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101. Survey of Surveys

Author

Tsantaki, M., primary, Pancino, E., additional, Marrese, P., additional, Marinoni, S., additional, Rainer, M., additional, Sanna, N., additional, Turchi, A., additional, Randich, S., additional, Gallart, C., additional, Battaglia, G., additional, and Masseron, T., additional

Published
2022
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102. Exploring the S-process History in the Galactic Disk: Cerium Abundances and Gradients in Open Clusters from the OCCAM/APOGEE Sample

Author

Sales-Silva, J. V., primary, Daflon, S., additional, Cunha, K., additional, Souto, D., additional, Smith, V. V., additional, Chiappini, C., additional, Donor, J., additional, Frinchaboy, P. M., additional, García-Hernández, D. A., additional, Hayes, C., additional, Majewski, S. R., additional, Masseron, T., additional, Schiavon, R. P., additional, Weinberg, D. H., additional, Beaton, R. L., additional, Fernández-Trincado, J. G., additional, Jönsson, H., additional, Lane, R. R., additional, Minniti, D., additional, Manchado, A., additional, Moni Bidin, C., additional, Nitschelm, C., additional, O’Connell, J., additional, and Villanova, S., additional

Published
2022
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103. Estimating fundamental parameters of nearby M dwarfs from SPIRou spectra

Author

Cristofari, P I, primary, Donati, J-F, additional, Masseron, T, additional, Fouqué, P, additional, Moutou, C, additional, Delfosse, X, additional, Artigau, E, additional, Folsom, C P, additional, Carmona, A, additional, Gaidos, E, additional, do Nascimento, J-D, additional, Jahandar, F, additional, and Hébrard, G, additional

Published
2021
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105. Gaia-ESO survey: Lithium abundances in open cluster Red Clump stars

Author

Magrini, L., primary, Smiljanic, R., additional, Franciosini, E., additional, Pasquini, L., additional, Randich, S., additional, Casali, G., additional, Viscasillas Vázquez, C., additional, Bragaglia, A., additional, Spina, L., additional, Biazzo, K., additional, Tautvaišienė, G., additional, Masseron, T., additional, Van der Swaelmen, M., additional, Pancino, E., additional, Jiménez-Esteban, F., additional, Guiglion, G., additional, Martell, S., additional, Bensby, T., additional, D’Orazi, V., additional, Baratella, M., additional, Korn, A., additional, Jofre, P., additional, Gilmore, G., additional, Worley, C., additional, Hourihane, A., additional, Gonneau, A., additional, Sacco, G. G., additional, and Morbidelli, L., additional

Published
2021
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106. Atomic data for the Gaia-ESO Survey

Author

Heiter, Ulrike, Lind, K., Bergemann, M., Asplund, M., Mikolaitis, S., Barklem, Paul, Masseron, T., de Laverny, P., Magrini, L., Edvardsson, Bengt, Jonsson, H., Pickering, J. C., Ryde, N., Aran, A. Bayo, Bensby, T., Casey, A. R., Feltzing, S., Jofre, P., Korn, Andreas, Pancino, E., Damiani, F., Lanzafame, A., Lardo, C., Monaco, L., Morbidelli, L., Smiljanic, R., Worley, C., Zaggia, S., Randich, S., Gilmore, G. F., Heiter, Ulrike, Lind, K., Bergemann, M., Asplund, M., Mikolaitis, S., Barklem, Paul, Masseron, T., de Laverny, P., Magrini, L., Edvardsson, Bengt, Jonsson, H., Pickering, J. C., Ryde, N., Aran, A. Bayo, Bensby, T., Casey, A. R., Feltzing, S., Jofre, P., Korn, Andreas, Pancino, E., Damiani, F., Lanzafame, A., Lardo, C., Monaco, L., Morbidelli, L., Smiljanic, R., Worley, C., Zaggia, S., Randich, S., and Gilmore, G. F.

Abstract

Context. We describe the atomic and molecular data that were used for the abundance analyses of FGK-type stars carried out within the Gaia-ESO Public Spectroscopic Survey in the years 2012 to 2019. The Gaia-ESO Survey is one among several current and future stellar spectroscopic surveys producing abundances for Milky-Way stars on an industrial scale.Aims. We present an unprecedented effort to create a homogeneous common line list, which was used by several abundance analysis groups using different radiative transfer codes 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 at the CDS.Methods. 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 a hyperfine structure or isotopic splitting, a concerted effort has been made to collate the necessary data for the individual line components. Synthetic stellar spectra calculated for the Sun and Arcturus were used to assess the blending properties of the lines. We also performed adetailed investigation of available data for line broadening due to collisions with neutral hydrogen atoms.Results. Among a subset of over 1300 lines of 35 elements in the wavelength ranges from 475 to 685 nm and from 850 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 possible. We recommend avoiding lines of neutral species for which these are not available. Theoretical broadening data by R.L. Kurucz should be used for ScII, TiII, and YII lines; additionally, for ionised rare-earth species

Published
2021
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108. The Gaia-ESO Survey : Calibrating the lithium-age relation with open clusters and associations I. Cluster age range and initial membership selections

Author

Gutierrez Albarran, M. L., Montes, D., Gomez Garrido, M., Tabernero, H. M., Gonzalez Hernandez, J. , I, Marfil, E., Frasca, A., Lanzafame, A. C., Klutsch, A., Franciosini, E., Randich, S., Smiljanic, R., Korn, Andreas, Gilmore, G., Alfaro, E. J., Baratella, M., Bayo, A., Bensby, T., Bonito, R., Carraro, G., Delgado Mena, E., Feltzing, S., Gonneau, A., Heiter, Ulrike, Hourihane, A., Jimenez Esteban, F., Jofre, P., Masseron, T., Monaco, L., Morbidelli, L., Prisinzano, L., Roccatagliata, V, Sousa, S., Van der Swaelmen, M., Worley, C. C., Zaggia, S., Gutierrez Albarran, M. L., Montes, D., Gomez Garrido, M., Tabernero, H. M., Gonzalez Hernandez, J. , I, Marfil, E., Frasca, A., Lanzafame, A. C., Klutsch, A., Franciosini, E., Randich, S., Smiljanic, R., Korn, Andreas, Gilmore, G., Alfaro, E. J., Baratella, M., Bayo, A., Bensby, T., Bonito, R., Carraro, G., Delgado Mena, E., Feltzing, S., Gonneau, A., Heiter, Ulrike, Hourihane, A., Jimenez Esteban, F., Jofre, P., Masseron, T., Monaco, L., Morbidelli, L., Prisinzano, L., Roccatagliata, V, Sousa, S., Van der Swaelmen, M., Worley, C. C., and Zaggia, S.

Abstract

Context: Previous studies of open clusters have shown that lithium depletion is not only strongly age dependent but also shows a complex pattern with other parameters that is not yet understood. For pre- and main-sequence late-type stars, these parameters include metallicity, mixing mechanisms, convection structure, rotation, and magnetic activity. Aims: We perform a thorough membership analysis for a large number of stars observed within the Gaia-ESO survey (GES) in the field of 20 open clusters, ranging in age from young clusters and associations, to intermediate-age and old open clusters. Methods: Based on the parameters derived from the GES spectroscopic observations, we obtained lists of candidate members for each of the clusters in the sample by deriving radial velocity distributions and studying the position of the kinematic selections in the EW(Li)-versus-T-eff plane to obtain lithium members. We used gravity indicators to discard field contaminants and studied [Fe/H] metallicity to further confirm the membership of the candidates. We also made use of studies using recent data from the Gaia DR1 and DR2 releases to assess our member selections. Results: We identified likely member candidates for the sample of 20 clusters observed in GES (iDR4) with UVES and GIRAFFE, and conducted a comparative study that allowed us to characterize the properties of these members as well as identify field contaminant stars, both lithium-rich giants and non-giant outliers. Conclusions: This work is the first step towards the calibration of the lithium-age relation and its dependence on other GES parameters. During this project we aim to use this relation to infer the ages of GES field stars, and identify their potential membership to young associations and stellar kinematic groups of different ages.

Published
2020
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110. Atomic data for the Gaia-ESO Survey

Author

Heiter, U., primary, Lind, K., additional, Bergemann, M., additional, Asplund, M., additional, Mikolaitis, Š., additional, Barklem, P. S., additional, Masseron, T., additional, de Laverny, P., additional, Magrini, L., additional, Edvardsson, B., additional, Jönsson, H., additional, Pickering, J. C., additional, Ryde, N., additional, Bayo Arán, A., additional, Bensby, T., additional, Casey, A. R., additional, Feltzing, S., additional, Jofré, P., additional, Korn, A. J., additional, Pancino, E., additional, Damiani, F., additional, Lanzafame, A., additional, Lardo, C., additional, Monaco, L., additional, Morbidelli, L., additional, Smiljanic, R., additional, Worley, C., additional, Zaggia, S., additional, Randich, S., additional, and Gilmore, G. F., additional

Published
2021
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111. The Gaia-ESO Survey: Calibrating the lithium–age relation with open clusters and associations

Author

Gutiérrez Albarrán, M. L., primary, Montes, D., additional, Gómez Garrido, M., additional, Tabernero, H. M., additional, González Hernández, J. I., additional, Marfil, E., additional, Frasca, A., additional, Lanzafame, A. C., additional, Klutsch, A., additional, Franciosini, E., additional, Randich, S., additional, Smiljanic, R., additional, Korn, A. J., additional, Gilmore, G., additional, Alfaro, E. J., additional, Baratella, M., additional, Bayo, A., additional, Bensby, T., additional, Bonito, R., additional, Carraro, G., additional, Delgado Mena, E., additional, Feltzing, S., additional, Gonneau, A., additional, Heiter, U., additional, Hourihane, A., additional, Jiménez Esteban, F., additional, Jofre, P., additional, Masseron, T., additional, Monaco, L., additional, Morbidelli, L., additional, Prisinzano, L., additional, Roccatagliata, V., additional, Sousa, S., additional, Van der Swaelmen, M., additional, Worley, C. C., additional, and Zaggia, S., additional

Published
2020
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113. The Gaia-ESO Survey: A new diagnostic for accretion and outflow activity in the young cluster NGC 2264

Author

Bonito, R., primary, Prisinzano, L., additional, Venuti, L., additional, Damiani, F., additional, Micela, G., additional, Sacco, G., additional, Traven, G., additional, Biazzo, K., additional, Sbordone, L., additional, Masseron, T., additional, Zwitter, T., additional, Gonneau, A., additional, Bayo, A., additional, Roccatagliata, V., additional, Randich, S., additional, Vink, J. S., additional, Jofre, P., additional, Flaccomio, E., additional, Magrini, L., additional, Carraro, G., additional, Morbidelli, L., additional, Frasca, A., additional, Monaco, L., additional, Rigliaco, E., additional, Worley, C., additional, Hourihane, A., additional, Gilmore, G., additional, Franciosini, E., additional, Lewis, J., additional, and Koposov, S., additional

Published
2020
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114. TheGaia-ESO Survey: detection and characterisation of single-line spectroscopic binaries

Author

Merle, T., primary, Van der Swaelmen, M., additional, Van Eck, S., additional, Jorissen, A., additional, Jackson, R. J., additional, Traven, G., additional, Zwitter, T., additional, Pourbaix, D., additional, Klutsch, A., additional, Sacco, G., additional, Blomme, R., additional, Masseron, T., additional, Gilmore, G., additional, Randich, S., additional, Badenes, C., additional, Bayo, A., additional, Bensby, T., additional, Bergemann, M., additional, Biazzo, K., additional, Damiani, F., additional, Feuillet, D., additional, Frasca, A., additional, Gonneau, A., additional, Jeffries, R. D., additional, Jofré, P., additional, Morbidelli, L., additional, Mowlavi, N., additional, Pancino, E., additional, and Prisinzano, L., additional

Published
2020
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115. Homogeneous analysis of globular clusters from the APOGEE survey with the BACCHUS code

Author

Masseron, T., García-Hernández, D., Mészáros, Sz., Zamora, O., Dell’Agli, F., Allende Prieto, C., Edvardsson, B., Shetrone, M., PLEZ, Bertrand, Fernández-Trincado, J., Cunha, K., Jonsson, H., Geisler, D., Beers, T., Cohen, R., Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)

Subjects
[SDU]Sciences of the Universe [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2019
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116. ExoMol molecular line lists − XXXIII. The spectrum of Titanium Oxide

Author

McKemmish, LK, Masseron, T, Hoeijmakers, HJ, Pérez-Mesa, V, Grimm, SL, Yurchenko, SN, Tennyson, J, McKemmish, LK, Masseron, T, Hoeijmakers, HJ, Pérez-Mesa, V, Grimm, SL, Yurchenko, SN, and Tennyson, J

Abstract

© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. Accurate line lists are crucial for correctly modelling a variety of astrophysical phenomena, including stellar photospheres and the atmospheres of extrasolar planets. This paper presents a new line database TOTO for the main isotopologues of titanium oxide (TiO): 46Ti16O, 47Ti16O,48Ti16O, 49Ti16O, and 50Ti16O. The 48Ti16O line list contains transitions with wave-numbers up to 30 000 cm−1, i.e. longwards of 0.33 μm. The TOTO line list includes all dipole-allowed transitions between 13 low-lying electronic states (X3∆, a 1∆, d 1∑+, E 3∏, A 3Φ, B 3∏, C 3∆, b 1∏, c 1Φ, f 1∆, e 1∑+). Ab initio potential energy curves (PECs) are computed at the icMRCI level and combined with spin–orbit and other coupling curves. These PECs and couplings are iteratively refined to match known empirical energy levels. Accurate line intensities are generated using ab initio dipole moment curves. The TOTO line lists are appropriate for temperatures below 5000 K and contain 30 million transitions for 48Ti16O; it is made available in electronic form via the CDS data centre and via www.exomol.com. Tests of the line lists show greatly improved agreement with observed spectra for objects such as M-dwarfs GJ876 and GL581.

Published
2019

118. The Gaia-ESO survey: Calibrating a relationship between age and the [C/N] abundance ratio with open clusters

Author

Casali, G., primary, Magrini, L., additional, Tognelli, E., additional, Jackson, R., additional, Jeffries, R. D., additional, Lagarde, N., additional, Tautvaišienė, G., additional, Masseron, T., additional, Degl’Innocenti, S., additional, Prada Moroni, P. G., additional, Kordopatis, G., additional, Pancino, E., additional, Randich, S., additional, Feltzing, S., additional, Sahlholdt, C., additional, Spina, L., additional, Friel, E., additional, Roccatagliata, V., additional, Sanna, N., additional, Bragaglia, A., additional, Drazdauskas, A., additional, Mikolaitis, Š., additional, Minkevičiūtė, R., additional, Stonkutė, E., additional, Chorniy, Y., additional, Bagdonas, V., additional, Jimenez-Esteban, F., additional, Martell, S., additional, Van der Swaelmen, M., additional, Gilmore, G., additional, Vallenari, A., additional, Bensby, T., additional, Koposov, S. E., additional, Korn, A., additional, Worley, C., additional, Smiljanic, R., additional, Bergemann, M., additional, Carraro, G., additional, Damiani, F., additional, Prisinzano, L., additional, Bonito, R., additional, Franciosini, E., additional, Gonneau, A., additional, Hourihane, A., additional, Jofre, P., additional, Lewis, J., additional, Morbidelli, L., additional, Sacco, G., additional, Sousa, S. G., additional, Zaggia, S., additional, Lanzafame, A. C., additional, Heiter, U., additional, Frasca, A., additional, and Bayo, A., additional

Published
2019
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119. H-band discovery of additional second-generation stars in the Galactic bulge globular cluster NGC 6522 as observed by APOGEE and Gaia

Author

Fernández-Trincado, J. G., primary, Zamora, O., additional, Souto, Diogo, additional, Cohen, R. E., additional, Dell’Agli, F., additional, García-Hernández, D. A., additional, Masseron, T., additional, Schiavon, R. P., additional, Mészáros, Sz., additional, Cunha, K., additional, Hasselquist, S., additional, Shetrone, M., additional, Schiappacasse Ulloa, J., additional, Tang, B., additional, Geisler, D., additional, Schleicher, D. R. G., additional, Villanova, S., additional, Mennickent, R. E., additional, Minniti, D., additional, Alonso-García, J., additional, Manchado, A., additional, Beers, T. C., additional, Sobeck, J., additional, Zasowski, G., additional, Schultheis, M., additional, Majewski, S. R., additional, Rojas-Arriagada, A., additional, Almeida, A., additional, Santana, F., additional, Oelkers, R. J., additional, Longa-Peña, P., additional, Carrera, R., additional, Burgasser, A. J., additional, Lane, R. R., additional, Roman-Lopes, A., additional, Ivans, I. I., additional, and Hearty, F. R., additional

Published
2019
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120. High-resolution spectroscopy of Boyajian’s star during optical dimming events

Author

Martínez González, M J, primary, González-Fernández, C, additional, Asensio Ramos, A, additional, Socas-Navarro, H, additional, Westendorp Plaza, C, additional, Boyajian, T S, additional, Wright, J T, additional, Collier Cameron, A, additional, González Hernández, J I, additional, Holgado, G, additional, Kennedy, G M, additional, Masseron, T, additional, Molinari, E, additional, Saario, J, additional, Simón-Díaz, S, additional, and Toledo-Padrón, B, additional

Published
2019
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122. J-PLUS: Identification of low-metallicity stars with artificial neural networks using SPHINX

Author

Whitten, D. D., primary, Placco, V. M., additional, Beers, T. C., additional, Chies-Santos, A. L., additional, Bonatto, C., additional, Varela, J., additional, Cristóbal-Hornillos, D., additional, Ederoclite, A., additional, Masseron, T., additional, Lee, Y. S., additional, Akras, S., additional, Borges Fernandes, M., additional, Caballero, J. A., additional, Cenarro, A. J., additional, Coelho, P., additional, Costa-Duarte, M. V., additional, Daflon, S., additional, Dupke, R. A., additional, Lopes de Oliveira, R., additional, López-Sanjuan, C., additional, Marín-Franch, A., additional, Mendes de Oliveira, C., additional, Moles, M., additional, Orsi, A. A., additional, Rossi, S., additional, Sodré, L., additional, and Vázquez Ramió, H., additional

Published
2019
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123. TheGaia-ESO Survey: impact of extra mixing on C and N abundances of giant stars

Author

Lagarde, N., primary, Reylé, C., additional, Robin, A. C., additional, Tautvaišienė, G., additional, Drazdauskas, A., additional, Mikolaitis, Š., additional, Minkevičiūtė, R., additional, Stonkutė, E., additional, Chorniy, Y., additional, Bagdonas, V., additional, Miglio, A., additional, Nasello, G., additional, Gilmore, G., additional, Randich, S., additional, Bensby, T., additional, Bragaglia, A., additional, Flaccomio, E., additional, Francois, P., additional, Korn, A. J., additional, Pancino, E., additional, Smiljanic, R., additional, Bayo, A., additional, Carraro, G., additional, Costado, M. T., additional, Jiménez-Esteban, F., additional, Jofré, P., additional, Martell, S. L., additional, Masseron, T., additional, Monaco, L., additional, Morbidelli, L., additional, Sbordone, L., additional, Sousa, S. G., additional, and Zaggia, S., additional

Published
2018
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124. The Gaia-ESO Survey : matching chemodynamical simulations to observations of the Milky Way

Author

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, Andreas, 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., Zaggia, S., 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, Andreas, 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.

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 Milky Way-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.

Published
2018
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125. The Gaia-ESO Survey: The origin and evolution of s-process elements

Author

European Research Council, Leverhulme Trust, Istituto Nazionale di Astrofisica, European Science Foundation, Ministerio de Economía y Competitividad (España), European Commission, Fundação para a Ciência e a Tecnologia (Portugal), Science and Technology Facilities Council (UK), Ministerio de Economía, Fomento y Turismo (Chile), Ministry of Science and Higher Education (Poland), Knut and Alice Wallenberg Foundation, Magrini, L., Spina, Lorenzo, Randich, S., Friel, E., Kordopatis, G., Worley, C., Pancino, E., Bragaglia, A., Donati, P., Tautvaišienė, G., Bagdonas, V., Delgado-Mena, E., Adibekyan, V., Sousa, S. G., Jiménez-Esteban, Francisco M., Sanna, N., Roccatagliata, V., Bonito, R., Sbordone, L., Duffau, S., Gilmore, Gerry, Feltzing, S., Jeffries, R.D., Vallenari, A., Alfaro, Emilio J., Bensby, T., Francois, P., Koposov, S., Korn, A.J., Recio-Blanco, A., Smiljanic, R., Bayo, A., Carraro, G., Casey, A. R., Costado, M. T., Damiani, F., Franciosini, E., Frasca, A., Hourihane, A., Jofré, P., de Laverny, P., Lewis, J., Masseron, T., Monaco, L., Morbidelli, L., Prisinzano, L., Sacco, G., Zaggia, S., European Research Council, Leverhulme Trust, Istituto Nazionale di Astrofisica, European Science Foundation, Ministerio de Economía y Competitividad (España), European Commission, Fundação para a Ciência e a Tecnologia (Portugal), Science and Technology Facilities Council (UK), Ministerio de Economía, Fomento y Turismo (Chile), Ministry of Science and Higher Education (Poland), Knut and Alice Wallenberg Foundation, Magrini, L., Spina, Lorenzo, Randich, S., Friel, E., Kordopatis, G., Worley, C., Pancino, E., Bragaglia, A., Donati, P., Tautvaišienė, G., Bagdonas, V., Delgado-Mena, E., Adibekyan, V., Sousa, S. G., Jiménez-Esteban, Francisco M., Sanna, N., Roccatagliata, V., Bonito, R., Sbordone, L., Duffau, S., Gilmore, Gerry, Feltzing, S., Jeffries, R.D., Vallenari, A., Alfaro, Emilio J., Bensby, T., Francois, P., Koposov, S., Korn, A.J., Recio-Blanco, A., Smiljanic, R., Bayo, A., Carraro, G., Casey, A. R., Costado, M. T., Damiani, F., Franciosini, E., Frasca, A., Hourihane, A., Jofré, P., de Laverny, P., Lewis, J., Masseron, T., Monaco, L., Morbidelli, L., Prisinzano, L., Sacco, G., and Zaggia, S.

Abstract

Context. Several works have found an increase of the abundances of the s-process neutron-capture elements in the youngest Galactic stellar populations. These trends provide important constraints on stellar and Galactic evolution and they need to be confirmed with large and statistically significant samples of stars spanning wide age and distance intervals. Aims. We aim to trace the abundance patterns and the time evolution of five s-process elements - two belonging to the first peak, Y and Zr, and three belonging to the second peak, Ba, La, and Ce - using the Gaia-ESO IDR5 results for open clusters and disc stars. Methods. From the UVES spectra of cluster member stars, we determined the average composition of clusters with ages >0.1 Gyr. We derived statistical ages and distances of field stars, and we separated them into thin and thick disc populations. We studied the time-evolution and dependence on metallicity of abundance ratios using open clusters and field stars whose parameters and abundances were derived in a homogeneous way. Results. Using our large and homogeneous sample of open clusters, thin and thick disc stars, spanning an age range larger than 10 Gyr, we confirm an increase towards young ages of s-process abundances in the solar neighbourhood. These trends are well defined for open clusters and stars located nearby the solar position and they may be explained by a late enrichment due to significant contribution to the production of these elements from long-living low-mass stars. At the same time, we find a strong dependence of the s-process abundance ratios on the Galactocentric distance and on the metallicity of the clusters and field stars. Conclusions. Our results, derived from the largest and most homogeneous sample of s-process abundances in the literature, confirm the growth with decreasing stellar ages of the s-process abundances in both field and open cluster stars. At the same time, taking advantage of the abundances of open clusters located i

Published
2018

126. The Gaia-ESO survey: Matching chemodynamical simulations to observations of the Milky Way

Author

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, Thompson, B. B., Few, C. G., Bergemann, Maria, Gibson, Brad K., MacFarlane, B. A., Serenelli, Aldo, Gilmore, Gerry, Randich, S., Vallenari, A., Alfaro, Emilio J., Bensby, T., Francois, P., Korn, A.J., Bayo, A., Carraro, Giovanni, Casey, Andrew R., Costado, M. T., Donati, P., Franciosini, E., Frasca, A., Hourihane, A., Jofré, P, Hill, V., Heiter, Ulrike, Koposov, Sergey E., Lanzafame, A., Lardo, C., de Laverny, P., Lewis, J., Magrini, Laura, Marconi, G., Masseron, T., Monaco, L., Morbidelli, L., Pancino, E., Prisinzano, L., Recio-Blanco, A., Sacco, G., Sousa, S. G., Tautvaišiene, G., Worley, C. C., Zaggia, S., 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, Thompson, B. B., Few, C. G., Bergemann, Maria, Gibson, Brad K., MacFarlane, B. A., Serenelli, Aldo, Gilmore, Gerry, Randich, S., Vallenari, A., Alfaro, Emilio J., Bensby, T., Francois, P., Korn, A.J., Bayo, A., Carraro, Giovanni, Casey, Andrew R., Costado, M. T., Donati, P., Franciosini, E., Frasca, A., Hourihane, A., Jofré, P, Hill, V., Heiter, Ulrike, Koposov, Sergey E., Lanzafame, A., Lardo, C., de Laverny, P., Lewis, J., Magrini, Laura, Marconi, G., Masseron, T., Monaco, L., Morbidelli, L., Pancino, E., Prisinzano, L., Recio-Blanco, A., Sacco, G., Sousa, S. G., Tautvaišiene, G., Worley, C. C., and Zaggia, S.

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).

Published
2018

127. The Gaia -ESO Survey: Double-, triple-, and quadruple-line spectroscopic binary candidates

Author

Merle, T. Van Eck, S. Jorissen, A. Van Der Swaelmen, M. Masseron, T. Zwitter, T. Hatzidimitriou, D. Klutsch, A. Pourbaix, D. Blomme, R. Worley, C.C. Sacco, G. Lewis, J. Abia, C. Traven, G. Sordo, R. Bragaglia, A. Smiljanic, R. Pancino, E. Damiani, F. Hourihane, A. Gilmore, G. Randich, S. Koposov, S. Casey, A. Morbidelli, L. Franciosini, E. Magrini, L. Jofre, P. Costado, M.T. Jeffries, R.D. Bergemann, M. Lanzafame, A.C. Bayo, A. Carraro, G. Flaccomio, E. Monaco, L. Zaggia, S.

Abstract

Context. The Gaia-ESO Survey (GES) is a large spectroscopic survey that provides a unique opportunity to study the distribution of spectroscopic multiple systems among different populations of the Galaxy. Aims. Our aim is to detect binarity/multiplicity for stars targeted by the GES from the analysis of the cross-correlation functions (CCFs) of the GES spectra with spectral templates. Methods. We developed a method based on the computation of the CCF successive derivatives to detect multiple peaks and determine their radial velocities, even when the peaks are strongly blended. The parameters of the detection of extrema (doe) code have been optimized for each GES GIRAFFE and UVES setup to maximize detection. The doe code therefore allows to automatically detect multiple line spectroscopic binaries (SBn, n ≥ 2). Results. We apply this method on the fourth GES internal data release and detect 354 SBn candidates (342 SB2, 11 SB3, and even one SB4), including only nine SBs known in the literature. This implies that about 98% of these SBn candidates are new because of their faint visual magnitude that can reach V = 19. Visual inspection of the SBn candidate spectra reveals that the most probable candidates have indeed a composite spectrum. Among the SB2 candidates, an orbital solution could be computed for two previously unknown binaries: CNAME 06404608+0949173 (known as V642 Mon) in NGC 2264 and CNAME 19013257-0027338 in Berkeley 81 (Be 81). A detailed analysis of the unique SB4 (four peaks in the CCF) reveals that CNAME 08414659-5303449 (HD 74438) in the open cluster IC 2391 is a physically bound stellar quadruple system. The SB candidates belonging to stellar clusters are reviewed in detail to discard false detections. We suggest that atmospheric parameters should not be used for these system components; SB-specific pipelines should be used instead. Conclusions. Our implementation of an automatic detection of spectroscopic binaries within the GES has allowed the efficient discovery of many new multiple systems. With the detection of the SB1 candidates that will be the subject of a forthcoming paper, the study of the statistical and physical properties of the spectroscopic multiple systems will soon be possible for the entire GES sample. © ESO 2017.

Published
2017

128. When binaries keep track of recent nucleosynthesis

Author

Karinkuzhi, D., primary, Van Eck, S., additional, Jorissen, A., additional, Goriely, S., additional, Siess, L., additional, Merle, T., additional, Escorza, A., additional, Van der Swaelmen, M., additional, Boffin, H. M. J., additional, Masseron, T., additional, Shetye, S., additional, and Plez, B., additional

Published
2018
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129. The Gaia-ESO Survey: the origin and evolution of s-process elements

Author

Magrini, L., primary, Spina, L., additional, Randich, S., additional, Friel, E., additional, Kordopatis, G., additional, Worley, C., additional, Pancino, E., additional, Bragaglia, A., additional, Donati, P., additional, Tautvaišienė, G., additional, Bagdonas, V., additional, Delgado-Mena, E., additional, Adibekyan, V., additional, Sousa, S. G., additional, Jiménez-Esteban, F. M., additional, Sanna, N., additional, Roccatagliata, V., additional, Bonito, R., additional, Sbordone, L., additional, Duffau, S., additional, Gilmore, G., additional, Feltzing, S., additional, Jeffries, R. D., additional, Vallenari, A., additional, Alfaro, E. J., additional, Bensby, T., additional, Francois, P., additional, Koposov, S., additional, Korn, A. J., additional, Recio-Blanco, A., additional, Smiljanic, R., additional, Bayo, A., additional, Carraro, G., additional, Casey, A. R., additional, Costado, M. T., additional, Damiani, F., additional, Franciosini, E., additional, Frasca, A., additional, Hourihane, A., additional, Jofré, P., additional, de Laverny, P., additional, Lewis, J., additional, Masseron, T., additional, Monaco, L., additional, Morbidelli, L., additional, Prisinzano, L., additional, Sacco, G., additional, and Zaggia, S., additional

Published
2018
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130. The Gaia-ESO Survey: properties of newly discovered Li-rich giants

Author

Smiljanic, R., primary, Franciosini, E., additional, Bragaglia, A., additional, Tautvaišienė, G., additional, Fu, X., additional, Pancino, E., additional, Adibekyan, V., additional, Sousa, S. G., additional, Randich, S., additional, Montalbán, J., additional, Pasquini, L., additional, Magrini, L., additional, Drazdauskas, A., additional, García, R. A., additional, Mathur, S., additional, Mosser, B., additional, Régulo, C., additional, de Assis Peralta, R., additional, Hekker, S., additional, Feuillet, D., additional, Valentini, M., additional, Morel, T., additional, Martell, S., additional, Gilmore, G., additional, Feltzing, S., additional, Vallenari, A., additional, Bensby, T., additional, Korn, A. J., additional, Lanzafame, A. C., additional, Recio-Blanco, A., additional, Bayo, A., additional, Carraro, G., additional, Costado, M. T., additional, Frasca, A., additional, Jofré, P., additional, Lardo, C., additional, de Laverny, P., additional, Lind, K., additional, Masseron, T., additional, Monaco, L., additional, Morbidelli, L., additional, Prisinzano, L., additional, Sbordone, L., additional, and Zaggia, S., additional

Published
2018
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131. A Chemical and Kinematical Analysis of the Intermediate-age Open Cluster IC 166 from APOGEE and Gaia DR2

Author

Schiappacasse-Ulloa, J., primary, Tang, B., additional, Fernández-Trincado, J. G., additional, Zamora, O., additional, Geisler, D., additional, Frinchaboy, P., additional, Schultheis, M., additional, Dell’Agli, F., additional, Villanova, S., additional, Masseron, T., additional, Mészáros, Sz., additional, Souto, D., additional, Hasselquist, S., additional, Cunha, K., additional, Smith, V. V., additional, García-Hernández, D. A., additional, Vieira, K., additional, Robin, A. C., additional, Minniti, D., additional, Zasowski, G., additional, Moreno, E., additional, Pérez-Villegas, A., additional, Lane, R. R., additional, Ivans, I. I., additional, Pan, K., additional, Nitschelm, C., additional, Santana, F. A., additional, Carrera, R., additional, and Roman-Lopes, A., additional

Published
2018
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134. TheGaia-ESO Survey: double-, triple-, and quadruple-line spectroscopic binary candidates

Author

Merle, T., primary, Van Eck, S., additional, Jorissen, A., additional, Van der Swaelmen, M., additional, Masseron, T., additional, Zwitter, T., additional, Hatzidimitriou, D., additional, Klutsch, A., additional, Pourbaix, D., additional, Blomme, R., additional, Worley, C. C., additional, Sacco, G., additional, Lewis, J., additional, Abia, C., additional, Traven, G., additional, Sordo, R., additional, Bragaglia, A., additional, Smiljanic, R., additional, Pancino, E., additional, Damiani, F., additional, Hourihane, A., additional, Gilmore, G., additional, Randich, S., additional, Koposov, S., additional, Casey, A., additional, Morbidelli, L., additional, Franciosini, E., additional, Magrini, L., additional, Jofre, P., additional, Costado, M. T., additional, Jeffries, R. D., additional, Bergemann, M., additional, Lanzafame, A. C., additional, Bayo, A., additional, Carraro, G., additional, Flaccomio, E., additional, Monaco, L., additional, and Zaggia, S., additional

Published
2017
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135. Gaia FGK benchmark stars : opening the black box of stellar element abundance determination

Author

Jofre, P., Heiter, U., Worley, C. C., Blanco-Cuaresma, S., Soubiran, C., Masseron, T., Hawkins, K., Adibekyan, V., Buder, S., Casamiquela, L., Gilmore, G., Hourihane, A., Tabernero, H., Jofre, P., Heiter, U., Worley, C. C., Blanco-Cuaresma, S., Soubiran, C., Masseron, T., Hawkins, K., Adibekyan, V., Buder, S., Casamiquela, L., Gilmore, G., Hourihane, A., and Tabernero, H.

Abstract

Gaia and its complementary spectroscopic surveys combined will yield the most comprehensive database of kinematic and chemical information of stars in the Milky Way. The Gaia FGK benchmark stars play a central role in this matter as they are calibration pillars for the atmospheric parameters and chemical abundances for various surveys. The spectroscopic analyses of the benchmark stars are done by combining different methods, and the results will be affected by the systematic uncertainties inherent in each method. In this paper, we explore some of these systematic uncertainties. We determined line abundances of Ca, Cr, Mn and Co for four benchmark stars using six different methods. We changed the default input parameters of the different codes in a systematic way and found, in some cases, significant differences between the results. Since there is no consensus on the correct values for many of these default parameters, we urge the community to raise discussions towards standard input parameters that could alleviate the difference in abundances obtained by different methods. In this work, we provide quantitative estimates of uncertainties in elemental abundances due to the effect of differing technical assumptions in spectrum modelling.

Published
2017
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136. MARVEL Analysis of the Measured High-resolution Rovibronic Spectra of 48Ti16O

Author

McKemmish, LK, Masseron, T, Sheppard, S, Sandeman, E, Schofield, Z, Furtenbacher, T, Császár, AG, Tennyson, J, Sousa-Silva, C, McKemmish, LK, Masseron, T, Sheppard, S, Sandeman, E, Schofield, Z, Furtenbacher, T, Császár, AG, Tennyson, J, and Sousa-Silva, C

Abstract

Accurate, experimental rovibronic energy levels, with associated labels and uncertainties, are reported for 11 lowlying electronic states of the diatomic 48Ti16O molecule, determined using the MARVEL (Measured Active Rotational-Vibrational Energy Levels) algorithm. All levels are based on lines corresponding to critically reviewed and validated high-resolution experimental spectra taken from 24 literature sources. The transition data are in the 2-22,160 cm-1 region. Out of the 49,679 measured transitions, 43,885 are triplet-triplet, 5710 are singlet-singlet, and 84 are triplet-singlet transitions. A careful analysis of the resulting experimental spectroscopic network (SN) allows 48,590 transitions to be validated. The transitions determine 93 vibrational band origins of 48Ti16O, including 71 triplet and 22 singlet ones. There are 276 (73) triplet-triplet (singlet-singlet) band-heads derived from MARVEL experimental energies, 123(38) of which have never been assigned in low- or high-resolution experiments. The highest J value, where J stands for the total angular momentum, for which an energy level is validated is 163. The number of experimentally derived triplet and singlet 48Ti16O rovibrational energy levels is 8682 and 1882, respectively. The lists of validated lines and levels for 48Ti16O are deposited in the supporting information to this paper.

Published
2017

137. VizieR Online Data Catalog: Gaia FGK stars: low-metallicities candidates (Hawkins+, 2016)

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., Worley, C. C., and Pomies, Marie-Paule

Subjects
Stars: K-type, Abundances: [Fe/H], [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Stars: G-type, Stars: F-type
Abstract

The line-by-line Fe abundance of the metal-poor candidate Gaia FGK benchmark stars. This table also includes the line-by-line equivalent widths (EW) and NLTE corrections.(11 data files).

Published
2016

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

Author

Thompson, B. B., primary, Few, C. G., additional, Bergemann, M., additional, Gibson, B. K., additional, MacFarlane, B. A., additional, Serenelli, A., additional, Gilmore, G., additional, Randich, S., additional, Vallenari, A., additional, Alfaro, E. J., additional, Bensby, T., additional, Francois, P., additional, Korn, A. J., additional, Bayo, A., additional, Carraro, G., additional, Casey, A. R., additional, Costado, M. T., additional, Donati, P., additional, Franciosini, E., additional, Frasca, A., additional, Hourihane, A., additional, Jofré, P., additional, Hill, V., additional, Heiter, U., additional, Koposov, S. E., additional, Lanzafame, A., additional, Lardo, C., additional, de Laverny, P., additional, Lewis, J., additional, Magrini, L., additional, Marconi, G., additional, Masseron, T., additional, Monaco, L., additional, Morbidelli, L., additional, Pancino, E., additional, Prisinzano, L., additional, Recio-Blanco, A., additional, Sacco, G., additional, Sousa, S. G., additional, Tautvaišienė, G., additional, Worley, C. C., additional, and Zaggia, S., additional

Published
2017
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139. Atypical Mg-poor Milky Way Field Stars with Globular Cluster Second-generation-like Chemical Patterns

Author

Fernández-Trincado, J. G., primary, Zamora, O., additional, García-Hernández, D. A., additional, Souto, Diogo, additional, Dell’Agli, F., additional, Schiavon, R. P., additional, Geisler, D., additional, Tang, B., additional, Villanova, S., additional, Hasselquist, Sten, additional, Mennickent, R. E., additional, Cunha, Katia, additional, Shetrone, M., additional, Prieto, Carlos Allende, additional, Vieira, K., additional, Zasowski, G., additional, Sobeck, J., additional, Hayes, C. R., additional, Majewski, S. R., additional, Placco, V. M., additional, Beers, T. C., additional, Schleicher, D. R. G., additional, Robin, A. C., additional, Mészáros, Sz., additional, Masseron, T., additional, Pérez, Ana E. García, additional, Anders, F., additional, Meza, A., additional, Alves-Brito, A., additional, Carrera, R., additional, Minniti, D., additional, Lane, R. R., additional, Fernández-Alvar, E., additional, Moreno, E., additional, Pichardo, B., additional, Pérez-Villegas, A., additional, Schultheis, M., additional, Roman-Lopes, A., additional, Fuentes, C. E., additional, Nitschelm, C., additional, Harding, P., additional, Bizyaev, D., additional, Pan, K., additional, Oravetz, D., additional, Simmons, A., additional, Ivans, Inese I., additional, Blanco-Cuaresma, S., additional, Hernández, J., additional, Alonso-García, J., additional, Valenzuela, O., additional, and Chanamé, J., additional

Published
2017
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142. Gaia FGK benchmark stars : new candidates at low metallicities

Author

Hawkins, K., Jofre, P., Heiter, Ulrike, Soubiran, C., Blanco-Cuaresma, S., Casagrande, L., Gilmore, G., Lind, K., Magrini, L., Masseron, T., Pancino, E., Randich, S., Worley, C. C., Hawkins, K., Jofre, P., Heiter, Ulrike, Soubiran, C., Blanco-Cuaresma, S., Casagrande, L., Gilmore, G., Lind, K., Magrini, L., Masseron, T., Pancino, E., Randich, S., and Worley, C. C.

Abstract

Context. 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 has up to five metal-poor stars but no recommended stars within 2.0 < [Fe/H] < -1.0 dex. However, this metallicity regime is critical to calibrate properly. Aims. In this paper, we aim to add candidate Gaia benchmark stars inside of this metal-poor gap. We began with a sample of 21 metal poor stars which was reduced to 10 stars by requiring accurate photometry and parallaxes, and high-resolution archival spectra. Methods. The procedure used to determine the stellar parameters was similar to the previous works in this series for consistency. The difference was to homogeneously determine the angular diameter and effective temperature (T-eff) of all of our stars using the Infrared Flux Method utilizing multi-band photometry. The surface gravity (log g) was determined through fitting stellar evolutionary tracks. The [Fe/H] was determined using four different spectroscopic methods fixing the T-eff and log g from the values determined independent of spectroscopy. Results. We discuss, star-by-star, the quality of each parameter including how it compares to literature, how it compares to a spectroscopic run where all parameters are free, and whether Fe I ionisation-excitation balance is achieved. Conclusions. From the 10 stars, we recommend a sample of five new metal-poor benchmark candidate stars which have consistent T-eff, log g, and [Fe/H] determined through several means. These stars, which are within -1.3 < [Fe/H] < 1.0, can be used for calibration and validation purpose of stellar parameter and abundance pipelines and should be of h

Published
2016
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143. HE 0017+0055:A probable pulsating CEMP-rs star and long-period binary

Author

Jorissen, A., Hansen, T., Van Eck, S., Andersen, Johannes, Nordström, Birgitta, Siess, L., Torres, G., Masseron, T., Van Winckel, H., Jorissen, A., Hansen, T., Van Eck, S., Andersen, Johannes, Nordström, Birgitta, Siess, L., Torres, G., Masseron, T., and Van Winckel, H.

Published
2016

144. Binary properties of CH and carbon-enhanced metal-poor stars

Author

Jorissen, A., Van Eck, S., Van Winckel, H., Merle, T., Boffin, H. M. J., Andersen, Johannes, Nordström, Birgitta, Udry, S., Masseron, T., Lenaerts, L., Waelkens, C., Jorissen, A., Van Eck, S., Van Winckel, H., Merle, T., Boffin, H. M. J., Andersen, Johannes, Nordström, Birgitta, Udry, S., Masseron, T., Lenaerts, L., and Waelkens, C.

Published
2016

145. VizieR Online Data Catalog: Gaia FGK benchmark stars: metallicity (Jofre+, 2014)

Author

Jofre, P., Heiter, U., Soubiran, C., Blanco-Cuaresma, S., Pancino, E., Bergemann, M., Cantat-Gaudin, T., Gonzalez Hernandez, J. I., Hill, V., Lardo, C., de Laverny, P., Lind, K., Magrini, L., Masseron, T., Montes, D., Mucciarelli, A., Nordlander, T., Recio Blanco, A., Sobeck, J., Sordo, R., Sousa, S. G., Tabernero, H., Vallenari, A., van Eck, S., and Pomies, Marie-Paule

Subjects
Abundances: [Fe/H], [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Stars: standard, Equivalent widths, [PHYS.ASTR.IM] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Spectroscopy
Abstract

The metallicity of the Gaia FGK benchmark stars is determined by combining 6 methods. The Tables indicate the iron abundance and equivalent width determined for each star, iron line and method. (5 data files).

Published
2014

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

Author

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. Jiménez-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. Jofré, P. De Laverny, P. Masseron, T. Morbidelli, L. Prisinzano, L. Sacco, G.G. Sbordone, L. Worley, C.C.

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
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 NGC≠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 NGC≠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 316≠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. © 2014 ESO .

Published
2014

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