trend with the presence of near-infrared excess and with anomalous (λ Boo-like) abundances, but this would require confirmation by expanding the sample.
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, Enrique; 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.; 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, Enrique; Yoldas, A.; Lebreton, Y.; Royer, F.; Schultheis, M.; Viala, Y.; Kordopatis, G.; Becciani, U.; Leccia, S.; Mora, A.; Roux, W.; Barache, C.; Sagristà Sellés, A.; Tonello, N.; Busso, G.; Bramante, S.; Abbas, U.; Sadowski, G.; García Lario, P.; Recio Blanco, A.; Le Fustec, Y.; Marcos Santos, M. M. S.; Roegiers, T.; Madrero Pardo, P.; Nicolas, C.; Castañeda, J.; Segovia, J. C.; Altmann, M.; Sozzetti, A.; Bakker, J.; Crifo, F.; Masip, A.; Di Stefano, E.; Hernández, J.; Carlucci, T.; Halbwachs, J. L.; Spoto, F.; Mignard, F.; Fabricius, C.; Riello, M.; Carnerero, M. I.; Del Pozo, E.; Baudesson Stella, A.; Dapergolas, A.; Souami, D.; Aerts, C.; Creevey, O. L.; Alves, J.; Juaristi Campillo, J.; Molinaro, R.; Ordénovic, C.; Haigron, R.; Morbidelli, R.; Livanou, E.; García Reinaldos, M.; Bellas Velidis, I.; Van Dillen, E.; Guiraud, J.; Marchal, O.; Racero, E.; Burgess, P. W.; Balog, Z.; Andrae, R.; Portell, J.; Penttilä, A.; Giuffrida, G.; Carrasco, J. M.; Samaras, N.; Pagani, C.; Anglada Varela, E.; Garofalo, A.; Granvik, M.; Pailler, F.; Gosset, E.; Raiteri, C. M.; Zorec, J.; Fouesneau, M.; Poggio, E.; Garabato, D.; Ramos, P.; Cooper, W. J.; Baker, S. G.; Fienga, A.; Zwitter, T.; Brugaletta, E.; Bertone, S.; Gómez, A.; Zurbach, C.; Breedt, E.; Babusiaux, C.; Rainer, M.; Rybicki, K. A.; David, P.; Robin, C.; Anderson, R. I.; Van Reeven, W.; Guerrier, A.; De Ridder, J.; Van Leeuwen, M.; Korn, A. J.; Salguero, E.; Lammers, U.; Cancelliere, R.; Huckle, H. E.; Busonero, D.; Sordo, R.; Pauwels, T.; Dafonte, C.; Jansen, F.; Licata, E.; Gai, M.; Lanza, A. F.; Riclet, F.; Delisle, J. B.; Lorca, A.; Dolding, C.; Peñalosa Esteller, X.; Solitro, F.; Burlacu, A.; Semeux, D.; Rixon, G.; Bressan, A.; Bauchet, N.; Damerdji, Y.; Helmi, A.; Charlot, P.; Bastian, U.; Fernique, P.; Bassilana, J. L.; Barros, M.; Szabados, L.; Morel, T.; Jasniewicz, G.; Van Leeuwen, F.; Spagna, A.; Enke, H.; Hodgkin, S. T.; Antoja, T.; Brucciarelli, B.; Vaillant, M.; Hambly, N. C.; Accart, S.; Teixeira, R.; Michalik, D.; Vanel, O.; Kontizas, M.; Faigler, S.; Heiter, U.; Bellazzini, M.; Gavras, P.; Morris, D.; Hatzidimitriou, D.; González Santamaría, I.; Löffler, W.; Unger, C.; Zucker, S.; Le Campion, J. F.; Eappachen, D.; De Torres, A.; Ajaj, M.; Klioner, S. A.; De Teodoro, P.; Poretti, E.; Lattanzi, M. G.; Osborne, Paul; Hilger, T.; Palicio, P. A.; Balaguer Núñez, L.; Crosta, M.; Lambert, S.; Moitinho, A.; Reylé, C.; Messina, S.; Randich, S.; Baines, D.; Lister, T. A.; Castro Sampol, P.; Bailer Jones, C. A. L.; Panuzzo, P.; Gutierrez Sánchez, R.; Jean Antonie Piccolo, A.; Cropper, M.; González Vidal, J. J.; Franke, F.; Bombrun, A.; Holl, B.; Kervella, P.; Martín Polo, L.; Fraile, E.; Figueras, F.; Teyssier, D.; Siddiqui, H. I.; Panahi, A.; Utrilla, E.; Seabroke, G. M.; Marchant, J. M.; Cantat Gaudin, T.; Hutton, A.; Cheek, N.; Butkevich, A. G.; Delgado, A.; Berthier, J.; Sarasso, M.; Davidson, M.; Plum, G.; Marocco, F.; Caffau, E.; Molina, D.; Siebert, A.; Prusti, T.; Mulone, A. F.; De Bruijne, J. H. J.; Cellino, A.; Harrison, D. L.; Ragaini, S.; Mann, R. G.; Forderung der wissenschaftlichen Forschung (FWF); Belgian federal Science Policy Office (BELSPO); Hertha Firnberg Programme; Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP); Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES); Comite Francais d'Evaluation de la Cooperation Universitaire et Scientifique avec le Bresil (COFECUB); National Natural Science Foundation of China (NSFC); China Scholarship Council (CSC); European Commission (EC); European Research Council (ERC); Agence Nationale de la Recherche (ANR); European Space Agency (ESA); Centre National D'Etudes Spatiales (CNES); Istituto Nazionale di Astrofisica (INAF); Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR); Narodowe Centrum Nauki (NCN); Fundacao para a Ciencia e a Tecnologia (FCT); Slovenian Research Agency; Agencia Estatal de Investigación (AEI); Xunta de Galicia; Universitat de Barcelona (UB); Generalitat de Catalunya; Swedish National Space Agency (SNSA); United Kingdom Science and Technology Facilities Council (STFC); Krone Martins, A. [0000-0002-2308-6623]; Seabroke, G. [0000-0003-4072-9536]; Chiavassa, A. [0000-0003-3891-7554]; Castro Ginard, A. [0000-0002-9419-3725]; McMillan, P. [0000-0002-8861-2620]; Siltala, L. [0000-0002-6938-794X]; Delise, J. B. [0000-0001-5844-9888]; Aerts, C. [0000-0003-1822-7126]; Fedorets, G. [0000-0002-8418-4809]; Centro de Excelencia Científica Severo Ochoa, Instituto de Ciencias del Cosmos de la Universidad de Barcelona, SEV2015-0493; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2014-0369
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, Enrique; Di Matteo, P.; Gracia Abril, G.; Smart, R. L.; Lambert, S.; Creylé, C.; Cancelliere, R.; Murphy, C. P.; Teyssier, D.; Ulla, A.; Baudesson Stella, A.; Casamiquela, L.; Distefano, E.; Chiavassa, A.; Haztdimitriou, D.; Thévenin, F.; Dolding, C.; Delchambre, L.; Rybizki, J.; Pancino, E.; Dafonte, C.; Dapergolas, A.; Hernández, J.; De Ridder, J.; Caffau, E.; Faigler, S.; Rybicki, K. A.; Sadowski, G.; Sagristà Sellés, A.; Sahlmann, J.; Samaras, N.; Schultheis, M.; Garofalo, A.; Siddiqui, H. I.; Dell´Oro, A.; Gosset, E.; Spagna, A.; Holland, G.; Krone Martins, A.; Juaristi Campillo, J.; Castro Ginard, A.; Romero Gómez, M.; Ragaini, S.; Robichon, N.; Fouron, C.; Zurbach, C.; Morel, T.; Löffler, W.; Leccia, S.; Molnár, L.; Riva, A.; Gai, M.; Frémat, Y.; Panem, C.; Gómez, A.; Moitinho, A.; Osinde, J.; Hobbs, D.; Julbe, F.; Guy, L. P.; Muñoz, D.; Michalik, D.; Gerlach, E.; De Angeli, F.; Le Campion, J. F.; Nienartowicz, K.; Van Leeuwen, M.; Madrero Pardo, P.; Millar, N. R.; Damerdji, Y.; Pojoulet, E.; Guerrier, A.; Haywood, M.; Cooper, W. J.; Barros, M.; De Souza, R.; Huckle, H. E.; Burgess, P. W.; Karbevska, L.; Bellazzini, M.; Barache, C.; Bellas Velidis, I.; Bouquillon, S.; David, P.; Fabre, C.; Lanza, A. F.; Cánovas, H.; Leclerc, N.; Bagaglia, A.; Bernet, M.; Riclet, F.; Roux, W.; Sordo, R.; Tanga, P.; Portell, J.; Benson, K.; Carry, B.; Mulone, A. F.; Bucciarelli, B.; Galluccio, L.; Palaversa, L.; Castellani, M.; Peñalosa Esteller, X.; Luri, X.; Holl, B.; Muinonen, K.; Mastrobuono Battisti, A.; Destroffer, D.; Semeux, D.; Castro Sampol, P.; Raiteri, C. M.; Cropper, M.; Jean Antonie Piccolo, A.; Esquej, P.; Eyer, L.; Pauwels, T.; Cioni, M. R. L.; Souchay, J.; Pagano, I.; Penttilä, A.; Noval, L.; Siltala, L.; Guerra, R.; Bastian, U.; Accart, S.; Racero, E.; Bossini, D.; Rixon, G.; Santoveña, R.; Bombrun, A.; Zwitter, T.; Aguado, J. J.; Sánchez Giménez, V.; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MINECO/ICTI2013-2016/MDM-2014-0369; Centrode Excelencia Científica Instituto de Ciencias del Cosmos Universidad de Barcelona, MINECO/ICTI2013-2016/SEV2015-0493; Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP); Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES); National Natural Science Foundation of China (NSFC); Estonian Ministry of Education and Research; Centre National D'Etudes Spatiales (CNES); Agence Nationale de la Recherche (ANR); Centre National de la Recherche Scientifique (CNRS); European Commission (EC); European Research Council (ERC); Institut des Sciences de l'Univers (INSU); Institut National Polytechnique (INP); Institut National de Physique nucleaire et de Physique des Particules (IN2P3); Deutsches Zentrum für Luft- und Raumfahrt (DLR); Hungarian Academy of Sciences; Hungarian National Research, Development, and Innovation Office (NKFIH); Science Foundation Ireland (SFI); Israel Science Foundation (ISF); Agenzia Spaziale Italiana (ASI); Italian Istituto Nazionale di Astrofisica (INAF); Netherlands Organisation for Scientific Research (NWO); Polish National Science Centre; Ministry of Science and Higher Education (MNiSW); Fundacao para a Ciencia e a Tecnologia (FCT); Slovenian Research Agency; Xunta de Galicia; Agencia Estatal de Investigación (AEI); Generalitat de Catalunya; United Kingdom Science and Technology Facilities Council (STFC); United Kingdom Space Agency (UKSA); Krone Martins, A. [0000-0002-2308-6623]; McMillan, P. [0000-0002-8861-2620]; Carrasco Martínez, J. P. [0000-0002-3029-5853]; Sozzetti, A. [0000-0002-7504-365X]; Centros de Excelencia Severo Ochoa, BARCELONA SUPERCOMPUTING CENTER (BSC), SEV2015-0493
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
The A-shell star ϕ Leo revisited: its photospheric and circumstellar spectra
(EDP Sciences, 2021-09-21) Eiroa, C.; Montesinos Comino, B.; Rebollido, I.; Henning, T.; Launhardt, R.; Maldonado, J.; Meeus, G.; Mora, A.; Rivière Marichalar, P.; Villaver, E.; Agencia Estatal de Investigación (AEI); Ministerio de Economía y Competitividad (MINECO); Istituto Nazionale di Astrofisica (INAF); Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Context. We previously suggested that variable red- and blueshifted absorption features observed in the Ca II K line towards the A-type shell star ϕ Leo are likely due to solid, comet-like bodies in the circumstellar (CS) environment. Aims. Our aim is to expand our observational study of ϕ Leo to other characteristic spectral lines of A-type photospheres as well as to lines arising in their CS shells. Methods. We obtained more than 500 high-resolution optical spectra collected at different telescopes over 37 nights in several observing runs from December 2015 to January 2019. Consecutive time-series spectra were taken, covering intervals of up to ~9 h on some nights. We analysed some photospheric lines, in particular Ca I 4226 Å and Mg II 4481 Å, as well as the circumstellar shell lines Ca II H and K, the Ca II IR triplet, Fe II 4924, 5018, and 5169 Å, Ti II 3685, 3759, and 3761 Å, and the Balmer lines Hα and Hβ. Results. Our observational study reveals that ϕ Leo is a variable δ Scuti star whose spectra show remarkable dumps and bumps superimposed on the photospheric line profiles, which vary in strength and sharpness, propagate from blue- to more redshifted radial velocities, and persist for a few hours. Similarly to other δ Scuti stars, these features are likely produced by non-radial pulsations. At the same time, all shell lines present emission at ~3 km s−1 centred at the core of the CS features, and two variable absorption minima at both sides of the emission; those absorption minima occur at almost the same velocity for each line, that is, no apparent dynamical evolution is observed. The variations observed in the Ca II H and K, Fe II, and Ti II lines occur on a range of timescales from minutes to days and between observing runs, but without any clear correlation or recognisable temporal pattern among the different lines. In the case of Hα, the CS contribution is also variable in just one of the observing runs. Conclusions. We suggest that ϕ Leo is a rapidly rotating δ Scuti star surrounded by a variable, (nearly) edge-on CS disk possibly re-supplied by the δ Scuti pulsations. The behaviour of the CS shell lines is reminiscent of that of rapidly rotating Be shell stars with an edge-on CS disk, and is clear evidence that the variations observed in the CS features of ϕ Leo are highly unlikely to be produced by exocomets. In addition, the observational results presented in this work, together with some recent results concerning the shell star HR 10, highlight the need for critical revision of the Ca II K features, which have been attributed to exocomets in other shell stars.