Examinando por Autor "Babusiaux, C."
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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 Survey: Empirical determination of the precision of stellar radial velocities and projected rotation velocities(EDP Sciences, 2015-08) Jackson, R.J.; Jeffries, R.D.; Lewis, J.; Koposov, S.E.; Sacco, G.G.; Randich, S.; Asplund, M.; Binney, J.; Bonifacio, P.; Drew, J.E.; Feltzing, S.; Ferguson, A.M.N.; Micela, G.; Neguerela, I.; Prusti, T.; Rix, H.-W.; Vallenari, A.; Alfaro, E.J.; Allende Prieto, C.; Babusiaux, C.; Bensby, T.; Blomme, R.; Bragaglia, A.; Flaccomio, E.; Francois, P.; Hambly, N.; Irwin, M.; Korn, A.J.; Lanzafame, A.C.; Pancino, E.; Recio-Blanco, A.; Smiljanic, R.; Van Eck, S.; Walton, N.; Bayo, A.; Bergemann, M.; Carraro, G.; Costado, M.T.; Damiani, Edvardsson B.; Franciosini, E.; Frasca, A.; Heiter, U.; Hill, V.; Hourihane, A.; Jofré, P.; Lardo, C.; De Laverny, P.; Lind, K.; Magrini, L.; Marconi, G.; Martayan, C.; Masseron, T.; Monaco, L.; Prisinzano, L.; Sbordone, L.; Sousa, S.G.; Worley, C.C.; Zaggia, S.Context. The Gaia-ESO Survey (GES) is a large public spectroscopic survey at the European Southern Observatory Very Large Telescope. Aims. A key aim is to provide precise radial velocities (RVs) and projected equatorial velocities (v sin i) for representative samples of Galactic stars, which will complement information obtained by the Gaia astrometry satellite. Methods. We present an analysis to empirically quantify the size and distribution of uncertainties in RV and v sin i using spectra from repeated exposures of the same stars. Results. We show that the uncertainties vary as simple scaling functions of signal-to-noise ratio (S/N) and v sin i, that the uncertainties become larger with increasing photospheric temperature, but that the dependence on stellar gravity, metallicity and age is weak. The underlying uncertainty distributions have extended tails that are better represented by Student's t-distributions than by normal distributions. Conclusions. Parametrised results are provided, which enable estimates of the RV precision for almost all GES measurements, and estimates of the v sin i precision for stars in young clusters, as a function of S/N, v sin i and stellar temperature. The precision of individual high S/N GES RV measurements is 0.22-0.26 kms-1, dependent on instrumental configuration. © ESO, 2015.Ítem The Gaia -ESO Survey: Metallicity and kinematic trends in the Milky Way bulge(EDP Sciences, 2014-09) Rojas-Arriagada, A.; Recio-Blanco, A.; Hill, V.; De Laverny, P.; Schultheis, M.; Babusiaux, C.; Zoccali, M.; Minniti, D.; Gonzalez, O.A.; Feltzing, S.; Gilmore, G.; Randich, S.; Vallenari, A.; Alfaro, E.J.; Bensby, T.; Bragaglia, A.; Flaccomio, E.; Lanzafame, A.C.; Pancino, E.; Smiljanic, R.; Bergemann, M.; Costado, M.T.; Damiani, F.; Hourihane, A.; Jofré, P.; Lardo, C.; Magrini, L.; Maiorca, E.; Morbidelli, L.; Sbordone, L.; Worley, C.C.; Zaggia, S.; Wyse, R.Aims. Observational studies of the Milky Way bulge are providing increasing evidence of its complex chemo-dynamical patterns and morphology. Our intent is to use the iDR1 Gaia-ESO Survey (GES) data set to provide new constraints on the metallicity and kinematic trends of the Galactic bulge, exploring the viability of the currently proposed formation scenarios. Methods. We analyzed the stellar parameters and radial velocities of ∼1200 stars in five bulge fields wich are located in the region −10◦ < l < 7 ◦ and −10◦ < b < −4 ◦ . We use VISTA Variables in the Via Lactea (VVV) photometry to verify the internal consistency of the atmospheric parameters recommended by the consortium. As a by-product, we obtained reddening values using a semi-empirical Teff-color calibration. We constructed the metallicity distribution functions and combined them with photometric and radial velocity data to analyze the properties of the stellar populations in the observed fields. Results. From a Gaussian decomposition of the metallicity distribution functions, we unveil a clear bimodality in all fields, with the relative size of components depending of the specific position on the sky. In agreement with some previous studies, we find a mild gradient along the minor axis (−0.05 dex/deg between b = −6 ◦ and b = −10◦ ) that arises from the varying proportion of metal-rich and metal-poor components. The number of metal-rich stars fades in favor of the metal-poor stars with increasing b. The K-magnitude distribution of the metal-rich population splits into two peaks for two of the analyzed fields that intersects the near and far branches of the X-shaped bulge structure. In addition, two lateral fields at (l, b) = (7, −9) and (l, b) = (−10, −8) present contrasting characteristics. In the former, the metallicity distribution is dominated by metal-rich stars, while in the latter it presents a mix of a metal-poor population and and a metal-intermediate one, of nearly equal sizes. Finally, we find systematic differences in the velocity dispersion between the metal-rich and the metal-poor components of each field. Conclusions. The iDR1 bulge data show chemo-dynamical distributions that are consistent with varying proportions of stars belonging to (i) a metal-rich boxy/peanut X-shaped component, with bar-like kinematics; and (ii) a metal-poor more extended rotating structure with a higher velocity dispersion that dominates far from the Galactic plane. These first GES data already allow studying the detailed spatial dependence of the Galactic bulge populations, thanks to the analysis of individual fields with relatively high statistics.Ítem The Gaia-ESO Survey: Low-α element stars in the Galactic bulge(EDP Sciences, 2017-06) Recio-Blanco, A.; Rojas-Arriagada, A.; de Laverny, P.; Mikolaitis, S.; Hill, V.; Zoccali, M.; Fernández-Trincado, J. G.; Robin, A. C.; Babusiaux, C.; Gilmore, G.; Randich, S.; Alfaro, E.; C., Allende Prieto; Bragaglia, A.; Carraro, G.; Jofré, P.; Lardo, C.; Monaco, L.; Morbidelli, L.; Zaggia, S.A.R.B., P.d.L., and V.H. acknowledge financial support form the ANR 14-CE33-014-01. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell'Istruzione, dell'Universit? e della Ricerca (MIUR) in the form of the grant "Premiale VLT 2012". The results presented here benefit from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. M. Zoccali gratefully acknowledge support by the Ministry of Economy, Development, and Tourism's Millenium Science Initiative through grant IC120009, awarded to the Millenium Institute of Astrophysics (MAS), by Fondecyt Regular 1150345 and by the BASAL-CATA Center for Astrophysics and Associated Technologies PFB-06.Ítem The GIRAFFE Inner Bulge Survey (GIBS): II. Metallicity distributions and alpha element abundances at fixed Galactic latitude(EDP Sciences, 2015-12) Gonzalez, O.; Zoccali, M.; Vasquez, S.; Hill, V.; Rejkuba; Valenti, E.; Rojas-Arriagada, A.; Renzini, A.; Babusiaux, C.; Minniti, D.; Brown, T.M.Aims. We investigate metallicity and α-element abundance gradients along a Galactic longitude strip, at latitude b -4°, with the aim of providing observational constraints for the structure and origin of the Milky Way bulge. Methods. High-resolution (R ∼ 22 500) spectra for 400 K giants, in four fields within-4.8° ≤ b ≤-3.4° and-10° ≤ l ≤ +10°, were obtained within the GIRAFFE Inner Bulge Survey (GIBS) project. To this sample we added another ∼400 stars in Baade's Window at (l,b) = (1°,-4°), observed with the identical instrumental configuration: FLAMES GIRAFFE in Medusa mode with HR13 setup. All target stars lie within the red clump of the bulge colour-magnitude diagram, thus minimising contamination from the disc or halo stars. The spectroscopic stellar surface parameters were derived with an automatic method based on the GALA code, while the [Ca/Fe] and [Mg/Fe] abundances as a function of [Fe/H] were derived through a comparison with the synthetic spectra using MOOG. We constructed the metallicity distributions for the entire sample, and for each field individually, in order to investigate the presence of gradients or field-to-field variations in the shape of the distributions. Results. The metallicity distributions in the five fields are consistent with being drawn from a single parent population, indicating the absence of a gradient along the major axis of the Galactic bar. The global metallicity distribution is nicely fitted by two Gaussians. The metal-poor component is rather broad, with a mean at [Fe/H] =-0.31 dex and σ = 0.31 dex. The metal-rich component is narrower, with mean [Fe/H] = + 0.26 and σ = 0.2 dex. The [Mg/Fe] ratio follows a tight trend with [Fe/H], with enhancement with respect to solar in the metal-poor regime similar to the value observed for giant stars in the local thick disc. [Ca/Fe] abundances follow a similar trend, but with a considerably larger scatter than [Mg/Fe]. A decrease in [Mg/Fe] is observed at [Fe/H] =-0.44 dex. This knee is in agreement with our previous bulge study of K-giants along the minor axis, but is 0.1 dex lower in metallicity than the value reported for the microlensed dwarf and subgiant stars in the bulge. We found no variation in α-element abundance distributions between different fields. © 2015 ESO.