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Ítem Gaia Focused Product Release: Radial velocity time series of long-period variables(EDP Sciences, 2023-12) Trabucchi, M.; Mowlavi, N.; Lebzelter, T.; Lecoeur-Taibi, I.; Audard, M.; Eyer, L.; García-Lario, P.; Gavras, P.; Holl, B.; Jevardat De Fombelle, G.; Nienartowicz, K.; Rimoldini, L.; Sartoretti, P.; Blomme, R.; Frémat, Y.; Marchal, O.; Damerdji, Y.; Brown A.G.A.; Guerrier, A.; Panuzzo, P.; Katz, D.; Seabroke, G.M.; Benson, K.; Haigron, R.; Smith, M.; Lobel, A.; Vallenari, A.; Prusti, T.; De Bruijne, J.H.J.; Arenou, F.; Babusiaux, C.; Barbier, A.; Biermann, M.; Creevey, O.L.; Ducourant, C.; Evans, D.W.; Guerra, R.; Hutton, A.; Jordi, C.; Klioner, S.A.; Lammers, U.; Lindegren, L.; Luri, X.; Mignard, F.; Randich, S.; Smiljanic, R.; Tanga, P.; Walton, N.A.; Bailer-Jones, C.A.L.; Bastian, U.; Cropper, M.; Drimmel, R.; Lattanzi, M.G.; Soubiran, C.; Van Leeuwen, F.; Bakker, J.; Castañeda, J.; De Angeli, F.; Fabricius, C.; Fouesneau, M.; Galluccio, L.; Masana, E.; Messineo, R.; Nicolas, C.; Pailler, F.; Riclet, F.; Roux, W.; Sordo, R.; Thévenin, F.; Gracia-Abril G.; Portell, J.; Teyssier, D.; Altmann, M.; Berthier, J; Burgess, P.W.; Busonero, D.; Busso, G.; Cánovas, H.; Carry, B.; Cheek, N.; Clementini, G.; Davidson, M.; De Teodoro, P.; Delchambre, L.; Dell'oro, A.; Fraile Garcia, E.; Garabato, D.; Garralda Torres, N.; Hambly, N.C.; Harrison, D.L.; Hatzidimitriou, D.; Hernández, J.; Hodgkin, S.T.; Jamal, S.; Jordan, S.; Krone-Martins, A.; Lanzafame, A.C.; Löffler, W.; Lorca, A.; Marrese, P.M.; Moitinho, A.; Muinonen, K.; Nuñez Campos, M.; Oreshina-Slezak, I.; Osborne, P.; Pancino, E.; Pauwels, T.; Recio-Blanco, A.; Riello, M.; Robin, A.C.; Roegiers, T.; Sarro, L.M.; Schultheis, M.; Siopis, C.; Siopis, C.; 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.; Anders, F.; 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.; David, M.; De Laverny, P.; De Luise, F.; De March, R.; De Ridder, J.; De Souza, R.; De Torres A.; Del Peloso, E.F.; Delbo, M.; 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.; Fouron, C.; 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.; Leccia, S.; Lecoutre, G.; Liao, S.; Liberato, L.; Licata, E.; Lindstrøm, H.E.P.; Lister, T.A.; Livanou, E.; 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.; Mary, N.; 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.; Munoz, D.; Muraveva, T.; Murphy, C.P.; Musella, I.; Nagy, Z.; Nieto, S.; Noval, L.; Ogden, A.; Ordenovic, C.; Pagani, C.; Pagano, I.; Palaversa, L.; Palicio, P.A.; Pallas-Quintela, L.; Panahi, A.; Panem, C.; 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.; Spoto, F.; 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.; 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-Nunez, L.; Leclerc, N.; Morgenthaler, S.; Robert, G.; Zucker, S.Context. The third Gaia Data Release (DR3) provided photometric time series of more than 2 million long-period variable (LPV) candidates. Anticipating the publication of full radial-velocity data planned with Data Release 4, this Focused Product Release (FPR) provides radial-velocity time series for a selection of LPV candidates with high-quality observations. Aims. We describe the production and content of the Gaia catalog of LPV radial-velocity time series, and the methods used to compute the variability parameters published as part of the Gaia FPR. Methods. Starting from the DR3 catalog of LPV candidates, we applied several filters to construct a sample of sources with high-quality radial-velocity measurements. We modeled their radial-velocity and photometric time series to derive their periods and amplitudes, and further refined the sample by requiring compatibility between the radial-velocity period and at least one of the G, GBP, or GRP photometric periods. Results. The catalog includes radial-velocity time series and variability parameters for 9614 sources in the magnitude range 6 ≲ G/mag ≲ 14, including a flagged top-quality subsample of 6093 stars whose radial-velocity periods are fully compatible with the values derived from the G, GBP, and GRP photometric time series. The radial-velocity time series contain a mean of 24 measurements per source taken unevenly over a duration of about three years. We identify the great majority of the sources (88%) as genuine LPV candidates, with about half of them showing a pulsation period and the other half displaying a long secondary period. The remaining 12% of the catalog consists of candidate ellipsoidal binaries. Quality checks against radial velocities available in the literature show excellent agreement. We provide some illustrative examples and cautionary remarks. Conclusions. The publication of radial-velocity time series for almost ten thousand LPV candidates constitutes, by far, the largest such database available to date in the literature. The availability of simultaneous photometric measurements gives a unique added value to the Gaia catalog. © The Authors 2023.Ítem The Gaia-ESO Public Spectroscopic Survey: Implementation, data products, open cluster survey, science, and legacy(EDP Sciences, 2022-10-01) Randich, S.; Gilmore, G.; Magrini, L.; Sacco, G.G.; Jackson, R.J.; Jeffries, R.D.; Worley, C.C.; Hourihane, A.; Gonneau, A.; Viscasillas Vázquez, C.; Franciosini, E.; Lewis, J.R.; Alfaro, E.J.; Allende Prieto, C.; Bensby, T.; Blomme, R.; Bragaglia, A.; Flaccomio, E.; François, P.; Irwin, M.J.; Koposov, S.E.; Korn, A.J.; Lanzafame, A.C.; Pancino, E.; Recio Blanco, A.; Smiljanic, R.; Van Eck, S.; Zwitter, T.; Asplund, M.; Bonifacio, P.; Feltzing, S.; Binney, J.; Drew, J.; Ferguson, A.M.N.; Micela, G.; Negueruela, I.; Prusti, T.; Rix, H.-W.; Vallenari, A.; Bayo, A.; Bergemann, M.; Biazzo, K.; Carraro, G.; Casey, A.R.; Damiani, F.; Frasca, A.; Heiter, U.; Hill, V.; Jofré, P.; de Laverny, P.; Lind, K.; Marconi, G.; Martayan, C.; Masseron, T.; Monaco, L.; Morbidelli, L.; Prisinzano, L.; Sbordone, L.; Sousa, S.G.; Zaggia, S.; Adibekyan, V.; Bonito, R.; Caffau, E.; Daflon, S.; Feuillet, D.K.; Gebran, M.; González Hernández, J.I.; Guiglion, G.; Herrero, A.; Lobel, A.; Maíz Apellániz, J.; Merle, T.; Mikolaitis, S.; Montes, D.; Morel, T.; Soubiran, C.; Spina, L.; Tabernero, H.M.; Tautvaišiene, G.; Traven, G.; Valentini, M.; Van der Swaelmen, M.; Villanova, S.; Wright, N.J.; Abbas, U.; Aguirre Børsen-Koch, V.; Alves, J.; Balaguer Núnez, L.; Barklem, P.S.; Barrado, D.; Berlanas, S.R.; Binks, A.S.; Bressan, A.; Capuzzo Dolcetta, R.; Casagrande, L.; Casamiquela, L.; Collins, R.S.; D’Orazi, V.; Dantas, M.L.L.; Debattista, V.P.; Delgado Mena, E.; Di Marcantonio, P.; Drazdauskas, A.; Evans, N.W.; Famaey, B.; Franchini, M.; Frémat, Y.; Friel, E.D.; Fu, X.; Geisler, D.; Gerhard, O.; González Solares, E.A.; Grebel, E.K.; Gutiérrez Albarrán, M.L.; Hatzidimitriou, D.; Held, E.V.; Jiménez Esteban, F.; Jönsson, H.; Jordi, C.; Khachaturyants, T.; Kordopatis, G.; Kos, J.; Lagarde, N.; Mahy, L.; Mapelli, M.; Marfil, E.; Martell, S.L.; Messina, S.; Miglio, A.; Minchev, I.; Moitinho, A.; Montalban, J.; Monteiro, M.J.P.F.G.; Morossi, C.; Mowlavi, N.; Mucciarelli, A.; Murphy, D.N.A.; Nardetto, N.; Ortolani, S.; Paletou, F.; Palous, J.; Paunzen, E.; Pickering, J.C.; Quirrenbach, A.; Re Fiorentin, P.; Read, J.I.; Romano, D.; Ryde, N.; Sanna, N.; Santos, W.; Seabroke, G.M.; Spagna, A.; Steinmetz, M.; Stonkuté, E.; Sutorius, E.; Thévenin, F.; Tosi, M.; Tsantaki, M.; Vink, J.S.; Wright, N.; Wyse, R.F.G.; Zoccali, M.; Zorec, J.; Zucker, D.B.; Walton, N.A.Context. In the last 15 years different ground-based spectroscopic surveys have been started (and completed) with the general aim of delivering stellar parameters and elemental abundances for large samples of Galactic stars, complementing Gaia astrometry. Among those surveys, the Gaia-ESO Public Spectroscopic Survey, the only one performed on a 8m class telescope, was designed to target 100 000 stars using FLAMES on the ESO VLT (both Giraffe and UVES spectrographs), covering all the Milky Way populations, with a special focus on open star clusters. Aims. This article provides an overview of the survey implementation (observations, data quality, analysis and its success, data products, and releases), of the open cluster survey, of the science results and potential, and of the survey legacy. A companion article reviews the overall survey motivation, strategy, Giraffe pipeline data reduction, organisation, and workflow. Methods. We made use of the information recorded and archived in the observing blocks; during the observing runs; in a number of relevant documents; in the spectra and master catalogue of spectra; in the parameters delivered by the analysis nodes and the working groups; in the final catalogue; and in the science papers. Based on these sources, we critically analyse and discuss the output and products of the Survey, including science highlights. We also determined the average metallicities of the open clusters observed as science targets and of a sample of clusters whose spectra were retrieved from the ESO archive. Results. The Gaia-ESO Survey has determined homogeneous good-quality radial velocities and stellar parameters for a large fraction of its more than 110 000 unique target stars. Elemental abundances were derived for up to 31 elements for targets observed with UVES. Lithium abundances are delivered for about 1/3 of the sample. The analysis and homogenisation strategies have proven to be successful; several science topics have been addressed by the Gaia-ESO consortium and the community, with many highlight results achieved. Conclusions. The final catalogue will be released through the ESO archive in the first half of 2022, including the complete set of advanced data products. In addition to these results, the Gaia-ESO Survey will leave a very important legacy, for several aspects and for many years to come. © ESO 2022.Ítem The Gaia-ESO Public Spectroscopic Survey: Motivation, implementation, GIRAFFE data processing, analysis, and final data products?(EDP Sciences, 2022-10-01) Gilmore, G.; Randich, S.; Worley, C.C.; Hourihane, A.; Gonneau, A.; Sacco, G.G.; Lewis, J.R.; Magrini, L.; François, P.; Jeffries, R.D.; Koposov, S.E.; Bragaglia, A.; Alfaro, E.J.; Allende Prieto, C.; Blomme, R.; Korn, A.J.; Lanzafame, A.C.; Pancino, E.; Recio Blanco, A.; Smiljanic, R.; Van Eck, S.; Zwitter, T.; Bensby, T.; Flaccomio, E.; Irwin, M.J.; Franciosini, E.; Morbidelli, L.; Damiani, F.; Bonito, R.; Friel, E.D.; Vink, J.S.; Prisinzano, L.; Abbas, U.; Hatzidimitriou, D.; Held, E.V.; Jordi, C.; Paunzen, E.; Spagna, A.; Jackson, R.J.; Maíz Apellániz, J.; Asplund, M.; Bonifacio, P.; Feltzing, S.; Binney, J.; Drew, J.; Ferguson, A.M.N.; Micela, G.; Negueruela, I.; Prusti, T.; Rix, H.-W.; Vallenari, A.; Bergemann, M.; Casey, A.R.; Laverny, P.; Frasca, A.; Hill, V.; Lind, K.; Sbordone, L.; Sousa, S.G.; Adibekyan, V.; Caffau, E.; Daflon, S.; Feuillet, D.K.; Gebran, M.; González Hernández, J.I.; Guiglion, G.; Herrero, A.; Lobel, A.; Merle, T.; Mikolaitis, S.; Montes, D.; Morel, T.; Ruchti, G.; Soubiran, C.; Tabernero, H.M.; Tautvaišiene, G.; Traven, G.; Valentini, M.; Van der Swaelmen, M.; Villanova, S.; Viscasillas Vázquez, C.; Bayo, A.; Biazzo, K.; Carraro, G.; Edvardsson, B.; Heiter, U.; Jofré, P.; Marconi, G.; Martayan, C.; Masseron, T.; Monaco, L.; Walton, N.A.; Zaggia, S.; Aguirre Børsen-Koch, V.; Alves, J.; Balaguer Núnez, L.; Barklem, P.S.; Barrado, D.; Bellazzini, M.; Berlanas, S.R.; Binks, A.S.; Bressan, A.; Capuzzo Dolcetta, R.; Casagrande, L.; Casamiquela, L.; Collins, R.S.; D’Orazi, V.; Dantas, M.L.L.; Debattista, V.P.; Delgado Mena, E.; Marcantonio, P. Di; Drazdauskas, A.; Evans, N.W.; Famaey, B.; Franchini, M.; Frémat, Y.; Fu, X.; Geisler, D.; Gerhard, O.; González Solares, E.A.; Grebel, E.K.; Albarrán Gutiérrez, M.L.; Jiménez Esteban, F.; Jönsson, H.; Khachaturyants, T.; Kordopatis, G.; Kos, J.; Lagarde, N.; Ludwig, H.-G.; Mahy, L.; Mapelli, M.; Marfil, E.; Martell, S.L.; Messina, S.; Miglio, A.; Minchev, I.; Moitinho, A.; Montalban, J.; Monteiro, M.J.P.F.G.; Morossi, C.; Mowlavi, N.; Mucciarelli, A.; Murphy, D.N.A.; Nardetto, N.; Ortolani, S.; Paletou, F.; Palous, J.; Pickering, J.C.; Quirrenbach, A.; Re Fiorentin, P.; Read, J.I.; Romano, D.; Ryde, N.; Sanna, N.; Santos, W.; Seabroke, G.M.; Spina, L.; Steinmetz, M.; Stonkuté, E.; Sutorius, E.; Thévenin, F.; Tosi, M.; Tsantaki, M.; Wright, N.; Wyse, R.F.G.; Zoccali, M.; Zorec, J.; Zucker, D.B.Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia’s astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products. © G. Gilmore et al. 2022.Ítem The Gaia-ESO Survey: A lithium-rotation connection at 5 Myr?(EDP Sciences, 2016-05) Bouvier, J.; Lanzafame, A.C.; Venuti, L.; Klutsch, A.; Jeffries, R.; Frasca, A.; Moraux, E.; Biazzo, K.; Messina, S.; Micela, G.; Randich, S.; Stauffer, J.; Cody, A.M.; Flaccomio, E.; Gilmore, G.; Bayo, A.; Bensby, T.; Bragaglia, A.; Carraro, G.; Casey, A.; Costado, M.T.; Damiani, F.; Delgado Mena, E.; Donati, P.; Franciosini, E.; Hourihane, A.; Koposov, S.; Lardo, C.; Lewis, J.; Magrini, L.; Monaco, L.; Morbidelli, L.; Prisinzano, L.; Sacco, G.; Sbordone, L.; Sousa, S.G.; Vallenari, A.; Worley, C.C.; Zaggia, S.; Zwitter, T.Context. The evolution of lithium abundance in cool dwarfs provides a unique probe of nonstandard processes in stellar evolution. Aims. We investigate the lithium content of young low-mass stars in the 5 Myr old, star forming region NGC 2264 and its relationship with rotation. Methods. We combine lithium equivalent width measurements (EW(Li)) from the Gaia-ESO Survey with the determination of rotational periods from the CSI 2264 survey. We only consider bona fide nonaccreting cluster members to minimize the uncertainties on EW(Li). Results. We report the existence of a relationship between lithium content and rotation in NGC 2264 at an age of 5 Myr. The Li-rotation connec tion is seen over a restricted temperature range (Teff = 3800–4400 K), where fast rotators are Li-rich compared to slow rotators. This correlation is similar to, albeit of lower amplitude than, the Li-rotation connection previously reported for K dwarfs in the 125 Myr old Pleiades cluster. We investigate whether the nonstandard pre-main-sequence models developed so far to explain the Pleiades results, which are based on episodic accre tion, pre-main-sequence, core-envelope decoupling, and/or radius inflation due to enhanced magnetic activity, can account for early development of the Li-rotation connection. While radius inflation appears to be the most promising possibility, each of these models has issues. We therefore also discuss external causes that might operate during the first few Myr of pre-main-sequence evolution, such as planet engulfment and/or steady disk accretion, as possible candidates for the common origin for Li excess and fast rotation in young low-mass pre-main-sequence stars. Conclusions. The emergence of a connection between lithium content and rotation rate at such an early age as 5 Myr suggests a complex link between accretion processes, early angular momentum evolution, and possibly planet formation, which likely impacts early stellar evolution and has yet to be fully deciphered.