Examinando por Autor "Bressan A."

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    Gaia focused product release : asteroid orbital solution: properties and assessmen
    (EDP Sciences, 2023-12) David P.; Mignard F.; Hestroffer D.; Tanga P.; Spoto F.; Berthier J.; Pauwels T.; Roux W.; Barbier A.; Cellino A.; Carry B.; Delbo M.; Dell'oro A.; Fouron C.; Galluccio L.; Klioner S.A.; Mary N.; Muinonen K.; Ordenovic C.; Oreshina-Slezak I.; Panem C.; Petit J.-M.; Portell J.; Brown A.G.A; Thuillot W.; Vallenari A.; Prusti T.; De Bruijne J.H.J.; Arenou F.; Babusiaux C.; Biermann M.; Creevey O.L.; Ducourant C.; Evans D.W.; Eyer L.; Guerra R.; Hutton A.; Jordi C.; Lammers U.; Lindegren L.; Luri X.; Randich S.; Sartoretti P.; Smiljanic R.; Walton N.A.; Bailer-Jones C.A.L.; Bastian U.; Cropper M.; Drimmel R.; Katz D.; Soubiran C.; Van Leeuwen F.; Audard M.; Bakker J.; Blomme R.; Castañeda J.; De Angeli F.; Fabricius C.; Fouesneau M; Frémat Y.; Guerrier A.; Masana E.; Messineo R.; Nicolas C.; Nienartowicz K.; Pailler F.; Panuzzo P.; Riclet F.; Seabroke G.M.; Sordo R.; Thévenin F.; Gracia-Abril G.; Teyssier D.; Altmann M.; Benson K.; Burgess P.W.; Busonero D.; Busso G.; Cánovas H.; Cheek N.; Clementini G.; Damerdji Y.; Davidson M.; De Teodoro P.; Delchambre L.; Fraile Garcia E.; Garabato D.; García-Lario P.; Garralda Torres N.; Gavras P.; Haigron R.; Hambly N.C.; Harrison D.L.; Hatzidimitriou D.; Hernández J.; Hodgkin S.T.; Holl B.; Jamal S.; Jordan S.; Krone-Martins A.; Lanzafame A.C.; Löffler W.; Lorca A.; Marchal O.; Marrese P.M.; Moitinho A.; Nuñez Campos M.; Osborne P.; Pancino E.; Recio-Blanco A.; Riello M.; Rimoldini L.; Robin A.C.; Roegiers T.; Sarro L.M.; Schultheis M.; Siopis C.; Smith M.; Sozzetti A.; Utrilla E.; Van Leeuwen M.; Weingrill K.; Abbas U.; Ábrahám P.; Abreu Aramburu A.; Aerts C.; Altavilla G.; Álvarez M.A.; Alves J.; Anderson R.I.; Antoja T.; Baines D.; Baker S.G.; Balog Z.; Barache C.; Barbato D.; Barros M.; Barstow M.A.; Bartolomé S.; Bashi D.; Bauchet N.; Baudeau N.; Becciani U.; Bedin L.R.; Bellas-Velidis I.; Bellazzini M.; Beordo W.; Berihuete A.; Bernet M.; Bertolotto C.; Bertone S.; Bianchi L.; Binnenfeld A.; Blazere A.; Boch T.; Bombrun A.; Bouquillon S.; Bragaglia A.; Braine J.; Bramante L.; Breedt E.; Bressan A.; Brouillet N.; Brugaletta E.; Bucciarelli B.; Butkevich A.G.; Buzzi R.; Caffau E.; Cancelliere R.; Cannizzo S.; Carballo R.; Carlucci T.; Carnerero M.I.; Carrasco J.M.; Carretero J.; Carton S.; Casamiquela L.; Castellani M.; Castro-Ginard A.; Cesare V.; Charlot P.; Chemin L.; Chiaramida V.; Chiavassa A.; Chornay N.; Collins R.; Contursi G.; Cooper W.J.; Cornez T.; Crosta M.; Crowley C.; Dafonte C.; De Laverny P.; De Luise F.; De March R.; De Souza R.; De Torres A.; Del Peloso E.F.; Delgado A.; Dharmawardena T.E.; Diakite S.; Diener C.; Distefano E.; Dolding C.; Dsilva K.; Durán J.; Enke H.; Esquej P.; Fabre C.; Fabrizio M.; Faigler S.; Fatović M.; Fedorets G.; Fernández-Hernández J.; Fernique P.; Figueras F.; Fournier Y.; Gai M.; Galinier M.; Garcia-Gutierrez A.; García-Torres M.; Garofalo A.; Gerlach E; Geyer R.; Giacobbe P.; Gilmore G.; Girona S.; Giuffrida G.; Gomel R.; Gomez A.; González-Núñez J.; González-Santamaría I.; Gosset E.; Granvik M.; Gregori Barrera V.; Gutiérrez-Sánchez R.; Haywood M.; Helmer A.; Helmi A.; Henares K.; Hidalgo S.L.; Hilger T.; Hobbs D.; Hottier C.; Huckle H.E.; Jabłońska M.; Jansen F.; Jiménez-Arranz Ó.; Juaristi Campillo J.; Khanna S.; Kordopatis G.; Kóspál Á.; Kostrzewa-Rutkowska Z.; Kun M.; Lambert S.; Lanza A.F.; Le Campion J.-F.; Lebreton Y.; Lebzelter T.; Leccia S.; Lecoeur-Taibi I.; Lecoutre G.; Liao S.; Liberato L.; Licata E.; Lindstrøm H.E.P.; Lister T.A.; Livanou E.; Lobel A.; Loup C.; Mahy L.; Mann R.G.; Manteiga M.; Marchant J.M.; Marconi M.; Marín Pina D.; Marinoni S.; Marshall D.J.; Martín Lozano J.; Martín-Fleitas J.M.; Marton G.; Masip A.; Massari D.; Mastrobuono-Battisti A.; Mazeh T.; McMillan P.J.; Meichsner J.; Messina S.; Michalik D.; Millar N.R.; Mints A.; Molina D.; Molinaro R.; Molnár L.; Monari G.; Monguió M.; Montegriffo P.; Montero A.; Mor R.; Mora A.; Morbidelli R.; Morel T.; Morris D.; Mowlavi N.; Munoz D.; Muraveva T.; Murphy C.P.; Musella I.; Nagy Z.; Nieto S.; Noval L.; Ogden A.; Pagani C.; Pagano I.; Palaversa L.; Palicio P.A.; Pallas-Quintela L.; Panahi A.; Payne-Wardenaar S.; Pegoraro L.; Penttilä A.; Pesciullesi P.; Piersimoni A.M.; Pinamonti M.; Pineau F.-X.; Plachy E.; Plum G.; Poggio E.; Pourbaix D.; Prša A.; Pulone L.; Racero E.; Rainer M.; Raiteri C.M.; Ramos P.; Ramos-Lerate M.; Ratajczak M.; Re Fiorentin P.; Regibo S.; Reylé C.; Ripepi V.; Riva A.; Rix H.-W.; Rixon G.; Robichon N.; Robin C.; Romero-Gómez M.; Rowell N.; Royer F.; Ruz Mieres D.; Rybicki K.A.; Sadowski G.; Sáez Núñez A.; Sagristà Sellés A.; Sahlmann J.; Sanchez Gimenez V.; Sanna N.; Santoveña R.; Sarasso M.; Sarrate Riera C.; Sciacca E.; Segovia J.C.; Ségransan D.; Shahaf S.; Siebert A.; Siltala L.; Slezak E.; Smart R.L.; Snaith O.N.; Solano E.; Solitro F.; Souami D.; Souchay J.; Spina L.; Spitoni E.; Squillante L.A.; Steele I.A.; Steidelmüller H.; Surdej J.; Szabados L.; Taris F.; Taylor M.B.; Teixeira R.; Tisanić K.; Tolomei L.; Torra F.; Torralba Elipe G.; Trabucchi M.; Tsantaki M.; Ulla A.; Unger N.; Vanel O.; Vecchiato A.; Vicente D.; Voutsinas S.; Weiler M.; Wyrzykowski Ł.; Zhao H.; Zorec J.; Zwitter T.; Balaguer-Núñez L.; Leclerc N.; Morgenthaler S.; Robert G.; Zucker S.
    Context. We report the exploitation of a sample of Solar System observations based on data from the third Gaia Data Release (Gaia DR3) of nearly 157 000 asteroids. It extends the epoch astrometric solution over the time coverage planned for the Gaia DR4, which is not expected before the end of 2025. This data set covers more than one full orbital period for the vast majority of these asteroids. The orbital solutions are derived from the Gaia data alone over a relatively short arc compared to the observation history of many of these asteroids. Aims. The work aims to produce orbital elements for a large set of asteroids based on 66 months of accurate astrometry provided by Gaia and to assess the accuracy of these orbital solutions with a comparison to the best available orbits derived from independent observations. A second validation is performed with accurate occultation timings. Methods. We processed the raw astrometric measurements of Gaia to obtain astrometric positions of moving objects with 1D sub-mas accuracy at the bright end. For each asteroid that we matched to the data, an orbit fitting was attempted in the form of the best fit of the initial conditions at the median epoch. The force model included Newtonian and relativistic accelerations to derive the observation equations, which were solved with a linear least-squares fit. Results. Orbits are provided in the form of state vectors in the International Celestial Reference Frame for 156 764 asteroids, including near-Earth objects, main-belt asteroids, and Trojans. For the asteroids with the best observations, the (formal) relative uncertainty σa/a is better than 10-10. Results are compared to orbits available from the Jet Propulsion Laboratory and MPC. Their orbits are based on much longer data arcs, but from positions of lower quality. The relative differences in semi-major axes have a mean of 5 × 10-10 and a scatter of 5 × 10-9 © The Authors 2023.
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    The Gaia -ESO Survey: Lithium enrichment histories of the Galactic thick and thin disc
    (EDP Sciences, 2018-02) Fu X.; Romano D.; Bragaglia A.; Mucciarelli A.; Lind K.; Delgado Mena E.; Sousa S.G.; Randich S.; Bressan A.; Sbordone L.; Martell S.; Korn A.J.; Abia C.; Smiljanic R.; Jofré P.; Pancino E.; Tautvaišiene G.; Tang B.; Magrini L.; Lanzafame A.C.; Carraro G.; Bensby T.; Damiani F.; Alfaro E.J.; Flaccomio E.; Morbidelli L.; Zaggia S.; Lardo C.; Monaco L.; Frasca A.; Donati P.; Drazdauskas A.; Chorniy Y.; Bayo A.; Kordopatis G.
    Lithium abundance in most of the warm metal-poor main sequence stars shows a constarnt plateau (A(Li) ~ 2.2 dex) and then the upper envelope of the lithium vs. metallicity distribution increases as we approach solar metallicity. Meteorites, which carry information about the chemical composition of the interstellar medium (ISM) at the solar system formation time, show a lithium abundance A(Li) ~ 3.26 dex. This pattern reflects the Li enrichment history of the ISM during the Galaxy lifetime. After the initial Li production in big bang nucleosynthesis, the sources of the enrichment include asymptotic giant branch (AGB) stars, low-mass red giants, novae, type II supernovae, and Galactic cosmic rays. The total amount of enriched Li is sensitive to the relative contribution of these sources. Thus different Li enrichment histories are expected in the Galactic thick and thin disc. We investigate the main sequence stars observed with UVES in Gaia-ESO Survey iDR4 catalogue and find a Li-anticorrelation independent of [Fe/H], Teff, and log(g). Since in stellar evolution different α enhancements at the same metallicity do not lead to a measurable Li abundance change, the anticorrelation indicates that more Li is produced during the Galactic thin disc phase than during the Galactic thick disc phase. We also find a correlation between the abundance of Li and s-process elements Ba and Y, and they both decrease above the solar metallicity, which can be explained in the framework of the adopted Galactic chemical evolution models. © ESO 2018.