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1. PLATO as it is: A legacy mission for Galactic archaeology

Author: A. Miglio, C. Chiappini, B. Mosser, G. R. Davies, K. Freeman, L. Girardi, P. Jofré, D. Kawata, B. M. Rendle, M. Valentini, L. Casagrande, W. J. Chaplin, G. Gilmore, K. Hawkins, B. Holl, T. Appourchaux, K. Belkacem, D. Bossini, K. Brogaard, M.‐J. Goupil, J. Montalbán, A. Noels, F. Anders, T. Rodrigues, G. Piotto, D. Pollacco, H. Rauer, C. Allende Prieto, P. P. Avelino, C. Babusiaux, C. Barban, B. Barbuy, S. Basu, F. Baudin, O. Benomar, O. Bienaymé, J. Binney, J. Bland‐Hawthorn, A. Bressan, C. Cacciari, T. L. Campante, S. Cassisi, J. Christensen‐Dalsgaard, F. Combes, O. Creevey, M. S. Cunha, R. S. Jong, P. Laverny, S. Degl'Innocenti, S. Deheuvels, É. Depagne, J. Ridder, P. Di Matteo, M. P. Di Mauro, M.‐A. Dupret, P. Eggenberger, Y. Elsworth, B. Famaey, S. Feltzing, R. A. García, O. Gerhard, B. K. Gibson, L. Gizon, M. Haywood, R. Handberg, U. Heiter, S. Hekker, D. Huber, R. Ibata, D. Katz, S. D. Kawaler, H. Kjeldsen, D. W. Kurtz, N. Lagarde, Y. Lebreton, M. N. Lund, S. R. Majewski, P. Marigo, M. Martig, S. Mathur, I. Minchev, T. Morel, S. Ortolani, M. H. Pinsonneault, B. Plez, P. G. Prada Moroni, D. Pricopi, A. Recio‐Blanco, C. Reylé, A. Robin, I. W. Roxburgh, M. Salaris, B. X. Santiago, R. Schiavon, A. Serenelli, S. Sharma, V. Silva Aguirre, C. Soubiran, M. Steinmetz, D. Stello, K. G. Strassmeier, P. Ventura, R. Ventura, N. A. Walton, and C. C. Worley
Published: 2017
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2. Ultracool dwarfs in Gaia DR3

Author: L. M. Sarro, A. Berihuete, R. L. Smart, C. Reylé, D. Barrado, M. García-Torres, W. J. Cooper, H. R. A. Jones, F. Marocco, O. L. Creevey, R. Sordo, C. A. L. Bailer-Jones, P. Montegriffo, R. Carballo, R. Andrae, M. Fouesneau, A. C. Lanzafame, F. Pailler, F. Thévenin, A. Lobel, L. Delchambre, A. J. Korn, A. Recio-Blanco, M. S. Schultheis, F. De Angeli, N. Brouillet, L. Casamiquela, G. Contursi, P. de Laverny, P. García-Lario, G. Kordopatis, Y. Lebreton, E. Livanou, A. Lorca, P. A. Palicio, I. Slezak-Oreshina, C. Soubiran, A. Ulla, H. Zhao, University of Cadiz, INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), OSU-THETA - Observatoire des Sciences de l'Univers - Terre Homme Environnement Temps Astronomie (OSU-THETA), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), INAF - Osservatorio Astronomico di Bologna (OABO), Max Planck Institute for Astronomy (MPIA), Max-Planck Institute for Astronomy, Konigstuhl 17, D-69117, Heidelberg, Germany, Centre National d'Études Spatiales [Toulouse] (CNES), Royal Observatory of Belgium [Brussels] (ROB), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Physique de Rennes (IPR), and Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), stars, pre-main sequence, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, methods, Astrophysics - Solar and Stellar Astrophysics, Astronomi, astrofysik och kosmologi, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), low-mass, Hertzsprung-Russell and C-M diagrams, Astronomy, Astrophysics and Cosmology, late-type, statistical, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics, brown dwarfs
Abstract: Aims. In this work we use the Gaia DR3 set of ultracool dwarf candidates and complement the Gaia spectrophotometry with additional photometry in order to characterise its global properties. This includes the inference of the distances, their locus in the Gaia colour-absolute magnitude diagram and the (biased through selection) luminosity function in the faint end of the Main Sequence. We study the overall changes in the Gaia RP spectra as a function of spectral type. We study the UCDs in binary systems, attempt to identify low-mass members of nearby young associations, star forming regions and clusters, and analyse their variability properties. Results. We detect 57 young, kinematically homogeneous groups some of which are identified as well known star forming regions, associations and clusters of different ages. We find that the primary members of 880 binary systems with a UCD belong mainly to the thin and thick disk components of the Milky Way. We identify 1109 variable UCDs using the variability tables in the Gaia archive, 728 of which belong to the star forming regions defined by HMAC. We define two groups of variable UCDs with extreme bright or faint outliers. Conclusions. The set of sources identified as UCDs in the Gaia archive contains a wealth of information that will require focused follow-up studies and observations. It will help to advance our understanding of the nature of the faint end of the Main Sequence and the stellar/substellar transition., Accepted by Astronomy and Astrophysics. 29 pages, 20 figures plus 3 appendices
Published: 2023
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3. Gaia Early Data Release 3 The Gaia Catalogue of Nearby Stars

Author: Zoltan Balog, G. Tauran, Vincenzo Ripepi, Gerry Gilmore, M. Barros, Łukasz Wyrzykowski, Alberto Cellino, E. Poggio, P. Gavras, Simchon Faigler, Marc Audard, C. Nicolas, M. Vaillant, A. Mora, Paolo Tanga, Silvio Leccia, Despina Hatzidimitriou, A. Dapergolas, Eva Sciacca, Alberto Krone-Martins, N. Cheek, M. Hauser, Ulrike Heiter, S. Managau, L. Rohrbasser, Mathias Schultheis, E. Utrilla, Minia Manteiga, Marcella Marconi, Xavier Luri, F. De Angeli, Shay Zucker, Paolo Giacobbe, J. Juaristi Campillo, H. I. Siddiqui, J. Torra, F. X. Pineau, Roy Gomel, Thierry Morel, T. Cornez, Eric Gosset, Mario Gai, Jose M Hernandez, G. Giuffrida, A. de Torres, Laszlo Szabados, S. Ragaini, E. van Dillen, D. Semeux, Leanne P. Guy, R. Drimmel, L. M. Sarro, S. Voutsinas, Johannes Sahlmann, Damien Ségransan, S. Liao, Derek W. Morris, Jan Rybizki, André Moitinho, T. Roegiers, Bengt Edvardsson, Tristan Cantat-Gaudin, Martin Altmann, C. Turon, Laurent Chemin, K. Janßen, D. Garabato, Alejandra Recio-Blanco, Michał Pawlak, Lorenzo Rimoldini, Sergei A. Klioner, F. Torra, Carine Babusiaux, Alfred Castro-Ginard, G. Plum, Mariateresa Crosta, Iain A. Steele, A. Yoldas, Alex Lobel, J.-L. Bassilana, Harry Enke, Rosanna Sordo, Francesca Fragkoudi, F. De Luise, M. Bernet, Alessandro Sozzetti, M. Kontizas, Roberto Molinaro, C. Diener, S. Regibo, D. Barbato, T. Pauwels, R. E. de Souza, C. Fabricius, D. Souami, L. Martin Polo, M. Ramos-Lerate, Douglas J. Marshall, A. G. Butkevich, P. Madrero Pardo, P. Re Fiorentin, J. F. Le Campion, Jérôme Berthier, N. Tonello, Ummi Abbas, Y. Lebreton, M. Biermann, D. Munoz, N. Brouillet, David Teyssier, O. Vanel, P. A. Palicio, A. Jean-Antoine Piccolo, A. F. Lanza, Jesus Salgado, E. del Pozo, Antti Penttilä, R. Geyer, Ramachrisna Teixeira, L. Chaoul, Mike Smith, Rossella Cancelliere, J. M. Martín-Fleitas, D. Baines, M. Romero-Gómez, E. Anglada Varela, E. Livanou, X. Peñalosa Esteller, S. Diakite, Alberto Vecchiato, Thomas Wevers, Daniel Hestroffer, Sebastian L. Hidalgo, M. David, Angela Bragaglia, J. De Ridder, Mark Taylor, Roberto Morbidelli, A. Sagristà Sellés, Nigel Hambly, Arnaud Siebert, R. L. Smart, P. Burgess, Y. Le Fustec, Alessandro Bressan, H. Steidelmüller, Alberto Riva, H. E. Huckle, Morgan Fouesneau, N. Bauchet, P. Osborne, S. Marinoni, Krzysztof A. Rybicki, A. Masip, Laia Casamiquela, R. Messineo, A. Garofalo, Antonella Vallenari, R. Mor, Sahar Shahaf, P. de Laverny, G. Sadowski, Peter G. Jonker, A. Kochoska, F. Taris, A. F. Mulone, M. Ajaj, C. Ducourant, T. A. Lister, F. A. Jansen, Ruth Carballo, J. M. Carrasco, Tatiana Muraveva, W. van Reeven, P. Sartoretti, Jordi Portell, Andreas Korn, E. Salguero, Ana Ulla, P. Di Matteo, Coryn A. L. Bailer-Jones, J. Bakker, F. Riclet, G. Altavilla, Ulrich Bastian, P. Esquej, R. Buzzi, M. Segol, A. C. Lanzafame, L. Balaguer-Núñez, Beatrice Bucciarelli, C. Panem, E. Balbinot, T. Carlucci, Davide Massari, P. de Teodoro, Sébastien Lambert, M. I. Carnerero, Amina Helmi, F. Solitro, C. Robin, Carlos Dafonte, Tsevi Mazeh, A. Panahi, C. Fabre, Sergi Blanco-Cuaresma, Deborah Busonero, Maroussia Roelens, O. Marchal, Tomaz Zwitter, B. Holl, G. Holland, William Thuillot, Michael Davidson, E. Licata, Michele Bellazzini, Teresa Antoja, E. Szegedi-Elek, Francesca Figueras, Eric Slezak, Sergio Messina, N. Samaras, E. Poujoulet, Mark Cropper, A. Burlacu, R. Blomme, Elmé Breedt, Annie C. Robin, H. E. Delgado, Z. Kostrzewa-Rutkowska, Georges Kordopatis, Conny Aerts, L. Noval, Daniel Michalik, P. J. Richards, L. Karbevska, Grigori Fedorets, Maria Süveges, F. Crifo, J. Guiraud, D. Eappachen, K. Kruszyńska, Gisella Clementini, P. Yvard, Carme Jordi, L. Bramante, G. Busso, P. David, E. Fraile, Ugo Becciani, A. Lorca, Sanjeev Khanna, Alex Bombrun, Isabella Pagano, C. Dolding, A. M. Piersimoni, Paolo Montegriffo, A. Abreu Aramburu, Anthony G. A. Brown, Simon Hodgkin, Ennio Poretti, M. Fabrizio, I. Gonzalez-Santamaria, N. A. Walton, P. Panuzzo, Benoit Carry, Raphael Guerra, J. J. González-Vidal, T. Lebzelter, Nami Mowlavi, C. Barache, M. M. S. Marcos Santos, S. Cowell, Marco Castellani, J. J. Aguado, N. R. Millar, A. Baudesson-Stella, N. Leclerc, S. Bartolomé, J. Álvarez Cid-Fuentes, F. van Leeuwen, S. Bouquillon, Uwe Lammers, D. W. Evans, L. Eyer, M. van Leeuwen, A. Guerrier, J. González-Núñez, H. E. P. Lindstrøm, Miguel García-Torres, Ilaria Musella, L. Palaversa, W. Roux, W. Löffler, J.-B. Delisle, Dimitri Pourbaix, Timo Prusti, J. Osinde, M. Riello, G. Orrù, C. Crowley, Alessandra Mastrobuono-Battisti, Hector Canovas, D. L. Harrison, Y. Lasne, E. F. del Peloso, Laurent Galluccio, N. Hładczuk, T. Boch, Martin A. Barstow, László Molnár, Aldo Dell'Oro, C. Pagani, Krzysztof Nienartowicz, Stefano Bertone, Patrick Charlot, Eduard Masana, Elisabetta Caffau, N. Robichon, Luciana Bianchi, Federica Spoto, Felix Franke, J. L. Halbwachs, R. Gutiérrez-Sánchez, L. Pulone, Yassine Damerdji, Frédéric Arenou, Richard I. Anderson, Elena Pancino, David Hobbs, P. Castro Sampol, Yves Fremat, Pierre Kervella, C. Zurbach, Sofia Randich, Robert G. Mann, J. C. Segovia, Diego Bossini, D. Katz, Nicholas Rowell, P. Ramos, E. Racero, G. Gracia-Abril, R. Santoveña, R. Haigron, N. Unger, Enrique Solano, S. G. Baker, W. J. Cooper, F. Royer, S. Accart, George M. Seabroke, João Alves, Emese Plachy, Thomas Hilger, Pedro García-Lario, Gérard Jasniewicz, Kevin Benson, Christos Siopis, J. Souchay, Agnes Fienga, Giovanni Comoretto, F. Julbe, A. Hutton, Pierre Fernique, Céline Reylé, F. Pailler, Stefan Jordan, J. H. J. de Bruijne, C. A. Stephenson, E. Gerlach, Elisa Distefano, Karri Muinonen, Y. Viala, H. Zhao, L. Siltala, C. P. Murphy, Maria-Rosa L. Cioni, Andrea Chiavassa, D. Molina, J. Fernández-Hernández, G. Jevardat de Fombelle, Federico Marocco, Nicoletta Sanna, Alexey Mints, Juan Zorec, Ángel Gómez, I. Bellas-Velidis, M. G. Lattanzi, C. M. Raiteri, E. Brugaletta, Mikael Granvik, O. L. Creevey, Guy Rixon, Francois Mignard, P. M. Marrese, M. A. Álvarez, Caroline Soubiran, Rene Andrae, C. Ordénovic, A. Delgado, V. Sanchez Gimenez, J. Castañeda, D. Vicente, R. De March, A. Garcia-Gutierrez, M. Weiler, F. Thévenin, Lennart Lindegren, Isabelle Lecoeur-Taïbi, Jon Marchant, Monica Rainer, Alessandro Spagna, Andrej Prsa, M. Sarasso, Nicolas Rambaux, Paul J. McMillan, Ludovic Delchambre, M. Garcia-Reinaldos, M. Haywood, C. Fouron, S. Girona, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Universidad de Barcelona, Xunta de Galicia, Generalitat de Catalunya, INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astronomische Rechen-Institut [Heidelberg] (ARI), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg]-Universität Heidelberg [Heidelberg], Systèmes de Référence Temps Espace (SYRTE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Mésocentre de calcul (MESOCENTRE), Université de Franche-Comté (UFC), Centre de Données Astronomiques de Strasbourg, Partenaires INRAE, Géoazur (GEOAZUR 7329), Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), THALES, Université de Namur [Namur] (UNamur), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Universität Heidelberg [Heidelberg] = Heidelberg University-Universität Heidelberg [Heidelberg] = Heidelberg University, Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), THALES [France], Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Universidad de Cantabria, Gaia Collaboration, Planetary-system research, Department of Physics, Particle Physics and Astrophysics, Astronomy, and ITA
Subjects: trigonometric parallaxes, Solar neighborhood, Stars: luminosity function, mass function, Astronomy, Astrophysics, 01 natural sciences, luminosity function, mass function [Stars], Astronomi, astrofysik och kosmologi, luminosity: mass function [Stars], Astronomy, Astrophysics and Cosmology, MAIN-SEQUENCE, Hertzsprung-Russell-diagram, 010303 astronomy & astrophysics, Stars:low-mass brown-dwarfs, wide binaries, Physics, education.field_of_study, north galactic pole, Astrophysics::Instrumentation and Methods for Astrophysics, Astrometry, BROWN DWARF, Astrophysics - Solar and Stellar Astrophysics, mass function, NORTH GALACTIC POLE, Physical Sciences, symbols, CIRCULAR-VELOCITY CURVE, Halo, astro-ph.SR, Hertzsprung–Russell diagram, stars: luminosity function, astro-ph.GA, Posterior probability, Population, main-sequence, Luminosity-Function, FOS: Physical sciences, Mass-Function, Astronomy & Astrophysics, Computer Science::Digital Libraries, Photometry (optics), DWARF LUMINOSITY-FUNCTION, dwarf luminosity-function, sky-survey, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, luminosity function [stars], low-mass [Stars], 0103 physical sciences, Stars: luminosity: mass function, Stars: low-mass, WHITE-DWARFS, education, Solar and Stellar Astrophysics (astro-ph.SR), brown dwarf, catalogs, astrometry, Hertzsprung-Russell and C-M diagrams, stars: low-mass, solar neighborhood, Astrophysics - Astrophysics of Galaxies, SKY-SURVEY, white-dwarfs, Science & Technology, 010308 nuclear & particles physics, Luminosity function, White dwarf, TRIGONOMETRIC PARALLAXES, Astronomy and Astrophysics, Low-mass, 115 Astronomy, Space science, WIDE BINARIES, Stars, Physics::History of Physics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), solar-neighborhood, Catalogs, circular-velocity curve, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Aims. We produce a clean and well-characterised catalogue of objects within 100 pc of the Sun from the Gaia Early Data Release 3. We characterise the catalogue through comparisons to the full data release, external catalogues, and simulations. We carry out a first analysis of the science that is possible with this sample to demonstrate its potential and best practices for its use., Methods. Theselection of objects within 100 pc from the full catalogue used selected training sets, machine-learning procedures, astrometric quantities, and solution quality indicators to determine a probability that the astrometric solution is reliable. The training set construction exploited the astrometric data, quality flags, and external photometry. For all candidates we calculated distance posterior probability densities using Bayesian procedures and mock catalogues to define priors. Any object with reliable astrometry and a non-zero probability of being within 100 pc is included in the catalogue., Results. We have produced a catalogue of 331 312 objects that we estimate contains at least 92% of stars of stellar type M9 within 100 pc of the Sun. We estimate that 9% of the stars in this catalogue probably lie outside 100 pc, but when the distance probability function is used, a correct treatment of this contamination is possible. We produced luminosity functions with a high signal-to-noise ratio for the main-sequence stars, giants, and white dwarfs. We examined in detail the Hyades cluster, the white dwarf population, and wide-binary systems and produced candidate lists for all three samples. We detected local manifestations of several streams, superclusters, and halo objects, in which we identified 12 members of Gaia Enceladus. We present the first direct parallaxes of five objects in multiple systems within 10 pc of the Sun., Conclusions. We provide the community with a large, well-characterised catalogue of objects in the solar neighbourhood. This is a primary benchmark for measuring and understanding fundamental parameters and descriptive functions in astronomy.
Published: 2021
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4. Characterising the AGB bump and its potential to constrain mixing processes in stellar interiors

Author: G. Dréau, Y. Lebreton, B. Mosser, D. Bossini, J. Yu, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Centro de Astrofísica da Universidade do Porto (CAUP), and Universidade do Porto = University of Porto
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics - Solar and Stellar Astrophysics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: In the 90's, theoretical studies motivated the use of the asymptotic-giant branch bump (AGBb) as a standard candle given the weak dependence between its luminosity and stellar metallicity. Because of the small size of observed asymptotic-giant branch (AGB) samples, detecting the AGBb is not an easy task. However, this is now possible thanks to the wealth of data collected by the CoRoT, Kepler, and TESS space-borne missions. It is well-know that the AGB bump provides valuable information on the internal structure of low-mass stars, particularly on mixing processes such as core overshooting during the core He-burning phase. In this context, we analysed ~ 4,000 evolved giants observed by Kepler and TESS, including red-giant branch stars and AGB stars, for which asteroseismic and spectrometric data are available. By using statistical mixture models, we detected the AGBb both in frequency at maximum oscillation power and in effective temperature. Then, we used the Modules for Experiments in Stellar Astrophysics MESA stellar evolution code to model AGB stars and match the AGBb occurrence with observations. From observations, we could derive the AGBb location in 15 bins of mass and metallicity. We noted that the higher the mass, the later the AGBb occurs in the evolutionary track, which agrees with theoretical works. Moreover, we found a slight increase of the luminosity at the AGBb when the metallicity increases, which complicates the use of the AGBb as a standard candle. By fitting those observations with stellar models, we noticed that low-mass stars (M < 1.0 $M_{\odot}$) require a small core overshooting region during the core He-burning phase. This core overshooting extent increases toward high mass, but above M > 1.5 $M_{\odot}$ we found that the AGBb location cannot be reproduced with a realistic He-core overshooting alone, and instead additional mixing processes have to be invoked., 20 pages, 7 figures, accepted in A&A
Published: 2022
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5. Properties of the ionisation glitch: I. Modelling the ionisation region

Author: Marie-Jo Goupil, Pierre S. Houdayer, Daniel R. Reese, Y. Lebreton, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université de Rennes 1 (UR1), and Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Oscillation, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, 01 natural sciences, Computational physics, Astrophysics - Solar and Stellar Astrophysics, Convection zone, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Electron degeneracy pressure, 0103 physical sciences, Stellar structure, Glitch (astronomy), 010306 general physics, Adiabatic process, Degeneracy (mathematics), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Context. Determining the properties of solar-like oscillating stars can be subject to many biases. A particularly important example is the helium-mass degeneracy, where the uncertainties regarding the internal physics can cause a poor determination of both the mass and surface helium content. Accordingly, an independent helium estimate is needed to overcome this degeneracy. A promising way to obtain such an estimate is to exploit the so-called ionisation glitch, that is, the deviation from the asymptotic oscillation frequency pattern caused by the rapid structural variation in the He ionisation zones. Aims. Although it is progressively becoming more sophisticated, the glitch-based approach faces problems inherent to its current modelling such as the need for calibration using realistic stellar models. This requires a physical model of the ionisation region that explicitly involves the parameters of interest, such as the surface helium abundance, Ys. Methods. Through a thermodynamic treatment of the ionisation region, an analytical approximation for the first adiabatic exponent Γ1 is presented. Results. The induced stellar structure is found to depend on only three parameters, including the surface helium abundance Ys and the electron degeneracy ψCZ in the convective region. The model thus defined allows a wide variety of structures to be described, and it is in particular able to approximate a realistic model in the ionisation region. The modelling work we conducted enables us to study the structural perturbations causing the glitch. More elaborate forms of perturbations than those that are usually assumed are found. It is also suggested that there might be a stronger dependence of the structure on the electron degeneracy in the convection zone and on the position of the ionisation region rather than on the amount of helium itself. Conclusions. When analysing the ionisation glitch signature, we emphasise the importance of having a relation that can take these additional dependences into account.
Published: 2021
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6. Seismic constraints on the internal structure of evolved stars: From high-luminosity RGB to AGB stars

Author: Y. Lebreton, B. Mosser, Thomas Kallinger, G. Dréau, Charlotte Gehan, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Vancouver], University of British Columbia (UBC), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, 010504 meteorology & atmospheric sciences, Stellar mass, Oscillation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Metallicity, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Red-giant branch, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Asymptotic giant branch, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Stellar evolution, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: The space-borne missions CoRoT and Kepler opened up a new opportunity for better understanding stellar evolution by probing stellar interiors with unrivalled high-precision photometric data. Kepler has observed stellar oscillation for four years, which gave access to excellent frequency resolution that enables deciphering the oscillation spectrum of evolved red giant branch and asymptotic giant branch stars. The internal structure of stars in the upper parts of the red and asymptotic giant branches is poorly constrained, which makes the distinction between red and asymptotic giants difficult. We perform a thorough seismic analysis to address the physical conditions inside these stars and to distinguish them. We studied the oscillation mode properties of about 2.000 evolved giants in a model described by the asymptotic pressure-mode pattern of red giants, which includes the signature of the helium second-ionisation zone. We extracted the mode properties up to the degree l = 3 and investigated their dependence on stellar mass, metallicity, and evolutionary status. We identify a clear difference in the signature of the helium second-ionisation zone between red and asymptotic giants. We also detect a clear shortage of the energy of l = 1 modes after the core-He-burning phase. Furthermore, we note that the mode damping observed on the asymptotic giant branch is similar to that observed on the red giant branch. We highlight that the signature of the helium second-ionisation zone varies with stellar evolution. This provides us with a physical basis for distinguishing red giant branch stars from asymptotic giants. Here, our investigation of stellar oscillations allows us to constrain the physical processes and the key events that occur during the advanced stages of stellar evolution, with emphasis on the ascent along the asymptotic giant branch, including the asymptotic giant branch bump., Comment: 20 pages, 12 figures, accepted in A&A
Published: 2021
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7. Weighing stars from birth to death: mass determination methods across the HRD

Author: Paul G. Beck, M. G. Pedersen, Maria Bergemann, Vincent Van Eylen, Ignasi Ribas, Conny Aerts, Ian Czekala, Nicolas Lodieu, Eline Tolstoy, Marie Martig, Nate Bastian, Benard Nsamba, Davide Gandolfi, Ana Escorza, Keivan G. Stassun, Aldo Serenelli, George C. Angelou, Y. Lebreton, J. M. Bestenlehner, A. Moya, Krešimir Pavlovski, Achim Weiss, M. M. Miller Bertolami, J. S. G. Mombarg, D. Baroch, Victor Silva Aguirre, Diane Feuillet, Fabian Schneider, Juan Carlos Morales, Konstanze Zwintz, Mark Gieles, Nancy Elias-Rosa, Léo Girardi, Pier-Emmanuel Tremblay, University of Leuven, University of Heidelberg, Ministerio de Ciencia, Innovación y Universidades (España), National Aeronautics and Space Administration (US), Alexander von Humboldt Foundation, European Commission, Royal Society (UK), German Research Foundation, Fundação para a Ciência e a Tecnologia (Portugal), Generalitat de Catalunya, Ministerio de Economía y Competitividad (España), Max Planck Society, Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Max Planck Institute for Astronomy (MPIA), Max Planck Institute for Astrophysics, Max-Planck-Gesellschaft, Institute of Astronomy [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Radboud university [Nijmegen], Liverpool John Moores University (LJMU), Karl-Franzens-Universität Graz, Instituto de Astrofisica de Canarias (IAC), University of Sheffield [Sheffield], University of California, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institut d'Astronomie et d'Astrophysique [Bruxelles] (IAA), Université libre de Bruxelles (ULB), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), University College of London [London] (UCL), Lund Observatory, Lund University [Lund], Università degli studi di Torino (UNITO), Universitat de Barcelona (UB), Institució Catalana de Recerca i Estudis Avançats (ICREA), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Universidad de La Laguna [Tenerife - SP] (ULL), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET), Universidad Nacional de la Plata [Argentine] (UNLP), Universidad Politécnica de Madrid (UPM), University of Birmingham [Birmingham], Universidade do Porto, University of Zagreb, University of California [Santa Barbara] (UCSB), Heidelberger Institut für Theoretische Studien (H-ITS), Universität Heidelberg, Aarhus University [Aarhus], Vanderbilt University [Nashville], University of Groningen [Groningen], University of Warwick [Coventry], Universität Innsbruck [Innsbruck], A.S. acknowledges support from Grants ESP2017-82674-R and PID2019-108709GB-I00 (MICINN) and 2017-SGR-1131 (AGAUR). C.A., J.S.G.M., and M.G.P. received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement no. 670519: MAMSIE) and from the KU Leuven Research Council (grant C16/18/005: PARADISE). M.B. is supported through the Lise Meitner grant from the Max Planck Society and acknowledges support by the Collaborative Research centre SFB 881 (projects A5, A10), Heidelberg University, of the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation). V.S.A. acknowledges support from the Independent Research Fund Denmark (Research grant 7027-00096B) and the Carlsberg foundation (Grant agreement CF19-0649). Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement No. DNRF106). D.B., J.C.M., and I.R. acknowledge support from the Spanish Ministry of Science, Innovation and Universities (MICIU), and the Fondo Europeo de Desarrollo Regional (FEDER) through Grants ESP2016-80435-C2-1-R and PGC2018-098153-B-C33, as well as the support of the Generalitat de Catalunya (CERCA programme). N.B. gratefully acknowledge financial support from the Royal Society (University Research Fellowships) and from the European Research Council (ERC-CoG-646928, Multi-Pop). A.E. acknowledges support from the Research Foundation Flanders (FWO) under contract ZKD1501-00-W01 (Grant no. 792848). D.K.F. acknowledges funds from the Alexander von Humboldt Foundation in the framework of the Sofia Kovalevskaja Award endowed by the Federal Ministry of Education and Research and grant 2016-03412 from the Swedish Research Council. D.G. gratefully acknowledges financial support from the CRT foundation under Grant no. 2018.2323 'Gaseous or rocky? Unveiling the nature of small worlds'. L.G. acknowledges funding from LSST-Italy and from project MITiC 2015. N.L. was financially supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under Grant number AYA2015-69350-C3-2-P. A.M. acknowledges funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No 749962 (project THOT). B.N. is supported by Fundação para a Ciência e a Tecnologia (FCT, Portugal) under Grant PD/BD/113744/2015 from PhD::SPACE, an FCT PhD program, and by the Alexander von Humboldt Foundation. Further support from FEDER – Fundo Europeu de Desenvolvimento Regional funds through the COMPETE 2020 – Operacional Programme for Competitiveness and Internationalisation (POCI), and by Portuguese funds through FCT – Fundação para a Ciência e a Tecnologia in the framework of the Project POCI-01-0145-FEDER-030389 is also acknowledged. K.P. acknowledges support from the Croatian Science Foundation (HRZZ research Grant IP-2014-09-8656). P-E.T. has received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation programme n. 677706 (WD3D). The authors thank our colleagues G. Bono, T.L. Campante, M.S. Cunha, P. Das, C. Johnston, F. Kiefer, P. Maxted, M.J.P.F.G. Monteiro, Th. Rodrigues, V. Schaffenroth, M. Vučković for helpful comments and useful discussions. This work presents results from the European Space Agency (ESA) space mission Gaia and from the American National Aeronautics and Space Administration (NASA) space missions Kepler and TESS., Radboud University [Nijmegen], University of California (UC), Università degli studi di Torino = University of Turin (UNITO), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Universidade do Porto = University of Porto, and University of California [Santa Barbara] (UC Santa Barbara)
Subjects: 010504 meteorology & atmospheric sciences, Astronomy, Astrophysics, 01 natural sciences, planetary systems [Stars], Range (statistics), stellar content [Galaxy], Astrophysics::Solar and Stellar Astrophysics, PRECISION RADIAL-VELOCITIES, 010303 astronomy & astrophysics, QC, Stars: fundamental parameters, Complement (set theory), QB, Physics, Sequence, Galaxy: stellar content, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], BROWN DWARF CANDIDATES, Methods: numerical, Asteroseismology, Exoplanet, Stars: evolution, LINED SPECTROSCOPIC BINARIES, Astrophysics - Solar and Stellar Astrophysics, Physical Sciences, INTERMEDIATE ASTROMETRIC DATA, Determination methods, Astrophysics::Earth and Planetary Astrophysics, Solar and stellar Astrophysics, FOS: Physical sciences, evolution [Stars], Astronomy & Astrophysics, fundamental parameters [Stars], binaries: eclipsing [Stars], Stars: planetary systems, 0103 physical sciences, GALACTIC GLOBULAR-CLUSTERS, Stars: binaries: eclipsing, Stellar archaeology, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Science & Technology, numerical [Methods], [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], FUNDAMENTAL STELLAR PARAMETERS, Astronomy and Astrophysics, TRANSITING EXTRASOLAR PLANETS, COMMON ENVELOPE BINARY, Astronomía, Stars, DETACHED ECLIPSING BINARIES, RED GIANT BRANCH, Space and Planetary Science
Abstract: The mass of a star is the most fundamental parameter for its structure, evolution, and final fate. It is particularly important for any kind of stellar archaeology and characterization of exoplanets. There exist a variety of methods in astronomy to estimate or determine it. In this review we present a significant number of such methods, beginning with the most direct and model-independent approach using detached eclipsing binaries. We then move to more indirect and model-dependent methods, such as the quite commonly used isochrone or stellar track fitting. The arrival of quantitative asteroseismology has opened a completely new approach to determine stellar masses and to complement and improve the accuracy of other methods. We include methods for different evolutionary stages, from the pre-main sequence to evolved (super)giants and final remnants. For all methods uncertainties and restrictions will be discussed. We provide lists of altogether more than 200 benchmark stars with relative mass accuracies between [0.3 , 2] % for the covered mass range of M∈[0.1,16]M⊙, 75 % of which are stars burning hydrogen in their core and the other 25 % covering all other evolved stages. We close with a recommendation how to combine various methods to arrive at a “mass-ladder” for stars., The authors are much indebted to all colleagues participating in the workshop, even though they were not involved in the textual contributions for this review paper. A.S. acknowledges support from Grants ESP2017-82674-R and PID2019-108709GB-I00 (MICINN) and 2017-SGR-1131 (AGAUR). C.A., J.S.G.M., and M.G.P. received funding from the European Research Council (ERC) under the European Union?s Horizon 2020 research and innovation programme (Grant agreement no.?670519: MAMSIE) and from the KU?Leuven Research Council (grant C16/18/005: PARADISE). M.B. is supported through the Lise Meitner grant from the Max Planck Society and acknowledges support by the Collaborative Research centre SFB 881 (projects A5, A10), Heidelberg University, of the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation). V.S.A. acknowledges support from the Independent Research Fund Denmark (Research grant 7027-00096B) and the Carlsberg foundation (Grant agreement CF19-0649). Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement No.?DNRF106). D.B., J.C.M., and I.R. acknowledge support from the Spanish Ministry of Science, Innovation and Universities (MICIU), and the Fondo Europeo de Desarrollo Regional (FEDER) through Grants ESP2016-80435-C2-1-R and PGC2018-098153-B-C33, as well as the support of the Generalitat de Catalunya (CERCA programme). N.B. gratefully acknowledge financial support from the Royal Society (University Research Fellowships) and from the European Research Council (ERC-CoG-646928, Multi-Pop). A.E. acknowledges support from the Research Foundation Flanders (FWO) under contract ZKD1501-00-W01 (Grant no. 792848). D.K.F. acknowledges funds from the Alexander von Humboldt Foundation in the framework of the Sofia Kovalevskaja Award endowed by the Federal Ministry of Education and Research and grant 2016-03412 from the Swedish Research Council. D.G. gratefully acknowledges financial support from the CRT foundation under Grant no. 2018.2323 ?Gaseous or rocky? Unveiling the nature of small worlds ?. L.G. acknowledges funding from LSST-Italy and from project MITiC 2015. N.L. was financially supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under Grant number AYA2015-69350-C3-2-P. A.M. acknowledges funding from the European Union?s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No?749962 (project THOT). B.N. is supported by Funda??o para a Ci?ncia e a Tecnologia (FCT, Portugal) under Grant PD/BD/113744/2015 from PhD::SPACE, an FCT PhD program, and by the Alexander von?Humboldt Foundation. Further support from FEDER ? Fundo Europeu de Desenvolvimento Regional funds through the COMPETE 2020 ? Operacional Programme for Competitiveness and Internationalisation (POCI), and by Portuguese funds through FCT ? Funda??o para a Ci?ncia e a Tecnologia in the framework of the Project POCI-01-0145-FEDER-030389 is also acknowledged. K.P. acknowledges support from the Croatian Science Foundation (HRZZ research Grant IP-2014-09-8656). P-E.T. has received funding from the European Research Council under the European Union?s Horizon 2020 research and innovation programme n.?677706 (WD3D). The authors thank our colleagues G.?Bono, T.L.?Campante, M.S.?Cunha, P. Das, C.?Johnston, F.?Kiefer, P.?Maxted, M.J.P.F.G.?Monteiro, Th.?Rodrigues, V. Schaffenroth, M. Vu?kovi? for helpful comments and useful discussions. This work presents results from the European Space Agency (ESA) space mission Gaia and from the American National Aeronautics and Space Administration (NASA) space missions Kepler and TESS.
Published: 2021
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8. Gaia Early Data Release 3: Structure and properties of the Magellanic Clouds

Author: 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. Cioni, M.-R.L. Fabricius, C. Garofalo, A. Helmi, A. Muraveva, T. Brown, A.G.A. Vallenari, A. Prusti, T. De Bruijne, J.H.J. Babusiaux, C. Biermann, M. Creevey, O.L. Evans, D.W. Eyer, L. Hutton, A. Jansen, F. Jordi, C. Klioner, S.A. Lammers, U. Lindegren, L. Mignard, F. Panem, C. Pourbaix, D. Randich, S. Sartoretti, P. Soubiran, C. Walton, N.A. Arenou, F. Bailer-Jones, C.A.L. Bastian, U. Cropper, M. Drimmel, R. Katz, D. Lattanzi, M.G. Van Leeuwen, F. Bakker, J. Castañeda, J. De Angeli, F. Ducourant, C. Fouesneau, M. Frémat, Y. Guerra, R. Guerrier, A. Guiraud, J. Jean-Antoine Piccolo, A. Masana, E. Messineo, R. Mowlavi, N. Nicolas, C. Nienartowicz, K. Pailler, F. Panuzzo, P. Riclet, F. Roux, W. Seabroke, G.M. Sordo, R. Tanga, P. Thévenin, F. Gracia-Abril, G. Portell, J. Teyssier, D. Altmann, M. Andrae, R. Bellas-Velidis, I. Benson, K. Berthier, J. Blomme, R. Brugaletta, E. Burgess, P.W. Busso, G. Carry, B. Cellino, A. Cheek, N. Damerdji, Y. Davidson, M. Delchambre, L. Dell'Oro, A. Fernández-Hernández, J. Galluccio, L. García-Lario, P. Garcia-Reinaldos, M. González-Núñez, J. Gosset, E. Haigron, R. Halbwachs, J.-L. Hambly, N.C. Harrison, D.L. Hatzidimitriou, D. Heiter, U. Hernández, J. Hestroffer, D. Hodgkin, S.T. Holl, B. Janßen, K. Jevardat De Fombelle, G. Jordan, S. Krone-Martins, A. Lanzafame, A.C. Löffler, W. Lorca, A. Manteiga, M. Marchal, O. Marrese, P.M. Moitinho, A. Mora, A. Muinonen, K. Osborne, P. Pancino, E. Pauwels, T. Recio-Blanco, A. Richards, P.J. Riello, M. Rimoldini, L. Robin, A.C. Roegiers, T. Rybizki, J. Siopis, C. Smith, M. Sozzetti, A. Ulla, A. Utrilla, E. Van Leeuwen, M. Van Reeven, W. Abbas, U. Abreu Aramburu, A. Accart, S. Aerts, C. Aguado, J.J. Ajaj, M. Altavilla, G. Álvarez, M.A. Álvarez Cid-Fuentes, J. Alves, J. Anderson, R.I. Anglada Varela, E. Antoja, T. Audard, M. Baines, D. Baker, S.G. Balaguer-Núñez, L. Balog, Z. Barache, C. Barbato, D. Barros, M. Barstow, M.A. Bartolomé, S. Bassilana, J.-L. Bauchet, N. Baudesson-Stella, A. Becciani, U. Bellazzini, M. Bernet, M. Bertone, S. Bianchi, L. Blanco-Cuaresma, S. Boch, T. Bombrun, A. Bossini, D. Bouquillon, S. Bragaglia, A. Bramante, L. Breedt, E. Bressan, A. Brouillet, N. Bucciarelli, B. Burlacu, A. Busonero, D. Butkevich, A.G. Buzzi, R. Caffau, E. Cancelliere, R. Cánovas, H. Cantat-Gaudin, T. Carballo, R. Carlucci, T. Carnerero, M.I. Carrasco, J.M. Casamiquela, L. Castellani, M. Castro Sampol, P. Chaoul, L. Charlot, P. Chiavassa, A. Comoretto, G. Cooper, W.J. Cornez, T. Cowell, S. Crifo, F. Crosta, M. Crowley, C. Dafonte, C. Dapergolas, A. David, M. David, P. De Laverny, P. De Luise, F. De March, R. De Ridder, J. De Souza, R. De Teodoro, P. De Torres, A. Del Peloso, E.F. Del Pozo, E. Delgado, A. Delisle, J.-B. Di Matteo, P. Diakite, S. Diener, C. Distefano, E. Dolding, C. Eappachen, D. Enke, H. Esquej, P. Fabre, C. Fabrizio, M. Faigler, S. Fedorets, G. Fernique, P. Fienga, A. Figueras, F. Fouron, C. Fragkoudi, F. Fraile, E. Franke, F. Gai, M. Garabato, D. Garcia-Gutierrez, A. García-Torres, M. Gavras, P. Gerlach, E. Geyer, R. Giacobbe, P. Gilmore, G. Girona, S. Giuffrida, G. Gomez, A. Gonzalez-Santamaria, I. González-Vidal, J.J. Granvik, M. Gutiérrez-Sánchez, R. Guy, L.P. Hauser, M. Haywood, M. Hidalgo, S.L. Hilger, T. Hładczuk, N. Hobbs, D. Holland, G. Huckle, H.E. Jasniewicz, G. Jonker, P.G. Juaristi Campillo, J. Julbe, F. Karbevska, L. Kervella, P. Khanna, S. Kochoska, A. Kontizas, M. Kordopatis, G. Korn, A.J. Kostrzewa-Rutkowska, Z. Kruszyńska, K. Lambert, S. Lanza, A.F. Lasne, Y. Le Campion, J.-F. Le Fustec, Y. Lebreton, Y. Lebzelter, T. Leccia, S. Leclerc, N. Lecoeur-Taibi, I. Liao, S. Licata, E. Lindstrøm, H.E.P. Lister, T.A. Livanou, E. Lobel, A. Madrero Pardo, P. Managau, S. Mann, R.G. Marchant, J.M. Marconi, M. Marcos Santos, M.M.S. Marinoni, S. Marocco, F. Marshall, D.J. Martin Polo, L. Martín-Fleitas, J.M. Masip, A. Massari, D. Mastrobuono-Battisti, A. Mazeh, T. Messina, S. Michalik, D. Millar, N.R. Mints, A. Molina, D. Molinaro, R. Molnár, L. Montegriffo, P. Morbidelli, R. Morel, T. Morris, D. Mulone, A.F. Munoz, D. Murphy, C.P. Musella, I. Noval, L. Ordénovic, C. Orrù, G. Osinde, J. Pagani, C. Pagano, I. Palaversa, L. Palicio, P.A. Panahi, A. Pawlak, M. Peñalosa Esteller, X. Penttilä, A. Piersimoni, A.M. Pineau, F.-X. Plachy, E. Plum, G. Poggio, E. Poretti, E. Poujoulet, E. Prša, A. Pulone, L. Racero, E. Ragaini, S. Rainer, M. Raiteri, C.M. Rambaux, N. Ramos, P. Ramos-Lerate, M. Re Fiorentin, P. Regibo, S. Reylé, C. Riva, A. Rixon, G. Robichon, N. Robin, C. Roelens, M. Rohrbasser, L. Rowell, N. Royer, F. Rybicki, K.A. Sadowski, G. Sagristà Sellés, A. Sahlmann, J. Salgado, J. Salguero, E. Samaras, N. Gimenez, V.S. Sanna, N. Santoveña, R. Sarasso, M. Schultheis, M. Sciacca, E. Segol, M. Segovia, J.C. Ségransan, D. Semeux, D. Siddiqui, H.I. Siebert, A. Siltala, L. Slezak, E. Smart, R.L. Solano, E. Solitro, F. Souami, D. Souchay, J. Spagna, A. Spoto, F. Steele, I.A. Steidelmüller, H. Stephenson, C.A. Süveges, M. Szabados, L. Szegedi-Elek, E. Taris, F. Tauran, G. Taylor, M.B. Teixeira, R. Thuillot, W. Tonello, N. Torra, F. Torra, J. Turon, C. Unger, N. Vaillant, M. Van Dillen, E. Vanel, O. Vecchiato, A. Viala, Y. Vicente, D. Voutsinas, S. Weiler, M. Wevers, T. Wyrzykowski, L. Yoldas, A. Yvard, P. Zhao, H. Zorec, J. Zucker, S. Zurbach, C. Zwitter, T.
Abstract: 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. © ESO 2021.
Published: 2021

9. Modeling of two CoRoT solar analogues constrained by seismic and spectroscopic analysis

Author: J P Marques, Frédéric Baudin, Othman Benomar, Matthieu Castro, Caroline Barban, J. S. da Costa, Patrick Boumier, J. D. do Nascimento, Thierry Morel, Y. Lebreton, R. Samadi, Univesidade Federal do Rio Grande do Norte, Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), New York University [Abu Dhabi], NYU System (NYU), National Astronomical Observatory of Japan (NAOJ), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Liège, Universidade Federal do Rio Grande do Norte [Natal] (UFRN), Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), CNPq (Bolsa de Produtividade)Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ), Belspo Belgian Federal Science Policy Office, Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Harvard University-Smithsonian Institution, and Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS)
Subjects: stars: abundances, Metallicity, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, asteroseismology, stars: interiors, 7. Clean energy, 01 natural sciences, Luminosity, Seismic analysis, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Stellar evolution, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Mode (statistics), Astronomy and Astrophysics, stars: solar-type, Radius, Effective temperature, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, stars: fundamental parameters
Abstract: Solar analogues are important stars to study for understanding the properties of the Sun. Evolutionary modeling, combined with seismic and spectroscopic analysis, becomes a powerful method to characterize stellar intrinsic parameters, such as mass, radius, metallicity and age.However, these characteristics, relevant for other aspects of astrophysics or exoplanetary system physics for example, are difficult to obtain with a high precision and/or accuracy. The goal of this study is to characterize the two solar analogues HD42618 and HD43587, observed by CoRoT. In particular, we aim to infer precise mass, radius, and age, using evolutionary modeling constrained by spectroscopic, photometric, and seismic analysis. These stars show evidences of being older than the Sun but with a relatively large lithium abundance. We present the seismic analysis of HD42618, and the modeling of the two solar analogs HD42618 andHD43587 using the CESTAM stellar evolution code. Models were computed to reproduce the spectroscopic (effective temperature and metallicity) and seismic (mode frequencies) data,and the luminosity of the stars, based on Gaia parallaxes. We infer very similar values of mass and radius for both stars compared to the literature, within the uncertainties, and reproduce correctly the seismic constraints. For HD42618, the modeling shows it is slightly less massive and older than the Sun. For HD43587, it confirms it is more massive and older than the Sun,in agreement with previous results. The use of chemical clocks improves the reliability of our age estimates., 8 pages, 5 figures, 4 tables
Published: 2021
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10. Gaia Early Data Release 3: Acceleration of the Solar System from Gaia astrometry

Author: 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. Gerlach, E. Geyer, R. Hilger, T. Lammers, U. Steidelmüller, H. Stephenson, C.A. Brown, A.G.A. Vallenari, A. Prusti, T. De Bruijne, J.H.J. Babusiaux, C. Creevey, O.L. Evans, D.W. Eyer, L. Hutton, A. Jansen, F. Jordi, C. Luri, X. Panem, C. Pourbaix, D. Randich, S. Sartoretti, P. Soubiran, C. Walton, N.A. Arenou, F. Bailer-Jones, C.A.L. Cropper, M. Drimmel, R. Katz, D. Lattanzi, M.G. Van Leeuwen, F. Bakker, J. Castañeda, J. De Angeli, F. Ducourant, C. Fabricius, C. Fouesneau, M. Frémat, Y. Guerra, R. Guerrier, A. Guiraud, J. Jean-Antoine Piccolo, A. Masana, E. Messineo, R. Mowlavi, N. Nicolas, C. Nienartowicz, K. Pailler, F. Panuzzo, P. Riclet, F. Roux, W. Seabroke, G.M. Sordo, R. Tanga, P. Thévenin, F. Gracia-Abril, G. Portell, J. Teyssier, D. Altmann, M. Andrae, R. Bellas-Velidis, I. Benson, K. Berthier, J. Blomme, R. Brugaletta, E. Burgess, P.W. Busso, G. Carry, B. Cellino, A. Cheek, N. Clementini, G. Damerdji, Y. Davidson, M. Delchambre, L. Dell'Oro, A. Fernández-Hernández, J. Galluccio, L. García-Lario, P. Garcia-Reinaldos, M. González-Núñez, J. Gosset, E. Haigron, R. Halbwachs, J.-L. Hambly, N.C. Harrison, D.L. Hatzidimitriou, D. Heiter, U. Hestroffer, D. Hodgkin, S.T. Holl, B. Janßen, K. Jevardat De Fombelle, G. Jordan, S. Krone-Martins, A. Lanzafame, A.C. Löffler, W. Lorca, A. Manteiga, M. Marchal, O. Marrese, P.M. Moitinho, A. Mora, A. Muinonen, K. Osborne, P. Pancino, E. Pauwels, T. Recio-Blanco, A. Richards, P.J. Riello, M. Rimoldini, L. Robin, A.C. Roegiers, T. Rybizki, J. Sarro, L.M. Siopis, C. Smith, M. Sozzetti, A. Ulla, A. Utrilla, E. Van Leeuwen, M. Van Reeven, W. Abbas, U. Abreu Aramburu, A. Accart, S. Aerts, C. Aguado, J.J. Ajaj, M. Altavilla, G. Álvarez, M.A. Álvarez Cid-Fuentes, J. Alves, J. Anderson, R.I. Anglada Varela, E. Antoja, T. Audard, M. Baines, D. Baker, S.G. Balaguer-Núñez, L. Balbinot, E. Balog, Z. Barache, C. Barbato, D. Barros, M. Barstow, M.A. Bartolomé, S. Bassilana, J.-L. Bauchet, N. Baudesson-Stella, A. Becciani, U. Bellazzini, M. Bernet, M. Bertone, S. Bianchi, L. Blanco-Cuaresma, S. Boch, T. Bossini, D. Bouquillon, S. Bramante, L. Breedt, E. Bressan, A. Brouillet, N. Bucciarelli, B. Burlacu, A. Busonero, D. Butkevich, A.G. Buzzi, R. Caffau, E. Cancelliere, R. Cánovas, H. Cantat-Gaudin, T. Carballo, R. Carlucci, T. Carnerero, M.I. Carrasco, J.M. Casamiquela, L. Castellani, M. Castro-Ginard, A. Castro Sampol, P. Chaoul, L. Charlot, P. Chemin, L. Chiavassa, A. Comoretto, G. Cooper, W.J. Cornez, T. Cowell, S. Crifo, F. Crosta, M. Crowley, C. Dafonte, C. Dapergolas, A. David, M. David, P. De Laverny, P. De Luise, F. De March, R. De Ridder, J. De Souza, R. De Teodoro, P. Del Peloso, E.F. Del Pozo, E. Delgado, A. Delgado, H.E. Delisle, J.-B. Di Matteo, P. Diakite, S. Diener, C. Distefano, E. Dolding, C. Eappachen, D. Enke, H. Esquej, P. Fabre, C. Fabrizio, M. Faigler, S. Fedorets, G. Fernique, P. Fienga, A. Figueras, F. Fouron, C. Fragkoudi, F. Fraile, E. Franke, F. Gai, M. Garabato, D. Garcia-Gutierrez, A. García-Torres, M. Garofalo, A. Gavras, P. Giacobbe, P. Gilmore, G. Girona, S. Giuffrida, G. Gomez, A. Gonzalez-Santamaria, I. González-Vidal, J.J. Granvik, M. Gutiérrez-Sánchez, R. Guy, L.P. Hauser, M. Haywood, M. Helmi, A. Hidalgo, S.L. Hładczuk, N. Holland, G. Huckle, H.E. Jasniewicz, G. Jonker, P.G. Juaristi Campillo, J. Julbe, F. Karbevska, L. Kervella, P. Khanna, S. Kochoska, A. Kordopatis, G. Korn, A.J. Kostrzewa-Rutkowska, Z. Kruszyńska, K. Lambert, S. Lanza, A.F. Lasne, Y. Le Campion, J.-F. Le Fustec, Y. Lebreton, Y. Lebzelter, T. Leccia, S. Leclerc, N. Lecoeur-Taibi, I. Liao, S. Licata, E. Lindstrøm, H.E.P. Lister, T.A. Livanou, E. Lobel, A. Madrero Pardo, P. Managau, S. Mann, R.G. Marchant, J.M. Marconi, M. Marcos Santos, M.M.S. Marinoni, S. Marocco, F. Marshall, D.J. Martin Polo, L. Martín-Fleitas, J.M. Masip, A. Massari, D. Mastrobuono-Battisti, A. Mazeh, T. Messina, S. Michalik, D. Millar, N.R. Mints, A. Molina, D. Molinaro, R. Molnár, L. Montegriffo, P. Mor, R. Morbidelli, R. Morel, T. Morris, D. Mulone, A.F. Munoz, D. Muraveva, T. Murphy, C.P. Musella, I. Noval, L. Ordénovic, C. Orrù, G. Osinde, J. Pagani, C. Pagano, I. Palaversa, L. Palicio, P.A. Panahi, A. Pawlak, M. Peñalosa Esteller, X. Penttilä, A. Piersimoni, A.M. Pineau, F.-X. Plachy, E. Plum, G. Poggio, E. Poretti, E. Poujoulet, E. Prša, A. Pulone, L. Racero, E. Ragaini, S. Rainer, M. Raiteri, C.M. Rambaux, N. Ramos, P. Re Fiorentin, P. Regibo, S. Reylé, C. Ripepi, V. Riva, A. Rixon, G. Robichon, N. Robin, C. Roelens, M. Rohrbasser, L. Romero-Gómez, M. Rowell, N. Royer, F. Rybicki, K.A. Sadowski, G. Sagristà Sellés, A. Sahlmann, J. Salgado, J. Salguero, E. Samaras, N. Sanchez Gimenez, V. Sanna, N. Santoveña, R. Sarasso, M. Schultheis, M. Sciacca, E. Segol, M. Segovia, J.C. Ségransan, D. Semeux, D. Siddiqui, H.I. Siebert, A. Siltala, L. Slezak, E. Smart, R.L. Solano, E. Solitro, F. Souami, D. Souchay, J. Spagna, A. Spoto, F. Steele, I.A. Süveges, M. Szabados, L. Szegedi-Elek, E. Taris, F. Tauran, G. Taylor, M.B. Teixeira, R. Thuillot, W. Tonello, N. Torra, F. Torra, J. Turon, C. Unger, N. Vaillant, M. Van Dillen, E. Vanel, O. Vecchiato, A. Viala, Y. Vicente, D. Voutsinas, S. Weiler, M. Wevers, T. Wyrzykowski, L. Yoldas, A. Yvard, P. Zhao, H. Zorec, J. Zucker, S. Zurbach, C. Zwitter, T.
Abstract: 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. © ESO 2021.
Published: 2021

11. The Galactic Anticentre

Author: Vincenzo Ripepi, A. de Torres, Annie C. Robin, Mariateresa Crosta, C. Diener, L. Noval, Daniel Michalik, P. J. Richards, L. Karbevska, K. Kruszyńska, E. Fraile, André Moitinho, Michał Pawlak, P. Panuzzo, M. Riello, Benoit Carry, A. Yoldas, Harry Enke, N. Tonello, P. Gavras, M. Vaillant, Rosanna Sordo, E. del Pozo, Lorenzo Rimoldini, M. Bernet, G. Orrù, W. van Reeven, J. M. Martín-Fleitas, S. Diakite, P. Burgess, P. Osborne, Derek W. Morris, M. I. Carnerero, Amina Helmi, Mike Smith, Iain A. Steele, Alessandro Sozzetti, M. Kontizas, A. Sagristà Sellés, Roberto Molinaro, B. Holl, D. Baines, D. Molina, J. Fernández-Hernández, S. Marinoni, Michele Bellazzini, Maria Süveges, Teresa Antoja, D. Barbato, Uwe Lammers, Isabella Pagano, Davide Massari, G. Plum, P. Ramos, G. Jevardat de Fombelle, M. Biermann, C. Crowley, Mathias Schultheis, D. W. Evans, P. A. Palicio, Paolo Montegriffo, Ramachrisna Teixeira, R. Blomme, Elmé Breedt, T. A. Lister, F. A. Jansen, Ruth Carballo, Marcella Marconi, A. Abreu Aramburu, J. M. Carrasco, F. Royer, S. Accart, A. Burlacu, S. Regibo, Andrej Prsa, M. Sarasso, Nicolas Rambaux, A. F. Mulone, Ana Ulla, Eric Gosset, Alessandra Mastrobuono-Battisti, George M. Seabroke, H. E. Delgado, Federico Marocco, C. Nicolas, T. Lebzelter, Nami Mowlavi, C. Barache, Nicoletta Sanna, G. Gracia-Abril, R. Santoveña, R. Haigron, N. Unger, Silvio Leccia, A. Jean-Antoine Piccolo, A. F. Lanza, Alberto Vecchiato, Thomas Wevers, F. Figueras, G. Busso, C. Fabre, P. Di Matteo, F. Riclet, F. Solitro, Eric Slezak, N. Samaras, João Alves, Emese Plachy, Timo Prusti, F. van Leeuwen, J. Osinde, O. Marchal, M. Ajaj, C. Ducourant, Tatiana Muraveva, Shay Zucker, H. Steidelmüller, Alberto Riva, D. Semeux, N. Cheek, Laurent Galluccio, Martin A. Barstow, Alex Bombrun, S. Liao, M. van Leeuwen, R. E. de Souza, P. de Laverny, T. Roegiers, Paul J. McMillan, G. Holland, Alexey Mints, G. Giuffrida, L. M. Sarro, Juan Zorec, G. Sadowski, P. Yvard, Carme Jordi, J. L. Halbwachs, Laurent Chemin, Ludovic Delchambre, M. Garcia-Reinaldos, Ugo Becciani, Diego Bossini, Ángel Gómez, Sergi Blanco-Cuaresma, Rossella Cancelliere, C. Fabricius, J. De Ridder, L. Eyer, L. Pulone, Simon Hodgkin, Ennio Poretti, F. De Angeli, M. Haywood, E. Anglada Varela, Antonella Vallenari, F. X. Pineau, D. Garabato, A. Guerrier, H. E. P. Lindstrøm, Thomas Hilger, I. Bellas-Velidis, Frédéric Arenou, Paolo Giacobbe, Ilaria Musella, Tristan Cantat-Gaudin, L. Palaversa, Pedro García-Lario, David Hobbs, C. Turon, E. Balbinot, P. de Teodoro, Sébastien Lambert, D. Katz, Angela Bragaglia, Anthony G. A. Brown, Paolo Tanga, P. Castro Sampol, J. C. Segovia, Alejandra Recio-Blanco, Yves Fremat, Jon Marchant, Jose M Hernandez, S. Ragaini, Sofia Randich, P. Re Fiorentin, J. F. Le Campion, Gisella Clementini, M. Segol, P. David, R. Drimmel, F. Crifo, J. Guiraud, M. David, R. L. Smart, M. Fabrizio, I. Gonzalez-Santamaria, D. Eappachen, M. G. Lattanzi, Miguel García-Torres, Andreas Korn, S. Voutsinas, László Molnár, Simchon Faigler, A. Mora, Nicholas Rowell, Antti Penttilä, R. Geyer, Sanjeev Khanna, Aldo Dell'Oro, H. E. Huckle, C. Dolding, N. Leclerc, Monica Rainer, R. Mor, J. Bakker, Maroussia Roelens, Douglas J. Marshall, A. G. Butkevich, Nigel Hambly, A. Masip, Laia Casamiquela, R. Messineo, Martin Altmann, A. M. Piersimoni, Alessandro Spagna, Gerry Gilmore, Stefano Bertone, Patrick Charlot, O. Vanel, Daniel Hestroffer, Marco Castellani, Sebastian L. Hidalgo, W. Roux, Łukasz Wyrzykowski, Krzysztof A. Rybicki, M. M. S. Marcos Santos, Raphael Guerra, Alberto Cellino, E. Poggio, Gérard Jasniewicz, J. J. González-Vidal, S. Cowell, Peter G. Jonker, C. M. Raiteri, S. Bartolomé, J. Álvarez Cid-Fuentes, Elisabetta Caffau, J. J. Aguado, N. R. Millar, Ulrike Heiter, Federica Spoto, Felix Franke, A. Baudesson-Stella, M. Barros, Tsevi Mazeh, A. Panahi, E. Brugaletta, R. Buzzi, Elena Pancino, G. Altavilla, E. Racero, Enrique Solano, Mikael Granvik, Minia Manteiga, C. Robin, Tomaz Zwitter, Deborah Busonero, Alberto Krone-Martins, Marc Audard, Kevin Benson, Christos Siopis, L. Balaguer-Núñez, C. A. L. Bailer-Jones, E. Poujoulet, O. L. Creevey, E. Szegedi-Elek, C. Fouron, Michael Davidson, E. Licata, Despina Hatzidimitriou, Mark Cropper, Z. Kostrzewa-Rutkowska, S. Managau, A. Dapergolas, Sergio Messina, Laszlo Szabados, H. I. Siddiqui, W. Löffler, Mario Gai, J.-B. Delisle, Leanne P. Guy, S. G. Baker, W. J. Cooper, Alfred Castro-Ginard, Conny Aerts, A. Lorca, Xavier Luri, Damien Ségransan, Grigori Fedorets, A. Garofalo, J. Juaristi Campillo, F. De Luise, F. Pailler, F. Taris, L. Bramante, Thierry Morel, T. Cornez, L. Martin Polo, M. Ramos-Lerate, Jordi Portell, E. Salguero, Sergei A. Klioner, K. Janßen, Ulrich Bastian, Stefan Jordan, P. Esquej, A. C. Lanzafame, Beatrice Bucciarelli, C. Panem, Y. Lebreton, Carlos Dafonte, S. Girona, D. Munoz, Dimitri Pourbaix, William Thuillot, J. H. J. de Bruijne, N. Brouillet, L. Chaoul, F. Torra, Alex Lobel, J.-L. Bassilana, Francesca Fragkoudi, M. Romero-Gómez, C. A. Stephenson, T. Pauwels, Eva Sciacca, Alessandro Bressan, Morgan Fouesneau, E. Livanou, E. Gerlach, X. Peñalosa Esteller, Roberto Morbidelli, L. Rohrbasser, Johannes Sahlmann, Elisa Distefano, P. Sartoretti, Karri Muinonen, Zoltan Balog, Y. Viala, J. Torra, H. Zhao, L. Siltala, G. Tauran, D. Souami, P. Madrero Pardo, David Teyssier, Jesus Salgado, J. Souchay, C. P. Murphy, Maria-Rosa L. Cioni, N. A. Walton, S. Bouquillon, Andrea Chiavassa, Agnes Fienga, Giovanni Comoretto, F. Julbe, A. Hutton, Yassine Damerdji, Richard I. Anderson, Pierre Fernique, Céline Reylé, M. Hauser, E. Utrilla, Pierre Kervella, C. Zurbach, Robert G. Mann, Ummi Abbas, Hector Canovas, D. L. Harrison, Y. Lasne, Mark Taylor, Y. Le Fustec, E. F. del Peloso, N. Bauchet, E. van Dillen, Jan Rybizki, N. Hładczuk, T. Boch, J. González-Núñez, Carine Babusiaux, C. Pagani, Krzysztof Nienartowicz, Eduard Masana, G. Kordopatis, N. Robichon, Luciana Bianchi, R. Gutiérrez-Sánchez, Arnaud Siebert, A. Kochoska, T. Carlucci, Jérôme Berthier, J. Castañeda, D. Vicente, R. De March, A. Garcia-Gutierrez, M. Weiler, F. Thévenin, Lennart Lindegren, Isabelle Lecoeur-Taïbi, Guy Rixon, Francois Mignard, P. M. Marrese, M. A. Álvarez, Caroline Soubiran, Rene Andrae, C. Ordénovic, A. Delgado, V. Sanchez Gimenez, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Universidad de Barcelona, Xunta de Galicia, European Commission, Centros de Excelencia Severo Ochoa, BARCELONA SUPERCOMPUTING CENTER (BSC), SEV2015-0493, 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], 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, Agencia Estatal de Investigación (AEI), Generalitat de Catalunya, United Kingdom Science and Technology Facilities Council (STFC), United Kingdom Space Agency (UKSA), Gaia Collaboration, Universidad de Cantabria, Astronomy, Kapteyn Astronomical Institute, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), M2A 2021, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Planetary-system research, Department of Physics, Particle Physics and Astrophysics, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: trigonometric parallaxes, SOLAR NEIGHBORHOOD, Astronomy, SAGITTARIUS DWARF GALAXY, Astrophysics, 01 natural sciences, sagittarius dwarf galaxy, 010303 astronomy & astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], solar neighborhood, Astrophysics::Instrumentation and Methods for Astrophysics, Astrometry, Gelexy: kinematics and dynamics, Kinematics and Dynamics, Open clusters and asssociations: individual: Berkeley 29, sky survey, Disk, Physical Sciences, kinematics and dynamics [Gelexy], old open clusters, MILKY-WAY, Astrophysics::Earth and Planetary Astrophysics, open clusters and associations: individual: Berkeley 29, Galaxy: kinematics and dynamics, disk [Galaxy], individual: Berkeley 29 [open clusters and associations], Astrometria, Berkeley 29, EXPLORING HALO SUBSTRUCTURE, LOCAL KINEMATICS, Milky Way, FOS: Physical sciences, Open Clusters and Associations, Individual, exploring halo substructure, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Computer Science::Digital Libraries, stellar structure, Galaxy: disk, Open clusters and associations: individual: Saurer 1, Galactic halo, Halo, Settore FIS/05 - Astronomia e Astrofisica, individual: Berkeley 29 [Open clusters and asssociations], 0103 physical sciences, distances [stars], halo [Galaxy], Disc, Stars: distances, milky-way, Saurer 1, Astrophysics::Galaxy Astrophysics, canis-major, Science & Technology, 010308 nuclear & particles physics, TRIGONOMETRIC PARALLAXES, Galaxy: halo, stars: distances, open clusters and associations: individual: Saurer 1, Astrophysics - Astrophysics of Galaxies, Astronomy and Astrophysics, Galactic plane, kinematics and dynamics [Galaxy], 115 Astronomy, Space science, CANIS-MAJOR, Stars, Galaxy, Physics::History of Physics, Estels, individual: Saurer 1 [open clusters and associations], Distances, local kinematics, OLD OPEN CLUSTERS, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), SKY SURVEY, Open cluster, STELLAR STRUCTURE
Abstract: 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.
Published: 2021
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12. Gaia early data release 3: summary of the contents and survey properties (Corrigendum)

Author: Mathias Schultheis, Marcella Marconi, N. Robichon, Luciana Bianchi, F. Crifo, J. Guiraud, D. Eappachen, R. Gutiérrez-Sánchez, Sanjeev Khanna, A. M. Piersimoni, Raphael Guerra, J. J. González-Vidal, J. J. Aguado, N. R. Millar, A. Baudesson-Stella, Tristan Cantat-Gaudin, Alejandra Recio-Blanco, Ummi Abbas, Francesca Figueras, R. Blomme, Elmé Breedt, G. Busso, A. Jean-Antoine Piccolo, Gerry Gilmore, A. Panahi, S. Messina, C. Babusiaux, Łukasz Wyrzykowski, Mark Taylor, Alex Bombrun, M. Barros, M. Riello, M. Ajaj, C. Ducourant, Tatiana Muraveva, Alberto Cellino, E. Poggio, Y. Le Fustec, C. P. Murphy, Maria-Rosa L. Cioni, Hector Canovas, D. L. Harrison, Y. Lasne, Elena Pancino, N. Bauchet, G. Orrù, Sergi Blanco-Cuaresma, Simon Hodgkin, Ennio Poretti, A. F. Lanza, Alberto Vecchiato, Thomas Wevers, Andrea Chiavassa, E. Szegedi-Elek, A. G. A. Brown, Laszlo Szabados, A. Masip, Laia Casamiquela, R. Messineo, C. Crowley, Alessandra Mastrobuono-Battisti, E. Poujoulet, Zoltan Balog, L. Eyer, A. Guerrier, H. E. P. Lindstrøm, Ilaria Musella, Laurent Galluccio, Martin A. Barstow, Aldo Dell'Oro, Mark Cropper, Z. Kostrzewa-Rutkowska, Angela Bragaglia, Arnaud Siebert, Damien Ségransan, A. Kochoska, J. L. Halbwachs, E. F. del Peloso, N. Hładczuk, F. Pailler, Stefan Jordan, Stefano Bertone, L. Pulone, Frédéric Arenou, Patrick Charlot, David Hobbs, P. Castro Sampol, Yves Fremat, Sofia Randich, Marc Audard, Despina Hatzidimitriou, A. Dapergolas, L. Palaversa, W. van Reeven, M. Hauser, E. Utrilla, Georges Kordopatis, Sergei A. Klioner, Alex Lobel, J.-L. Bassilana, G. Tauran, T. Prusti, H. Steidelmüller, Alberto Riva, Diego Bossini, Maria Süveges, Isabella Pagano, J. H. J. de Bruijne, Elisabetta Caffau, Federica Spoto, Felix Franke, T. Boch, M. I. Carnerero, T. Carlucci, Grigori Fedorets, J. Castañeda, W. Löffler, Enrique Solano, Paolo Montegriffo, A. Abreu Aramburu, T. Lebzelter, Nami Mowlavi, C. Barache, C. A. Stephenson, A. Lorca, L. Bramante, Amina Helmi, J.-B. Delisle, B. Holl, D. Molina, J. Fernández-Hernández, G. Jevardat de Fombelle, F. van Leeuwen, C. Robin, D. Katz, E. Gerlach, Elisa Distefano, Michele Bellazzini, P. de Laverny, G. Sadowski, Tomaz Zwitter, A. Burlacu, Teresa Antoja, Rossella Cancelliere, F. Torra, C. Pagani, Annie C. Robin, Johannes Sahlmann, Karri Muinonen, Eva Sciacca, D. Vicente, Krzysztof Nienartowicz, A. F. Mulone, Shay Zucker, Nicholas Rowell, H. E. Delgado, Dimitri Pourbaix, G. Giuffrida, H. E. Huckle, Federico Marocco, L. Noval, Daniel Michalik, P. J. Richards, Y. Viala, E. van Dillen, L. Karbevska, H. Zhao, L. Siltala, Nicoletta Sanna, K. Kruszyńska, E. Fraile, R. De March, Y. Lebreton, C. M. Raiteri, D. W. Evans, Ana Ulla, Francesca Fragkoudi, Jan Rybizki, E. Brugaletta, L. Rohrbasser, Andreas Korn, S. G. Baker, A. Garcia-Gutierrez, L. M. Sarro, R. Buzzi, T. Pauwels, Jérôme Berthier, L. Chaoul, W. J. Cooper, Eduard Masana, M. van Leeuwen, D. Garabato, P. Panuzzo, Maroussia Roelens, Benoit Carry, Deborah Busonero, Michael Davidson, J. González-Núñez, Thomas Hilger, E. Licata, M. Weiler, Mikael Granvik, Alessandro Bressan, Morgan Fouesneau, Miguel García-Torres, W. Roux, Pedro García-Lario, Iain A. Steele, P. Ramos, Alessandro Sozzetti, Roberto Molinaro, O. L. Creevey, D. Barbato, Lorenzo Rimoldini, Uwe Lammers, Alexey Mints, P. Sartoretti, E. Livanou, D. Souami, P. Madrero Pardo, David Teyssier, M. Bernet, Yassine Damerdji, X. Peñalosa Esteller, C. Fabre, F. Thévenin, Gérard Jasniewicz, Roberto Morbidelli, Jesus Salgado, Juan Zorec, Ángel Gómez, Douglas J. Marshall, A. G. Butkevich, M. Biermann, E. Racero, J. Torra, R. Gomel, O. Vanel, Daniel Hestroffer, Sebastian L. Hidalgo, P. A. Palicio, F. De Angeli, Richard L. Smart, J. M. Martín-Fleitas, Derek W. Morris, F. Royer, S. Diakite, S. Accart, C. Dolding, P. Burgess, Richard I. Anderson, A. Garofalo, I. Bellas-Velidis, George M. Seabroke, P. Osborne, Claus Fabricius, Jon Marchant, Ramachrisna Teixeira, João Alves, G. Gracia-Abril, R. Santoveña, R. Haigron, N. Unger, Lennart Lindegren, Isabelle Lecoeur-Taïbi, Paolo Giacobbe, Emese Plachy, M. Fabrizio, I. Gonzalez-Santamaria, F. Taris, Kevin Benson, Christos Siopis, M. M. S. Marcos Santos, S. Cowell, Jose M Hernandez, S. Ragaini, Jordi Portell, Linda K. Molnar, R. Drimmel, Pierre Kervella, C. Zurbach, S. Bartolomé, J. Álvarez Cid-Fuentes, E. Salguero, Ulrich Bastian, Robert G. Mann, Marco Castellani, J. Osinde, E. Balbinot, Caroline Soubiran, Rene Andrae, J. Souchay, M. G. Lattanzi, S. Voutsinas, Agnes Fienga, Giovanni Comoretto, P. Esquej, A. C. Lanzafame, Beatrice Bucciarelli, C. Panem, Carlos Dafonte, Alfred Castro-Ginard, J. C. Segovia, Monica Rainer, F. Julbe, A. Hutton, Peter G. Jonker, William Thuillot, A. de Torres, F. De Luise, Pierre Fernique, Céline Reylé, M. Kontizas, G. Plum, Martin Altmann, L. Martin Polo, M. Ramos-Lerate, P. de Teodoro, Sébastien Lambert, G. Altavilla, André Moitinho, D. Munoz, N. Brouillet, Alessandro Spagna, C. Ordénovic, Gisella Clementini, C. Nicolas, Michał Pawlak, Silvio Leccia, A. Delgado, M. Romero-Gómez, N. Cheek, A. Yoldas, Harry Enke, Rosanna Sordo, V. Sanchez Gimenez, Mike Smith, P. David, D. Baines, Paolo Tanga, Guy Rixon, Alberto Krone-Martins, S. Managau, N. A. Walton, S. Bouquillon, C. Fouron, Francois Mignard, Xavier Luri, J. Juaristi Campillo, S. Girona, Thierry Morel, T. Cornez, P. M. Marrese, M. A. Álvarez, S. Liao, Andrej Prsa, M. Sarasso, Nicolas Rambaux, Paul J. McMillan, Ludovic Delchambre, M. Garcia-Reinaldos, M. Haywood, E. Anglada Varela, Antonella Vallenari, S. Regibo, R. E. de Souza, Sahar Shahaf, J. De Ridder, M. Segol, Simchon Faigler, A. Mora, Ulrike Heiter, Carla Cacciari, Minia Manteiga, H. I. Siddiqui, Mario Gai, Leanne P. Guy, N. Leclerc, T. A. Lister, F. A. Jansen, Ruth Carballo, J. M. Carrasco, Bengt Edvardsson, P. Di Matteo, K. Janßen, F. Riclet, F. Solitro, O. Marchal, G. Holland, F. X. Pineau, C. Turon, P. Re Fiorentin, Tsevi Mazeh, Mariateresa Crosta, C. Diener, J. F. Le Campion, Vincenzo Ripepi, M. David, R. Mor, N. Tonello, E. del Pozo, J. Bakker, Davide Massari, A. Sagristà Sellés, Marco Delbo, Eric Slezak, P. Gavras, N. Samaras, S. Marinoni, M. Vaillant, J. M. Petit, P. Yvard, Carme Jordi, Ugo Becciani, Antti Penttilä, R. Geyer, Nigel Hambly, Krzysztof A. Rybicki, L. Balaguer-Núñez, C. A. L. Bailer-Jones, Conny Aerts, Eric Gosset, D. Semeux, T. Roegiers, and Laurent Chemin
Subjects: Physics, Addenda, 010504 meteorology & atmospheric sciences, Errata, Parallaxes, Astronomy, Astronomy and Astrophysics, Astrophysics, Astrometry, Photometric, 01 natural sciences, Techniques, catalogs, astrometry, parallaxes, proper motions, techniques: photometric, errata, addenda, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, 0103 physical sciences, Proper motions, Catalogs, 010303 astronomy & astrophysics, Data release, 0105 earth and related environmental sciences
Abstract: We present the early installment of the third Gaia data release, Gaia EDR3, consisting of astrometry and photometry for 1.8 billion sources brighter than magnitude 21, complemented with the list of radial velocities from Gaia DR2. Gaia EDR3 contains celestial positions and the apparent brightness in G for approximately 1.8 billion sources. For 1.5 billion of those sources, parallaxes, proper motions, and the (G_BP-G_RP) colour are also available. The passbands for G, G_BP, and G_RP are provided as part of the release. For ease of use, the 7 million radial velocities from Gaia DR2 are included in this release, after the removal of a small number of spurious values. New radial velocities will appear as part of Gaia DR3. Finally, Gaia EDR3 represents an updated materialisation of the celestial reference frame (CRF) in the optical, the Gaia-CRF3, which is based solely on extragalactic sources. The creation of the source list for Gaia EDR3 includes enhancements that make it more robust with respect to high proper motion stars, and the disturbing effects of spurious and partially resolved sources. The source list is largely the same as that for Gaia DR2, but it does feature new sources and there are some notable changes. The source list will not change for Gaia DR3. Gaia EDR3 represents a significant advance over Gaia DR2, with parallax precisions increased by 30 percent, proper motion precisions increased by a factor of 2, and the systematic errors in the astrometry suppressed by 30--40 percent for the parallaxes and by a factor ~2.5 for the proper motions. The photometry also features increased precision, but above all much better homogeneity across colour, magnitude, and celestial position. A single passband for G, G_BP, and G_RP is valid over the entire magnitude and colour range, with no systematics above the 1 percent level.
Published: 2021

13. Gaia Early Data Release 3 Summary of the contents and survey properties

Author: Brown, A. G. A. Vallenari, A. Prusti, T. de Bruijne, J. H. J. Babusiaux, C. Biermann, M. Creevey, O. L. Evans, D. W. Eyer, L. Hutton, A. Jansen, F. Jordi, C. Klioner, S. A. Lammers, U. Lindegren, L. Luri, X. Mignard, F. and Panem, C. Pourbaix, D. Randich, S. Sartoretti, P. and Soubiran, C. Walton, N. A. Arenou, F. Bailer-Jones, C. A. L. and Bastian, U. Cropper, M. Drimmel, R. Katz, D. and Lattanzi, M. G. van Leeuwen, F. Bakker, J. Cacciari, C. and Castaneda, J. De Angeli, F. Ducourant, C. Fabricius, C. and Fouesneau, M. Fremat, Y. Guerra, R. Guerrier, A. and Guiraud, J. Jean-Antoine Piccolo, A. Masana, E. Messineo, R. and Mowlavi, N. Nicolas, C. Nienartowicz, K. Pailler, F. and Panuzzo, P. Riclet, F. Roux, W. Seabroke, G. M. Sordo, R. Tanga, P. Thevenin, F. Gracia-Abril, G. Portell, J. and Teyssier, D. Altmann, M. Andrae, R. Bellas-Velidis, I. and Benson, K. Berthier, J. Blomme, R. Brugaletta, E. and Burgess, P. W. Busso, G. Carry, B. Cellino, A. Cheek, N. and Clementini, G. Damerdji, Y. Davidson, M. Delchambre, L. and Dell'Oro, A. Fernandez-Hernandez, J. Galluccio, L. and Garcia-Lario, P. Garcia-Reinaldos, M. Gonzalez-Nunez, J. and Gosset, E. Haigron, R. Halbwachs, J. -L. Hambly, N. C. and Harrison, D. L. Hatzidimitriou, D. Heiter, U. Hernandez, J. and Hestroffer, D. Hodgkin, S. T. Holl, B. Janssen, K. and Jevardat de Fombelle, G. Jordan, S. Krone-Martins, A. and Lanzafame, A. C. Loeffler, W. Lorca, A. Manteiga, M. and Marchal, O. Marrese, P. M. Moitinho, A. Mora, A. and Muinonen, K. Osborne, P. Pancino, E. Pauwels, T. Petit, J. -M. Recio-Blanco, A. Richards, P. J. Riello, M. and Rimoldini, L. Robin, A. C. Roegiers, T. Rybizki, J. and Sarro, L. M. Siopis, C. Smith, M. Sozzetti, A. Ulla, A. and Utrilla, E. van Leeuwen, M. van Reeven, W. Abbas, U. and Abreu Aramburu, A. Accart, S. Aerts, C. Aguado, J. J. and Ajaj, M. Altavilla, G. Alvarez, M. A. Alvarez Cid-Fuentes, J. Alves, J. Anderson, R. I. Anglada Varela, E. Antoja, T. Audard, M. Baines, D. Baker, S. G. Balaguer-Nunez, L. and Balbinot, E. Balog, Z. Barache, C. Barbato, D. and Barros, M. Barstow, M. A. Bartolome, S. Bassilana, J. -L. and Bauchet, N. Baudesson-Stella, A. Becciani, U. and Bellazzini, M. Bernet, M. Bertone, S. Bianchi, L. and Blanco-Cuaresma, S. Boch, T. Bombrun, A. Bossini, D. and Bouquillon, S. Bragaglia, A. Bramante, L. Breedt, E. and Bressan, A. Brouillet, N. Bucciarelli, B. Burlacu, A. and Busonero, D. Butkevich, A. G. Buzzi, R. Caffau, E. and Cancelliere, R. Canovas, H. Cantat-Gaudin, T. Carballo, R. and Carlucci, T. Carnerero, I, M. Carrasco, J. M. and Casamiquela, L. Castellani, M. Castro-Ginard, A. Castro Sampol, P. Chaoul, L. Charlot, P. Chemin, L. Chiavassa, A. Cioni, M. -R. L. Comoretto, G. Cooper, W. J. Cornez, T. Cowell, S. Crifo, F. Crosta, M. Crowley, C. and Dafonte, C. Dapergolas, A. David, M. David, P. de Laverny, P. De Luise, F. De March, R. De Ridder, J. de Souza, R. de Teodoro, P. de Torres, A. del Peloso, E. F. and del Pozo, E. Delbo, M. Delgado, A. Delgado, H. E. and Delisle, J. -B. Di Matteo, P. Diakite, S. Diener, C. and Distefano, E. Dolding, C. Eappachen, D. Edvardsson, B. and Enke, H. Esquej, P. Fabre, C. Fabrizio, M. Faigler, S. and Fedorets, G. Fernique, P. Fienga, A. Figueras, F. and Fouron, C. Fragkoudi, F. Fraile, E. Franke, F. Gai, M. and Garabato, D. Garcia-Gutierrez, A. Garcia-Torres, M. and Garofalo, A. Gavras, P. Gerlach, E. Geyer, R. Giacobbe, P. Gilmore, G. Girona, S. Giuffrida, G. Gomel, R. and Gomez, A. Gonzalez-Santamaria, I. Gonzalez-Vidal, J. J. and Granvik, M. Gutierrez-Sanchez, R. Guy, L. P. Hauser, M. and Haywood, M. Helmi, A. Hidalgo, S. L. Hilger, T. and Hladczuk, N. Hobbs, D. Holland, G. Huckle, H. E. and Jasniewicz, G. Jonker, P. G. Juaristi Campillo, J. Julbe, F. and Karbevska, L. Kervella, P. Khanna, S. Kochoska, A. and Kontizas, M. Kordopatis, G. Korn, A. J. Kostrzewa-Rutkowska, Z. Kruszynska, K. Lambert, S. Lanza, A. F. Lasne, Y. and Le Campion, J. -F. Le Fustec, Y. Lebreton, Y. Lebzelter, T. and Leccia, S. Leclerc, N. Lecoeur-Taibi, I. Liao, S. and Licata, E. Lindstrom, E. P. Lister, T. A. Livanou, E. and Lobel, A. Madrero Pardo, P. Managau, S. Mann, R. G. and Marchant, J. M. Marconi, M. Marcos Santos, M. M. S. and Marinoni, S. Marocco, F. Marshall, D. J. Martin Polo, L. and Martin-Fleitas, J. M. Masip, A. Massari, D. and Mastrobuono-Battisti, A. Mazeh, T. McMillan, P. J. Messina, S. Michalik, D. Millar, N. R. Mints, A. Molina, D. and Molinaro, R. Molnar, L. Montegriffo, P. Mor, R. and Morbidelli, R. Morel, T. Morris, D. Mulone, A. F. Munoz, D. Muraveva, T. Murphy, C. P. Musella, I. Noval, L. and Ordenovic, C. Orru, G. Osinde, J. Pagani, C. Pagano, I. and Palaversa, L. Palicio, P. A. Panahi, A. Pawlak, M. and Penalosa Esteller, X. Penttila, A. Piersimoni, A. M. Pineau, F. -X. Plachy, E. Plum, G. Poggio, E. Poretti, E. and Poujoulet, E. Prsa, A. Pulone, L. Racero, E. Ragaini, S. and Rainer, M. Raiteri, C. M. Rambaux, N. Ramos, P. and Ramos-Lerate, M. Re Fiorentin, P. Regibo, S. Reyle, C. and Ripepi, V. Riva, A. Rixon, G. Robichon, N. Robin, C. and Roelens, M. Rohrbasser, L. Romero-Gomez, M. Rowell, N. and Royer, F. Rybicki, K. A. Sadowski, G. Sagrista Selles, A. and Sahlmann, J. Salgado, J. Salguero, E. Samaras, N. and Sanchez Gimenez, V. Sanna, N. Santovena, R. Sarasso, M. and Schultheis, M. Sciacca, E. Segol, M. Segovia, J. C. and Segransan, D. Semeux, D. Shahaf, S. Siddiqui, H. I. and Siebert, A. Siltala, L. Slezak, E. Smart, R. L. Solano, E. Solitro, F. Souami, D. Souchay, J. Spagna, A. and Spoto, F. Steele, I. A. Steidelmueller, H. Stephenson, C. A. and Suveges, M. Szabados, L. Szegedi-Elek, E. Taris, F. and Tauran, G. Taylor, M. B. Teixeira, R. Thuillot, W. and Tonello, N. Torra, F. Torra, J. Turon, C. Unger, N. and Vaillant, M. van Dillen, E. Vanel, O. Vecchiato, A. and Viala, Y. Vicente, D. Voutsinas, S. Weiler, M. Wevers, T. Wyrzykowski, L. Yoldas, A. Yvard, P. Zhao, H. and Zorec, J. Zucker, S. Zurbach, C. Zwitter, T. Gaia Collaboration
Abstract: Context. We present the early installment of the third Gaia data release, Gaia EDR3, consisting of astrometry and photometry for 1.8 billion sources brighter than magnitude 21, complemented with the list of radial velocities from Gaia DR2. Aims. A summary of the contents of Gaia EDR3 is presented, accompanied by a discussion on the differences with respect to Gaia DR2 and an overview of the main limitations which are present in the survey. Recommendations are made on the responsible use of Gaia EDR3 results. Methods. The raw data collected with the Gaia instruments during the first 34 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium and turned into this early third data release, which represents a major advance with respect to Gaia DR2 in terms of astrometric and photometric precision, accuracy, and homogeneity. Results. Gaia EDR3 contains celestial positions and the apparent brightness in G for approximately 1.8 billion sources. For 1.5 billion of those sources, parallaxes, proper motions, and the (G(BP) - G(RP)) colour are also available. The passbands for G, G(BP), and G(RP) are provided as part of the release. For ease of use, the 7 million radial velocities from Gaia DR2 are included in this release, after the removal of a small number of spurious values. New radial velocities will appear as part of Gaia DR3. Finally, Gaia EDR3 represents an updated materialisation of the celestial reference frame (CRF) in the optical, the Gaia-CRF3, which is based solely on extragalactic sources. The creation of the source list for Gaia EDR3 includes enhancements that make it more robust with respect to high proper motion stars, and the disturbing effects of spurious and partially resolved sources. The source list is largely the same as that for Gaia DR2, but it does feature new sources and there are some notable changes. The source list will not change for Gaia DR3. Conclusions. Gaia EDR3 represents a significant advance over Gaia DR2, with parallax precisions increased by 30 per cent, proper motion precisions increased by a factor of 2, and the systematic errors in the astrometry suppressed by 30-40% for the parallaxes and by a factor similar to 2.5 for the proper motions. The photometry also features increased precision, but above all much better homogeneity across colour, magnitude, and celestial position. A single passband for G, G(BP), and G(RP) is valid over the entire magnitude and colour range, with no systematics above the 1% level
Published: 2021

14. Gaia Early Data Release 3: The Gaia Catalogue of Nearby Stars

Author: Smart, R.L. Sarro, L.M. Rybizki, J. Reylé, C. Robin, A.C. Hambly, N.C. Abbas, U. Barstow, M.A. De Bruijne, J.H.J. Bucciarelli, B. Carrasco, J.M. Cooper, W.J. Hodgkin, S.T. Masana, E. Michalik, D. Sahlmann, J. Sozzetti, A. Brown, A.G.A. Vallenari, A. Prusti, T. Babusiaux, C. Biermann, M. Creevey, O.L. Evans, D.W. Eyer, L. Hutton, A. Jansen, F. Jordi, C. Klioner, S.A. Lammers, U. Lindegren, L. Luri, X. Mignard, F. Panem, C. Pourbaix, D. Randich, S. Sartoretti, P. Soubiran, C. Walton, N.A. Arenou, F. Bailer-Jones, C.A.L. Bastian, U. Cropper, M. Drimmel, R. Katz, D. Lattanzi, M.G. Van Leeuwen, F. Bakker, J. Castañeda, J. De Angeli, F. Ducourant, C. Fabricius, C. Fouesneau, M. Frémat, Y. Guerra, R. Guerrier, A. Guiraud, J. Jean-Antoine Piccolo, A. Messineo, R. Mowlavi, N. Nicolas, C. Nienartowicz, K. Pailler, F. Panuzzo, P. Riclet, F. Roux, W. Seabroke, G.M. Sordo, R. Tanga, P. Thévenin, F. Gracia-Abril, G. Portell, J. Teyssier, D. Altmann, M. Andrae, R. Bellas-Velidis, I. Benson, K. Berthier, J. Blomme, R. Brugaletta, E. Burgess, P.W. Busso, G. Carry, B. Cellino, A. Cheek, N. Clementini, G. Damerdji, Y. Davidson, M. Delchambre, L. Dell'Oro, A. Fernández-Hernández, J. Galluccio, L. García-Lario, P. Garcia-Reinaldos, M. González-Núñez, J. Gosset, E. Haigron, R. Halbwachs, J.-L. Harrison, D.L. Hatzidimitriou, D. Heiter, U. Hernández, J. Hestroffer, D. Holl, B. Janßen, K. Jevardat De Fombelle, G. Jordan, S. Krone-Martins, A. Lanzafame, A.C. Löffler, W. Lorca, A. Manteiga, M. Marchal, O. Marrese, P.M. Moitinho, A. Mora, A. Muinonen, K. Osborne, P. Pancino, E. Pauwels, T. Recio-Blanco, A. Richards, P.J. Riello, M. Rimoldini, L. Roegiers, T. Siopis, C. Smith, M. Ulla, A. Utrilla, E. Van Leeuwen, M. Van Reeven, W. Abreu Aramburu, A. Accart, S. Aerts, C. Aguado, J.J. Ajaj, M. Altavilla, G. Álvarez, M.A. Álvarez Cid-Fuentes, J. Alves, J. Anderson, R.I. Anglada Varela, E. Antoja, T. Audard, M. Baines, D. Baker, S.G. Balaguer-Núñez, L. Balbinot, E. Balog, Z. Barache, C. Barbato, D. Barros, M. Bartolomé, S. Bassilana, J.-L. Bauchet, N. Baudesson-Stella, A. Becciani, U. Bellazzini, M. Bernet, M. Bertone, S. Bianchi, L. Blanco-Cuaresma, S. Boch, T. Bombrun, A. Bossini, D. Bouquillon, S. Bragaglia, A. Bramante, L. Breedt, E. Bressan, A. Brouillet, N. Burlacu, A. Busonero, D. Butkevich, A.G. Buzzi, R. Caffau, E. Cancelliere, R. Cánovas, H. Cantat-Gaudin, T. Carballo, R. Carlucci, T. Carnerero, M.I. Casamiquela, L. Castellani, M. Castro-Ginard, A. Castro Sampol, P. Chaoul, L. Charlot, P. Chemin, L. Chiavassa, A. Cioni, M.-R.L. Comoretto, G. Cornez, T. Cowell, S. Crifo, F. Crosta, M. Crowley, C. Dafonte, C. Dapergolas, A. David, M. David, P. De Laverny, P. De Luise, F. De March, R. De Ridder, J. De Souza, R. De Teodoro, P. De Torres, A. Del Peloso, E.F. Del Pozo, E. Delgado, A. Delgado, H.E. Delisle, J.-B. DI Matteo, P. DIakite, S. DIener, C. DIstefano, E. Dolding, C. Eappachen, D. Edvardsson, B. Enke, H. Esquej, P. Fabre, C. Fabrizio, M. Faigler, S. Fedorets, G. Fernique, P. Fienga, A. Figueras, F. Fouron, C. Fragkoudi, F. Fraile, E. Franke, F. Gai, M. Garabato, D. Garcia-Gutierrez, A. García-Torres, M. Garofalo, A. Gavras, P. Gerlach, E. Geyer, R. Giacobbe, P. Gilmore, G. Girona, S. Giuffrida, G. Gomel, R. Gomez, A. Gonzalez-Santamaria, I. González-Vidal, J.J. Granvik, M. Gutiérrez-Sánchez, R. Guy, L.P. Hauser, M. Haywood, M. Helmi, A. Hidalgo, S.L. Hilger, T. Hładczuk, N. Hobbs, D. Holland, G. Huckle, H.E. Jasniewicz, G. Jonker, P.G. Juaristi Campillo, J. Julbe, F. Karbevska, L. Kervella, P. Khanna, S. Kochoska, A. Kontizas, M. Kordopatis, G. Korn, A.J. Kostrzewa-Rutkowska, Z. Kruszyńska, K. Lambert, S. Lanza, A.F. Lasne, Y. Le Campion, J.-F. Le Fustec, Y. Lebreton, Y. Lebzelter, T. Leccia, S. Leclerc, N. Lecoeur-Taibi, I. Liao, S. Licata, E. Lindstrøm, H.E.P. Lister, T.A. Livanou, E. Lobel, A. Madrero Pardo, P. Managau, S. Mann, R.G. Marchant, J.M. Marconi, M. Marcos Santos, M.M.S. Marinoni, S. Marocco, F. Marshall, D.J. Martin Polo, L. Martín-Fleitas, J.M. Masip, A. Massari, D. Mastrobuono-Battisti, A. Mazeh, T. McMillan, P.J. Messina, S. Millar, N.R. Mints, A. Molina, D. Molinaro, R. Molnár, L. Montegriffo, P. Mor, R. Morbidelli, R. Morel, T. Morris, D. Mulone, A.F. Munoz, D. Muraveva, T. Murphy, C.P. Musella, I. Noval, L. Ordénovic, C. Orrù, G. Osinde, J. Pagani, C. Pagano, I. Palaversa, L. Palicio, P.A. Panahi, A. Pawlak, M. Peñalosa Esteller, X. Penttilä, A. Piersimoni, A.M. Pineau, F.-X. Plachy, E. Plum, G. Poggio, E. Poretti, E. Poujoulet, E. Prša, A. Pulone, L. Racero, E. Ragaini, S. Rainer, M. Raiteri, C.M. Rambaux, N. Ramos, P. Ramos-Lerate, M. Re Fiorentin, P. Regibo, S. Ripepi, V. Riva, A. Rixon, G. Robichon, N. Robin, C. Roelens, M. Rohrbasser, L. Romero-Gómez, M. Rowell, N. Royer, F. Rybicki, K.A. Sadowski, G. Sagristà Sellés, A. Salgado, J. Salguero, E. Samaras, N. Sanchez Gimenez, V. Sanna, N. Santoveña, R. Sarasso, M. Schultheis, M. Sciacca, E. Segol, M. Segovia, J.C. Ségransan, D. Semeux, D. Shahaf, S. Siddiqui, H.I. Siebert, A. Siltala, L. Slezak, E. Solano, E. Solitro, F. Souami, D. Souchay, J. Spagna, A. Spoto, F. Steele, I.A. Steidelmüller, H. Stephenson, C.A. Süveges, M. Szabados, L. Szegedi-Elek, E. Taris, F. Tauran, G. Taylor, M.B. Teixeira, R. Thuillot, W. Tonello, N. Torra, F. Torra, J. Turon, C. Unger, N. Vaillant, M. Van DIllen, E. Vanel, O. Vecchiato, A. Viala, Y. Vicente, D. Voutsinas, S. Weiler, M. Wevers, T. Wyrzykowski, L. Yoldas, A. Yvard, P. Zhao, H. Zorec, J. Zucker, S. Zurbach, C. Zwitter, T.
Abstract: Aims. We produce a clean and well-characterised catalogue of objects within 100 pc of the Sun from the Gaia Early Data Release 3. We characterise the catalogue through comparisons to the full data release, external catalogues, and simulations. We carry out a first analysis of the science that is possible with this sample to demonstrate its potential and best practices for its use. Methods. Theselection of objects within 100 pc from the full catalogue used selected training sets, machine-learning procedures, astrometric quantities, and solution quality indicators to determine a probability that the astrometric solution is reliable. The training set construction exploited the astrometric data, quality flags, and external photometry. For all candidates we calculated distance posterior probability densities using Bayesian procedures and mock catalogues to define priors. Any object with reliable astrometry and a non-zero probability of being within 100 pc is included in the catalogue. Results. We have produced a catalogue of 331 312 objects that we estimate contains at least 92% of stars of stellar type M9 within 100 pc of the Sun. We estimate that 9% of the stars in this catalogue probably lie outside 100 pc, but when the distance probability function is used, a correct treatment of this contamination is possible. We produced luminosity functions with a high signal-to-noise ratio for the main-sequence stars, giants, and white dwarfs. We examined in detail the Hyades cluster, the white dwarf population, and wide-binary systems and produced candidate lists for all three samples. We detected local manifestations of several streams, superclusters, and halo objects, in which we identified 12 members of Gaia Enceladus. We present the first direct parallaxes of five objects in multiple systems within 10 pc of the Sun. Conclusions. We provide the community with a large, well-characterised catalogue of objects in the solar neighbourhood. This is a primary benchmark for measuring and understanding fundamental parameters and descriptive functions in astronomy. © ESO 2021.
Published: 2021

15. Gaia Early Data Release 3: Summary of the contents and survey properties (vol 649, A1, 2021)

Author: Brown, A. G. A. Vallenari, A. Prusti, T. de Bruijne, J. H. J. Babusiaux, C. Biermann, M. Creevey, O. L. Evans, D. W. Eyer, L. Hutton, A. Jansen, F. Jordi, C. Klioner, S. A. Lammers, U. Lindegren, L. Luri, X. Mignard, F. and Panem, C. Pourbaix, D. Randich, S. Sartoretti, P. and Soubiran, C. Walton, N. A. Arenou, F. Bailer-Jones, C. A. L. and Bastian, U. Cropper, M. Drimmel, R. Katz, D. and Lattanzi, M. G. van Leeuwen, F. Bakker, J. Cacciari, C. and Castaneda, J. De Angeli, F. Ducourant, C. Fabricius, C. and Fouesneau, M. Fremat, Y. Guerra, R. Guerrier, A. and Guiraud, J. Piccolo, A. Jean-Antoine Masana, E. Messineo, R. and Mowlavi, N. Nicolas, C. Nienartowicz, K. Pailler, F. and Panuzzo, P. Riclet, F. Roux, W. Seabroke, G. M. Sordo, R. Tanga, P. Thevenin, F. Gracia-Abril, G. Portell, J. and Teyssier, D. Altmann, M. Andrae, R. Bellas-Velidis, I. and Benson, K. Berthier, J. Blomme, R. Brugaletta, E. and Burgess, P. W. Busso, G. Carry, B. Cellino, A. Cheek, N. and Clementini, G. Damerdji, Y. Davidson, M. Delchambre, L. and Dell'Oro, A. Fernandez-Hernandez, J. Galluccio, L. and Garcia-Lario, P. Garcia-Reinaldos, M. Gonzalez-Nunez, J. and Gosset, E. Haigron, R. Halbwachs, J. -L. Hambly, N. C. and Harrison, D. L. Hatzidimitriou, D. Heiter, U. Hernandez, J. and Hestroffer, D. Hodgkin, S. T. Holl, B. Janssen, K. and de Fombelle, G. Jevardat Jordan, S. Krone-Martins, A. and Lanzafame, A. C. Loffler, W. Lorca, A. Manteiga, M. and Marchal, O. Marrese, P. M. Moitinho, A. Mora, A. and Muinonen, K. Osborne, P. Pancino, E. Pauwels, T. Petit, J. -M. Recio-Blanco, A. Richards, P. J. Riello, M. and Rimoldini, L. Robin, A. C. Roegiers, T. Rybizki, J. and Sarro, L. M. Siopis, C. Smith, M. Sozzetti, A. Ulla, A. and Utrilla, E. van Leeuwen, M. van Reeven, W. Abbas, U. and Aramburu, A. Abreu Accart, S. Aerts, C. Aguado, J. J. and Ajaj, M. Altavilla, G. Alvarez, M. A. Cid-Fuentes, J. Alvarez Alves, J. Anderson, R. I. Varela, E. Anglada and Antoja, T. Audard, M. Baines, D. Baker, S. G. and Balaguer-Nunez, L. Balbinot, E. Balog, Z. Barache, C. and Barbato, D. Barros, M. Barstow, M. A. Bartolome, S. and Bassilana, J. -L. Bauchet, N. Baudesson-Stella, A. Becciani, U. Bellazzini, M. Bernet, M. Bertone, S. Bianchi, L. and Blanco-Cuaresma, S. Boch, T. Bombrun, A. Bossini, D. and Bouquillon, S. Bragaglia, A. Bramante, L. Breedt, E. and Bressan, A. Brouillet, N. Bucciarelli, B. Burlacu, A. and Busonero, D. Butkevich, A. G. Buzzi, R. Caffau, E. and Cancelliere, R. Canovas, H. Cantat-Gaudin, T. Carballo, R. and Carlucci, T. Carnerero, M. I. Carrasco, J. M. and Casamiquela, L. Castellani, M. Castro-Ginard, A. Sampol, P. Castro Chaoul, L. Charlot, P. Chemin, L. Chiavassa, A. and Cioni, M. -R. L. Comoretto, G. Cooper, W. J. Cornez, T. and Cowell, S. Crifo, F. Crosta, M. Crowley, C. Dafonte, C. Dapergolas, A. David, M. David, P. de Laverny, P. and De Luise, F. De March, R. De Ridder, J. de Souza, R. de Teodoro, P. de Torres, A. del Peloso, E. F. del Pozo, E. and Delbo, M. Delgado, A. Delgado, H. E. Delisle, J. -B. Di Matteo, P. Diakite, S. Diener, C. Distefano, E. Dolding, C. Eappachen, D. Edvardsson, B. Enke, H. Esquej, P. and Fabre, C. Fabrizio, M. Faigler, S. Fedorets, G. and Fernique, P. Fienga, A. Figueras, F. Fouron, C. and Fragkoudi, F. Fraile, E. Franke, F. Gai, M. Garabato, D. and Garcia-Gutierrez, A. Garcia-Torres, M. Garofalo, A. and Gavras, P. Gerlach, E. Geyer, R. Giacobbe, P. Gilmore, G. Girona, S. Giuffrida, G. Gomel, R. Gomez, A. and Gonzalez-Santamaria, I. Gonzalez-Vidal, J. J. Granvik, M. and Gutierrez-Sanchez, R. Guy, L. P. Hauser, M. Haywood, M. and Helmi, A. Hidalgo, S. L. Hilger, T. Hladczuk, N. Hobbs, D. Holland, G. Huckle, H. E. Jasniewicz, G. Jonker, P. G. Campillo, J. Juaristi Julbe, F. Karbevska, L. and Kervella, P. Khanna, S. Kochoska, A. Kontizas, M. and Kordopatis, G. Korn, A. J. Kostrzewa-Rutkowska, Z. and Kruszynska, K. Lambert, S. Lanza, A. F. Lasne, Y. Le Campion, J. -F. Le Fustec, Y. Lebreton, Y. Lebzelter, T. and Leccia, S. Leclerc, N. Lecoeur-Taibi, I. Liao, S. and Licata, E. Lindstrom, H. E. P. Lister, T. A. Livanou, E. and Lobel, A. Pardo, P. Madrero Managau, S. Mann, R. G. and Marchant, J. M. Marconi, M. Santos, M. M. S. Marcos and Marinoni, S. Marocco, F. Marshall, D. J. Polo, L. Martin and Martin-Fleitas, J. M. Masip, A. Massari, D. and Mastrobuono-Battisti, A. Mazeh, T. McMillan, P. J. Messina, S. Michalik, D. Millar, N. R. Mints, A. Molina, D. and Molinaro, R. Molnar, L. Montegriffo, P. Mor, R. and Morbidelli, R. Morel, T. Morris, D. Mulone, A. F. Munoz, D. Muraveva, T. Murphy, C. P. Musella, I. Noval, L. and Ordenovic, C. Orru, G. Osinde, J. Pagani, C. Pagano, I. and Palaversa, L. Palicio, P. A. Panahi, A. Pawlak, M. and Esteller, X. Penalosa Penttila, A. Piersimoni, A. M. Pineau, F. -X. Plachy, E. Plum, G. Poggio, E. Poretti, E. and Poujoulet, E. Prsa, A. Pulone, L. Racero, E. Ragaini, S. and Rainer, M. Raiteri, C. M. Rambaux, N. Ramos, P. and Ramos-Lerate, M. Fiorentin, P. Re Regibo, S. Reyle, C. and Ripepi, V. Riva, A. Rixon, G. Robichon, N. Robin, C. and Roelens, M. Rohrbasser, L. Romero-Gomez, M. Rowell, N. and Royer, F. Rybicki, K. A. Sadowski, G. Selles, A. Sagrista and Sahlmann, J. Salgado, J. Salguero, E. Samaras, N. and Gimenez, V. Sanchez Sanna, N. Santovena, R. Sarasso, M. and Schultheis, M. Sciacca, E. Segol, M. Segovia, J. C. and Segransan, D. Semeux, D. Shahaf, S. Siddiqui, H. I. and Siebert, A. Siltala, L. Slezak, E. Smart, R. L. Solano, E. Solitro, F. Souami, D. Souchay, J. Spagna, A. and Spoto, F. Steele, I. A. Steidelmuller, H. Stephenson, C. A. and Suveges, M. Szabados, L. Szegedi-Elek, E. Taris, F. and Tauran, G. Taylor, M. B. Teixeira, R. Thuillot, W. and Tonello, N. Torra, F. Torra, J. Turon, C. Unger, N. and Vaillant, M. van Dillen, E. Vanel, O. Vecchiato, A. and Viala, Y. Vicente, D. Voutsinas, S. Weiler, M. Wevers, T. Wyrzykowski, L. Yoldas, A. Yvard, P. Zhao, H. and Zorec, J. Zucker, S. Zurbach, C. Zwitter, T. Gaia Collaboration
Published: 2021

16. Gaia Early Data Release 3: The Galactic anticentre

Author: Antoja, T. McMillan, P.J. Kordopatis, G. Ramos, P. Helmi, A. Balbinot, E. Cantat-Gaudin, T. Chemin, L. Figueras, F. Jordi, C. Khanna, S. Romero-Gómez, M. Seabroke, G.M. Brown, A.G.A. Vallenari, A. Prusti, T. De Bruijne, J.H.J. Babusiaux, C. Biermann, M. Creevey, O.L. Evans, D.W. Eyer, L. Hutton, A. Jansen, F. Klioner, S.A. Lammers, U. Lindegren, L. Luri, X. Mignard, F. Panem, C. Pourbaix, D. Randich, S. Sartoretti, P. Soubiran, C. Walton, N.A. Arenou, F. Bailer-Jones, C.A.L. Bastian, U. Cropper, M. Drimmel, R. Katz, D. Lattanzi, M.G. Van Leeuwen, F. Bakker, J. Castañeda, J. De Angeli, F. Ducourant, C. Fabricius, C. Fouesneau, M. Frémat, Y. Guerra, R. Guerrier, A. Guiraud, J. Jean-Antoine Piccolo, A. Masana, E. Messineo, R. Mowlavi, N. Nicolas, C. Nienartowicz, K. Pailler, F. Panuzzo, P. Riclet, F. Roux, W. Sordo, R. Tanga, P. Thévenin, F. Gracia-Abril, G. Portell, J. Teyssier, D. Altmann, M. Andrae, R. Bellas-Velidis, I. Benson, K. Berthier, J. Blomme, R. Brugaletta, E. Burgess, P.W. Busso, G. Carry, B. Cellino, A. Cheek, N. Clementini, G. Damerdji, Y. Davidson, M. Delchambre, L. Dell'Oro, A. Fernández-Hernández, J. Galluccio, L. García-Lario, P. Garcia-Reinaldos, M. González-Núñez, J. Gosset, E. Haigron, R. Halbwachs, J.-L. Hambly, N.C. Harrison, D.L. Hatzidimitriou, D. Heiter, U. Hernández, J. Hestroffer, D. Hodgkin, S.T. Holl, B. Janßen, K. Jevardat De Fombelle, G. Jordan, S. Krone-Martins, A. Lanzafame, A.C. Löffler, W. Lorca, A. Manteiga, M. Marchal, O. Marrese, P.M. Moitinho, A. Mora, A. Muinonen, K. Osborne, P. Pancino, E. Pauwels, T. Recio-Blanco, A. Richards, P.J. Riello, M. Rimoldini, L. Robin, A.C. Roegiers, T. Rybizki, J. Sarro, L.M. Siopis, C. Smith, M. Sozzetti, A. Ulla, A. Utrilla, E. Van Leeuwen, M. Van Reeven, W. Abbas, U. Abreu Aramburu, A. Accart, S. Aerts, C. Aguado, J.J. Ajaj, M. Altavilla, G. Álvarez, M.A. Álvarez Cid-Fuentes, J. Alves, J. Anderson, R.I. Varela, E.A. Audard, M. Baines, D. Baker, S.G. Balaguer-Núñez, L. Balog, Z. Barache, C. Barbato, D. Barros, M. Barstow, M.A. Bartolomé, S. Bassilana, J.-L. Bauchet, N. Baudesson-Stella, A. Becciani, U. Bellazzini, M. Bernet, M. Bertone, S. Bianchi, L. Blanco-Cuaresma, S. Boch, T. Bombrun, A. Bossini, D. Bouquillon, S. Bragaglia, A. Bramante, L. Breedt, E. Bressan, A. Brouillet, N. Bucciarelli, B. Burlacu, A. Busonero, D. Butkevich, A.G. Buzzi, R. Caffau, E. Cancelliere, R. Cánovas, H. Carballo, R. Carlucci, T. Carnerero, M.I. Carrasco, J.M. Casamiquela, L. Castellani, M. Castro-Ginard, A. Castro Sampol, P. Chaoul, L. Charlot, P. Chiavassa, A. Cioni, M.-R.L. Comoretto, G. Cooper, W.J. Cornez, T. Cowell, S. Crifo, F. Crosta, M. Crowley, C. Dafonte, C. Dapergolas, A. David, M. David, P. De Laverny, P. De Luise, F. De March, R. De Ridder, J. De Souza, R. De Teodoro, P. De Torres, A. Del Peloso, E.F. Del Pozo, E. Delgado, A. Delgado, H.E. Delisle, J.-B. Di Matteo, P. Diakite, S. Diener, C. Distefano, E. Dolding, C. Eappachen, D. Enke, H. Esquej, P. Fabre, C. Fabrizio, M. Faigler, S. Fedorets, G. Fernique, P. Fienga, A. Fouron, C. Fragkoudi, F. Fraile, E. Franke, F. Gai, M. Garabato, D. Garcia-Gutierrez, A. García-Torres, M. Garofalo, A. Gavras, P. Gerlach, E. Geyer, R. Giacobbe, P. Gilmore, G. Girona, S. Giuffrida, G. Gomez, A. Gonzalez-Santamaria, I. González-Vidal, J.J. Granvik, M. Gutiérrez-Sánchez, R. Guy, L.P. Hauser, M. Haywood, M. Hidalgo, S.L. Hilger, T. Hładczuk, N. Hobbs, D. Holland, G. Huckle, H.E. Jasniewicz, G. Jonker, P.G. Juaristi Campillo, J. Julbe, F. Karbevska, L. Kervella, P. Kochoska, A. Kontizas, M. Korn, A.J. Kostrzewa-Rutkowska, Z. Kruszyńska, K. Lambert, S. Lanza, A.F. Lasne, Y. Le Campion, J.-F. Le Fustec, Y. Lebreton, Y. Lebzelter, T. Leccia, S. Leclerc, N. Lecoeur-Taibi, I. Liao, S. Licata, E. Lindstrøm, H.E.P. Lister, T.A. Livanou, E. Lobel, A. Madrero Pardo, P. Managau, S. Mann, R.G. Marchant, J.M. Marconi, M. Marcos Santos, M.M.S. Marinoni, S. Marocco, F. Marshall, D.J. Martin Polo, L. Martín-Fleitas, J.M. Masip, A. Massari, D. Mastrobuono-Battisti, A. Mazeh, T. Messina, S. Michalik, D. Millar, N.R. Mints, A. Molina, D. Molinaro, R. Molnár, L. Montegriffo, P. Mor, R. Morbidelli, R. Morel, T. Morris, D. Mulone, A.F. Munoz, D. Muraveva, T. Murphy, C.P. Musella, I. Noval, L. Ordénovic, C. Orrù, G. Osinde, J. Pagani, C. Pagano, I. Palaversa, L. Palicio, P.A. Panahi, A. Pawlak, M. Peñalosa Esteller, X. Penttilä, A. Piersimoni, A.M. Pineau, F.-X. Plachy, E. Plum, G. Poggio, E. Poretti, E. Poujoulet, E. Prša, A. Pulone, L. Racero, E. Ragaini, S. Rainer, M. Raiteri, C.M. Rambaux, N. Ramos-Lerate, M. Re Fiorentin, P. Regibo, S. Reylé, C. Ripepi, V. Riva, A. Rixon, G. Robichon, N. Robin, C. Roelens, M. Rohrbasser, L. Rowell, N. Royer, F. Rybicki, K.A. Sadowski, G. Sagristà Sellés, A. Sahlmann, J. Salgado, J. Salguero, E. Samaras, N. Sanchez Gimenez, V. Sanna, N. Santoveña, R. Sarasso, M. Schultheis, M. Sciacca, E. Segol, M. Segovia, J.C. Ségransan, D. Semeux, D. Siddiqui, H.I. Siebert, A. Siltala, L. Slezak, E. Smart, R.L. Solano, E. Solitro, F. Souami, D. Souchay, J. Spagna, A. Spoto, F. Steele, I.A. Steidelmüller, H. Stephenson, C.A. Süveges, M. Szabados, L. Szegedi-Elek, E. Taris, F. Tauran, G. Taylor, M.B. Teixeira, R. Thuillot, W. Tonello, N. Torra, F. Torra, J. Turon, C. Unger, N. Vaillant, M. Van Dillen, E. Vanel, O. Vecchiato, A. Viala, Y. Vicente, D. Voutsinas, S. Weiler, M. Wevers, T. Wyrzykowski, L. Yoldas, A. Yvard, P. Zhao, H. Zorec, J. Zucker, S. Zurbach, C. Zwitter, T.
Subjects: Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: 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. © ESO 2021.
Published: 2021

17. GAIA AND PHYSICS OF STELLAR INTERIORS

Author: Y. Lebreton, A. Baglin, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Astronomie du LESIA, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
Subjects: Physics, General Engineering, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Space (mathematics), Asteroseismology, Stars, Photometry (astronomy), Space and Planetary Science, Fundamental physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: Understanding the stellar interiors is an important issue for astrophysics, but also for fundamental physics. The physical description of the stellar material implies statistical physics as well as hydrodynamics. We give examples of unsolved physical problems and their consequences for predictions of stellar properties and evolution. It is shown that the accumulation of high-quality data like distances and photometry on a large variety of objects, as proposed by GAIA, will be very useful. During the same period, asteroseismology will develop both from the ground in velocimetry, and from space in photometry, providing for the closest stars, a direct insight into their interiors. This ensemble of new data will constitute the basis of the general physical description of stellar interiors.
Published: 2020
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18. The Aarhus red giants challenge

Author: J. Christensen-Dalsgaard, V. Silva Aguirre, S. Cassisi, M. Miller Bertolami, A. Serenelli, D. Stello, A. Weiss, G. Angelou, C. Jiang, Y. Lebreton, F. Spada, E. P. Bellinger, S. Deheuvels, R. M. Ouazzani, A. Pietrinferni, J. R. Mosumgaard, R. H. D. Townsend, T. Battich, D. Bossini, T. Constantino, P. Eggenberger, S. Hekker, A. Mazumdar, A. Miglio, K. B. Nielsen, M. Salaris
Published: 2020
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19. Gaia Early Data Release 3: Acceleration of the solar system from Gaia astrometry

Author: Vincenzo Ripepi, P. Gavras, M. Vaillant, Mathias Schultheis, László Molnár, E. Poujoulet, Mark Cropper, C. Babusiaux, D. Molina, J. Fernández-Hernández, G. Jevardat de Fombelle, A. de Torres, Aldo Dell'Oro, J. Castañeda, Z. Kostrzewa-Rutkowska, A. Bombrun, André Moitinho, Marcella Marconi, Rossella Cancelliere, M. Hauser, M. Ajaj, C. M. Raiteri, L. Eyer, Michał Pawlak, H. I. Siddiqui, C. Ducourant, Tatiana Muraveva, Tsevi Mazeh, A. Panahi, Federico Marocco, Stefano Bertone, D. Vicente, Patrick Charlot, A. Guerrier, R. De March, Mario Gai, J. Souchay, H. E. P. Lindstrøm, Nicoletta Sanna, Agnes Fienga, Giovanni Comoretto, Jon Marchant, A. Lorca, E. Utrilla, A. Garcia-Gutierrez, Ilaria Musella, L. Balaguer-Núñez, Leanne P. Guy, N. Leclerc, E. Brugaletta, A. Yoldas, Harry Enke, Rosanna Sordo, Zoltan Balog, H. E. Huckle, L. Palaversa, Monica Rainer, T. A. Lister, F. A. Jansen, Ruth Carballo, Alessandro Spagna, J. M. Carrasco, Mikael Granvik, Derek W. Morris, F. Julbe, A. Hutton, J. Osinde, D. W. Evans, M. van Leeuwen, M. Weiler, F. Thévenin, F. Torra, Iain A. Steele, Lorenzo Rimoldini, Alessandro Sozzetti, Francesca Fragkoudi, K. Janßen, O. L. Creevey, J. González-Núñez, T. Pauwels, R. Buzzi, Miguel García-Torres, S. Liao, G. Tauran, Lennart Lindegren, C. Fouron, Pierre Fernique, Céline Reylé, P. Di Matteo, E. Szegedi-Elek, F. Pailler, Stefan Jordan, Roberto Molinaro, Elisabetta Caffau, Federica Spoto, Felix Franke, D. Barbato, Isabelle Lecoeur-Taïbi, Tristan Cantat-Gaudin, Alejandra Recio-Blanco, E. Livanou, W. Roux, X. Peñalosa Esteller, P. A. Palicio, J. H. J. de Bruijne, Sergi Blanco-Cuaresma, Deborah Busonero, F. Riclet, Conny Aerts, Georges Kordopatis, Guy Rixon, F. Solitro, Davide Massari, Mike Smith, D. Baines, Roberto Morbidelli, Gerry Gilmore, G. Plum, Alexey Mints, O. Marchal, Juan Zorec, Ángel Gómez, C. A. Stephenson, Michael Davidson, C. Fabricius, E. Licata, Sergio Messina, Laszlo Szabados, M. Biermann, A. Garofalo, G. Holland, F. De Angeli, Andreas Korn, E. Anglada Varela, Grigori Fedorets, S. Girona, E. Gerlach, Antonella Vallenari, M. Riello, Łukasz Wyrzykowski, Damien Ségransan, F. Taris, L. Bramante, Alberto Cellino, S. Regibo, Andrej Prsa, M. Sarasso, E. Poggio, W. Löffler, Paolo Giacobbe, Jordi Portell, Elisa Distefano, Eric Slezak, I. Bellas-Velidis, Nicolas Rambaux, E. Balbinot, J.-B. Delisle, Maroussia Roelens, E. Salguero, P. de Teodoro, E. van Dillen, Y. Lebreton, Francois Mignard, Sergei A. Klioner, Ulrich Bastian, N. Samaras, G. Orrù, R. E. de Souza, P. Esquej, Paul J. McMillan, A. C. Lanzafame, Sébastien Lambert, Beatrice Bucciarelli, Jose M Hernandez, M. Bernet, S. Ragaini, Gisella Clementini, A. F. Mulone, Ludovic Delchambre, C. Panem, Eric Gosset, P. David, M. Garcia-Reinaldos, Ana Ulla, F. Crifo, J. Guiraud, Mariateresa Crosta, L. Chaoul, C. Diener, Carlos Dafonte, Karri Muinonen, Alex Lobel, J.-L. Bassilana, Maria Süveges, Isabella Pagano, Dimitri Pourbaix, D. Eappachen, M. Haywood, R. Drimmel, Y. Viala, S. Voutsinas, D. Semeux, William Thuillot, N. A. Walton, Paolo Montegriffo, A. Abreu Aramburu, C. Fabre, H. Zhao, Alessandro Bressan, S. Bouquillon, Sanjeev Khanna, T. Lebzelter, N. Tonello, L. Siltala, M. G. Lattanzi, C. Crowley, P. Yvard, Carme Jordi, Elena Pancino, E. del Pozo, Jan Rybizki, Nami Mowlavi, C. Barache, Morgan Fouesneau, J. De Ridder, Ugo Becciani, Martin Altmann, F. van Leeuwen, P. M. Marrese, M. A. Álvarez, A. Jean-Antoine Piccolo, A. F. Lanza, Alberto Vecchiato, Thomas Wevers, Caroline Soubiran, C. P. Murphy, A. M. Piersimoni, Alessandra Mastrobuono-Battisti, Peter G. Jonker, A. Sagristà Sellés, T. Roegiers, S. Marinoni, Johannes Sahlmann, Rene Andrae, P. Sartoretti, G. Altavilla, Raphael Guerra, F. X. Pineau, M. Segol, T. Prusti, J. J. González-Vidal, J. J. Aguado, N. R. Millar, A. Baudesson-Stella, Andrea Chiavassa, Laurent Chemin, C. Turon, H. Steidelmüller, Douglas J. Marshall, A. G. Butkevich, Alberto Riva, P. de Laverny, Simchon Faigler, Laurent Galluccio, A. Mora, P. Re Fiorentin, C. Ordénovic, J. F. Le Campion, A. Delgado, V. Sanchez Gimenez, M. David, G. Sadowski, R. L. Smart, A. Masip, Laia Casamiquela, R. Messineo, R. Mor, J. Bakker, C. Dolding, J. M. Martín-Fleitas, S. Diakite, Coryn A. L. Bailer-Jones, D. Souami, P. Madrero Pardo, Martin A. Barstow, David Teyssier, Ummi Abbas, Jesus Salgado, Paolo Tanga, A. Burlacu, O. Vanel, Ulrike Heiter, Daniel Hestroffer, Sebastian L. Hidalgo, H. E. Delgado, Alberto Krone-Martins, C. Robin, Kevin Benson, Christos Siopis, S. Managau, P. Burgess, Tomaz Zwitter, M. M. S. Marcos Santos, S. Cowell, J. L. Halbwachs, Xavier Luri, Antti Penttilä, R. Geyer, Minia Manteiga, Yassine Damerdji, Nigel Hambly, S. Bartolomé, J. Álvarez Cid-Fuentes, P. Osborne, J. Juaristi Campillo, Mark Taylor, Richard I. Anderson, Y. Le Fustec, Thierry Morel, T. Cornez, Krzysztof A. Rybicki, L. Pulone, N. Bauchet, Pierre Kervella, C. Zurbach, Alfred Castro-Ginard, Frédéric Arenou, P. Ramos, Robert G. Mann, Annie C. Robin, J. C. Segovia, M. Barros, Hector Canovas, D. L. Harrison, Y. Lasne, L. Noval, David Hobbs, E. F. del Peloso, P. Castro Sampol, Yves Fremat, F. De Luise, Daniel Michalik, P. J. Richards, L. Karbevska, N. Hładczuk, K. Kruszyńska, T. Boch, Sofia Randich, A. G. A. Brown, C. Pagani, L. Martin Polo, M. Ramos-Lerate, Krzysztof Nienartowicz, Eduard Masana, E. Racero, E. Fraile, Marc Audard, N. Robichon, Luciana Bianchi, G. Gracia-Abril, R. Santoveña, R. Haigron, N. Unger, Jérôme Berthier, Despina Hatzidimitriou, R. Gutiérrez-Sánchez, M. Fabrizio, I. Gonzalez-Santamaria, A. Dapergolas, P. Panuzzo, Benoit Carry, Francesca Figueras, R. Blomme, Elmé Breedt, D. Munoz, Diego Bossini, G. Busso, D. Katz, Simon Hodgkin, Ennio Poretti, N. Brouillet, Marco Castellani, Nicholas Rowell, Arnaud Siebert, M. Romero-Gómez, Shay Zucker, W. van Reeven, A. Kochoska, G. Giuffrida, Eva Sciacca, T. Carlucci, L. M. Sarro, M. I. Carnerero, Amina Helmi, D. Garabato, B. Holl, Michele Bellazzini, L. Rohrbasser, Teresa Antoja, J. Torra, Thomas Hilger, Pedro García-Lario, Gérard Jasniewicz, Enrique Solano, S. G. Baker, W. J. Cooper, F. Royer, S. Accart, George M. Seabroke, João Alves, Emese Plachy, C. Nicolas, Silvio Leccia, N. Cheek, Uwe Lammers, Ramachrisna Teixeira, Techniche Universtât Desden, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Lund Observatory, Lund University [Lund], Zentrum für astronomie, Universität Heidelberg [Heidelberg], Department of nuclear medicine, Haukeland University Hospital, University of Bergen (UiB)-University of Bergen (UiB), Merck Serono S.A [Geneva Research Center], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Universität Heidelberg [Heidelberg] = Heidelberg University, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Planetary-system research, Department of Physics, Particle Physics and Astrophysics, Gaia Collaboration, 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, Deliste, J. B. [0000-0001-5844-9888], Sozzeti, A. [0000-0002-7504-365X], 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, Universidad de Cantabria, ITA, European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), Astronomy, and Kapteyn Astronomical Institute
Subjects: Data Analysis, Solar System, Astronomy, kinematics and dynamics, virgo cluster, Astrophysics, 01 natural sciences, bar, Astronomi, astrofysik och kosmologi, large-magellanic-cloud, Methods, Astronomy, Astrophysics and Cosmology, 010303 astronomy & astrophysics, Physics, Astrophysics of Galaxies, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, Astrometry, VIRGO CLUSTER, Kinematics and Dynamics, Amplitude, kinematics, Physical Sciences, MILKY-WAY, astrometry, Galaxy: kinematics and dynamics, PROPER MOTION, Proper motion, perturbation, proper motions, reference systems, methods: data analysis, Astrophysics - Astrophysics of Galaxies, FOS: Physical sciences, Context (language use), proper motion, Astronomy & Astrophysics, MASS, Computer Science::Digital Libraries, Gravitational potential, Acceleration, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, data analysis [methods], Vector spherical harmonics, KINEMATICS, distance, milky-way, Science & Technology, PERTURBATION, 010308 nuclear & particles physics, Astronomy and Astrophysics, kinematics and dynamics [Galaxy], 115 Astronomy, Space science, Physics::History of Physics, BAR, Galaxy, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), DISTANCE, mass, LARGE-MAGELLANIC-CLOUD
Abstract: 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) x 10(-10) m s(-2) (or 7.33 +/- 0.51 km s(-1) Myr-1) towards alpha = 269.1 degrees +/- 5.4 degrees, delta = -31.6 degrees +/- 4.1 degrees, corresponding to a proper motion amplitude of 5.05 +/- 0.35 mu as 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 mu as yr(-1).
Published: 2020
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20. The magnetic fields of intermediate-mass T Tauri stars. I. Magnetic detections and fundamental stellar parameters

Author: Oleg Kochukhov, G. Hussain, Christopher M. Johns-Krull, Colin P. Folsom, Evelyne Alecian, Pascal Petit, Stephen C. Marsden, Y. Lebreton, Jerome Bouvier, Julien Morin, F. Villebrun, Corinne Charbonnel, Lionel Haemmerlé, Torsten Böhm, Louis Amard, François Gallet, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Université de Genève (UNIGE), Rice University [Houston], Uppsala University, University of Southern Queensland (USQ), Laboratoire Univers et Particules de Montpellier (LUPM), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2)
Subjects: Stellar mass, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, stars: pre-main sequence, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Stellar evolution, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, stars: variables: T Tauri, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Computer Science::Information Retrieval, stars: magnetic field, Herbig Ae/Be, Astronomy and Astrophysics, Radius, Magnetic field, Stars, T Tauri star, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, stars: fundamental parameters, Main sequence
Abstract: Context. The origin of the fossil magnetic fields detected in 5 to 10% of intermediate-mass main sequence stars is still highly debated. Aims. We want to bring observational constraints to a large population of intermediate-mass pre-main sequence (PMS) stars in order to test the theory that convective-dynamo fields generated during the PMS phases of stellar evolution can occasionally relax into fossil fields on the main sequence. Methods. Using distance estimations, photometric measurements, and spectropolarimetric data from HARPSpol and ESPaDOnS of 38 intermediate-mass PMS stars, we determined fundamental stellar parameters (Teff, L and v sin i) and measured surface magnetic field characteristics (including detection limits for non-detections, and longitudinal fields and basic topologies for positive detections). Using PMS evolutionary models, we determined the mass, radius, and internal structure of these stars. We compared different PMS models to check that our determinations were not model-dependant. We then compared the magnetic characteristics of our sample accounting for their stellar parameters and internal structures. Results. We detect magnetic fields in about half of our sample. About 90% of the magnetic stars have outer convective envelopes larger than ~25% of the stellar radii, and heavier than ~2% of the stellar mass. Going to higher mass, we find that the magnetic incidence in intermediate-mass stars drops very quickly, within a time-scale of the order of few times 0.1 Myr. Finally, we propose that intermediate-mass T Tauri stars with large convective envelopes, close to the fully convective limit, have complex fields and that their dipole component strengths may decrease as the sizes of their convective envelopes decrease, similar to lower-mass T Tauri stars., accepted by A&A
Published: 2019
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21. APPENDIX B

Author: J. A. GUZIK and Y. LEBRETON
Published: 2018
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22. Spectroscopic survey of the Galaxy with Gaia- I. Design and performance of the Radial Velocity Spectrometer

Author: D. Katz, U. Munari, M. Cropper, T. Zwitter, F. Thevenin, M. David, Y. Viala, F. Crifo, A. Gomboc, F. Royer, F. Arenou, P. Marrese, R. Sordo, M. Wilkinson, A. Vallenari, C. Turon, A. Helmi, G. Bono, M. Perryman, A. Gomez, L. Tomasella, F. Boschi, D. Morin, M. Haywood, C. Soubiran, F. Castelli, A. Bijaoui, G. Bertelli, A. Prsa, S. Mignot, A. Sellier, M.- O. Baylac, Y. Lebreton, U. Jauregi, A. Siviero, R. Bingham, F. Chemla, J. Coker, T. Dibbens, B. Hancock, A. Holland, D. Horville, J.- M. Huet, P. Laporte, T. Melse, F. Sayede, T.- J. Stevenson, P. Vola, D. Walton, B. Winter, Kapteyn Astronomical Institute, Astronomy, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), University of Ljubljana, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Universiteit Antwerpen [Antwerpen], Faculty of Mathematics and Physics [Ljubljana] (FMF), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), INAF - Osservatorio Astronomico di Roma (OAR), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Trieste (OAT), Observatoire de Paris - Site de Paris (OP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Rutheford Appleton Laboratory, University of Leicester, Laboratoire Hubert Curien [Saint Etienne] (LHC), and Université Jean Monnet [Saint-Étienne] (UJM)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS)
Subjects: media_common.quotation_subject, Metallicity, FOS: Physical sciences, Astrophysics, 01 natural sciences, 7. Clean energy, Integral field spectrograph, ECHELLE SPECTRA, ATMOSPHERIC PARAMETERS, techniques: radial velocities, 0103 physical sciences, techniques : spectroscopic, LINE-DATA-BASE, space vehicles: instruments, 010303 astronomy & astrophysics, Spectrograph, techniques : radial velocities, space vehicles : instruments, instrumentation: spectrographs, media_common, Physics, DIFFUSE INTERSTELLAR BANDS, Spectrometer, instrumentation : spectrographs, LATE-TYPE STARS, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, STELLAR PARAMETERS, Galaxy, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Radial velocity, Stars, INFRARED SPECTRAL REGION, Space and Planetary Science, Sky, SYNTHETIC SPECTRA, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], techniques: spectroscopic, HIGH-RESOLUTION SPECTROSCOPY, WAVELENGTH CALIBRATION
Abstract: The definition and optimisation studies for the Gaia satellite spectrograph, the Radial Velocity Spectrometer (RVS), converged in late 2002 with the adoption of the instrument baseline. This paper reviews the characteristics of the selected configuration and presents its expected performance. The RVS is a 2.0 by 1.6 degree integral field spectrograph, dispersing the light of all sources entering its field of view with a resolving power R=11 500 over the wavelength range [848, 874] nm. The RVS will continuously and repeatedly scan the sky during the 5 years of the Gaia mission. On average, each source will be observed 102 times over this period. The RVS will collect the spectra of about 100-150 million stars up to magnitude V~17-18. At the end of the mission, the RVS will provide radial velocities with precisions of ~2 km/s at V=15 and \~15-20 km/s at V=17, for a solar metallicity G5 dwarf. The RVS will also provide rotational velocities, with precisions (at the end of the mission) for late type stars of sigma_vsini ~5 km/s at V~15 as well as atmospheric parameters up to V~14-15. The individual abundances of elements such as Silicon and Magnesium, vital for the understanding of Galactic evolution, will be obtained up to V~12-13. Finally, the presence of the 862.0 nm Diffuse Interstellar Band (DIB) in the RVS wavelength range will make it possible to derive the three dimensional structure of the interstellar reddening., 17 pages, 9 figures, accepted for publication in MNRAS. Fig. 1,2,4,5, 6 in degraded resolution; available in full resolution at http://blackwell-synergy.com/links/doi/10.1111/j.1365-2966.2004.08282.x/pdf
Published: 2017
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23. Chapter 4 : The Evolution of Oxygen in Galaxies

Author: Cristina Chiappini, V. Hill, M. Katsuma, F. Durret, Beatriz Barbuy, C. J. Zeippen, N. Grevesse, Hans-Günter Ludwig, Claudio Mendoza, Sergio Simón-Díaz, Marcel Arnould, Nikos Prantzos, Grazyna Stasinska, M. Dessauges-Zavadsky, P. Ferrando, A. Decourchelle, Y. Lebreton, Guillaume Hébrard, G. Meynet, and Corinne Charbonnel
Subjects: Physics, chemistry, 010308 nuclear & particles physics, Space and Planetary Science, 0103 physical sciences, General Engineering, chemistry.chemical_element, Astronomy and Astrophysics, Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences, Oxygen, Galaxy
Published: 2012
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24. Appendix A : The atomic physics of oxygen

Author: G. Meynet, N. Grevesse, C. J. Zeippen, Hans-Günter Ludwig, A. Decourchelle, Claudio Mendoza, Y. Lebreton, Sergio Simón-Díaz, Corinne Charbonnel, Grazyna Stasinska, Beatriz Barbuy, P. Ferrando, Nikos Prantzos, Marcel Arnould, F. Durret, Cristina Chiappini, V. Hill, M. Katsuma, M. Dessauges-Zavadsky, and Guillaume Hébrard
Subjects: Physics, Theoretical physics, 010504 meteorology & atmospheric sciences, chemistry, Space and Planetary Science, 0103 physical sciences, General Engineering, chemistry.chemical_element, Astronomy and Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences, Oxygen, 0105 earth and related environmental sciences
Published: 2012
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25. Chapter 2 : A Panorama of Oxygen in the Universe

Author: Beatriz Barbuy, F. Durret, C. J. Zeippen, Guillaume Hébrard, M. Arnould, Nikos Prantzos, Sergio Simón-Díaz, G. Meynet, Hans-Günter Ludwig, Cristina Chiappini, V. Hill, M. Katsuma, Claudio Mendoza, Grazyna Stasinska, Y. Lebreton, A. Decourchelle, C. Charbonnel, M. Dessauges-Zavadsky, P. Ferrando, and N. Grevesse
Subjects: Physics, Theoretical physics, Panorama, Space and Planetary Science, 0103 physical sciences, General Engineering, Astronomy and Astrophysics, 010402 general chemistry, 010303 astronomy & astrophysics, 01 natural sciences, 0104 chemical sciences
Published: 2012
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26. Can mass loss and overshooting prevent the excitation of g-modes in blue supergiants?

Author: M. Godart, A. Noels, M.-A. Dupret, Y. Lebreton, Département des Sciences et Gestion de l'Environnement/Océanologie [Liège], Université de Liège, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), SIMPA, Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS)-Université de Rennes 1 (UR1), and Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: stars, mass-loss -stars, Convection, Opacity, FOS: Physical sciences, Astrophysics, 01 natural sciences, evolution -stars, 0103 physical sciences, Blue supergiant, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, stars: evolution, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, oscillations -supergiants, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, supergiants, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Stars, Astrophysics - Solar and Stellar Astrophysics, Convection zone, Space and Planetary Science, Excited state, stars: oscillations, Supergiant, stars: mass-loss
Abstract: Thanks to their past history on the main sequence phase, supergiant massive stars develop a convective shell around the helium core. This intermediate convective zone (ICZ) plays an essential role in governing which g-modes are excited. Indeed a strong radiative damping occurs in the high density radiative core but the ICZ acts as a barrier preventing the propagation of some g-modes into the core. These g-modes can thus be excited in supergiant stars by the kappa-mechanism in the superficial layers due to the opacity bump of iron, at log T=5.2. However massive stars are submitted to various complex phenomena such as rotation, magnetic fields, semiconvection, mass loss, overshooting. Each of these phenomena exerts a significant effect on the evolution and some of them could prevent the onset of the convective zone. We develop a numerical method which allows us to select the reflected, thus the potentially excited, modes only. We study different cases in order to show that mass loss and overshooting, in a large enough amount, reduce the extent of the ICZ and are unfavourable to the excitation of g-modes., 9 pages, 11 figures, accepted for publication in MNRAS
Published: 2009
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27. Effects of level of feed intake on pancreatic exocrine secretions during the early postweaning period in piglets1

Author: Y Lebreton, E. Bobillier, Gérard Savary, I. Le Huërou-Luron, and A. Huguet
Subjects: medicine.medical_specialty, Meal, biology, Animal feed, General Medicine, Endocrinology, Postprandial, Internal medicine, Pancreatic juice, Digestive enzyme, Genetics, biology.protein, medicine, Weaning, Animal Science and Zoology, Amylase, Food Science, Antibacterial agent
Abstract: The objective of this study was to determine the influence of the level of feed intake and a 2-d feed restriction period on the postweaning adaptation of pancreatic exocrine secretions. At 33 d of age, 18 piglets fitted with 2 permanent catheters (for pancreatic juice collection and reintroduction) were weaned and allocated to 1 of the following 2 dietary treatments for 5 d: restricted feed allocation (restricted) or gradually increasing feed allocation (control). Pancreatic juice was collected daily during both basal and prandial periods. The basal period was defined as the period from 1400 to 1700 h (i.e., 5 to 8 h after the morning meal), whereas the prandial period was defined as the period from 30 min before to 60 min after the morning meal (given at 0900). Digestive enzyme activities and antibacterial activity were determined. Pancreatic protein secretion was 44% less (P < 0.05) in restricted piglets than in control piglets during the basal period. Trypsin secretion was affected by feed-restriction of piglets. The meal did not affect protein and trypsin secretions in restricted piglets, whereas at d 3 postweaning, protein and trypsin secretions and trypsin specific activity in control piglets were 9-, 105-, and 25-fold greater (P < 0.001) during the first 30 min after the meal than before the meal. Lipase and amylase secretions were not affected by variations in feed intake. The secretion of antibacterial activity in restricted piglets was greater (P < 0.05) than that of control piglets only at d 5. The extended feed restriction period increased the basal secretion of antibacterial activity (P = 0.09) and postprandial secretion of amylase (P = 0.05). In conclusion, a low level of feed intake during the early postweaning period decreased pancreatic protein and trypsin secretions, whereas a 2-d feed restriction period enhanced secretions of amylase and antibacterial activity. In addition, our results indicate that during periods of dietary adaptation, such as at weaning, measurements of enzyme activities in the tissue do not accurately reflect the enzyme secretion.
Published: 2006
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28. Measurement of blood flow through the mammary gland in lactating sows: methodological aspects1

Author: Y Lebreton, Jean Noblet, Jean-Yves Dourmad, and David Renaudeau
Subjects: medicine.medical_specialty, Meal, business.industry, Mammary gland, Ultrasound, General Medicine, Blood flow, Endocrinology, medicine.anatomical_structure, Animal science, Oxytocin, Internal medicine, Lactation, Genetics, Medicine, Weaning, Animal Science and Zoology, business, Food Science, medicine.drug, Artery
Abstract: Two replicates of three multiparous crossbred Large White x Landrace lactating sows were used to develop a technique for the continuous direct measurement of the blood flow through the mammary gland using transit time ultrasound. Four to six days after farrowing, an ultrasonic transit time flow probe was implanted around the right external pudic artery in order to measure the short-term variations of mammary blood flow through this vessel in response to postural change (standing vs lying), meal distribution, hand-milking, and weaning. After surgery, all sows were fed 3.8 kg/d of a lactation diet and housed either at 20 or 28 degrees C. The implantation of the ultrasonic blood flow probe was successful in all six operated sows. Postmortem examination did not indicate the presence of infection, any collateral bypassing the flow probe, or a reduction of artery diameter. The right pudic artery mammary blood flow (PMBF) was measured for 8.5 h over two periods of three days (d 11 to d 13 and d 18 to d 20 of lactation). The PMBF averaged 910 +/- 238 mL/min but was variable within 1 d. Compared with the lying position, PMBF was decreased (- 6%, P < 0.05) when sows were standing. Between 0 to 15 and 16 to 30 min after oxytocin injection (t = 0) and hand-milking, PMBF remained constant (P = 0.05; 801 vs 767 mL/ min) and increased (P = 0.02), respectively, in comparison with the mean calculated over the preceding 30-min period (982 vs 784 mL/min). The PMBF increased (P < 0.05) after meal distribution and reached a peak 65 min later (i.e., 980 mL/min). The PMBF decreased regularly after separation of piglets at weaning; at 8 and 16 h after weaning, PMBF was 60 and 40% of the value recorded before weaning, respectively. Assuming that PMBF drains one-quarter of the whole mammary gland, it can be calculated that blood flow through the entire mammary gland averages 3.6 L/min and that about 470 L of blood are required to produce 1 kg of milk. The proposed methodology constitutes a new technique to measure direct mammary blood flow and its short-term factors of variation.
Published: 2002
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29. Prediction of the standardized ileal true digestibility of amino acids from the chemical composition of oilseed meals in the growing pig

Author: C. Février, Y. Lechevestrier, Y. Lebreton, and Y. Jaguelin-Peyraud
Subjects: chemistry.chemical_classification, Methionine, biology, Lysine, Tryptophan, biology.organism_classification, Amino acid, chemistry.chemical_compound, Animal science, chemistry, Biochemistry, Palm kernel, Ruminant, Animal Science and Zoology, Composition (visual arts), Dry matter
Abstract: Digestibility experiments using growing pigs fitted with an ileorectal anastomosis were performed to measure the standardized ileal true digestibility (ITD) of amino acids in five cotton seed meals (CSM) and three palm kernel meals (PKM), differing in their level of non starch polysaccharides (NSP), as expressed by NDF content and the nitrogen content of NDF (N NDF). The NDF content in CSM ranged from 273 to 475 g kg−1 on dry matter (DM) and the crude protein content from 384 to 506 g kg−1 DM. The latter values were not correlated with the NDF content. For PKM, NDF varied from 592 to 686 g kg−1 and the crude protein content from 151 to 177 g kg−1. Results obtained for CSM clearly demonstrate a curvilinear relationship, except for methionine, between ITD of amino acids and NDF content. Furthermore, if the composition of the CSM as ash, fat, total nitrogen, nitrogen from NDF (N NDF) and total gossypol (TGOS) contents is known (g kg−1 DM), the quantity of digestible amino acid can be predicted for lysine, threonine and tryptophan with reasonable precision, but less for sulfur amino acids. As an example for lysine, dLys ( g kg −1 DM )=6.5116(1.0939)+0.1411 N (0.0158)−0.1673 NNDF (0.0091)−0.0124 NDF (0.0010) R2=0.993. For PKM, the relationships were more difficult to assess because of a narrow range in NDF level and the heterogeneity of response between pigs, especially for the higher NDF contents. In addition, the current data confirmed that the nitrogen content in the NDF fraction of NSP, often considered in ruminant protein nutrition, could be also an useful predictor of true ileal digestible values for selected amino acids in the pig
Published: 2001
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30. Cholangiocarcinome et hypercalcémie humorale maligne

Author: Dominique Béchade, Jean-Pierre Algayres, Stéphane Lecoules, Y. Lebreton, Jérôme Desramé, T. Carmoi, H. Blondon, Y. Sekkach, and M. Billhot
Subjects: Gynecology, medicine.medical_specialty, business.industry, Gastroenterology, medicine, General Medicine, business
Published: 2009
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31. Effects of dietary changes on the antibacterial activity of pancreatic juice in weaned piglets

Author: Y Lebreton, A. Huguet, I. Le Huërou-Luron, Gérard Savary, E. Bobillier, ProdInra, Migration, Systèmes d'Elevage, Nutrition Animale et Humaine (SENAH), and Ecole Nationale Supérieure Agronomique de Rennes-Institut National de la Recherche Agronomique (INRA)
Subjects: [SDV.SA]Life Sciences [q-bio]/Agricultural sciences, medicine.medical_specialty, animal diseases, ANTIBACTERIAL ACTIVITY, COLOSTRUM, Biology, 03 medical and health sciences, FEED INTAKE, fluids and secretions, Starter, Animal science, Internal medicine, medicine, Weaning, Secretion, ComputingMilieux_MISCELLANEOUS, PIGLETS, 030304 developmental biology, 2. Zero hunger, [SDV.SA] Life Sciences [q-bio]/Agricultural sciences, 0303 health sciences, General Veterinary, 0402 animal and dairy science, 04 agricultural and veterinary sciences, 040201 dairy & animal science, Small intestine, Endocrinology, medicine.anatomical_structure, Pancreatic juice, Colostrum, Animal Science and Zoology, Antibacterial activity, PANCREATIC JUICE, Homeostasis
Abstract: At weaning, low feed intake level is a major factor responsible for gut disorders. However, less is known on adaptation of the antibacterial activity of pancreatic juice in response to variations in feed intake level. Moreover bovine colostrum has been demonstrated to decrease coliform counts in duodenal digesta and to improve health status of weaned piglets. Aims of the present study were to evaluate effects of feed intake level and of a bovine colostrum-supplemented diet on the pancreatic secretion of antibacterial activity in piglets at weaning. At 33 days of age, twenty-eight piglets fitted with two permanent catheters (for pancreatic juice collection and reintroduction) were weaned and allocated to one of the following three dietary treatments for 5 days: low feed allocation with a starter diet (L), gradually increased feed allocation with a starter diet (Ctrl), or gradually increased feed allocation with a starter diet supplemented with bovine colostrum (Col). In Ctrl piglets, the post-weaning secretion of antibacterial activity did not significantly differed from pre-weaning values. The pancreatic secretion of antibacterial activity in L piglets was higher than that in Ctrl piglets at day 5 (+ 300%; P < 0.05). Moreover in Col piglets the secretion of the antibacterial activity tended to increase by 55% (P = 0.08) compared to Ctrl piglets. Variations in the pancreatic secretion of antibacterial activity could constitute an adaptive phenomenon to maintain bacterial homeostasis in the upper small intestine during the early post-weaning period.
Published: 2007
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32. Transport of angular momentum in solar-like oscillating stars

Author: B. Mosser, Rafa García, Joao Marques, Y. Lebreton, Marie-Jo Goupil, Sébastien Deheuvels, Stéphane Mathis, Kevin Belkacem, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Angular momentum, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], K-type main-sequence star, Astronomy and Astrophysics, Astrophysics, Compact star, T Tauri star, Stars, Space and Planetary Science, Stellar mass loss, Stellar dynamics, 14. Life underwater, Main sequence, ComputingMilieux_MISCELLANEOUS
Abstract: Our current understanding and modeling of angular momentum transport in low-mass stars are briefly reviewed. Emphasis is set on single stars slightly younger that the Sun and on subgiants and red giants observed by the space missionsCoRoTandKepler.
Published: 2013
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33. Accurate Parallaxes and Stellar Ages Determinations

Author: Y. Lebreton, E. Michel, M.J. Goupil, A. Baglin, and J. Fernandes
Subjects: 010504 meteorology & atmospheric sciences, 0103 physical sciences, 010303 astronomy & astrophysics, 01 natural sciences, 0105 earth and related environmental sciences
Abstract: Uncertainties on stellar ages due to the physical description of the stellar material entering the models and to measurements of global parameters and chemical composition are estimated in the case of A/F stars.With combined efforts on atmosphere modeling (to improve global parameters), on asteroseismology (to improve the physical description of the stellar interior) and on distance determination at the level of the sub-milliarcsecond (to improve luminosity), an accuracy on age determination of about 10% is foreseeable.
Published: 1995
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34. Chapter 1 : How to Derive Oxygen Abundances

Author: Marcel Arnould, C. J. Zeippen, Cristina Chiappini, V. Hill, M. Katsuma, Y. Lebreton, Guillaume Hébrard, M. Dessauges-Zavadsky, Nikos Prantzos, G. Meynet, Hans-Günter Ludwig, N. Grevesse, Sergio Simón-Díaz, Claudio Mendoza, Corinne Charbonnel, A. Decourchelle, Grazyna Stasinska, P. Ferrando, F. Durret, and Beatriz Barbuy
Subjects: Physics, 010504 meteorology & atmospheric sciences, General Engineering, chemistry.chemical_element, Astronomy and Astrophysics, 01 natural sciences, Oxygen, Nuclear physics, Theoretical physics, chemistry, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Published: 2012

35. Utilisations digestives comparées des laits UHT de chèvre et de vache. Effets nutritionnels de la gélification. Utilisation du modèle porcin

Author: Y. Lebreton, J. Mourot, A. Mounier, C. Février, Y. Jaguelin, and Revues Inra, Import
Subjects: [SDV.AEN] Life Sciences [q-bio]/Food and Nutrition, [SDV.IDA] Life Sciences [q-bio]/Food engineering, Biology, Food Science
Published: 1993
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36. The Asteroseismic Potential of Kepler: First Results for Solar-Type Stars

Author: W. J. Chaplin, T. Appourchaux, Y. Elsworth, R. A. García, G. Houdek, C. Karoff, T. S. Metcalfe, J. Molenda-Żakowicz, M. J. P. F. G. Monteiro, M. J. Thompson, T. M. Brown, J. Christensen-Dalsgaard, R. L. Gilliland, H. Kjeldsen, W. J. Borucki, D. Koch, J. M. Jenkins, J. Ballot, S. Basu, M. Bazot, T. R. Bedding, O. Benomar, A. Bonanno, I. M. Brandão, H. Bruntt, T. L. Campante, O. L. Creevey, M. P. Di Mauro, G. Doğan, S. Dreizler, P. Eggenberger, L. Esch, S. T. Fletcher, S. Frandsen, N. Gai, P. Gaulme, R. Handberg, S. Hekker, R. Howe, D. Huber, S. G. Korzennik, J. C. Lebrun, S. Leccia, M. Martic, S. Mathur, B. Mosser, R. New, P.-O. Quirion, C. Régulo, I. W. Roxburgh, D. Salabert, J. Schou, S. G. Sousa, D. Stello, G. A. Verner, T. Arentoft, C. Barban, K. Belkacem, S. Benatti, K. Biazzo, P. Boumier, P. A. Bradley, A.-M. Broomhall, D. L. Buzasi, R. U. Claudi, M. S. Cunha, F. D'Antona, S. Deheuvels, A. Derekas, A. García Hernández, M. S. Giampapa, M. J. Goupil, M. Gruberbauer, J. A. Guzik, S. J. Hale, M. J. Ireland, L. L. Kiss, I. N. Kitiashvili, K. Kolenberg, H. Korhonen, A. G. Kosovichev, F. Kupka, Y. Lebreton, B. Leroy, H.-G. Ludwig, S. Mathis, E. Michel, A. Miglio, J. Montalbán, A. Moya, A. Noels, R. W. Noyes, P. L. Pallé, L. Piau, H. L. Preston, T. Roca Cortés, M. Roth, K. H. Sato, J. Schmitt, A. M. Serenelli, V. Silva Aguirre, I. R. Stevens, J. C. Suárez, M. D. Suran, R. Trampedach, S. Turck-Chièze, K. Uytterhoeven, R. Ventura, P. A. Wilson, School of Physics and Astronomy [Birmingham], University of Birmingham [Birmingham], Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institute for Astronomy [Vienna], University of Vienna [Vienna], High Altitude Observatory (HAO), National Center for Atmospheric Research [Boulder] (NCAR), Astronomical Institute [Wroclaw], University of Wrocław [Poland] (UWr), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, School of Mathematics and Statistics [Sheffield] (SoMaS), University of Sheffield [Sheffield], Las Cumbres Observatory (LCO), Department of Physics and Astronomy [Aarhus], Aarhus University [Aarhus], Space Telescope Science Institute (STSci), NASA Ames Research Center (ARC), SETI Institute, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Department of Astronomy [New Haven], Yale University [New Haven], Sydney Institute for Astronomy (SIfA), The University of Sydney, INAF - Osservatorio Astrofisico di Catania (OACT), Istituto Nazionale di Astrofisica (INAF), Observatoire de Paris, Université Paris sciences et lettres (PSL), Departamento de Astrofísica [La laguna], Universidad de La Laguna [Tenerife - SP] (ULL), Instituto de Astrofisica de Canarias (IAC), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Institut für Astrophysik [Göttingen], Georg-August-University [Göttingen], Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Materials and Engineering Research Institute [Sheffield] (MERI), Sheffield Hallam University, Beijing Normal University (BNU), National Solar Observatory [Tucson] (NSO/Tucson), National Science Foundation [Arlington] (NSF)-Association of Universities for Research in Astronomy (AURA), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), INAF - Osservatorio Astronomico di Capodimonte (OAC), Indian Institute of Astrophysics (IIA), Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Canadian Space Agency (CSA), Astronomy Unit [London] (AU), Queen Mary University of London (QMUL), Hansen Experimental Physics Lab [Stanford] (HEPL), Stanford University, Département d'astrophysique, Géophysique et Océanographie (AGO), Université de Liège, Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, INAF - Osservatorio Astrofisico di Arcetri (OAA), Los Alamos National Laboratory (LANL), Eureka Scientific, INAF - Osservatorio Astronomico di Padova (OAPD), INAF - Osservatorio Astronomico di Roma (OAR), Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Astronomy and Physics [Halifax], Saint Mary's University [Halifax], Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'Astrophysique et de Géophysique [Liège], Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Universidade do Porto = University of Porto, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Georg-August-University = Georg-August-Universität Göttingen, Université de Genève = University of Geneva (UNIGE), Harvard University-Smithsonian Institution, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Università degli Studi di Padova = University of Padua (Unipd), and Faculdade de Ciências
Subjects: oscillations [stars], Física [Ciências exactas e naturais], FOS: Physical sciences, Astrophysics, Type (model theory), Star (graph theory), stars: interiors, 01 natural sciences, Kepler, Spectral line, Physical sciences [Natural sciences], Astrophysics, Astronomy, Physical sciences, Physical sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrofísica, Astronomia, Ciências Físicas, Física, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, interiors [stars], 010308 nuclear & particles physics, Oscillation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], stars: late-type, Astronomy and Astrophysics, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, late-type [stars], Astrophysics::Earth and Planetary Astrophysics, stars: oscillations
Abstract: We present preliminary asteroseismic results from Kepler on three G-type stars. The observations, made at one-minute cadence during the first 33.5d of science operations, reveal high signal-to-noise solar-like oscillation spectra in all three stars: About 20 modes of oscillation may be clearly distinguished in each star. We discuss the appearance of the oscillation spectra, use the frequencies and frequency separations to provide first results on the radii, masses and ages of the stars, and comment in the light of these results on prospects for inference on other solar-type stars that Kepler will observe., Comment: 16 pages, 3 figures, 1 table; now accepted for publication in ApJ Letters
Published: 2010
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37. CoRot observations of active giants: preliminary results

Author: P. Gondoin, M. Fridlund, M. J. Goupil, F. Baudin, R. Samadi, C. Barban, K. Belkacem, T. Corbard, M. A. Dupret, B. Foing, R. den Hartog, Y. Lebreton, J. Lochard, P. Mathias, E. Michel, P. Morel, A. Moya, A. Palacios, J. P. Zahn, Eric Stempels, Geneva Observatory, University of Geneva [Switzerland], Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Airbus Defence and Space [Toulouse], Laboratoire Hippolyte Fizeau (FIZEAU), DAM Île-de-France (DAM/DIF), Direction des Applications Militaires (DAM), Institut Cavanilles de Biodiversitat i Biologia Evolutiva (ICBiBE), Universitat de València (UV), Institute of Environmental Assessment and Water Research (IDAEA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Physics and Astronomy [Uppsala], Uppsala University, Université de Genève = University of Geneva (UNIGE), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Rotation period, Physics, 13. Climate action, Star formation, Stellar rotation, Astronomy, Astrophysics, Effective temperature, Rotation, Giant star, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], ComputingMilieux_MISCELLANEOUS
Abstract: We have analysed rotation modulated light‐curves of active giants observed with CoRot using spots model. Preliminary results suggest an increase of the surface spot coverage with decreasing rotation period. A maximum of the surface spot coverage seems to occur on giants with effective temperature around 5100 K. Confirmation and interpretation of these preliminary results require groundbased follow‐up observations to measure activity indicators, to identify binary systems, and to determine the stellar parameters and evolutionary status of the sample giants.
Published: 2008
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38. ENEAS: the European Network of Excellence in AsteroSeismology

Author: Zoltán Kolláth, Arlette Noels, Michael Thompson, Carla Maceroni, Hans Kjeldsen, Günter Houdek, E. Solano, A. Baglin, Conny Aerts, A. Schwarzenberg-Czerny, P. Skoda, M. J. Goupil, Jørgen Christensen-Dalsgaard, D. W. Kurtz, Y. Lebreton, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Astronomie du LESIA, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
Subjects: Engineering, Operations research, business.industry, Network of excellence, Public relations, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business, Asteroseismology, Space exploration
Abstract: In this contribution we briefly introduce the history of the European Network of Excellence in AsteroSeismology, its goals and some concrete action items that have been defined. We invite all interested scientists to take part in our initiative, to make use of the facilities of the network and to propose suggestions for its future activities and structure. History and Goal of ENEAS The European Network of Excellence in AsteroSeismology (ENEAS) was created on 11 October 2002 during a kick-off meeting held in Leuven (Belgium). This kick-off meeting was the result of the need felt by several astronomers in leading institutes in asteroseismology to develop an efficient exchange programme and to create closer collaborations across Europe in this research field. This need became evident during the numerous meetings of the European consortia of the future asteroseismic space missions planned for launch within a couple of years from now. We need not convince the readers of this journal that asteroseismology is one of the major important science topics in astrophysics in the coming decade. Very substantial investments are being made in Europe to ensure observations of stellar oscillations of unforeseen quality. It concerns both upgraded groundbased instruments and asteroseismic space missions, COROT and Eddington, planned for launch between 2005 and 2008. Besides these European missions, NASA’s WIRE satellite was recently put back into operation and the Canadian MOST mission was just launched successfully (see elsewhere this volume).
Published: 2007
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39. Spectroscopic survey of the Galaxy with Gaia - II. The expected science yield from the Radial Velocity Spectrometer

Author: M. I. Wilkinson, A. Vallenari, C. Turon, U. Munari, D. Katz, G. Bono, M. Cropper, A. Helmi, N. Robichon, F. Thévenin, S. Vidrih, T. Zwitter, F. Arenou, M.-O. Baylac, G. Bertelli, A. Bijaoui, F. Boschi, F. Castelli, F. Crifo, M. David, A. Gomboc, A. Gómez, M. Haywood, U. Jauregi, P. de Laverny, Y. Lebreton, P. Marrese, T. Marsh, S. Mignot, D. Morin, S. Pasetto, M. Perryman, A. Prša, A. Recio-Blanco, F. Royer, A. Sellier, A. Siviero, R. Sordo, C. Soubiran, L. Tomasella, Y. Viala, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Departament Llenguatges i Sistemes Informatics, Universitat Politècnica de Catalunya [Barcelona] (UPC), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Faculty of Mathematics and Physics [Ljubljana] (FMF), University of Ljubljana, Griffith University [Brisbane], European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Galilée (Galilée), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: GRAVITATIONAL LENSING EXPERIMENT, Astrophysics, 01 natural sciences, stars : general, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Stellar evolution, stars: general, Galaxy: structure, Physics, [PHYS]Physics [physics], Settore FIS/05, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Radial velocity, AGE-METALLICITY RELATION, Galaxy: formation, PERIOD-LUMINOSITY RELATION, Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Galaxy: kinematics and dynamics, binaries: spectroscopic, Galaxy : kinematics and dynamics, Photometric system, FOS: Physical sciences, Galaxy : structure, MILKY-WAY DISK, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy : evolution, binaries : spectroscopic, 0103 physical sciences, Spectrograph, Astrophysics::Galaxy Astrophysics, Galaxy: evolution, SOLAR-TYPE STARS, Spectrometer, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], SURVEY COMMISSIONING DATA, Galaxy : formation, Astronomy and Astrophysics, HUBBLE-SPACE-TELESCOPE, Galaxy, Stars, Space and Planetary Science, DARK-MATTER HALOES, DIGITAL SKY SURVEY, LARGE-MAGELLANIC-CLOUD, Variable star, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The Gaia mission is designed as a Galaxy explorer, and will measure simultaneously, in a survey mode, the five or six phase space parameters of all stars brighter than 20th magnitude, as well as providing a description of their astrophysical characteristics. These measurements are obtained by combining an astrometric instrument with micro-arcsecond capabilities, a photometric system giving the magnitudes and colours in 15 bands and a medium resolution spectrograph named the Radial Velocity Spectrometer (RVS). The latter instrument will produce spectra in the 848 to 874 nm wavelength range, with a resolving power R = 11 500, from which radial velocities, rotational velocities, atmospheric parameters and abundances can be derived. A companion paper (Katz et al. 2004) presents the characteristics of the RVS and its performance. This paper details the outstanding scientific impact of this important part of the Gaia satellite on some key open questions in present day astrophysics. The unbiased and simultaneous acquisition of multi-epoch radial velocities and individual abundances of key elements in parallel with the astrometric parameters is essential for the determination of the dynamical state and formation history of our Galaxy. Moreover, for stars brighter than V=15, the resolving power of the RVS will give information about most of the effects which influence the position of a star in the Hertzsprung-Russell diagram, placing unprecedented constraints on the age, internal structure and evolution of stars of all types. Finally, the RVS multi-epoch observations are ideally suited to the identification, classification and characterisation of the many types of double, multiple and variable stars., 33 pages, 11 figures, in press at MNRAS. Figs 1, 3 and 9 included at reduced resolution; available in full resolution at http://www.blackwell-synergy.com/doi/pdf/10.1111/j.1365-2966.2005.09012.x
Published: 2005
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40. Preface

Author: Y. Lebreton, G. Vauclair, G. Alecian, and O. Richard
Subjects: Physics, Space and Planetary Science, Stellar physics, General Engineering, Astronomy, Astronomy and Astrophysics
Published: 2013
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41. Effet de la réduction du taux protéique de l'aliment sur la volatilisation ammoniacale des effluents porcins

Author: Y. Lebreton, S. Portejoie, José Mario Martínez, Jean-Yves Dourmad, Unité mixte de recherche veau et porc (UMR VP), Ecole Nationale Supérieure Agronomique de Rennes-Institut National de la Recherche Agronomique (INRA), Gestion environnementale et traitement biologique des déchets (UR GERE), Centre national du machinisme agricole, du génie rural, des eaux et forêts (CEMAGREF), and Institut National de la Recherche Agronomique (INRA)
Subjects: 2. Zero hunger, [SDV.SA]Life Sciences [q-bio]/Agricultural sciences, Manure management, General Veterinary, Chemistry, 0402 animal and dairy science, chemistry.chemical_element, 04 agricultural and veterinary sciences, Ammonia volatilization from urea, 040201 dairy & animal science, Nitrogen, Manure, 6. Clean water, Excretion, Ammonia, chemistry.chemical_compound, Animal science, Agronomy, [SDE]Environmental Sciences, 040103 agronomy & agriculture, Slurry, 0401 agriculture, forestry, and fisheries, Animal Science and Zoology, Ammoniacal nitrogen, ComputingMilieux_MISCELLANEOUS
Abstract: International audience; The aim of this study was to evaluate the effects of three strategies of protein feeding (12%, 16% and 20%), supplying adequate levels of all essential amino acids, on finishing pig performance, nitrogen excretion and ammonia emission in the laboratory and in the field. The animals (15 castrated males) were housed individually in metabolism cages and were fed one of the three diets. The experiment lasted 21 days and urine and faeces were collected separately. Samples of each type of manure (urine alone, fresh slurry and 18-day slurry) were placed for 6 days in a laboratory pilot scale system designed to measure ammonia emission. In the field, measurements of ammonia volatilization were made during storage and surface application of slurry. Lowering dietary crude protein, while maintaining similar levels of essential amino acids, reduced total amount of manure, because of a lower water consumption, without any negative effect on animal performance. Total ammoniacal nitrogen content in the slurry was reduced from 4.32 g N kg−1 to 3.13 and 1.92 g N kg−1 when dietary CP decreased from 20% to 16% and 12%, respectively (the corresponding figures for total nitrogen content were 5.48, 4.30 and 3.05 g N kg−1, respectively). The pH of slurry decreased by 1.3 units when dietary crude protein decreased from 20% to 12%. These changes in slurry composition and pH resulted in a reduction of ammonia emissions at each stage of manure management. Over the whole process of the slurry, ammonia emission was decreased by 63% when dietary protein decreased from 20% to 12%.; L'objectif de cette expérience est de déterminer l'influence de trois conduites alimentaires différenciées par l'apport de protéines (12, 16 et 20%) sur les performances zootechniques, sur l'excrétion azotée des animaux, sur la volatilisation de l'ammoniac des effluents, au laboratoire et sur le terrain. Quinze mâles castrés sont placés en cage de digestibilité et affectés aux trois traitements. La diminution de la teneur en protéines du régime permet une réduction importante de l'excrétion azotée, surtout au niveau de la fraction urinaire sans affecter les performances zootechniques. Tous ces facteurs contribuent à réduire les pertes par volatilisation de l'ammoniac aux différents stades de la gestion des effluents. Sur l'ensemble du processus de gestion des effluents, une réduction de la volatilisation de l'ammoniac de 63% est observée en abaissant le taux protéique de l'aliment de 20 à 12%.
Published: 2004

42. Measurement of blood flow through the mammary gland in lactating sows: methodological aspects

Author: D, Renaudeau, Y, Lebreton, J, Noblet, and J Y, Dourmad
Subjects: Mammary Glands, Animal, Regional Blood Flow, Swine, Animals, Lactation, Female, Ultrasonography, Mammary, Weaning, Oxytocin, Blood Flow Velocity
Abstract: Two replicates of three multiparous crossbred Large White x Landrace lactating sows were used to develop a technique for the continuous direct measurement of the blood flow through the mammary gland using transit time ultrasound. Four to six days after farrowing, an ultrasonic transit time flow probe was implanted around the right external pudic artery in order to measure the short-term variations of mammary blood flow through this vessel in response to postural change (standing vs lying), meal distribution, hand-milking, and weaning. After surgery, all sows were fed 3.8 kg/d of a lactation diet and housed either at 20 or 28 degrees C. The implantation of the ultrasonic blood flow probe was successful in all six operated sows. Postmortem examination did not indicate the presence of infection, any collateral bypassing the flow probe, or a reduction of artery diameter. The right pudic artery mammary blood flow (PMBF) was measured for 8.5 h over two periods of three days (d 11 to d 13 and d 18 to d 20 of lactation). The PMBF averaged 910 +/- 238 mL/min but was variable within 1 d. Compared with the lying position, PMBF was decreased (- 6%, P0.05) when sows were standing. Between 0 to 15 and 16 to 30 min after oxytocin injection (t = 0) and hand-milking, PMBF remained constant (P = 0.05; 801 vs 767 mL/ min) and increased (P = 0.02), respectively, in comparison with the mean calculated over the preceding 30-min period (982 vs 784 mL/min). The PMBF increased (P0.05) after meal distribution and reached a peak 65 min later (i.e., 980 mL/min). The PMBF decreased regularly after separation of piglets at weaning; at 8 and 16 h after weaning, PMBF was 60 and 40% of the value recorded before weaning, respectively. Assuming that PMBF drains one-quarter of the whole mammary gland, it can be calculated that blood flow through the entire mammary gland averages 3.6 L/min and that about 470 L of blood are required to produce 1 kg of milk. The proposed methodology constitutes a new technique to measure direct mammary blood flow and its short-term factors of variation.
Published: 2002

43. Let Us Begin by Modelling Two Observed Delta Scuti Stars Simultaneously

Author: E. Michel, M.J. Goupil, and Y. Lebreton
Subjects: Delta, Physics, Stars, Astrophysics
Abstract: We consider here two Delta Scuti stars GX Pegasi and V650 Tauri, which show very close masses and evolution stages as infered from photometrical calibration. The se two stars have been observed by the STEPHI team (Michel et al. 1990, Belmonte et al. this procedings) and they appear to be multiperiodic pulsators. For both these stars, an identification of the observed frequencies is proposed, from comparison with adiabatic eigenfrequencies computed for well suited stellar mode ls. This interpretation reveals very different pulsational behaviors despite the sta rs are expected to present very similar internal structures. We report here a first step toward constraining models by improving the fit between the observed and the calculated eigenfrequencies. The effect of overshooting and of the recent enhancement of the opacities are i nvestigated.
Published: 1993
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44. Effects of adding potassium diformate and phytase excess for weaned piglets

Author: C. Février, A. Aumaître, G. Gotterbarm, Y. Lebreton, F. Legouevec, and Y. Jaguelin-Peyraud
Subjects: Animal science, chemistry, Weaned piglets, Potassium, chemistry.chemical_element, Phytase, Biology
Published: 2001
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45. Ileal flow of endogenous amino acids in relation to energy source: consequences on the evaluation of ileal digestibility of protein in growing pigs

Author: Y. Jaguelin-Peyraud, Y. Lebreton, C. Février, N. Mézières, and F. Legouevec
Subjects: chemistry.chemical_classification, Chemistry, Endogeny, Food science, Energy source, Amino acid
Published: 2001
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46. Small-bowel feces sign

Author: Y. Lebreton, G. Weber-Donat, M. Lahutte, C. Chavihot, A. Saurel, and P. Calcina
Subjects: medicine.medical_specialty, medicine.diagnostic_test, business.industry, Internal medicine, Medicine, Radiology, Nuclear Medicine and imaging, Computed tomography, Radiology, business, Gastroenterology, Feces, Sign (mathematics)
Published: 2010
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47. Old, Low-Mass, Metal-Rich (SMR) Stars

Author: E. D. Friel, Caroline Soubiran, Y. Lebreton, and G. Cayrel de Strobel
Subjects: Physics, Stars, High resolution, Astronomy, Astrophysics, Effective temperature, Late-type star, Low Mass, Cosmology
Abstract: The authors of this paper try to disentangle the many problems arisen from a new enlarged sample of nearby low-mass, metal-rich-stars. These stars have reliable absolute magnitudes, deduced from Hipparcos parallaxes, precise bolometric corrections, effective temperatures and metal abundances from high resolution detailed spectroscopic analyses. Their ages have been derived from a grid of isochrones calculated with up to date physics. The main goal of this paper is to determine the ages of the slightly evolved SMR stars. Among those with well determinated ages about 80% of them have intermediate ages of (2 to 5 Gyr), but only 20% have ages of 8 Gyr or more. Nevertheless, the existence of very old metal-rich stars is confirmed.
Published: 1999
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48. Effets de l'incorporation de pulpe de betterave dans les aliments du porcelet et du porc en croissance : performances de croissance, digestibilité et composition corporelle

Author: R. Lizardo, J. Peiniau, A. Aumaitre, Y. Lebreton, Revues Inra, Import, ProdInra, Migration, Station de recherches porcines, and Institut National de la Recherche Agronomique (INRA)
Subjects: biology, business.industry, Pulp (paper), food and beverages, engineering.material, biology.organism_classification, Crossbreed, Feed conversion ratio, Biotechnology, Starter, Animal science, ALIMENT POUR ANIMAUX, [SDV.SA.SF]Life Sciences [q-bio]/Agricultural sciences/Silviculture, forestry, engineering, Weaning, Animal Science and Zoology, Dry matter, Sugar beet, [SDV.SA.SF] Life Sciences [q-bio]/Agricultural sciences/Silviculture, forestry, Beet pulp, business, [SDV.SA.ZOO] Life Sciences [q-bio]/Agricultural sciences/Zootechny, EFFICACITE ALIMENTAIRE, ComputingMilieux_MISCELLANEOUS
Abstract: Summary — Consequences of the inclusion of sugar beet pulp in diets for early weaned and growing pigs. The effect of extrusion of wheat and of the inclusion of 6% of sugar beet pulp in a pelleted starter on the performance of the weaned piglet has been studied in two experiments. In the first experiment, 80 crossbred castrated male and female piglets weaned at 21 days of age raised individually y were used in a 2 x 2 factorial arrangement to compare their performance between weaning and 25 kg g live weight. Average feed intake was similar between treatments, but extrusion of wheat had no significant effect on growth performance and feed conversion ratio. The association of normal wheat with sugar beet pulp improved significantly growth rate (P < 0.02) and feed conversion ratio (P < 0.06), in particular during the period following immediatly weaning, ie, 193 vs 156 g/day and 193 vs 2.32, respectively. In the second experiment, 32 crossbred castrated piglets were used to evaluate faecal, then ileal digestibilities of dietary components. Extrusion did not improve digestibility. Ileal digestibility but not faecal digestibility of dry matter and energy was reduced (P < 0.001 ) by the inclusion of sugar beet pulp in the diet. Post-ileal digestibility of all dietary components was higher in animals fed fibrous diet. During the growing-finishing period between 25 and 100 kg live weight, the inclusion of a similar level of 6% of sugar beet pulp in a normal wheat based diet was tested. Piglets of the first experiment were randomly affected to one of the two diets taking into account their previous diet, sex and weight. The average daily gain for the whole period was slighly but not significantly reduced and feed conversion ratio was unchanged in animals receiving sugar beet pulp. However, feed conversion ratio expressed as digeatible energy per kg of body weight gain was reduced in animals receiving beet pulp in their diet. At slaughter, the percentage of lean meat was improved from 52.8 to 54.0% (P < 0.05) as a consequence of a linear decrease in the backfat thickness (P < 0.05) of carcasses of animals receiving sugar beet pulp. No difference in the weight of lean cuts was observed but the use of sugar beet pulp decreased significantly the weight of fat cuts (P < 0.01 It was suggested that for a similar nitrogen retention a reduction in the digestible energy intake reduces the deposition of fatty tissues but the total amount of lean meat in the carcass was not affected by the inclusion of sugar beet in the diet.
Published: 1997

49. Effects of dietary protein sources differing in solubility on total tract and ileal apparent digestibility of nitrogen and pancreatic enzymes activity in early weaned pigs

Author: A. Aumaitre, Y. Lebreton, J. Peiniau, ProdInra, Migration, Station de recherches porcines, and Institut National de la Recherche Agronomique (INRA)
Subjects: [SDV.SA]Life Sciences [q-bio]/Agricultural sciences, 030309 nutrition & dietetics, Starch, Ileum, 03 medical and health sciences, chemistry.chemical_compound, Starter, Casein, medicine, Weaning, Food science, ComputingMilieux_MISCELLANEOUS, 2. Zero hunger, chemistry.chemical_classification, 0303 health sciences, Meal, [SDV.SA] Life Sciences [q-bio]/Agricultural sciences, Chymotrypsin, General Veterinary, biology, 0402 animal and dairy science, 04 agricultural and veterinary sciences, 040201 dairy & animal science, medicine.anatomical_structure, Enzyme, chemistry, biology.protein, Animal Science and Zoology
Abstract: A digestibility trial involving 28 castrated male piglets from seven litters weaned at 21 days of age was conducted to examine total tract apparent digestibility (TTAD) and ileal apparent digestibility (IAD) of nitrogen. Four experimental diets based on manioc starch were compared, containing 21.8% crude protein of different physical properties supplied either by casein (C), soluble fish protein concentrate (SFPC), soyabean meal (SBM) or soyabean meal concentrate (SBMC). Insoluble N represented more than 90% of total N in casein, soyabean meal and soyabean concentrate; opposite to that, approx. one-third of N was either insoluble, or alcohol soluble or TCA soluble. The percentage of the different protein fractions in the digesta at the end of the ileum was not affected by the source of protein. The TTAD of nitrogen in diets containing C, SFPC, SBM or SBMC was 93.3, 89.5, 81.1 and 89.8%, respectively. The corresponding values for IAD were 87.7, 79.1, 72.5 and 84.2%, respectively. Compared to animals fed casein diet, weight of pancreas and total activity of chymotrypsin were reduced in those fed the SFPC diet by 36 and 56%, respectively. Diets containing SBM or SBMC caused a reduction of 6 (NS) and up to 35% (NS) in the weight of pancreas and the total activity of chymotrypsin, respectively. Results suggested that the only use of a highly soluble protein source in the starter diet reduces the development of the digestive process in particular the biosynthesis of the enzymes in the pancreas of the weaned piglet.
Published: 1996

50. Endogenous amino nitrogen collected from pigs with end-to-end ileorectal anastomosis is affected by the method of estimation and altered by dietary fiber

Author: G, Mariscal-Landín, B, Sève, Y, Colléaux, and Y, Lebreton
Subjects: Dietary Fiber, Male, Nitrogen, Swine, Anastomosis, Surgical, Rectum, Amino Sugars, Feces, Ileum, Linear Models, Animals, Digestion, Dietary Proteins, Amino Acids
Abstract: Endogenous protein loss at the end of the small intestine was determined in two experiments using 10 pigs surgically prepared with end-to-end ileo-rectal anastomosis to allow total collection of ileal digesta. In the first experiment pigs were fed graded protein levels of 0 (protein-free), 55, 110 or 165 g/kg diet. Optimal durations for the adaptation and collection periods were found to be 4 and 3 d, respectively (combination 4:3), as shown by the higher correlation coefficient (r2 = 0.95) between excreted and ingested nitrogen compared with the other combinations tested (5:2, 5:3, 9:3, 9:5). The estimated amounts of endogenous N and amino acids were less accurate and tended to be smaller (P0.20) when obtained by extrapolation to zero nitrogen intake than when measured in pigs fed the protein-free diet. The endogenous protein was rich in proline, glutamic acid, glycine, aspartic acid, serine and threonine. In comparison to other amino acid patterns, this composition suggested a low bacterial contamination of the digesta. In the second experiment three levels of dietary fiber from wheat straw, corn cobs and wood cellulose were studied in pigs fed protein-free diets. Between 17 and 34 g crude fiber/kg diet, fiber increased the endogenous losses of nitrogen and amino acids per kilogram of dry matter intake (P0.05), but the excretion reached a plateau at higher dietary fiber concentration (102 g/kg). In contrast, glucosamine and galactosamine excretion increased continuously and linearly (P0.05) with fiber intake. We conclude that endogenous amino acid loss may be considered constant at usual and high levels of the fibrous mixture under study.
Published: 1995

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