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285 results on '"Masseron, T."'

251. Gaia FGK benchmark stars: new candidates at low metallicities

Author: Hawkins, K, Jofre, P, Heiter, U, Soubiran, C, Blanco-Cuaresma, S, Casagrande, L, Gilmore, G, Lind, K, Magrini, L, Masseron, T, Pancino, E, Randich, S, and Worley, CC
Subjects: 13. Climate action, Astrophysics::Instrumentation and Methods for Astrophysics, standards, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, stars: fundamental parameters, Astrophysics::Galaxy Astrophysics, techniques: spectroscopic
Abstract: We have entered an era of large spectroscopic surveys in which we can measure, through automated pipelines, the atmospheric parameters and chemical abundances for large numbers of stars. Calibrating these survey pipelines using a set of "benchmark stars" in order to evaluate the accuracy and precision of the provided parameters and abundances is of utmost importance. The recent proposed set of Gaia FGK benchmark stars of Heiter et al. (2015) has no recommended stars within the critical metallicity range of $-2.0

252. CARBON STARS WITHIN THE GAIA-ESO SURVEY.

Author: Abia, C., Van Eck, S., Masseron, T., Merle, T., Worley, C. C., and Zwitter, T.
Subjects: N stars, ASTRONOMICAL surveys, NEUTRON capture, BINARY number system, MILKY Way
Abstract: The overwhelming majority of the astronomical objects are oxygen-rich, showing an abundance ratio C/O < 1 (by number). The so-called intrinsic carbon stars (C/O > 1) are formed during the AGB phase evolution of l . 5
Published: 2014
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253. The Gaia-ESO Survey: detection and characterisation of single-line spectroscopic binaries.

Author: Merle, T., Van der Swaelmen, M., Van Eck, S., Jorissen, A., Jackson, R. J., Traven, G., Zwitter, T., Pourbaix, D., Klutsch, A., Sacco, G., Blomme, R., Masseron, T., Gilmore, G., Randich, S., Badenes, C., Bayo, A., Bensby, T., Bergemann, M., Biazzo, K., and Damiani, F.
Subjects: *GIANT stars, *STELLAR populations, *STAR formation, *STELLAR evolution, *SIGNAL-to-noise ratio, *RED giants, *GALACTIC bulges
Abstract: Context. Multiple stellar systems play a fundamental role in the formation and evolution of stellar populations in galaxies. Recent and ongoing large ground-based multi-object spectroscopic surveys significantly increase the sample of spectroscopic binaries (SBs) allowing analyses of their statistical properties. Aims. We investigate the repeated spectral observations of the Gaia-ESO Survey internal data release 5 (GES iDR5) to identify and characterise SBs with one visible component (SB1s) in fields covering mainly the discs, the bulge, the CoRot fields, and some stellar clusters and associations. Methods. A statistical X²-test is performed on spectra of the iDR5 subsample of approximately 43 500 stars characterised by at least two observations and a signal-to-noise ratio larger than three. In the GES iDR5, most stars have four observations generally split into two epochs. A careful estimation of the radial velocity (RV) uncertainties is performed. Our sample of RV variables is cleaned from contamination by pulsation- and/or convection-induced variables using Gaia DR2 parallaxes and photometry. Monte-Carlo simulations using the SB9 catalogue of spectroscopic orbits allow to estimate our detection efficiency and to correct the SB1 rate to evaluate the GES SB1 binary fraction and its relation to effective temperature and metallicity. Results. We find 641 (resp., 803) FGK SB1 candidates at the 5σ (resp., 3σ) level. The maximum RV differences range from 2.2 km s-1 at the 5σ confidence level (1.6 km s-1 at 3σ) to 133 km s-1 (in both cases). Among them a quarter of the primaries are giant stars and can be located as far as 10 kpc. The orbital-period distribution is estimated from the RV standard-deviation distribution and reveals that the detected SB1s probe binaries with log P[d] / 4. We show that SB1s with dwarf primaries tend to have shorter orbital periods than SB1s with giant primaries. This is consistent with binary interactions removing shorter period systems as the primary ascends the red giant branch. For two systems, tentative orbital solutions with periods of 4 and 6 d are provided. After correcting for detection efficiency, selection biases, and the present-day mass function, we estimate the global GES SB1 fraction to be in the range 7-14% with a typical uncertainty of 4%. A small increase of the SB1 frequency is observed from K- towards F-type stars, in agreement with previous studies. The GES SB1 frequency decreases with metallicity at a rate of (-9 ± 3)% dex-1 in the metallicity range -2.7 ≤ [Fe=H] ≤ +0.6. This anticorrelation is obtained with a confidence level higher than 93% on a homogeneous sample covering spectral types FGK and a large range of metallicities. When the present-day mass function is accounted for, this rate turns to (-4 ± 2)% dex-1 with a confidence level higher than 88%. In addition we provide the variation of the SB1 fraction with metallicity separately for F, G, and K spectral types, as well as for dwarf and giant primaries. [ABSTRACT FROM AUTHOR]
Published: 2020
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254. Gaia -ESO Survey: Analysis of pre-main sequence stellar spectra

Author: Antonio Frasca, G. G. Sacco, Ignacio Negueruela, Hugo M. Tabernero, Andreas Korn, Martin Asplund, C. Babusiaux, Loredana Prisinzano, Francesco Damiani, Nigel Hambly, M. T. Costado, G. Carraro, Gerry Gilmore, Giuseppina Micela, Emilio J. Alfaro, Piercarlo Bonifacio, Annette M. N. Ferguson, A. Hourihane, Maria Bergemann, N. A. Walton, E. Brugaletta, Manuel Meyer, John D. Lewis, H. W. Rix, Michael G. Irwin, Vardan Adibekyan, R. Blomme, P. Francois, R. D. Jeffries, A. C. Lanzafame, Sergey E. Koposov, Lorenzo Spina, James Binney, Thomas Masseron, L. Morbidelli, D. Montes, K. Biazzo, S. G. Sousa, Antonella Vallenari, Rodolfo Smiljanic, J. M. Alcalá, Thomas Bensby, C. Allende Prieto, Sergio Messina, Luca Sbordone, Amelia Bayo, A. Bragaglia, Simone Zaggia, C. C. Worley, Janet E. Drew, Ettore Flaccomio, S. Van Eck, Paula Jofre, Laura Magrini, Bengt Edvardsson, Gianni Marconi, J. I. González Hernández, Michiel Cottaar, Rosaria Bonito, Lorenzo Monaco, Ulrike Heiter, J. F. Gameiro, Carmela Lardo, Sofia Feltzing, E. Franciosini, T. Prusti, R. J. Jackson, Vanessa Hill, Sofia Randich, Karin Lind, Ch. Martayan, E. Delgado Mena, A. Klutsch, INAF - Osservatorio Astrofisico di Catania (OACT), Istituto Nazionale di Astrofisica (INAF), University of Turin, INAF - Osservatorio Astrofisico di Arcetri (OAA), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), Keele University [Keele], Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), 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), School of Physics, Astronomy and Mathematics [Hatfield], University of Hertfordshire [Hatfield] (UH), Lund Observatory, Lund University [Lund], INAF - Osservatorio Astronomico di Palermo (OAPa), Departamento de Fisica, Ingenieria de Sistemas y Teoria de la Señal [Alicante] (DFESTS), Universidad de Alicante, Agence Spatiale Européenne (ESA), European Space Agency (ESA), Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), 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), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Royal Observatory of Belgium [Brussels] (ROB), INAF - Osservatorio Astronomico di Bologna (OABO), Institut d'Astronomie et d'Astrophysique, Université libre de Bruxelles (ULB), Uppsala University, 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), Ecole Polytechnique Fédérale de Lausanne (EPFL), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), 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), Lanzafame A.C., Frasca A., Damiani F., Franciosini E., Cottaar M., Sousa S.G., Tabernero H.M., Klutsch A., Spina L., Biazzo K., Prisinzano L., Sacco G.G., Randich S., Brugaletta E., Delgado Mena E., Adibekyan V., Montes D., Bonito R., Gameiro J.F., Alcala J.M., Gonzalez Hernandez J.I., Jeffries R., Messina S., Meyer M., Gilmore G., Asplund M., Binney J., Bonifacio P., Drew J.E., Feltzing S., Ferguson A.M.N., Micela G., Negueruela 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., Koposov S.E., Korn A.J., Smiljanic R., Van Eck S., Walton N., Bayo A., Bergemann M., Carraro G., Costado M.T., Edvardsson B., Heiter U., Hill V., Hourihane A., Jackson R.J., Jofre P., Lardo C., Lewis J., Lind K., Magrini L., Marconi G., Martayan C., Masseron T., Monaco L., Morbidelli L., Sbordone L., Worley C.C., Zaggia S., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Astrofísica Estelar (AE), Lanzafame, A., Frasca, A., Damiani, F., Franciosini, E., Cottaar, M., Sousa, S., Tabernero, H., Klutsch, A., Spina, L., Biazzo, K., Prisinzano, L., Sacco, G., Randich, S., Brugaletta, E., Delgado Mena, E., Adibekyan, V., Montes, D., Bonito, R., Gameiro, J., Alcalá, J., González Hernández, J., Jeffries, R., Messina, S., Meyer, M., Gilmore, G., Asplund, M., Binney, J., Bonifacio, P., Drew, J., Feltzing, S., Ferguson, A., Micela, G., Negueruela, I., Prusti, T., Rix, H., Vallenari, A., Alfaro, E., Allende Prieto, C., Babusiaux, C., Bensby, T., Blomme, R., Bragaglia, A., Flaccomio, E., Francois, P., Hambly, N., Irwin, M., Koposov, S., Korn, A., Smiljanic, R., Van Eck, S., Walton, N., Bayo, A., Bergemann, M., Carraro, G., Costado, M., Edvardsson, B., Heiter, U., Hill, V., Hourihane, A., Jackson, R., Jofré, P., Lardo, C., Lewis, J., Lind, K., Magrini, L., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Morbidelli, L., Sbordone, L., Worley, C., and Zaggia, S.
Subjects: Accuracy and precision, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, stars: pre-main sequence, Surveys, fundamental parameters [Stars], Astronomical spectroscopy, surveys, Angular diameter, pre-main sequence [Stars], Astrophysics::Solar and Stellar Astrophysics, Survey, data analysis [Methods], education, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astronomía y Astrofísica, Physics, education.field_of_study, general [Open clusters and associations], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Stars: fundamental parameter, Astronomy and Astrophysic, Effective temperature, open clusters and associations: general, Surface gravity, methods: data analysis, Accretion (astrophysics), Stars, Astrophysics - Solar and Stellar Astrophysics, Methods: data analysis, Open clusters and associations: general, Stars: fundamental parameters, Stars: pre-main sequence, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, stars: fundamental parameters, Methods: data analysi
Abstract: This paper describes the analysis of UVES and GIRAFFE spectra acquired by the Gaia-ESO Public Spectroscopic Survey in the fields of young clusters whose population includes pre-main sequence (PMS) stars. Both methods that have been extensively used in the past and new ones developed in the contest of the Gaia-ESO survey enterprise are available and used. The internal precision of these quantities is estimated by inter-comparing the results obtained by such different methods, while the accuracy is estimated by comparison with independent external data, like effective temperature and surface gravity derived from angular diameter measurements, on a sample of benchmarks stars. Specific strategies are implemented to deal with fast rotation, accretion signatures, chromospheric activity, and veiling. The analysis carried out on spectra acquired in young clusters' fields during the first 18 months of observations, up to June 2013, is presented in preparation of the first release of advanced data products. Stellar parameters obtained with the higher resolution and larger wavelength coverage from UVES are reproduced with comparable accuracy and precision using the smaller wavelength range and lower resolution of the GIRAFFE setup adopted for young stars, which allows us to provide with confidence stellar parameters for the much larger GIRAFFE sample. Precisions are estimated to be $\approx$ 120 K r.m.s. in Teff, $\approx$0.3 dex r.m.s. in logg, and $\approx$0.15 dex r.m.s. in [Fe/H], for both the UVES and GIRAFFE setups., 22 pages, 18 figures, accepted for publication on A&A
Published: 2015
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255. The Gaia-ESO Survey: Chromospheric emission, accretion properties, and rotation in gamma Velorum and Chamaeleon

Author: A. Hourihane, Geert Barentsen, E. Brugaletta, Beate Stelzer, Gerry Gilmore, Paula Jofre, E. Franciosini, Thomas Masseron, G. Pace, K. Biazzo, L. Morbidelli, Luca Pasquini, Emilio J. Alfaro, A. C. Lanzafame, Lorenzo Spina, R. Bonito, Carmela Lardo, Sofia Randich, A. Bragaglia, M. T. Costado, A. Klutsch, C. C. Worley, Enrico Maiorca, S. G. Sousa, Antonio Frasca, J. F. Gameiro, G. G. Sacco, Loredana Prisinzano, Giuseppina Micela, J. M. Alcalá, V. Hill, D. Montes, Javier Lopez-Santiago, Amelia Bayo, R. D. Jeffries, Ettore Flaccomio, ITA, Frasca A., Biazzo K., Lanzafame A.C., Alcala J.M., Brugaletta E., Klutsch A., Stelzer B., Sacco G.G., Spina L., Jeffries R.D., Montes D., Alfaro E.J., Barentsen G., Bonito R., Gameiro J.F., Lopez-Santiago J., Pace G., Pasquini L., Prisinzano L., Sousa S.G., Gilmore G., Randich S., Micela G., Bragaglia A., Flaccomio E., Bayo A., Costado M.T., Franciosini E., Hill V., Hourihane A., Jofre P., Lardo C., Maiorca E., Masseron T., Morbidelli L., Worley C.C., Frasca, A., Biazzo, K., Lanzafame, A., Alcalá, J., Brugaletta, E., Klutsch, A., Stelzer, B., Sacco, G., Spina, L., Jeffries, R., Montes, D., Alfaro, E., Barentsen, G., Bonito, R., Gameiro, J., López-Santiago, J., Pace, G., Pasquini, L., Prisinzano, L., Sousa, S., Gilmore, G., Randich, S., Micela, G., Bragaglia, A., Flaccomio, E., Bayo, A., Costado, M., Franciosini, E., Hill, V., Hourihane, A., Jofré, P., Lardo, C., Maiorca, E., Masseron, T., Morbidelli, L., and Worley, C.
Subjects: Astrofísica, stars: chromospheres, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Rotation, Stars: chromosphere, Open clusters and associations: individual:γVelorum, stars: low-mass, Stars: low-ma, Astrophysics::Solar and Stellar Astrophysics, Open clusters and associations: individual: Chamaeleon I, open clusters and associations: individual: γ Velorum, QC, Astrophysics::Galaxy Astrophysics, QB, Line (formation), Physics, Accretion (meteorology), Diagram, Stars: rotation, Spectral density, Astronomy and Astrophysics, Astronomy and Astrophysic, Stars, Distribution (mathematics), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Chamaeleon, Stars: pre-main sequence, Astrophysics::Earth and Planetary Astrophysics, Stars: chromospheres, Stars: low-mass
Abstract: Aims: One of the goals of the Gaia-ESO Survey (GES), which is conducted with FLAMES at the VLT, is the census and the characterization of the low-mass members of very young clusters and associations. We conduct a comparative study of the main properties of the sources belonging to γ Velorum (γ Vel) and Chamaeleon I (Cha I) young associations, focusing on their rotation, chromospheric radiative losses, and accretion. Methods: We used the fundamental parameters (effective temperature, surface gravity, lithium abundance, and radial velocity) delivered by the GES consortium in the first internal data release to select the members of γ Vel and Cha I among the UVES and GIRAFFE spectroscopic observations. A total of 140 γ Vel members and 74 Cha I members were studied. The procedure adopted by the GES to derive stellar fundamental parameters also provided measures of the projected rotational velocity (vsini). We calculated stellar luminosities through spectral energy distributions, while stellar masses were derived by comparison with evolutionary tracks. The spectral subtraction of low-activity and slowly rotating templates, which are rotationally broadened to match the vsini of the targets, enabled us to measure the equivalent widths (EWs) and the fluxes in the Hα and Hβ lines. The Hα line was also used for identifying accreting objects, on the basis of its EW and the width at the 10% of the line peak (10%W), and for evaluating the mass accretion rate (Ṁacc). Results: The distribution of vsini for the members of γ Vel displays a peak at about 10 km s-1 with a tail toward faster rotators. There is also some indication of a different vsini distribution for the members of its two kinematical populations. Most of these stars have Hα fluxes corresponding to a saturated activity regime. We find a similar distribution, but with a narrower peak, for Cha I. Only a handful of stars in γ Vel display signatures of accretion, while many more accretors were detected in the younger Cha I, where the highest Hα fluxes are mostly due to accretion, rather than to chromospheric activity. Accreting and active stars occupy two different regions in a Teff-flux diagram and we propose a criterion for distinguishing them. We derive Ṁacc in the ranges 10-11-10-9 M☉ yr-1 and 10-10-10-7 M☉ yr-1 for γ Vel and Cha I accretors, respectively. We find less scatter in the Ṁacc - M⋆ relation derived through the Hα EWs, when compared to the Hα10%W diagnostics, in agreement with other authors. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002.Tables 5, 6, and Appendix A are available in electronic form at http://www.aanda.orgTables 2-4 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/575/A4
Published: 2015

256. The Gaia-ESO survey: placing constraints on the origin of r-process elements

Author: M. Van der Swaelmen, C. Viscasillas Vázquez, G. Cescutti, L. Magrini, S. Cristallo, D. Vescovi, S. Randich, G. Tautvaišienė, V. Bagdonas, T. Bensby, M. Bergemann, A. Bragaglia, A. Drazdauskas, F. Jiménez-Esteban, G. Guiglion, A. Korn, T. Masseron, R. Minkeviiūtė, R. Smiljanic, L. Spina, E. Stonkutė, S. Zaggia, Van der Swaelmen, M., Viscasillas Vázquez, C., Cescutti, G., Magrini, L., Cristallo, S., Vescovi, D., Randich, S., Tautvaišienė, G., Bagdonas, V., Bensby, T., Bergemann, M., Bragaglia, A., Drazdauskas, A., Jiménez-Esteban, F., Guiglion, G., Korn, A., Masseron, T., Minkevičiūtė, R., Smiljanic, R., Spina, L., Stonkutė, E., and Zaggia, S.
Subjects: CLUSTERS TRUMPLER 20, FOS: Physical sciences, NEUTRON-STAR MERGERS, Astrophysics, Astrophysics of Galaxies, Astrophysics Solar and Stellar Astrophysics, HEAVY-ELEMENTS, STELLAR POPULATIONS, Astrophysic, PROCESS NUCLEOSYNTHESIS, Astronomi, astrofysik och kosmologi, Astronomy, Astrophysics and Cosmology, STOCHASTIC CHEMICAL EVOLUTION, Astrophysics of Galaxie, GIANT BRANCH STARS, Solar and Stellar Astrophysics (astro-ph.SR), abundances [Galaxy], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, abundances [stars], ALPHA-RICH STARS, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), MILKY-WAY, CAPTURE ELEMENTS, general [open clusters and associations], disk [Galaxy]
Abstract: A renewed interest about the origin of \emph{r}-process elements has been stimulated by the multi-messenger observation of the gravitational event GW170817, with the detection of both gravitational waves and electromagnetic waves corresponding to the merger of two neutron stars. Such phenomenon has been proposed as one of the main sources of the \emph{r}-process. However, the origin of the \emph{r}-process elements at different metallicities is still under debate. We aim at investigating the origin of the \emph{r}-process elements in the Galactic thin disc population. From the sixth internal data release of the \emph{Gaia}-ESO we have collected a large sample of Milky Way thin- and thick-disc stars for which abundances of Eu, O, and Mg are available. The sample consists of members of 62 open clusters, located at a Galactocentric radius from $\sim 5$ kpc to $\sim 20$ kpc in the disc, in the metallicity range $[-0.5, 0.4]$ and covering an age interval from 0.1 to 7 Gy, and about 1300 Milky Way disc field stars in the metallicity range $[-1.5, 0.5]$. We compare the observations with the results of a chemical evolution model, in which we varied the nucleosynthesis sources for the three considered elements. Our main result is that Eu in the thin disc is predominantly produced by sources with short lifetimes, such as magneto-rotationally driven SNe. There is no strong evidence for additional sources at delayed times. Our findings do not imply that there cannot be a contribution from mergers of neutron stars in other environments, as in the halo or in dwarf spheroidal galaxies, but such a contribution is not needed to explain Eu abundances at thin disc metallicities., 20 pages, accepted for publication in A&A
Published: 2023
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257. The Gaia-ESO survey: Metallicity of the chamaeleon i star-forming region

Author: Antonio Frasca, A. Hourihane, Gerard Gilmore, M. T. Costado, Elisa Delgado-Mena, Angela Bragaglia, V. Adibekyan, A. C. Lanzafame, Rosaria Bonito, Lorenzo Spina, Ettore Flaccomio, Paula Jofre, D. Montes, Maria Bergemann, Carmela Lardo, Laura Magrini, Franco Palla, K. Biazzo, Alejandra Recio-Blanco, S. G. Sousa, Rodolfo Smiljanic, Thomas Masseron, Loredana Prisinzano, Antonella Vallenari, G. G. Sacco, L. Morbidelli, P. de Laverny, Clare Worley, Vanessa Hill, Grazina Tautvaisiene, Hugo M. Tabernero, Andreas Korn, Francesco Damiani, Elena Pancino, Thomas Bensby, Sofia Randich, J. I. González Hernández, Emilio J. Alfaro, E. Franciosini, R. D. Jeffries, Spina L., Randich S., Palla F., Biazzo K., Sacco G.G., Alfaro E.J., Franciosini E., Magrini L., Morbidelli L., Frasca A., Adibekyan V., Delgado-Mena E., Sousa S.G., Gonzalez Hernandez J.I., Montes D., Tabernero H., Tautvaisiene G., Bonito R., Lanzafame A.C., Gilmore G., Jeffries R.D., Vallenari A., Bensby T., Bragaglia A., Flaccomio E., Korn A.J., Pancino E., Recio-Blanco A., Smiljanic R., Bergemann M., Costado M.T., Damiani F., Hill V., Hourihane A., Jofre P., De Laverny P., Lardo C., Masseron T., Prisinzano L., Worley C.C., Spina, L., Randich, S., Palla, F., Biazzo, K., Sacco, G. G., Alfaro, E. J., Franciosini, E., Magrini, L., Morbidelli, L., Frasca, A., Adibekyan, V., Delgado-Mena, E., Sousa, S. G., González Hernández, J. I., Montes, D., Tabernero, H., Tautvaišienė, G., Bonito, R., Lanzafame, A. C., Gilmore, G., Jeffries, R. D., Vallenari, A., Bensby, T., Bragaglia, A., Flaccomio, E., Korn, A. J., Pancino, E., Recio-Blanco, A., Smiljanic, R., Bergemann, M., Costado, M. T., Damiani, F., Hill, V., Hourihane, A., Jofré, P., de Laverny, P., Lardo, C., Masseron, T., Prisinzano, L., and Worley, C. C.
Subjects: Astrofísica, Stars: abundance, Metallicity, FOS: Physical sciences, Techniques: spectroscopic, Context (language use), Astrophysics, Open clusters and associations: individual: Chamaeleon I, Solar and Stellar Astrophysics (astro-ph.SR), Line (formation), Physics, 85A04, open clusters and associations: individual: Chamaeleon I, stars: pre-main sequence, stars: abundances, techniques: spectroscopic, Stars: abundances, Astronomy and Astrophysics, Surface gravity, Astronomía, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Chamaeleon, Stars: pre-main sequence, individual: Chamaeleon I, stars: pre-main sequence, stars: abundances, techniques: spectroscopic [open clusters and associations], Equivalent width, Open cluster
Abstract: Context. Recent metallicity determinations in young open clusters and star-forming regions suggest that the latter may be characterized by a slightly lower metallicity than the Sun and older clusters in the solar vicinity. However, these results are based on small statistics and inhomogeneous analyses. The Gaia-ESO Survey is observing and homogeneously analyzing large samples of stars in several young clusters and star-forming regions, hence allowing us to further investigate this issue. Aims. We present a new metallicity determination of the Chamaeleon I star-forming region, based on the products distributed in the first internal release of the Gaia-ESO Survey. Methods. 48 candidate members of Chamaeleon I have been observed with the high-resolution spectrograph UVES. We use the surface gravity, lithium line equivalent width and position in the Hertzsprung-Russell diagram to confirm the cluster members and we use the iron abundance to derive the mean metallicity of the region. Results. Out of the 48 targets, we confirm 15 high probability members. Considering the metallicity measurements for 9 of them, we find that the iron abundance of Chamaeleon I is slightly subsolar with a mean value [Fe/H]=-0.08+/-0.04 dex. This result is in agreement with the metallicity determination of other nearby star-forming regions and suggests that the chemical pattern of the youngest stars in the solar neighborhood is indeed more metal-poor than the Sun. We argue that this evidence may be related to the chemical distribution of the Gould Belt that contains most of the nearby star-forming regions and young clusters., Comment: 13 pages, 11 figures, 3 tables, Accepted for publication in Astronomy & Astrophysics
Published: 2014

258. Atomic data for the Gaia-ESO Survey

Author: Martin Asplund, Nils Ryde, Paul S. Barklem, Andrew R. Casey, Bengt Edvardsson, Henrik Jönsson, A. C. Lanzafame, Andreas Korn, Šarūnas Mikolaitis, L. Morbidelli, Gerard Gilmore, Maria Bergemann, E. Pancino, Lorenzo Monaco, Ulrike Heiter, Francesco Damiani, P. de Laverny, Clare Worley, Laura Magrini, Carmela Lardo, Paula Jofre, Sofia Feltzing, Simone Zaggia, Thomas Bensby, A. Bayo Aran, Rodolfo Smiljanic, Sofia Randich, Karin Lind, Juliet C. Pickering, Thomas Masseron, Worley, Clare [0000-0001-9310-2898], Gilmore, Gerard [0000-0003-4632-0213], Apollo - University of Cambridge Repository, Heiter U., Lind K., Bergemann M., Asplund M., Mikolaitis S., Barklem P.S., Masseron T., De Laverny P., Magrini L., Edvardsson B., Jonsson H., Pickering J.C., Ryde N., Bayo Aran A., Bensby T., Casey A.R., Feltzing S., Jofre P., Korn A.J., Pancino E., Damiani F., Lanzafame A., Lardo C., Monaco L., Morbidelli L., Smiljanic R., Worley C., Zaggia S., Randich S., and Gilmore G.F.
Subjects: 010504 meteorology & atmospheric sciences, stars: abundances, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, Astronomical spectroscopy, Spectral line, Astronomi, astrofysik och kosmologi, surveys, 0103 physical sciences, Arcturus, Radiative transfer, atomic data, Astronomy, Astrophysics and Cosmology, 010303 astronomy & astrophysics, Hyperfine structure, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Line (formation), Physics, stars: late-type, Astronomy and Astrophysics, abundances [stars], Stars: Abundance, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, late-type [stars], Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We describe the atomic and molecular data that were used for the abundance analyses of FGK-type stars carried out within the Gaia-ESO Survey. We present an unprecedented effort to create a homogeneous line list, which was used by several abundance analysis groups to calculate synthetic spectra and equivalent widths. The atomic data are accompanied by quality indicators and detailed references to the sources. The atomic and molecular data are made publicly available in electronic form. In general experimental transition probabilities were preferred but theoretical values were also used. Astrophysical gf-values were avoided due to the model-dependence of such a procedure. For elements whose lines are significantly affected by hyperfine structure or isotopic splitting a concerted effort has been made to collate the necessary data for the individual line components. We also performed a detailed investigation of available data for line broadening due to collisions with neutral hydrogen atoms. Synthetic spectra calculated for the Sun and Arcturus were used to assess the blending properties of the lines. Among a subset of over 1300 lines of 35 elements in the wavelength ranges from 475 nm to 685 nm and from 850 nm to 895 nm we identified about 200 lines of 24 species which have accurate gf-values and are free of blends in the spectra of the Sun and Arcturus. For the broadening due to collisions with neutral hydrogen we recommend data based on Anstee-Barklem-O'Mara theory, where available, and to avoid lines of neutral species otherwise. Theoretical broadening data by R.L. Kurucz should be used for Sc II, Ti II, and Y II lines. For ionised rare-earth species the Uns\"old approximation with an enhancement factor of 1.5 for the line width can be used. Desirable improvements in atomic data were identified for a number of species, including Al I, S I, Cr II, Na I, Si I, Ca II, and Ni I., Comment: Accepted for publication in section 12. Atomic, molecular, and nuclear data of Astronomy and Astrophysics; main part 25 pages, 8 tables, 5 figures; appendices 53 pages, 23 tables, 29 figures
Published: 2021
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259. The 16th Data Release of the Sloan Digital Sky Surveys : First Release from the APOGEE-2 Southern Survey and Full Release of eBOSS Spectra

Author: Romina Ahumada, Carlos Allende Prieto, Andrés Almeida, Friedrich Anders, Scott F. Anderson, Brett H. Andrews, Borja Anguiano, Riccardo Arcodia, Eric Armengaud, Marie Aubert, Santiago Avila, Vladimir Avila-Reese, Carles Badenes, Christophe Balland, Kat Barger, Jorge K. Barrera-Ballesteros, Sarbani Basu, Julian Bautista, Rachael L. Beaton, Timothy C. Beers, B. Izamar T. Benavides, Chad F. Bender, Mariangela Bernardi, Matthew Bershady, Florian Beutler, Christian Moni Bidin, Jonathan Bird, Dmitry Bizyaev, Guillermo A. Blanc, Michael R. Blanton, Médéric Boquien, Jura Borissova, Jo Bovy, W. N. Brandt, Jonathan Brinkmann, Joel R. Brownstein, Kevin Bundy, Martin Bureau, Adam Burgasser, Etienne Burtin, Mariana Cano-Díaz, Raffaella Capasso, Michele Cappellari, Ricardo Carrera, Solène Chabanier, William Chaplin, Michael Chapman, Brian Cherinka, Cristina Chiappini, Peter Doohyun Choi, S. Drew Chojnowski, Haeun Chung, Nicolas Clerc, Damien Coffey, Julia M. Comerford, Johan Comparat, Luiz da Costa, Marie-Claude Cousinou, Kevin Covey, Jeffrey D. Crane, Katia Cunha, Gabriele da Silva Ilha, Yu Sophia Dai, Sanna B. Damsted, Jeremy Darling, James W. Davidson, Roger Davies, Kyle Dawson, Nikhil De, Axel de la Macorra, Nathan De Lee, Anna Bárbara de Andrade Queiroz, Alice Deconto Machado, Sylvain de la Torre, Flavia Dell’Agli, Hélion du Mas des Bourboux, Aleksandar M. Diamond-Stanic, Sean Dillon, John Donor, Niv Drory, Chris Duckworth, Tom Dwelly, Garrett Ebelke, Sarah Eftekharzadeh, Arthur Davis Eigenbrot, Yvonne P. Elsworth, Mike Eracleous, Ghazaleh Erfanianfar, Stephanie Escoffier, Xiaohui Fan, Emily Farr, José G. Fernández-Trincado, Diane Feuillet, Alexis Finoguenov, Patricia Fofie, Amelia Fraser-McKelvie, Peter M. Frinchaboy, Sebastien Fromenteau, Hai Fu, Lluís Galbany, Rafael A. Garcia, D. A. García-Hernández, Luis Alberto Garma Oehmichen, Junqiang Ge, Marcio Antonio Geimba Maia, Doug Geisler, Joseph Gelfand, Julian Goddy, Violeta Gonzalez-Perez, Kathleen Grabowski, Paul Green, Catherine J. Grier, Hong Guo, Julien Guy, Paul Harding, Sten Hasselquist, Adam James Hawken, Christian R. Hayes, Fred Hearty, S. Hekker, David W. Hogg, Jon A. Holtzman, Danny Horta, Jiamin Hou, Bau-Ching Hsieh, Daniel Huber, Jason A. S. Hunt, J. Ider Chitham, Julie Imig, Mariana Jaber, Camilo Eduardo Jimenez Angel, Jennifer A. Johnson, Amy M. Jones, Henrik Jönsson, Eric Jullo, Yerim Kim, Karen Kinemuchi, Charles C. Kirkpatrick IV, George W. Kite, Mark Klaene, Jean-Paul Kneib, Juna A. Kollmeier, Hui Kong, Marina Kounkel, Dhanesh Krishnarao, Ivan Lacerna, Ting-Wen Lan, Richard R. Lane, David R. Law, Jean-Marc Le Goff, Henry W. Leung, Hannah Lewis, Cheng Li, Jianhui Lian, Lihwai Lin, Dan Long, Penélope Longa-Peña, Britt Lundgren, Brad W. Lyke, J. Ted Mackereth, Chelsea L. MacLeod, Steven R. 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(INC)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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), Ahumada R., Prieto C.A., Almeida A., Anders F., Anderson S.F., Andrews B.H., Anguiano B., Arcodia R., Armengaud E., Aubert M., Avila S., Avila-Reese V., Badenes C., Balland C., Barger K., Barrera-Ballesteros J.K., Basu S., Bautista J., Beaton R.L., Beers T.C., Benavides B.I.T., Bender C.F., Bernardi M., Bershady M., Beutler F., Bidin C.M., Bird J., Bizyaev D., Blanc G.A., Blanton M.R., Boquien M., Borissova J., Bovy J., Brandt W.N., Brinkmann J., Brownstein J.R., Bundy K., Bureau M., Burgasser A., Burtin E., Cano-Diaz M., Capasso R., Cappellari M., Carrera R., Chabanier S., Chaplin W., Chapman M., Cherinka B., Chiappini C., Doohyun Choi P., Chojnowski S.D., Chung H., Clerc N., Coffey D., Comerford J.M., Comparat J., Da Costa L., Cousinou M.-C., Covey K., Crane J.D., Cunha K., Ilha G.D.S., Dai Y.S., Damsted S.B., Darling J., Davidson J.W., Davies R., Dawson K., De N., De La Macorra A., De Lee N., Queiroz A.B.D.A., Deconto Machado A., De La Torre S., Dell'Agli F., Du Mas Des Bourboux H., Diamond-Stanic A.M., Dillon S., Donor J., Drory N., Duckworth C., Dwelly T., Ebelke G., Eftekharzadeh S., Davis Eigenbrot A., Elsworth Y.P., Eracleous M., Erfanianfar G., Escoffier S., Fan X., Farr E., Fernandez-Trincado J.G., Feuillet D., Finoguenov A., Fofie P., Fraser-Mckelvie A., Frinchaboy P.M., Fromenteau S., Fu H., Galbany L., Garcia R.A., Garcia-Hernandez D.A., Oehmichen L.A.G., Ge J., Maia M.A.G., Geisler D., Gelfand J., Goddy J., Gonzalez-Perez V., Grabowski K., Green P., Grier C.J., Guo H., Guy J., Harding P., Hasselquist S., Hawken A.J., Hayes C.R., Hearty F., Hekker S., Hogg D.W., Holtzman J.A., Horta D., Hou J., Hsieh B.-C., Huber D., Hunt J.A.S., Chitham J.I., Imig J., Jaber M., Angel C.E.J., Johnson J.A., Jones A.M., Jonsson H., Jullo E., Kim Y., Kinemuchi K., Kirkpatrick Iv C.C., Kite G.W., Klaene M., Kneib J.-P., Kollmeier J.A., Kong H., Kounkel M., Krishnarao D., Lacerna I., Lan T.-W., Lane R.R., Law D.R., Le Goff J.-M., Leung H.W., Lewis H., Li C., Lian J., Lin L., Long D., Longa-Peña P., Lundgren B., Lyke B.W., Ted Mackereth J., Macleod C.L., Majewski S.R., Manchado A., Maraston C., Martini P., Masseron T., Masters K.L., Mathur S., McDermid R.M., Merloni A., Merrifield M., Meszaros S., Miglio A., Minniti D., Minsley R., Miyaji T., Mohammad F.G., Mosser B., Mueller E.-M., Muna D., Muñoz-Gutierrez A., Myers A.D., Nadathur S., Nair P., Nandra K., Do Nascimento J.C., Nevin R.J., Newman J.A., Nidever D.L., Nitschelm C., Noterdaeme P., O'Connell J.E., Olmstead M.D., Oravetz D., Oravetz A., Osorio Y., Pace Z.J., Padilla N., Palanque-Delabrouille N., Palicio P.A., Pan H.-A., Pan K., Parker J., Paviot R., Peirani S., Ramrez K.P., Penny S., Percival W.J., Perez-Fournon I., Perez-Rafols I., Petitjean P., Pieri M.M., Pinsonneault M., Poovelil V.J., Povick J.T., Prakash A., Price-Whelan A.M., Raddick M.J., Raichoor A., Ray A., Rembold S.B., Rezaie M., Riffel R.A., Riffel R., Rix H.-W., Robin A.C., Roman-Lopes A., Roman-Zuñiga C., Rose B., Ross A.J., Rossi G., Rowlands K., Rubin K.H.R., Salvato M., Sanchez A.G., Sanchez-Menguiano L., Sanchez-Gallego J.R., Sayres C., Schaefer A., Schiavon R.P., Schimoia J.S., Schlafly E., Schlegel D., Schneider D.P., Schultheis M., Schwope A., Seo H.-J., Serenelli A., Shafieloo A., Shamsi S.J., Shao Z., Shen S., Shetrone M., Shirley R., Aguirre V.S., Simon J.D., Skrutskie M.F., Slosar A., Smethurst R., Sobeck J., Sodi B.C., Souto D., Stark D.V., Stassun K.G., Steinmetz M., Stello D., Stermer J., Storchi-Bergmann T., Streblyanska A., Stringfellow G.S., Stutz A., Suarez G., Sun J., Taghizadeh-Popp M., Talbot M.S., Tayar J., Thakar A.R., Theriault R., Thomas D., Thomas Z.C., Tinker J., Tojeiro R., Toledo H.H., Tremonti C.A., Troup N.W., Tuttle S., Unda-Sanzana E., Valentini M., Vargas-Gonzalez J., Vargas-Magaña M., Vazquez-Mata J.A., Vivek M., Wake D., Wang Y., Weaver B.A., Weijmans A.-M., Wild V., Wilson J.C., Wilson R.F., Wolthuis N., Wood-Vasey W.M., Yan R., Yang M., Yeche C., Zamora O., Zarrouk P., Zasowski G., Zhang K., Zhao C., Zhao G., Zheng Z., Zhu G., Zou H., Alfred P. Sloan Foundation, and Department of Energy (US)
Subjects: Optical telescopes, SAMPLE, Astrophysics, 01 natural sciences, Astronomi, astrofysik och kosmologi, Infrared astronomy, Observatory, Astronomy, Astrophysics and Cosmology, Astrophysics::Solar and Stellar Astrophysics, REDSHIFT 0.8, redshift surveys, stellar spectral lines, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, Astronomy databases, Redshift surveys, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, stellar properties, CATALOG, astro-ph.CO, astronomy databases, Data release, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], infrared astonomy, TELESCOPE, astro-ph.GA, media_common.quotation_subject, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Galactic abundances, Stellar properties, 0103 physical sciences, Astrophysics::Galaxy Astrophysics, DISTANCES, Stellar spectral lines, 010308 nuclear & particles physics, Astronomy and Astrophysics, optical telescopes, 115 Astronomy, Space science, Galaxy, GALAXY, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], STELLAR, 13. Climate action, Space and Planetary Science, Sky, [SDU]Sciences of the Universe [physics], galactic abundances, MILKY, astro-ph.IM, SDSS-IV MANGA
Abstract: This paper documents the 16th data release (DR16) from the Sloan Digital Sky Surveys (SDSS), the fourth and penultimate from the fourth phase (SDSS-IV). This is the first release of data from the Southern Hemisphere survey of the Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2); new data from APOGEE-2 North are also included. DR16 is also notable as the final data release for the main cosmological program of the Extended Baryon Oscillation Spectroscopic Survey (eBOSS), and all raw and reduced spectra from that project are released here. DR16 also includes all the data from the Time Domain Spectroscopic Survey and new data from the SPectroscopic IDentification of ERosita Survey programs, both of which were co-observed on eBOSS plates. DR16 has no new data from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey (or the MaNGA Stellar Library "MaStar"). We also preview future SDSS-V operations (due to start in 2020), and summarize plans for the final SDSS-IV data release (DR17)., Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org.
Published: 2020
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260. Physical parameters of red supergiants in dwarf irregular galaxies in the Local Group

Author: N. Britavskiy, A. Herrero, K. B. W. McQuinn, A. Z. Bonanos, Andrea Mehner, Martha L. Boyer, Miguel Cerviño, D. Garcia-Alvarez, Thomas Masseron, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFÍSICA DE CANARIAS (IAC), SEV-2015-0548, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Cerviño, M. [0000-0001-8009-231X], Bonanos, A. [0000-0003-2851-1905], Mehner, A. [0000-0002-9564-3302], Masseron, T. [0000-0002-6939-0831], Ministerio de Economía y Competitividad (MINECO), Agencia Estatal de Investigación (AEI), Spanish State Research Agency, European Regional Development Fund (FEDER), and Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC
Subjects: Supergiant, individual: WLM [Galaxies], Metallicity, individual: sextans A [Galaxies], FOS: Physical sciences, Astrophysics, Stellar classification, fundamental parameters [Stars], 01 natural sciences, individual: IC 10 [Galaxies], 0103 physical sciences, Asymptotic giant branch, Red supergiant, 010303 astronomy & astrophysics, Stellar evolution, Solar and Stellar Astrophysics (astro-ph.SR), Physics, 010308 nuclear & particles physics, Local Group, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA)
Abstract: Increasing the statistics of evolved massive stars in the Local Group enables investigating their evolution at different metallicities. During the late stages of stellar evolution, the physics of some phenomena, such as episodic and systematic mass loss, are not well constrained. For example, the physical properties of red supergiants (RSGs) in different metallicity regimes remain poorly understood. Thus, we initiated a systematic study of RSGs in dwarf irregular galaxies (dIrrs) in the Local Group. The target selection is based on 3.6 $\mu$m and 4.5 $\mu$m photometry from archival Spitzer Space Telescope images of nearby galaxies. We selected 46 targets in the dIrrs IC 10, IC 1613, Sextans B, and the Wolf-Lundmark-Melotte (WLM) galaxy that we observed with the GTC-OSIRIS and VLT-FORS2 instruments. We used several photometric techniques together with a spectral energy distribution analysis to derive the luminosities and effective temperatures of known and newly discovered RSGs. We identified and spectroscopically confirmed 4 new RSGs, 5 previously known RSGs, and 5 massive asymptotic giant branch (AGB) stars. We added known objects from previous observations. In total, we present spectral classification and fundamental physical parameters of 25 late-type massive stars in the following dIrrs: Sextans A, Sextans B, IC 10, IC 1613, Pegasus, Phoenix, and WLM. This includes 17 RSGs and 8 AGB stars that have been identified here and previously. Based on our observational results and PARSEC evolutionary models, we draw the following conclusions: (i) a trend to higher minimum effective temperatures at lower metallicities and (ii) the maximum luminosity of RSGs appears to be constant at $log$($L/L$$_{\odot}$) $\approx$ $5.5$, independent of the metallicity of the host environment (up to $\mathrm{[Fe/H]}$ $\approx$ $-1$ dex)., Comment: 22 pages, 17 figures, in press (A&A)
Published: 2019

261. The Gaia -ESO Survey: Properties of newly discovered Li-rich giants

Author: C. Régulo, Giovanni Carraro, Luca Sbordone, Amelia Bayo, Rafael A. García, E. Franciosini, Thierry Morel, X. Fu, Arnas Drazdauskas, Thomas Bensby, Alejandra Recio-Blanco, Laura Magrini, B. Mosser, Angela Bragaglia, Savita Mathur, Simone Zaggia, L. Prisinzano, L. Morbidelli, R. de Assis Peralta, Lorenzo Monaco, A. C. Lanzafame, Antonio Frasca, Sofia Randich, M. T. Costado, Paula Jofre, V. Adibekyan, P. de Laverny, Karin Lind, Andreas J. Korn, Rodolfo Smiljanic, Grazina Tautvaisiene, L. Pasquini, Elena Pancino, Thomas Masseron, Marica Valentini, S. G. Sousa, Saskia Hekker, Antonella Vallenari, Josefina Montalbán, Gerard Gilmore, D. Feuillet, Carmela Lardo, Sofia Feltzing, Sarah L. Martell, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Matériaux divisés, interfaces, réactivité, électrochimie (MADIREL), Aix Marseille Université (AMU)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Space Science Institute [Boulder] (SSI), 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)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Departamento de Astrofísica [La laguna], Universidad de La Laguna [Tenerife - SP] (ULL), School of Physics and Astronomy, University of Birmingham [Birmingham], Dipartimento di Scienze e Tecnologie Aerospaziali - Politecnico, Politecnico di Milano [Milan] (POLIMI), Lund Observatory, Lund University [Lund], INAF - Osservatorio Astronomico di Padova (OAPD), Department of Astronomy and Space Physics [Uppsala], Uppsala University, INAF - Osservatorio Astrofisico di Catania (OACT), 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), Ecole Polytechnique Fédérale de Lausanne (EPFL), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Smiljanic R., Franciosini E., Bragaglia A., Tautvaisiene G., Fu X., Pancino E., Adibekyan V., Sousa S.G., Randich S., Montalban J., Pasquini L., Magrini L., Drazdauskas A., Garcia R.A., Mathur S., Mosser B., Regulo C., De Assis Peralta R., Hekker S., Feuillet D., Valentini M., Morel T., Martell S., Gilmore G., Feltzing S., Vallenari A., Bensby T., Korn A.J., Lanzafame A.C., Recio-Blanco A., Bayo A., Carraro G., Costado M.T., Frasca A., Jofre P., Lardo C., De Laverny P., Lind K., Masseron T., Monaco L., Morbidelli L., Prisinzano L., Sbordone L., Zaggia S., ITA, USA, GBR, FRA, DEU, ESP, AUS, BEL, CHL, DNK, LTU, POL, PRT, SWE, CHE, Universidade do Porto = University of Porto, 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), 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), Gilmore, Gerard [0000-0003-4632-0213], Apollo - University of Cambridge Repository, Osservatorio Astronomico di Bologna (OABO), Universidade do Porto [Porto], Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Universidad Nacional de Colombia, PSL Research University (PSL)-PSL Research University (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), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), 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), Istituto Nazionale di Fisica Nucleare [Milano] (INFN), and PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS)
Subjects: barium stars, k-giant, Astrophysics, Stars: late-type, GALACTIC BULGE, mass-loss, 7. Clean energy, 01 natural sciences, LITHIUM ENRICHMENT, Bulge, Planet, Asymptotic giant branch, EVOLVED STARS, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, K-GIANT, [PHYS]Physics [physics], open clusters, red giants, LATE-TYPE STARS, Evolution [Stars], Red-giant branch, evolved stars, Stars: evolution, Astrophysics - Solar and Stellar Astrophysics, late-type [Stars], chemical-composition, Astrophysics::Earth and Planetary Astrophysics, Stars: abundance, stars: abundances, late-type stars, FOS: Physical sciences, Abundances [Stars], Astrophysics::Cosmology and Extragalactic Astrophysics, galactic bulge, CHEMICAL-COMPOSITION, 0103 physical sciences, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Infrared excess, 010308 nuclear & particles physics, Astronomy and Astrophysics, MASS-LOSS, BARIUM STARS, Accretion (astrophysics), lithium enrichment, RED GIANTS, Stars, Stars: abundances, Space and Planetary Science, 13. Climate action, OPEN CLUSTERS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Open cluster
Abstract: Aims. We report 20 new lithium-rich giants discovered within the Gaia-ESO Survey, including the first Li-rich giant with an evolutionary stage confirmed by CoRoT (Convection, Rotation and planetary Transits) data. We present a detailed overview of the properties of these 20 stars., Methods. Atmospheric parameters and abundances were derived in model atmosphere analyses using medium-resolution GIRAFFE or high-resolution UVES (Ultraviolet and Visual Echelle Spectrograph) spectra. These results are part of the fifth internal data release of the Gaia-ESO Survey. The Li abundances were corrected for non-local thermodynamical equilibrium effects. Other stellar properties were investigated for additional peculiarities (the core of strong lines for signs of magnetic activity, infrared magnitudes, rotational velocities, chemical abundances, and Galactic velocities). We used Gaia DR2 parallaxes to estimate distances and luminosities., Results. The giants have A(Li) > 2.2 dex. The majority of them (14 of 20 stars) are in the CoRoT fields. Four giants are located in the field of three open clusters, but are not members. Two giants were observed in fields towards the Galactic bulge, but likely lie in the inner disc. One of the bulge field giants is super Li-rich with A(Li) = 4.0 dex., Conclusions. We identified one giant with infrared excess at 22 mu m. Two other giants, with large v sin i, might be Li-rich because of planet engulfment. Another giant is found to be barium enhanced and thus could have accreted material from a former asymptotic giant branch companion. Otherwise, in addition to the Li enrichment, the evolutionary stages are the only other connection between these new Li-rich giants. The CoRoT data confirm that one Li-rich giant is at the core-He burning stage. The other giants are concentrated in close proximity to the red giant branch luminosity bump, the core-He burning stages, or the early-asymptotic giant branch. This is very clear from the Gaia-based luminosities of the Li-rich giants. This is also seen when the CoRoT Li-rich giants are compared to a larger sample of 2252 giants observed in the CoRoT fields by the Gaia-ESO Survey, which are distributed throughout the red giant branch in the T-eff-log g diagram. These observations show that the evolutionary stage is a major factor for the Li enrichment in giants. Other processes, such as planet accretion, contribute at a smaller scale.
Published: 2018
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262. The Gaia-ESO Survey: matching chemodynamical simulations to observations of the Milky Way

Author: Grazina Tautvaisiene, P. Francois, G. G. Sacco, Andreas Korn, B. B. Thompson, P. Donati, Gianni Marconi, Thomas Masseron, A. C. Lanzafame, A. Hourihane, Brad K. Gibson, Carmela Lardo, B. A. Macfarlane, Jack Lewis, Aldo Serenelli, E. Franciosini, E. Pancino, Antonio Frasca, L. Morbidelli, Sergey E. Koposov, P. de Laverny, Clare Worley, Simone Zaggia, Paula Jofre, Gerard Gilmore, L. Prisinzano, Lorenzo Monaco, V. Hill, Laura Magrini, C. G. Few, Ulrike Heiter, Emilio J. Alfaro, Andrew R. Casey, M. T. Costado, S. G. Sousa, Maria Bergemann, Giovanni Carraro, Antonella Vallenari, Thomas Bensby, Sofia Randich, Amelia Bayo, A. Recio-Blanco, Jeremiah Horrocks Insitute, University of Central Lancashire [Preston] (UCLAN), Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Department of Physics and Astronomy [Uppsala], Uppsala University, Focas Research Institute, Dublin Institute of Technology, Institut national de recherche et de sécurité (Vandoeuvre lès Nancy) (INRS ( Vandoeuvre lès Nancy)), INAF - Osservatorio Astrofisico di Catania (OACT), 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), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Ecole Polytechnique Fédérale de Lausanne (EPFL), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), INAF - Osservatorio Astronomico di Bologna (OABO), Universidade de Sao Paulo, Instituto Ocenografico, Science and Technology Facilities Council (UK), European Research Council, Knut and Alice Wallenberg Foundation, Fundação para a Ciência e a Tecnologia (Portugal), European Commission, Swedish National Space Board, Leverhulme Trust, Istituto Nazionale di Astrofisica, European Science Foundation, Ministerio de Economía y Competitividad (España), German Research Foundation, National Science Foundation (US), Australian Research Council, Gilmore, Gerard [0000-0003-4632-0213], Casey, Andrew [0000-0003-0174-0564], Worley, Clare [0000-0001-9310-2898], Apollo - University of Cambridge Repository, Thompson B.B., Few C.G., Bergemann M., Gibson B.K., MacFarlane B.A., Serenelli A., Gilmore G., Randich S., Vallenari A., Alfaro E.J., Bensby T., Francois P., Korn A.J., Bayo A., Carraro G., Casey A.R., Costado M.T., Donati P., Franciosini E., Frasca A., Hourihane A., Jofre P., Hill V., Heiter U., Koposov S.E., Lanzafame A., Lardo C., de Laverny P., Lewis J., Magrini L., Marconi G., Masseron T., Monaco L., Morbidelli L., Pancino E., Prisinzano L., Recio-Blanco A., Sacco G., Sousa S.G., Tautvaisiene G., Worley C.C., and Zaggia S.
Subjects: Matching (statistics), Milky Way, astro-ph.GA, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, F500, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, methods: numerical, 0103 physical sciences, galaxies: formation, 010303 astronomy & astrophysics, Selection (genetic algorithm), Astrophysics::Galaxy Astrophysics, Physics, [PHYS]Physics [physics], numerical [Methods], 010308 nuclear & particles physics, galaxies: evolution - galaxies: formation, abundances [Galaxy], Astronomy and Astrophysics, Effective temperature, Surface gravity, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, formation [Galaxies], Galaxy, Galaxy: abundance, Galaxies: evolution, Galaxies: formation, Galaxy: abundances, Methods: numerical, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Survey data collection, methods: numerical - Galaxy: abundances, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The typical methodology for comparing simulated galaxies with observational surveys is usually to apply a spatial selection to the simulation to mimic the region of interest covered by a comparable observational survey sample. In this work, we compare this approach with a more sophisticated post-processing in which the observational uncertainties and selection effects (photometric, surface gravity and effective temperature) are taken into account. We compare a 'solar neighbourhood analogue' region in a model MilkyWay-like galaxy simulated with RAMSES-CH with fourth release Gaia-ESO survey data. We find that a simple spatial cut alone is insufficient and that the observational uncertainties must be accounted for in the comparison. This is particularly true when the scale of uncertainty is large compared to the dynamic range of the data, e.g. in our comparison, the [Mg/Fe] distribution is affected much more than the more accurately determined [Fe/H] distribution. Despite clear differences in the underlying distributions of elemental abundances between simulation and observation, incorporating scatter to our simulation results to mimic observational uncertainty produces reasonable agreement. The quite complete nature of the Gaia-ESO survey means that the selection function has minimal impact on the distribution of observed age and metal abundances but this would become increasingly more important for surveys with narrower selection functions.© 2017 The Author(s)., This is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002 (the Gaia-ESO Public Spectroscopic Survey). We acknowledge the insightful comments and support provided by our colleagues Stefano Pasetto, Daisuke Kawata, Rob Thacker and Dimitris Stamatellos. We would thank the anonymous referee for a very constructive report of the work presented here. BBT acknowledges the support of STFC through its PhD Studentship Programme (ST/F007701/1). We also acknowledge the generous allocation of resources from the Partnership for Advanced Computing in Europe (PRACE) via the DEISA Extreme Computing Initiative (PRACE-3IP Project RI-312763 and PRACE-4IP Project 653838) and STFC's DiRAC Facility (COSMOS: Galactic Archaeology). CGF acknowledges funding from the European Research Council for the FP7 ERC starting grant project LOCALSTAR and the DiRAC Complexity system, operated by the University of Leicester IT Services, which forms part of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment is funded by BIS National E-Infrastructure capital grant ST/K000373/1 and STFC DiRAC Operations grant ST/K0003259/1. DiRAC is part of the National E-Infrastructure. Continued access to the University of Hull's High Performance Computing Facility ('viper'), the HPC facility at the University of Central Lancashire and the computational facilities at Saint Mary's University are likewise gratefully acknowledged. TB was funded by the project grant 'The New Milky Way' from the Knut and Alice Wallenberg Foundation. SGS acknowledges the support by Fundacao para a Ciencia e Tecnologia (FCT) (ref: UID/FIS/04434/2013 & PTDC/FIS-AST/7073/2014 & Investigador FCT contract of reference IF/00028/2014) through national funds and by FEDER through COMPETE2020 (ref: POCI-01-0145-FEDER-007672 & POCI-01-0145-FEDER-016880). UH acknowledges support from the Swedish National Space Board (SNSB/Rymdstyrelsen). The Gaia-ESO Survey data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. 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' Universita' 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. MTC acknowledge the financial support from the Spanish Ministerio de Economia y Competitividad, through grant AYA2013-40611-P. UH acknowledges support from the Swedish National Space Board (SNSB/Rymdstyrelsen). This work was supported by Sonderforschungsbereich SFB 881 'The Milky Way System' (subprojects A5, C9) of the German Research Foundation (DFG). This work benefited from discussions at GNASH workshop, Victoria supported by the National Science Foundation under Grant No. PHY-1430152 (JINA Center for the Evolution of the Elements). ARC is supported by Australian Research Council Grant DP160100637
Published: 2018
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263. The Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars

Author: Thomas Nordlander, R. Sordo, C. Babusiaux, D. Montes, P. Gruyters, Ettore Flaccomio, Laura Magrini, C. Muñoz, Sergey E. Koposov, C. Allende Prieto, Eileen D. Friel, Giovanni Carraro, K. Biazzo, S. Duffau, Thomas Masseron, G. G. Sacco, Martin Asplund, Carmela Lardo, Luca Sbordone, M. T. Costado, Ignacio Negueruela, Annette M. N. Ferguson, S. Blanco-Cuaresma, Amelia Bayo, Ch. Martayan, I. San Roman, Lorenzo Monaco, Nuno C. Santos, L. Morbidelli, Ulrike Heiter, Enrico Maiorca, Sofia Feltzing, H. W. Rix, Janet E. Drew, Caroline Soubiran, Guillaume Guiglion, Gregory R. Ruchti, Antonella Vallenari, S. Van Eck, Vanessa Hill, P. Donati, S. G. Sousa, Rodolfo Smiljanic, Heather R. Jacobson, Marc Weber, James Binney, Giuseppina Micela, Bengt Edvardsson, R. D. Jeffries, Marica Valentini, Angela Bragaglia, Thierry Morel, Y. Chorniy, Michael G. Irwin, G. Barisevičius, A. C. Lanzafame, L. Prisinzano, Jack Lewis, E. Delgado-Mena, Lorenzo Spina, Hans-Günter Ludwig, Simone Zaggia, P. Francois, S. Villanova, Nils Ryde, N. A. Walton, E. Puzeras, R. J. Jackson, Elena Pancino, J. I. González Hernández, Piercarlo Bonifacio, Šarūnas Mikolaitis, Gerard Gilmore, Thomas Bensby, Alessio Mucciarelli, Douglas Geisler, Paula Jofre, T. Prusti, Sofia Randich, Matthias Steffen, Karin Lind, P. de Laverny, Gianni Marconi, Clare Worley, R. Blomme, Camilla Juul Hansen, Emilio J. Alfaro, E. Franciosini, Tristan Cantat-Gaudin, Alejandra Recio-Blanco, Henrik Jönsson, V. Zh. Adibekyan, Grazina Tautvaisiene, Hugo M. Tabernero, Andreas Korn, Elisabetta Caffau, Francesco Damiani, A. Hourihane, Aldo Serenelli, Maria Bergemann, Antonio Frasca, L. Pasquini, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Astrofísica Estelar (AE), Smiljanic, R., Korn, A. J., Bergemann, M., Frasca, A., Magrini, L., Masseron, T., Pancino, E., Ruchti, G., San Roman, I., Sbordone, L., Sousa, S. G., Tabernero, H., Tautvaišienė, G., Valentini, M., Weber, M., Worley, C. C., Adibekyan, V. Zh., Allende Prieto, C., Barisevičius, G., Biazzo, K., Blanco-Cuaresma, S., Bonifacio, P., Bragaglia, A., Caffau, E., Cantat-Gaudin, T., Chorniy, Y., de Laverny, P., Delgado-Mena, E., Donati, P., Duffau, S., Franciosini, E., Friel, E., Geisler, D., González Hernández, J. I., Gruyters, P., Guiglion, G., Hansen, C. J., Heiter, U., Hill, V., Jacobson, H. R., Jofre, P., Jönsson, H., Lanzafame, A. C., Lardo, C., Ludwig, H.-G., Maiorca, E., Mikolaitis, Š., Montes, D., Morel, T., Mucciarelli, A., Muñoz, C., Nordlander, T., Pasquini, L., Puzeras, E., Recio-Blanco, A., Ryde, N., Sacco, G., Santos, N. C., Serenelli, A. M., Sordo, R., Soubiran, C., Spina, L., Steffen, M., Vallenari, A., Van Eck, S., Villanova, S., Gilmore, G., Randich, S., Asplund, M., Binney, J., Drew, J., Feltzing, S., Ferguson, A., Jeffries, R., Micela, G., Negueruela, I., Prusti, T., Rix, H.-W., Alfaro, E., Babusiaux, C., Bensby, T., Blomme, R., Flaccomio, E., François, P., Irwin, M., Koposov, S., Walton, N., Bayo, A., Carraro, G., Costado, M. T., Damiani, F., Edvardsson, B., Hourihane, A., Jackson, R., Lewis, J., Lind, K., Marconi, G., Martayan, C., Monaco, L., Morbidelli, L., Prisinzano, L., Zaggia, S., Department of Astronomy and Space Physics [Uppsala], Uppsala University, M2A 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-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)-Centre National de la Recherche Scientifique (CNRS)-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), 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), Lund Observatory, Lund University [Lund], INAF - Osservatorio Astrofisico di Catania (OACT), Istituto Nazionale di Astrofisica (INAF), Université de Liège, Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto-Universidade do Porto, Laboratoire des Agrégats Moléculaires et Matériaux Inorganiques (LAMMI), Centre National de la Recherche Scientifique (CNRS)-Université Montpellier 2 - Sciences et Techniques (UM2), Institut d'Astronomie et d'Astrophysique, Université libre de Bruxelles (ULB), INAF - Osservatorio Astronomico di Palermo (OAPa), Agence Spatiale Européenne (ESA), European Space Agency (ESA), European Space Research and Technology Centre (ESTEC), European Southern Observatory (ESO), Naval Postgraduate School (U.S.), and Center for Interdisciplinary Remotely-Piloted Aircraft Studies (CIRPAS)
Subjects: Astrofísica, stars: abundances, High resolution, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, Type (model theory), Parameter space, Surveys, 01 natural sciences, fundamental parameters [Stars], Spectral line, surveys, 0103 physical sciences, Stars, fundamental parameters, methods, data analysis, data analysis [Methods], 010303 astronomy & astrophysics, methods: data analysis, surveys, stars: abundances, stars: fundamental parameters, stars: late-type, Solar and Stellar Astrophysics (astro-ph.SR), QC, Astronomía y Astrofísica, QB, Physics, 010308 nuclear & particles physics, stars: late-type, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], methods: data analysis, Stars, abundances, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astronomía, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Globular cluster, abundances [Stars], late-type [Stars], Stars, late type, stars: fundamental parameters, Dispersion (chemistry)
Abstract: The Gaia-ESO Survey is obtaining high-quality spectroscopic data for about 10^5 stars using FLAMES at the VLT. UVES high-resolution spectra are being collected for about 5000 FGK-type stars. These UVES spectra are analyzed in parallel by several state-of-the-art methodologies. Our aim is to present how these analyses were implemented, to discuss their results, and to describe how a final recommended parameter scale is defined. We also discuss the precision (method-to-method dispersion) and accuracy (biases with respect to the reference values) of the final parameters. These results are part of the Gaia-ESO 2nd internal release and will be part of its 1st public release of advanced data products. The final parameter scale is tied to the one defined by the Gaia benchmark stars, a set of stars with fundamental atmospheric parameters. A set of open and globular clusters is used to evaluate the physical soundness of the results. Each methodology is judged against the benchmark stars to define weights in three different regions of the parameter space. The final recommended results are the weighted-medians of those from the individual methods. The recommended results successfully reproduce the benchmark stars atmospheric parameters and the expected Teff-log g relation of the calibrating clusters. Atmospheric parameters and abundances have been determined for 1301 FGK-type stars observed with UVES. The median of the method-to-method dispersion of the atmospheric parameters is 55 K for Teff, 0.13 dex for log g, and 0.07 dex for [Fe/H]. Systematic biases are estimated to be between 50-100 K for Teff, 0.10-0.25 dex for log g, and 0.05-0.10 dex for [Fe/H]. Abundances for 24 elements were derived: C, N, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Y, Zr, Mo, Ba, Nd, and Eu. The typical method-to-method dispersion of the abundances varies between 0.10 and 0.20 dex., Comment: 39 pages, A&A accepted
Published: 2016
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264. The Gaia-ESO Survey: revisiting the Li-rich giant problem

Author: L. Morbidelli, Tomaž Zwitter, Thomas Masseron, Grant M. Kennedy, Lorenzo Monaco, S. G. Sousa, Rodolfo Smiljanic, A. Hourihane, Loredana Prisinzano, Giovanni Carraro, Laura Magrini, Angela Bragaglia, E. Franciosini, Alejandra Recio-Blanco, P. de Laverny, Clare Worley, Gražina Tautvaišienė, G. Ruchti, A. C. Lanzafame, P. Donati, G. G. Sacco, M. T. Costado, Sofia Randich, Karin Lind, Thierry Morel, Andreas Korn, Marica Valentini, E. Delgado Mena, Luca Sbordone, Simone Zaggia, Sergey E. Koposov, V. Silva Aguirre, Cristina Chiappini, Antonio Frasca, R. D. Jeffries, Francesco Damiani, P. Francois, Paula Jofre, James R. Lewis, Andrea Miglio, Ettore Flaccomio, Gerard Gilmore, Thomas Bensby, Y. Chorniy, Elena Pancino, Carmela Lardo, Sofia Feltzing, Sarah L. Martell, Josefina Montalbán, Andrew R. Casey, Antonella Vallenari, Casey, Andrew [0000-0003-0174-0564], Gilmore, Gerard [0000-0003-4632-0213], Kennedy, Grant [0000-0001-6831-7547], Koposov, Sergey [0000-0003-2644-135X], Worley, Clare [0000-0001-9310-2898], Apollo - University of Cambridge Repository, Casey A.R., Ruchti G., Masseron T., Randich S., Gilmore G., Lind K., Kennedy G.M., Koposov S.E., Hourihane A., Franciosini E., Lewis J.R., Magrini L., Morbidelli L., Sacco G.G., Worley C.C., Feltzing S., Jeffries R.D., Vallenari A., Bensby T., Bragaglia A., Flaccomio E., Francois P., Korn A.J., Lanzafame A., Pancino E., Recio-Blanco A., Smiljanic R., Carraro G., Costado M.T., Damiani F., Donati P., Frasca A., Jofre P., Lardo C., de Laverny P., Monaco L., Prisinzano L., Sbordone L., Sousa S.G., Tautvaisiene G., Zaggia S., Zwitter T., Mena E.D., Chorniy Y., Martell S.L., Aguirre V.S., Miglio A., Chiappini C., Montalban J., Morel T., and Valentini M.
Subjects: stars: abundancess, astro-ph.SR, stars: abundances, Metallicity, Bright giant, FOS: Physical sciences, CLUSTER NGC 362, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, GALACTIC BULGE, 01 natural sciences, Abundance, Planet, QB460, 0103 physical sciences, Hot Jupiter, EVOLVED STARS, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Stellar evolution, QC, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, QB, Physics, 010308 nuclear & particles physics, MASS RED GIANTS, Astronomy, Astronomy and Astrophysics, PLANET FORMATION, Giant star, Stars, Accretion (astrophysics), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, K-GIANTS, LITHIUM ABUNDANCES, STELLAR EVOLUTION, PRE-MAIN-SEQUENCE, SUN-LIKE STARS, Astrophysics::Earth and Planetary Astrophysics, QB799
Abstract: The discovery of lithium-rich giants contradicts expectations from canonical stellar evolution. Here we report on the serendipitous discovery of 20 Li-rich giants observed during the Gaia-ESO Survey, which includes the first nine Li-rich giant stars known towards the CoRoT fields. Most of our Li-rich giants have near-solar metallicities, and stellar parameters consistent with being before the luminosity bump. This is difficult to reconcile with deep mixing models proposed to explain lithium enrichment, because these models can only operate at later evolutionary stages: at or past the luminosity bump. In an effort to shed light on the Li-rich phenomenon, we highlight recent evidence of the tidal destruction of close-in hot Jupiters at the sub-giant phase. We note that when coupled with models of planet accretion, the observed destruction of hot Jupiters actually predicts the existence of Li-rich giant stars, and suggests Li-rich stars should be found early on the giant branch and occur more frequently with increasing metallicity. A comprehensive review of all known Li-rich giant stars reveals that this scenario is consistent with the data. However more evolved or metal-poor stars are less likely to host close-in giant planets, implying that their Li-rich origin requires an alternative explanation, likely related to mixing scenarios rather than external phenomena., This work is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the $\textit{Gaia}$-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. 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 the Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR) in the form of the grant Premiale VLT 2012 and the Chemical and Dynamical Evolution of the Milky Way and Local Group Galaxies (prot. 2010LY5N2T). The results presented here benefit from discussions held during the $\textit{Gaia}$-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. GR acknowledges support from the project grant ‘The New Milky Way’ from the Knut and Alice Wallenberg Foundation. GMK is supported by the Royal Society as a Royal Society University Research Fellow. LS acknowledges support provided by the Chilean Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to the Millennium Institute of Astrophysics, MAS. Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation. The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement no. 267864). VSA acknowledges support from VILLUM FONDEN (research grant 10118). SLM acknowledges support from the Australian Research Council through DECRA fellowship DE140100598. TM acknowledges financial support from Belspo for contract PRODEX Gaia-DPAC. JM acknowledges the support from the European Research Council Consolidator Grant funding scheme (project STARKEY, G.A. no. 615604). This research has made use of the ExoDat Database, operated at LAM-OAMP, Marseille, France, on behalf of the CoRoT/Exoplanet programme. This research made use of astropy, a community-developed core python package for Astronomy (Astropy Collaboration et al. 2013). This research has made use of NASA's Astrophysics Data System Bibliographic Services., This is the final version of the article. It first appeared from Oxford University Press via http://dx.doi.org/10.1093/mnras/stw1512
Published: 2016
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265. The Gaia-ESO Survey: Empirical determination of the precision of stellar radial velocities and projected rotation velocities

Author: Annette M. N. Ferguson, Francesco Damiani, Gerard Gilmore, Angela Bragaglia, Martin Asplund, Giovanni Carraro, Vanessa Hill, L. Morbidelli, Paula Jofre, Antonio Frasca, Elena Pancino, A. C. Lanzafame, M. T. Costado, Bengt Edvardsson, A. Hourihane, Thomas Bensby, Antonella Vallenari, T. Prusti, Andreas Korn, Nicholas A. Walton, Carmela Lardo, Lorenzo Monaco, Sofia Feltzing, Ulrike Heiter, P. de Laverny, L. Prisinzano, Emilio J. Alfaro, C. Babusiaux, E. Franciosini, Clare Worley, Hans-Walter Rix, C. Allende Prieto, S. G. Sousa, Laura Magrini, Rodolfo Smiljanic, Christophe Martayan, G. G. Sacco, Maria Bergemann, P. Francois, R. J. Jackson, R. Blomme, Alejandra Recio-Blanco, Nigel Hambly, Sofia Randich, Karin Lind, Piercarlo Bonifacio, Gianni Marconi, R. D. Jeffries, Luca Sbordone, James R. Lewis, S. Van Eck, Amelia Bayo, James Binney, I. Neguerela, Simone Zaggia, Ettore Flaccomio, Janet E. Drew, Mike Irwin, Giuseppina Micela, Sergey E. Koposov, Thomas Masseron, Jackson R.J., Jeffries R.D., Lewis J., Koposov S.E., Sacco G.G., Randich S., Gilmore G., 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 F., Edvardsson B., Franciosini E., Frasca A., Heiter U., Hill V., Hourihane A., Jofre P., Lardo C., De Laverny P., Lind K., Magrini L., Marconi G., Martayan C., Masseron T., Monaco L., Morbidelli L., Prisinzano L., Sbordone L., Sousa S.G., Worley C.C., Zaggia S., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Astrofísica Estelar (AE), Keele University [Keele], Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), 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), School of Physics, Astronomy and Mathematics [Hatfield], University of Hertfordshire [Hatfield] (UH), Lund Observatory, Lund University [Lund], INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Agence Spatiale Européenne (ESA), European Space Agency (ESA), INAF - Osservatorio Astronomico di Padova (OAPD), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Royal Observatory of Belgium [Brussels] (ROB), INAF - Osservatorio Astronomico di Bologna (OABO), Institut de Mécanique des Fluides et des Solides (IMFS), École Nationale du Génie de l'Eau et de l'Environnement de Strasbourg (ENGEES)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Uppsala], Uppsala University, INAF - Osservatorio Astrofisico di Catania (OACT), 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), Institut d'Astronomie et d'Astrophysique, Université libre de Bruxelles (ULB), University of Turin, Ecole Polytechnique Fédérale de Lausanne (EPFL), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), 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, and 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)
Subjects: Metallicity, FOS: Physical sciences, stars: kinematics and dynamics, open clusters and associations: general, Open clusters and associations: general, Stars: kinematics and dynamics, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spectral line, Normal distribution, Astronomi, astrofysik och kosmologi, Observatory, Astronomy, Astrophysics and Cosmology, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), kinematics and dynamics [stars], QC, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, QB, Astronomía y Astrofísica, [PHYS]Physics [physics], Physics, Very Large Telescope, Kinematics and dynamics, Astrometry, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Satellite, Astrophysics::Earth and Planetary Astrophysics, general [open clusters and associations], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The Gaia-ESO Survey (GES) is a large public spectroscopic survey at the European Southern Observatory Very Large Telescope. A key aim is to provide precise radial velocities (RVs) and projected equatorial velocities (v sin i) for representative samples of Galactic stars, that will complement information obtained by the Gaia astrometry satellite. 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. 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. Parametrised results are provided, that 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 km/s, dependent on instrumental configuration., 13 pages, accepted for publication in Astronomy & Astrophysics
Published: 2015
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266. Gaia FGK benchmark stars: abundances of α and iron-peak elements

Author: Rosanna Sordo, Caroline Soubiran, A. Hourihane, Tristan Cantat-Gaudin, Elena Pancino, Alejandra Recio-Blanco, Carmela Lardo, L. Chemin, J. I. González Hernández, Gerry Gilmore, Ulrike Heiter, S. G. Sousa, Vardan Adibekyan, Elisa Delgado-Mena, Šarūnas Mikolaitis, S. Blanco-Cuaresma, Guillaume Guiglion, D. Montes, Maria Bergemann, Hugo M. Tabernero, Thomas Masseron, S. Van Eck, Antonella Vallenari, P. de Laverny, Clare Worley, Karin Lind, Paula Jofre, Thomas Nordlander, Laura Magrini, M2A 2015, 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), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institut d'Astronomie et d'Astrophysique, Université libre de Bruxelles (ULB), Jofre P., Heiter U., Soubiran C., Blanco-Cuaresma S., Masseron T., Nordlander T., Chemin L., Worley C.C., Van Eck S., Hourihane A., Gilmore G., Adibekyan V., Bergemann M., Cantat-Gaudin T., Delgado-Mena E., Gonzalez Hernandez J.I., Guiglion G., Lardo C., De Laverny P., Lind K., Magrini L., Mikolaitis S., Montes D., Pancino E., Recio-Blanco A., Sordo R., Sousa S., Tabernero H.M., and Vallenari A.
Subjects: Astrofísica, Milky Way, FOS: Physical sciences, Astrophysics, Spectral line, Astronomi, astrofysik och kosmologi, Abundance (ecology), stars: atmospheres, data analysis [methods], Calibration, Astronomy, Astrophysics and Cosmology, Astrophysics::Solar and Stellar Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, QC, QB, atmospheres [stars], Physics, abundances [Galaxy], Astronomy and Astrophysics, Iron peak, methods: data analysis, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Galaxy: abundance, Astronomía, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Homogeneous, Benchmark (computing), Galaxy: abundances, Astrophysics::Earth and Planetary Astrophysics, Methods: data analysi
Abstract: In the current era of large spectroscopic surveys of the Milky Way, reference stars for calibrating astrophysical parameters and chemical abundances are of paramount importance. We determine elemental abundances of Mg, Si, Ca, Sc, Ti, V, Cr, Mn, Co and Ni for our predefined set of Gaia FGK benchmark stars. By analysing high-resolution and high-signal to noise spectra taken from several archive datasets, we combined results of eight different methods to determine abundances on a line-by-line basis. We perform a detailed homogeneous analysis of the systematic uncertainties, such as differential versus absolute abundance analysis, as well as we assess errors due to NLTE and the stellar parameters in our final abundances. Our results are provided by listing final abundances and the different sources of uncertainties, as well as line-by-line and method-by-method abundances. The Gaia FGK benchmark stars atmospheric parameters are already being widely used for calibration of several pipelines applied to different surveys. With the added reference abundances of 10 elements this set is very suitable to calibrate the chemical abundances obtained by these pipelines., Comment: Accepted for publication in A&A, Printer format: 65 pages, 18 figures, 25 tables
Published: 2015
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267. The Gaia-ESO Survey: Detailed abundances in the metal-poor globular cluster NGC 4372

Author: Francesco Damiani, Emilio J. Alfaro, C. Muñoz, Alejandra Recio-Blanco, S. G. Sousa, Rodolfo Smiljanic, Nikolay Kacharov, S. Villanova, A. Hourihane, Antonella Vallenari, Carmela Lardo, Maria Bergemann, Luca Sbordone, Thomas Masseron, Thomas Bensby, Giovanni Carraro, Grazina Tautvaisiene, Ulrike Heiter, I. San Roman, Ettore Flaccomio, Andreas Korn, P. de Laverny, Clare Worley, M. T. Costado, L. Morbidelli, Andreas Koch, Simone Zaggia, Elena Pancino, P. Francois, Douglas Geisler, Paula Jofre, Departamento de Fisica Teorica C-XI (FTUAM), Universidad Autonoma de Madrid (UAM), Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), 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), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), 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), Department of Physics and Astronomy [Uppsala], Uppsala University, INAF - Osservatorio Astronomico di Bologna (OABO), 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), University of Turin, Ecole Polytechnique Fédérale de Lausanne (EPFL), 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), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), San Roman I., Munoz C., Geisler D., Villanova S., Kacharov N., Koch A., Carraro G., Tautvaisiene G., Vallenari A., Alfaro E.J., Bensby T., Flaccomio E., Francois P., Korn A.J., Pancino E., Recio-Blanco A., Smiljanic R., Bergemann M., Costado M.T., Damiani F., Heiter U., Hourihane A., Jofre P., Lardo C., De Laverny P., Masseron T., Morbidelli L., Sbordone L., Sousa S.G., Worley C.C., and Zaggia S.
Subjects: Physics, stars: abundances, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Metallicity, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Giant star, Spectral line, abundances [stars], Red-giant branch, Stars, Astrophysics - Solar and Stellar Astrophysics, Abundance (ecology), Globular clusters: individual: NGC 4372, Stars: abundances, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Globular cluster, globular clusters: individual: NGC 4372, Physical Sciences, Cluster (physics), Fysik, individual: NGC 4372 [globular clusters], Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We present the abundance analysis for a sample of 7 red giant branch stars in the metal-poor globular cluster NGC 4372 based on UVES spectra acquired as part of the Gaia-ESO Survey. This is the first extensive study of this cluster from high resolution spectroscopy. We derive abundances of O, Na, Mg, Al, Si, Ca, Sc, Ti, Fe, Cr, Ni, Y, Ba, and La. We find a metallicity of [Fe/H] = -2.19 $\pm$ 0.03 and find no evidence for a metallicity spread. This metallicity makes NGC 4372 one of the most metal-poor galactic globular clusters. We also find an {\alpha}-enhancement typical of halo globular clusters at this metallicity. Significant spreads are observed in the abundances of light elements. In particular we find a Na-O anti-correlation. Abundances of O are relatively high compared with other globular clusters. This could indicate that NGC 4372 was formed in an environment with high O for its metallicity. A Mg-Al spread is also present which spans a range of more than 0.5 dex in Al abundances. Na is correlated with Al and Mg abundances at a lower significance level. This pattern suggests that the Mg-Al burning cycle is active. This behavior can also be seen in giant stars of other massive, metal-poor clusters. A relation between light and heavy s-process elements has been identified., Comment: 14 pages, 14 figures, accepted for publication in A&A
Published: 2015
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268. The Gaia -ESO Survey: CNO abundances in the open clusters Trumpler 20, NGC 4815, and NGC 6705

Author: G. Tautvaišienė, A. Drazdauskas, Š. Mikolaitis, G. Barisevičius, E. Puzeras, E. Stonkut*error*ė, Y. Chorniy, L. Magrini, D. Romano, R. Smiljanic, A. Bragaglia, G. Carraro, E. Friel, T. Morel, E. Pancino, P. Donati, F. Jiménez-Esteban, G. Gilmore, S. Randich, R. D. Jeffries, A. Vallenari, T. Bensby, E. Flaccomio, A. Recio-Blanco, M. T. Costado, V. Hill, P. Jofré, C. Lardo, P. de Laverny, T. Masseron, L. Moribelli, S. G. Sousa, S. Zaggia, Tautvaisiene G., Drazdauskas A., Mikolaitis S., Barisevicius G., Puzeras E., Stonkute E., Chorniy Y., Magrini L., Romano D., Smiljanic R., Bragaglia A., Carraro G., Friel E., Morel T., Pancino E., Donati P., Jimenez-Esteban F., Gilmore G., Randich S., Jeffries R.D., Vallenari A., Bensby T., Flaccomio E., Recio-Blanco A., Costado M.T., Hill V., Jofre P., Lardo C., De Laverny P., Masseron T., Moribelli L., Sousa S.G., and Zaggia S.
Subjects: [open clusters and associations], Stars: abundance, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Context (language use), Solar radius, Astrophysics, 01 natural sciences, 7. Clean energy, Spectral line, evolution [Galaxy], Open clusters and associations: individual: NGC 4815, individual: Trumpler 20 [and associations], 0103 physical sciences, Galaxy formation and evolution, Cluster (physics), Astronomy, Astrophysics and Cosmology, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), QB, 0105 earth and related environmental sciences, Line (formation), Physics, Galaxy: evolution, open clusters, Open clusters and associations: individual: Trumpler 20, Stars: abundances, individual: NGC4815 [associations], Astronomy and Astrophysics, Open clusters and associations: individual: NGC 6705, Stars: evolution, Space and Planetary Science, abundances [stars], open clusters and, NGC6705 [individual], Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, evolution [stars], Open cluster
Abstract: Aim of this work is to determine C, N, and O abundances in stars of Galactic open clusters of the Gaia-ESO survey and to compare the observed abundances with those predicted by current stellar and Galactic evolution models. In this pilot paper, we investigate the first three intermediate-age open clusters. High-resolution spectra, observed with the FLAMES-UVES spectrograph on the ESO VLT telescope, were analysed using a differential model atmosphere method. Abundances of carbon were derived using the C2 band heads at 5135 and 5635.5 {\AA}. The wavelength interval 6470- 6490 {\AA}, with CN features, was analysed to determine nitrogen abundances. Oxygen abundances were determined from the [O i] line at 6300 {\AA}. The mean values of the elemental abundances in Trumpler 20 as determined from 42 stars are: [Fe/H] = 0.10 +- 0.08 (s.d.), [C/H] = -0.10 +- 0.07, [N/H] = 0.50 +- 0.07, and consequently C/N = 0.98 +- 0.12. We measure from five giants in NGC 4815: [Fe/H] = -0.01 +- 0.04, [C/H] = -0.17 +- 0.08, [N/H] = 0.53 +- 0.07, [O/H] = 0.12 +- 0.09, and C/N = 0.79 +- 0.08. We obtain from 27 giants in NGC 6705: [Fe/H] = 0.0 +- 0.05, [C/H] = -0.08 +- 0.06, [N/H] = 0.61 +- 0.07, [O/H] = 0.13 +- 0.05, and C/N = 0.83 +- 0.19. The C/N ratios of stars in the investigated open clusters were compared with the ratios predicted by stellar evolutionary models. For the corresponding stellar turn-off masses from 1.9 to 3.3 solar masses, the observed C/N ratio values are very close to the predictions of standard first dredge-up models as well as to models of thermohaline extra-mixing. The average [O/H] abundance ratios of NGC 4815 and NGC 6705 are compared with the predictions of two Galactic chemical evolution models. The data are consistent with the evolution at the solar radius within the errors., Comment: 13 pages, 11 figures, accepted for publication in Astronomy & Astrophysics, 2014
Published: 2015

269. The Gaia-ESO Survey: Abundance ratios in the inner-disk open clusters Trumpler 20, NGC 4815, NGC 6705

Author: Gerard Gilmore, F. M. Jiménez-Esteban, Ulrike Heiter, Vanessa Hill, Jack Lewis, Lorenzo Spina, P. Donati, A. Hourihane, E. Friel, Grazina Tautvaisiene, E. Franciosini, Sergey E. Koposov, Enrico Maiorca, Carmela Lardo, Andreas Korn, Rodolfo Smiljanic, Sofia Feltzing, Antonella Vallenari, Monica Tosi, R. J. Jackson, Martin Asplund, Angela Bragaglia, Thomas Masseron, Heather R. Jacobson, P. Francois, C. Muñoz, P. de Laverny, Clare Worley, Nami Mowlavi, R. D. Jeffries, Maria Bergemann, I. San Roman, S. Villanova, S. Blanco-Cuaresma, Francesco Damiani, Tristan Cantat-Gaudin, Alejandra Recio-Blanco, Sofia Randich, Karin Lind, Donatella Romano, Ettore Flaccomio, Caroline Soubiran, Laura Magrini, Douglas Geisler, Paula Jofre, Simone Zaggia, Loredana Prisinzano, R. Sordo, G. G. Sacco, L. Morbidelli, Thomas Bensby, Elena Pancino, M. T. Costado, Laboratoire des Agrégats Moléculaires et Matériaux Inorganiques (LAMMI), Centre National de la Recherche Scientifique (CNRS)-Université Montpellier 2 - Sciences et Techniques (UM2), M2A 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-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)-Centre National de la Recherche Scientifique (CNRS)-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), Department of Astronomy and Space Physics [Uppsala], Uppsala University, 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), 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), Université Sciences et Technologies - Bordeaux 1, Magrini L., Randich S., Romano D., Friel E., Bragaglia A., Smiljanic R., Jacobson H., Vallenari A., Tosi M., Spina L., Donati P., Maiorca E., Cantat-Gaudin T., Sordo R., Bergemann M., Damiani F., Tautvaisiene G., Blanco-Cuaresma S., Jimenez-Esteban F., Geisler D., Mowlavi N., Munoz C., San Roman I., Soubiran C., Villanova S., Zaggia S., Gilmore G., Asplund M., Feltzing S., Jeffries R., Bensby T., Koposov S., Korn A.J., Flaccomio E., Pancino E., Recio-Blanco A., Sacco G., Costado M.T., Franciosini E., Jofre P., De Laverny P., Hill V., Heiter U., Hourihane A., Jackson R., Lardo C., Morbidelli L., Lewis J., Lind K., Masseron T., Prisinzano L., and Worley C.
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Globular clusters: individual: NGC 6705, Metallicity, astro-ph.GA, FOS: Physical sciences, Astrophysics, Galaxy: disk, Open clusters and associations: individual: NGC 4815, Bulge, Abundance (ecology), Disc, Galaxy: abundances, Open clusters and associations: general, Open clusters and associations: individual: Trumpler 20, Physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Galaxy: abundance, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Content (measure theory), Open cluster
Abstract: Open clusters are key tools to study the spatial distribution of abundances in the disk and their evolution with time. Using the first release of stellar parameters and abundances of the Gaia-ESO Survey, we analyse the chemical properties of stars in three old/intermediate-age open clusters, namely NGC 6705, NGC 4815, and Trumpler 20, all located in the inner part of the Galactic disk at Galactocentric radius R$_{GC}\sim$7 kpc, aiming at proving their homogeneity and at comparing them with the field population. We study the abundance ratios of elements belonging to two different nucleosynthetic channels: $\alpha$-elements and iron-peak elements. The main results can be summarised as follows: i) cluster members are chemically homogeneous within 3-$\sigma$ in all analysed elements; ii) the three clusters have comparable [El/Fe] patters within $\sim$1-$\sigma$, but they differ in their global metal content [El/H], with NGC 4815 having the lowest metallicity. Their [El/Fe] ratios show differences and analogies with those of the field population, both in the solar neighbourhood and in the bulge/inner disk; iii) comparing the abundance ratios with the results of two chemical evolution models and with field star abundance distributions, we find that the abundance ratios of Mg, Ni, Ca in NGC 6705 might require an inner birthplace, implying a subsequent variation of its R$_{GC}$ during its lifetime, consistent with previous orbit determination. The full dataset of the Gaia-ESO Survey will be a superlative tool to constrain the chemical evolution of our Galaxy by disentangling different formation and evolution scenarios., Comment: 17 pages, 11 figures, A&A accepted
Published: 2014
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270. The Gaia-ESO Survey: the most metal-poor stars in the Galactic bulge

Author: Alejandra Recio-Blanco, David M. Nataf, Sofia Randich, Karin Lind, A. Hourihane, Carmela Lardo, Sofia Feltzing, G. G. Sacco, Martin Asplund, C. C. Worley, Paula Jofre, Andreas Korn, David Yong, C. Allende Prieto, L. M. Howes, G. S. Da Costa, Enrico Maiorca, Manuela Zoccali, Francesco Damiani, L. Morbidelli, Vanessa Hill, Maria Bergemann, Ulrike Heiter, Andrew R. Casey, Rodolfo Smiljanic, Gerard Gilmore, Stefan Keller, Michael S. Bessell, Dante Minniti, Patrick Tisserand, Laura Magrini, Anna F. Marino, Brian P. Schmidt, Antonella Vallenari, Thomas Masseron, Luca Casagrande, Ettore Flaccomio, P. de Laverny, Elena Pancino, Thomas Bensby, Christopher Owen, M. T. Costado, Howes L.M., Asplund M., Casey A.R., Keller S.C., Yong D., Gilmore G., Lind K., Worley C., Bessell M.S., Casagrande L., Marino A.F., Nataf D.M., Owen C.I., Da Costa G.S., Schmidt B.P., Tisserand P., Randich S., Feltzing S., Vallenari A., Allende Prieto C., Bensby T., Flaccomio E., Korn A.J., Pancino E., Recio-Blanco A., Smiljanic R., Bergemann M., Costado M.T., Damiani F., Heiter U., Hill V., Hourihane A., Jofre P., Lardo C., de Laverny P., Magrini L., Maiorca E., Masseron T., Morbidelli L., Sacco G.G., Minniti D., and Zoccali M.
Subjects: 010504 meteorology & atmospheric sciences, Evolution, Metallicity, K-type main-sequence star, Milky Way, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Bulge, 0103 physical sciences, Galaxy formation and evolution, Population II-Galaxy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Spiral galaxy, Bulge-Galaxy, Astronomy, Astronomy and Astrophysics, Stars, Astrophysics - Astrophysics of Galaxies, Galaxy, Abundances-star, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics
Abstract: We present the first results of the EMBLA survey (Extremely Metal-poor BuLge stars with AAOmega), aimed at finding metal-poor stars in the Milky Way bulge, where the oldest stars should now preferentially reside. EMBLA utilises SkyMapper photometry to pre-select metal-poor candidates, which are subsequently confirmed using AAOmega spectroscopy. We describe the discovery and analysis of four bulge giants with -2.72, Comment: 7 pages, 5 figures. Accepted for publication by MNRAS
Published: 2014
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271. The Gaia-ESO Survey: Stellar content and elemental abundances in the massive cluster NGC 6705

Author: Douglas Geisler, Paula Jofre, Thomas Bensby, A. Hourihane, A. Kupcu-Yoldas, Gerard Gilmore, F. M. Jiménez-Esteban, Robert Greimel, L. Prisinzano, E. Puzeras, E. A. Gonzalez-Solares, Ettore Flaccomio, Carmela Lardo, Arnas Drazdauskas, P. Donati, Tristan Cantat-Gaudin, Alejandra Recio-Blanco, A. Klutsch, A. C. Lanzafame, I. San, L. Sampedro, Luca Sbordone, Emilio J. Alfaro, Enrico Maiorca, L. Balaguer-Núñez, S. Villanova, Elena Pancino, Simone Zaggia, Despina Hatzidimitriou, H. J. Farnhill, Laura Magrini, J. Eisloeffel, Rodolfo Smiljanic, Antonella Vallenari, Angela Bragaglia, A. Spagna, Ummi Abbas, Monica Tosi, R. Blomme, Heather R. Jacobson, Alberto Vecchiato, Clare Worley, G. G. Sacco, L. Morbidelli, Mike Irwin, Janet E. Drew, R. Sordo, Thomas Masseron, Carme Jordi, Sofia Randich, Grazina Tautvaisiene, Francesco Damiani, P. deLaverny, M. T. Costado, Eileen D. Friel, Cantat-Gaudin T., Vallenari A., Zaggia S., Bragaglia A., Sordo R., Drew J.E., Eisloeffel J., Farnhill H.J., Gonzalez-Solares E., Greimel R., Irwin M.J., Kupcu-Yoldas A., Jordi C., Blomme R., Sampedro L., Costado M.T., Alfaro E., Smiljanic R., Magrini L., Donati P., Friel E.D., Jacobson H., Abbas U., Hatzidimitriou D., Spagna A., Vecchiato A., Balaguer-Nunez L., Lardo C., Tosi M., Pancino E., Klutsch A., Tautvaisiene G., Drazdauskas A., Puzeras E., Jimenez-Esteban F., Maiorca E., Geisler D., San Roman I., Villanova S., Gilmore G., Randich S., Bensby T., Flaccomio E., Lanzafame A., Recio-Blanco A., Damiani F., Hourihane A., Jofre P., De Laverny P., Masseron T., Morbidelli L., Prisinzano L., Sacco G.G., Sbordone L., and Worley C.C.
Subjects: Physics, 010308 nuclear & particles physics, Milky Way, Metallicity, Stars: abundances, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Open clusters and associations: general, 01 natural sciences, Open clusters and associations: individual: NGC 6705, Photometry (optics), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Globular cluster, 0103 physical sciences, Cluster (physics), Mass segregation, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Red clump, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Open cluster
Abstract: Context. Chemically inhomogeneous populations are observed in most globular clusters, but not in open clusters. Cluster mass seems to play a key role in the existence of multiple populations. Aims. Studying the chemical homogeneity of the most massive open clusters is needed to better understand the mechanism of their formation and determine the mass limit under which clusters cannot host multiple populations. Here we studied NGCâ‰ 6705, which is a young and massive open cluster located towards the inner region of the Milky Way. This cluster is located inside the solar circle. This makes it an important tracer of the inner disk abundance gradient. Methods. This study makes use of BVI and ri photometry and comparisons with theoretical isochrones to derive the age of NGCâ‰ 6705. We study the density profile of the cluster and the mass function to infer the cluster mass. Based on abundances of the chemical elements distributed in the first internal data release of the Gaia-ESO Survey, we study elemental ratios and the chemical homogeneity of the red clump stars. Radial velocities enable us to study the rotation and internal kinematics of the cluster. Results. The estimated ages range from 250 to 316â‰ Myr, depending on the adopted stellar model. Luminosity profiles and mass functions show strong signs of mass segregation. We derive the mass of the cluster from its luminosity function and from the kinematics, finding values between 3700 M and 11 000 M. After selecting the cluster members from their radial velocities, we obtain a metallicity of [Fe/H] = 0.10 ± 0.06 based on 21 candidate members. Moreover, NGC 6705 shows no sign of the typical correlations or anti-correlations between Al, Mg, Si, and Na, which are expected in multiple populations. This is consistent with our cluster mass estimate, which is lower than the required mass limit proposed in the literature to develop multiple populations.
Published: 2014

272. TheGaia-ESO Survey: Kinematics of seven Galactic globular clusters

Author: Carmela Lardo, Sofia Feltzing, Alejandra Recio-Blanco, Elena Pancino, Maria Bergemann, Michele Bellazzini, C. Allende Prieto, Thomas Masseron, Sofia Randich, G. G. Sacco, Gerard Gilmore, R. D. Jeffries, Paolo Donati, Giovanni Carraro, Emilio J. Alfaro, Sergey E. Koposov, M. T. Costado, Francesco Damiani, L. Morbidelli, A. Hourihane, Angela Bragaglia, Paula Jofre, Ettore Flaccomio, Gianni Marconi, Antonella Vallenari, P. de Laverny, Clare Worley, Lardo C., Pancino E., Bellazzini M., Bragaglia A., Donati P., Gilmore G., Randich S., Feltzing S., Jeffries R.D., Vallenari A., Alfaro E.J., Allende Prieto C., Flaccomio E., Koposov S.E., Recio-Blanco A., Bergemann M., Carraro G., Costado M.T., Damiani F., Hourihane A., Jofre P., De Laverny P., Marconi G., Masseron T., Morbidelli L., Sacco G.G., Worley C.C., ITA, GBR, FRA, DEU, ESP, and SWE
Subjects: Physics, astro-ph.GA, Milky Way, FOS: Physical sciences, Velocity dispersion, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Kinematics, Astrophysics - Astrophysics of Galaxies, Galaxy, Radial velocity, Stars, General, Globular clusters, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Globular cluster, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB
Abstract: The Gaia-ESO survey is a large public spectroscopic survey aimed at investigating the origin and formation history of our Galaxy by collecting spectroscopy of representative samples (about 10^5 Milky Way stars) of all Galactic stellar populations, in the field and in clusters. The survey uses globular clusters as intra- and inter-survey calibrators, deriving stellar atmospheric parameters and abundances of a significant number of stars in clusters, along with radial velocity determinations. We used precise radial velocities of a large number of stars in seven globular clusters (NGC 1851, NGC 2808, NGC 4372, NGC 4833, NGC 5927, NGC 6752, and NGC 7078) to validate pipeline results and to preliminarily investigate the cluster internal kinematics. Radial velocity measurements were extracted from FLAMES/GIRAFFE spectra processed by the survey pipeline as part of the second internal data release of data products to ESO. We complemented our sample with ESO archival data obtained with different instrument configurations. Reliable radial velocity measurements for 1513 bona fide cluster star members were obtained in total. We measured systemic rotation, estimated central velocity dispersions, and present velocity dispersion profiles of all the selected clusters, providing the first velocity dispersion curve and the first estimate of the central velocity dispersion for the cluster NGC~5927. Finally, we explore the possible link between cluster kinematics and other physical parameters. The analysis we present here demonstrates that Gaia-ESO survey data are sufficiently accurate to be used in studies of kinematics of stellar systems and stellar populations in the Milky Way., Comment: 10 pages, 5 tables, 18 figures. Accepted to A&A
Published: 2015
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273. TheGaia-ESO Survey: radial metallicity gradients and age-metallicity relation of stars in the Milky Way disk

Author: M. Bergemann, G. R. Ruchti, A. Serenelli, S. Feltzing, A. Alves-Brito, M. Asplund, T. Bensby, P. Gruiters, U. Heiter, A. Hourihane, A. Korn, K. Lind, A. Marino, P. Jofre, T. Nordlander, N. Ryde, C. C. Worley, G. Gilmore, S. Randich, A. M. N. Ferguson, R. D. Jeffries, G. Micela, I. Negueruela, T. Prusti, H.-W. Rix, A. Vallenari, E. J. Alfaro, C. Allende Prieto, A. Bragaglia, S. E. Koposov, A. C. Lanzafame, E. Pancino, A. Recio-Blanco, R. Smiljanic, N. Walton, M. T. Costado, E. Franciosini, V. Hill, C. Lardo, P. de Laverny, L. Magrini, E. Maiorca, T. Masseron, L. Morbidelli, G. Sacco, G. Kordopatis, G. Tautvaišienė, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Astrofísica Estelar (AE), Bergemann M., Ruchti G.R., Serenelli A., Feltzing S., Alves-Brito A., Asplund M., Bensby T., Gruiters P., Heiter U., Hourihane A., Korn A., Lind K., Marino A., Jofre P., Nordlander T., Ryde N., Worley C.C., Gilmore G., Randich S., Ferguson A.M.N., Jeffries R.D., Micela G., Negueruela I., Prusti T., Rix H.-W., Vallenari A., Alfaro E.J., Allende Prieto C., Bragaglia A., Koposov S.E., Lanzafame A.C., Pancino E., Recio-Blanco A., Smiljanic R., Walton N., Costado M.T., Franciosini E., Hill V., Lardo C., De Laverny P., Magrini L., Maiorca E., Masseron T., Morbidelli L., Sacco G., Kordopatis G., and Tautvaisiene G.
Subjects: Solar neighborhood, Milky Way, Metallicity, Formation, FOS: Physical sciences, Galaxia, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Surveys, fundamental parameters [Stars], Astronomia ultravioleta, 01 natural sciences, Spectral line, Galaxy: disk, Stars:fundamental parameter, Fundamental parameters, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Abundances, Disc, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astronomía y Astrofísica, Mapeamentos astronômicos, Physics, 010308 nuclear & particles physics, Plane (geometry), Stars:abundance, Vertical distance, Astronomy and Astrophysics, Composicao estelar, Astrophysics - Astrophysics of Galaxies, Espectros estelares, Stars, Galaxy, formation [Galaxy], Galaxy: formation, Disk, Space and Planetary Science, abundances [Stars], Astrophysics of Galaxies (astro-ph.GA), Magnitude (astronomy), Astrophysics::Earth and Planetary Astrophysics, disk [Galaxy]
Abstract: We study the relationship between age, metallicity, and alpha-enhancement of FGK stars in the Galactic disk. The results are based upon the analysis of high-resolution UVES spectra from the Gaia-ESO large stellar survey. We explore the limitations of the observed dataset, i.e. the accuracy of stellar parameters and the selection effects that are caused by the photometric target preselection. We find that the colour and magnitude cuts in the survey suppress old metal-rich stars and young metal-poor stars. This suppression may be as high as 97% in some regions of the age-metallicity relationship. The dataset consists of 144 stars with a wide range of ages from 0.5 Gyr to 13.5 Gyr, Galactocentric distances from 6 kpc to 9.5 kpc, and vertical distances from the plane 0 < |Z| < 1.5 kpc. On this basis, we find that i) the observed age-metallicity relation is nearly flat in the range of ages between 0 Gyr and 8 Gyr; ii) at ages older than 9 Gyr, we see a decrease in [Fe/H] and a clear absence of metal-rich stars; this cannot be explained by the survey selection functions; iii) there is a significant scatter of [Fe/H] at any age; and iv) [Mg/Fe] increases with age, but the dispersion of [Mg/Fe] at ages > 9 Gyr is not as small as advocated by some other studies. In agreement with earlier work, we find that radial abundance gradients change as a function of vertical distance from the plane. The [Mg/Fe] gradient steepens and becomes negative. In addition, we show that the inner disk is not only more alpha-rich compared to the outer disk, but also older, as traced independently by the ages and Mg abundances of stars., accepted for publication in A&A
Published: 2014
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274. A hot-Jupiter progenitor on a super-eccentric retrograde orbit.

Author: Gupta AF, Millholland SC, Im H, Dong J, Jackson JM, Carleo I, Libby-Roberts J, Delamer M, Giovinazzi MR, Lin ASJ, Kanodia S, Wang XY, Stassun K, Masseron T, Dragomir D, Mahadevan S, Wright J, Alvarado-Montes JA, Bender C, Blake CH, Caldwell D, Cañas CI, Cochran WD, Dalba P, Everett ME, Fernandez P, Golub E, Guillet B, Halverson S, Hebb L, Higuera J, Huang CX, Klusmeyer J, Knight R, Leroux L, Logsdon SE, Loose M, McElwain MW, Monson A, Ninan JP, Nowak G, Palle E, Patel Y, Pepper J, Primm M, Rajagopal J, Robertson P, Roy A, Schneider DP, Schwab C, Schweiker H, Sgro L, Shimizu M, Simard G, Stefánsson G, Stevens DJ, Villanueva S, Wisniewski J, Will S, and Ziegler C
Abstract: Giant exoplanets orbiting close to their host stars are unlikely to have formed in their present configurations 1 . These 'hot Jupiter' planets are instead thought to have migrated inward from beyond the ice line and several viable migration channels have been proposed, including eccentricity excitation through angular-momentum exchange with a third body followed by tidally driven orbital circularization 2,3 . The discovery of the extremely eccentric (e = 0.93) giant exoplanet HD 80606 b (ref. 4 ) provided observational evidence that hot Jupiters may have formed through this high-eccentricity tidal-migration pathway 5 . However, no similar hot-Jupiter progenitors have been found and simulations predict that one factor affecting the efficacy of this mechanism is exoplanet mass, as low-mass planets are more likely to be tidally disrupted during periastron passage 6-8 . Here we present spectroscopic and photometric observations of TIC 241249530 b, a high-mass, transiting warm Jupiter with an extreme orbital eccentricity of e = 0.94. The orbit of TIC 241249530 b is consistent with a history of eccentricity oscillations and a future tidal circularization trajectory. Our analysis of the mass and eccentricity distributions of the transiting-warm-Jupiter population further reveals a correlation between high mass and high eccentricity., (© 2024. The Author(s).)
Published: 2024
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275. Phosphorus-rich stars with unusual abundances are challenging theoretical predictions.

Author: Masseron T, García-Hernández DA, Santoveña R, Manchado A, Zamora O, Manteiga M, and Dafonte C
Abstract: Almost all chemical elements have been made by nucleosynthetic reactions in various kind of stars and have been accumulated along our cosmic history. Among those elements, the origin of phosphorus is of extreme interest because it is known to be essential for life such as we know on Earth. However, current models of (Galactic) chemical evolution under-predict the phosphorus we observe in our Solar System. Here we report the discovery of 15 phosphorus-rich stars with unusual overabundances of O, Mg, Si, Al, and Ce. Phosphorus-rich stars likely inherit their peculiar chemistry from another nearby stellar source but their intriguing chemical abundance pattern challenge the present stellar nucleosynthesis theoretical predictions. Specific effects such as rotation or advanced nucleosynthesis in convective-reactive regions in massive stars represent the most promising alternatives to explain the existence of phosphorus-rich stars. The phosphorus-rich stars progenitors may significantly contribute to the phosphorus present on Earth today.
Published: 2020
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276. [High-sensitivity cardiac troponin T and hemodialysis: influence of gender, age and diabetes].

Author: Poux JM, Citarda S, Gérard C, Masseron T, Galland R, Bully C, Serusclat P, Caillette-Beaudoin A, and Labeeuw M
Subjects: Age Factors, Aged, Aged, 80 and over, Biomarkers analysis, Cardiomyopathy, Hypertrophic blood, Cardiomyopathy, Hypertrophic diagnosis, Cohort Studies, Coronary Disease blood, Coronary Disease complications, Coronary Disease epidemiology, Diabetes Mellitus diagnosis, Diabetes Mellitus epidemiology, Diabetic Cardiomyopathies blood, Diabetic Cardiomyopathies diagnosis, Diabetic Cardiomyopathies epidemiology, Female, Humans, Male, Middle Aged, Renal Insufficiency, Chronic diagnosis, Renal Insufficiency, Chronic epidemiology, Sex Factors, Troponin T analysis, Biomarkers blood, Diabetes Mellitus blood, Renal Dialysis methods, Renal Dialysis statistics & numerical data, Renal Insufficiency, Chronic blood, Renal Insufficiency, Chronic therapy, Troponin T blood
Published: 2018
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277. [A laboratory artefact to detect: the EDTA-dependent pseudothrombocytopenia].

Author: Gérôme P, Cardon N, Crevon L, Ehrmann P, Dusseau JY, Masseron T, Chaulet JF, and Bercion R
Subjects: Adult, Diagnostic Errors, Humans, Leukocyte Count, Male, Platelet Count, Thrombocytopenia blood, Artifacts, Edetic Acid adverse effects, Thrombocytopenia diagnosis
Published: 2003

278. [Predictive factors of mortality in severe shigellosis].

Author: de Widerspach-Thor A, d'Alteroche L, Rault A, Thuan JF, Masseron T, and Hovette P
Subjects: Adolescent, Adult, Child, Child, Preschool, Female, Humans, Infant, Male, Severity of Illness Index, Dysentery, Bacillary mortality
Published: 2002

279. [Implementation of a quality assurance manual at hospital laboratory].

Author: Cheminel V, Prévosto J, Muraillat D, Renard C, Thefenne H, Masseron T, and Chaulet J
Subjects: France, Quality Control, Laboratories, Hospital standards, Manuals as Topic standards
Published: 2000

280. [Frequency of pulmonary manifestations associated with visceral leishmaniasis].

Author: Hovette P, Rault A, Graffin B, and Masseron T
Subjects: Adult, Child, Female, Humans, Lung Diseases diagnosis, Lung Diseases parasitology, Male, Leishmaniasis, Visceral complications, Leishmaniasis, Visceral physiopathology, Lung Diseases etiology
Published: 1999

281. [Evolution of Shigella antibiotic resistance in Djibouti].

Author: Masseron T and Hovette P
Subjects: Djibouti epidemiology, Drug Resistance, Microbial, Dysentery, Bacillary drug therapy, Feces microbiology, Humans, Population Surveillance, Serotyping, Shigella classification, Dysentery, Bacillary epidemiology, Dysentery, Bacillary microbiology
Published: 1999

282. [Vancomycin resistant enterococcus in France. High prevalence in a young ambulatory care patient population].

Author: Guerin F, Perrier-Gros-Claude JD, Foissaud V, Masseron T, and Thierry J
Subjects: Adult, Ambulatory Care statistics & numerical data, Drug Resistance, Microbial, Enterococcus faecium drug effects, Feces microbiology, France, Humans, Male, Microbial Sensitivity Tests, Species Specificity, Enterococcus drug effects, Vancomycin pharmacology
Abstract: Objective: Assess the prevalence of asymptomatic carriage of vancomycin-resistant Enterococci in a population of healthy young French subjects., Methods: Stool samples obtained from 100 persons living in south-eastern France (20 sampling sites) were directly seeded on enriched selective media containing 6 mg/l vancomycin. Bacterial species and their resistant gene were identified with classical methods and multiplex genomic amplification., Results: The incidence of asymptomatic carriage was 17% with a homogeneous geographic distribution of the resistant strains. Nine Enterococcus faecium van A strains and 8 E. gallinarum van C1 strains were isolated., Conclusion: These findings demonstrate carriage of vancomycin-resistant Enterococci in a population of young ambulatory subjects in France. The incidence observed was much higher than in an earlier study conducted in France. These results might be explained by a much more sensitive detection technique. Care should be taken to avoid dissemination in hospital settings.
Published: 1998

283. [Antibiotic resistance of strains of Neisseria gonorrhoeae isolated in Dijibouti from 1995 to 1997].

Author: Masseron T and Hovette P
Subjects: Djibouti, Drug Resistance, Microbial, Neisseria gonorrhoeae isolation & purification, Species Specificity, Neisseria gonorrhoeae drug effects
Published: 1998

284. [Conjunctival dirofilariasis caused by Dirofilaria repens: report of a French case].

Author: Masseron T, Sailliol A, Niel L, and Floch JJ
Subjects: Animals, Dirofilaria isolation & purification, Dirofilariasis parasitology, Eye Infections, Parasitic parasitology, Female, France, Humans, Male, Middle Aged, Conjunctivitis diagnosis, Conjunctivitis parasitology, Dirofilariasis diagnosis, Eye Infections, Parasitic diagnosis
Abstract: Dirofilariasis involving Dirofilaria repens is an exceedingly rare event in France. Most cases have involved subcutaneous lesions but ocular and peri-ocular involvement have been observed. The present report describes a case of dirofilariasis involving the conjunctiva in a 61 year-old-man in France. Onset was characterized by the sudden appearance of painful conjunctival cyst. Clinical examination and laboratory tests did not allow diagnosis. Opening the cyst and extracting the parasite allowed diagnosis and treatment. Microscopic examination identified the parasite as a female Dirofilaria repens. This new case of ocular dirofilariasis emphasizes that this parasitic disease is present and probably underestimated in mainland France. Opening of the conjunctival cyst allowed identification of the parasite and successful treatment without sequels.
Published: 1995

285. Infrequent sites of extramedullary relapse after allogeneic bone marrow transplantation.

Author: Viard F, Bilhou-Nabera C, Marit G, Durrieu F, Dubus P, Masseron T, Boiron JM, Gharbi MJ, Salzes S, and Broustet A
Subjects: Adult, Humans, Leukemia physiopathology, Leukemia surgery, Male, Middle Aged, Recurrence, Bone Marrow Transplantation
Abstract: In the present report, we describe two cases of rare extramedullary relapse (skin, muscle) after allogeneic bone marrow transplantation (BMT). As both patients were male and had received sex mismatched (non T-depleted) BMT, marrow samples were analysed with a Y-chromosome specific probe allowing the sensitive detection of host DNA. The proportion of host DNA remained low in all post BMT samples from these patients, even at the time of extramedullary relapse.
Published: 1995

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285 results on '"Masseron, T."'

251. Gaia FGK benchmark stars: new candidates at low metallicities

252. CARBON STARS WITHIN THE GAIA-ESO SURVEY.

253. The Gaia-ESO Survey: detection and characterisation of single-line spectroscopic binaries.

254. Gaia -ESO Survey: Analysis of pre-main sequence stellar spectra

255. The Gaia-ESO Survey: Chromospheric emission, accretion properties, and rotation in gamma Velorum and Chamaeleon

256. The Gaia-ESO survey: placing constraints on the origin of r-process elements

257. The Gaia-ESO survey: Metallicity of the chamaeleon i star-forming region

258. Atomic data for the Gaia-ESO Survey

259. The 16th Data Release of the Sloan Digital Sky Surveys : First Release from the APOGEE-2 Southern Survey and Full Release of eBOSS Spectra

260. Physical parameters of red supergiants in dwarf irregular galaxies in the Local Group

261. The Gaia -ESO Survey: Properties of newly discovered Li-rich giants

262. The Gaia-ESO Survey: matching chemodynamical simulations to observations of the Milky Way

263. The Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars

264. The Gaia-ESO Survey: revisiting the Li-rich giant problem

265. The Gaia-ESO Survey: Empirical determination of the precision of stellar radial velocities and projected rotation velocities

266. Gaia FGK benchmark stars: abundances of α and iron-peak elements

267. The Gaia-ESO Survey: Detailed abundances in the metal-poor globular cluster NGC 4372

268. The Gaia -ESO Survey: CNO abundances in the open clusters Trumpler 20, NGC 4815, and NGC 6705

269. The Gaia-ESO Survey: Abundance ratios in the inner-disk open clusters Trumpler 20, NGC 4815, NGC 6705

270. The Gaia-ESO Survey: the most metal-poor stars in the Galactic bulge

271. The Gaia-ESO Survey: Stellar content and elemental abundances in the massive cluster NGC 6705

272. TheGaia-ESO Survey: Kinematics of seven Galactic globular clusters

273. TheGaia-ESO Survey: radial metallicity gradients and age-metallicity relation of stars in the Milky Way disk

274. A hot-Jupiter progenitor on a super-eccentric retrograde orbit.

275. Phosphorus-rich stars with unusual abundances are challenging theoretical predictions.

276. [High-sensitivity cardiac troponin T and hemodialysis: influence of gender, age and diabetes].

277. [A laboratory artefact to detect: the EDTA-dependent pseudothrombocytopenia].

278. [Predictive factors of mortality in severe shigellosis].

279. [Implementation of a quality assurance manual at hospital laboratory].

280. [Frequency of pulmonary manifestations associated with visceral leishmaniasis].

281. [Evolution of Shigella antibiotic resistance in Djibouti].

282. [Vancomycin resistant enterococcus in France. High prevalence in a young ambulatory care patient population].

283. [Antibiotic resistance of strains of Neisseria gonorrhoeae isolated in Dijibouti from 1995 to 1997].

284. [Conjunctival dirofilariasis caused by Dirofilaria repens: report of a French case].

285. Infrequent sites of extramedullary relapse after allogeneic bone marrow transplantation.

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