Examinando por Autor "Marinoni S."

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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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    On the Use of Field RR Lyrae as Galactic Probes. I. The Oosterhoff Dichotomy Based on Fundamental Variables Partially based on observations collected under ESO programs 297.D-5047 (PI: G. Bono) and 083.B-0281 (PI: D. Romano).
    (Institute of Physics Publishing, 2019-09-10) Fabrizio M.; Bono G.; Braga V.F.; Magurno D.; Marinoni S.; Marrese P.M.; Ferraro I.; Fiorentino G.; Giuffrida G.; Iannicola G.
    We collected a large data set of field RR Lyrae stars (RRLs) by using catalogs already available in the literature and Gaia DR2. We estimated the iron abundances for a subsample of 2382 fundamental RRLs (ΔS method: Ca ii K, Hβ, Hγ, and Hδ lines) for which there are publicly available medium-resolution SDSS-SEGUE spectra. We also included similar estimates available in the literature, ending up with the largest and most homogeneous spectroscopic data set ever collected for RRLs (2903). The metallicity scale was validated by using iron abundances based on high-resolution spectra for a fundamental field RRL (V Ind), for which we collected X-shooter spectra covering the entire pulsation cycle. The peak ([Fe/H] =-1.59 ± 0.01) and the standard deviation (σ = 0.43 dex) of the metallicity distribution agree quite well with similar estimates available in the literature. The current measurements disclose a well-defined metal-rich tail approaching solar iron abundance. The spectroscopic sample plotted in the Bailey diagram (period versus luminosity amplitude) shows a steady variation when moving from the metal-poor ([Fe/H] =-3.0/-2.5) to the metal-rich ([Fe/H] =-0.5/0.0) regime. The smooth transition in the peak of the period distribution as a function of the metallicity strongly indicates that the long-standing problem of the Oosterhoff dichotomy among Galactic globular clusters is the consequence of the lack of metal-intermediate clusters hosting RRLs. We also found that the luminosity amplitude, in contrast with period, does not show a solid correlation with metallicity. This suggests that period-amplitude-metallicity relations should be cautiously treated.
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    The gaia -ESO survey: Calibration strategy
    (EDP Sciences, 2017-02) Pancino E.; Lardo C.; Altavilla G.; Marinoni S.; Ragaini S.; Cocozza G.; Bellazzini M.; Sabbi E.; Zoccali M.; Donati P.; Heiter U.; Koposov S.E.; Blomme R.; Morel T.; Símon-Díaz S.; Lobel A.; Soubiran C.; Montalban J.; Valentini M.; Casey A.R.; Blanco-Cuaresma S.; Jofré P.; Worley C.C.; Magrini L.; Hourihane A.; François P.; Feltzing S.; Gilmore G.; Randich S.; Asplund M.; Bonifacio P.; Drew J.E.; Jeffries R.D.; Micela G.; Vallenari A.; Alfaro E.J.; Allende Prieto C.; Babusiaux C.; Bensby T.; Bragaglia A.; Flaccomio E.; Hambly N.; Korn A.J.; Lanzafame A.C.; Smiljanic R.; Van Eck S.; Walton N.A.; Bayo A.; Carraro G.; Costado M.T.; Damiani F.; Edvardsson B.; Franciosini E.; Frasca A.; Lewis J.; Monaco L.; Morbidelli L.; Prisinzano L.; Sacco G.G.; Sbordone L.
    The Gaia-ESO survey (GES) is now in its fifth and last year of observations and has produced tens of thousands of high-quality spectra of stars in all Milky Way components. This paper presents the strategy behind the selection of astrophysical calibration targets, ensuring that all GES results on radial velocities, atmospheric parameters, and chemical abundance ratios will be both internally consistent and easily comparable with other literature results, especially from other large spectroscopic surveys and from Gaia. The calibration of GES is particularly delicate because of (i) the large space of parameters covered by its targets, ranging from dwarfs to giants, from O to M stars; these targets have a large wide of metallicities and also include fast rotators, emission line objects, and stars affected by veiling; (ii) the variety of observing setups, with different wavelength ranges and resolution; and (iii) the choice of analyzing the data with many different state-of-the-art methods, each stronger in a different region of the parameter space, which ensures a better understanding of systematic uncertainties. An overview of the GES calibration and homogenization strategy is also given, along with some examples of the usage and results of calibrators in GES iDR4, which is the fourth internal GES data release and will form the basis of the next GES public data release. The agreement between GES iDR4 recommended values and reference values for the calibrating objects are very satisfactory. The average offsets and spreads are generally compatible with the GES measurement errors, which in iDR4 data already meet the requirements set by the main GES scientific goals. © ESO, 2017.