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

Author

Tautvaišienė, G., Drazdauskas, A., Mikolaitis, Š., Barisevičius, G., Puzeras, E., Stonkutė, E., Chorniy, Y., Magrini, L., Romano, D., Smiljanic, R., Bragaglia, A., Carraro, G., Friel, E., Morel, T., Pancino, E., Donati, P., Jiménez-Esteban, F., Gilmore, G., Randich, S., Jeffries, R. D., Vallenari, A., Bensby, T., Flaccomio, E., Recio-Blanco, A., Costado, M. T., Hill, V., Jofré, P., Lardo, C., de Laverny, P., Masseron, T., Moribelli, L., Sousa, S. G., and Zaggia, S.

Subjects
Astrophysics - Solar and Stellar Astrophysics
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
2014
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2. Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars

Author

Smiljanic, R., Korn, A. J., Bergemann, M., Frasca, A., Magrini, L., Masseron, T., Pancino, E., Ruchti, G., Roman, I. San, Sbordone, L., Sousa, S. G., Tabernero, H., Tautvaisiene, G., Valentini, M., Weber, M., Worley, C. C., Adibekyan, V. Zh., Prieto, C. Allende, Barisevicius, 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., Hernandez, J. I. Gonzalez, Gruyters, P., Guiglion, G., Hansen, C. J., Heiter, U., Hill, V., Jacobson, H. R., Jofre, P., Jonsson, H., Lanzafame, A. C., Lardo, C., Ludwig, H. G., Maiorca, E., Mikolaitis, S., Montes, D., Morel, T., Mucciarelli, A., Munoz, 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., Francois, 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., and Zaggia, S.

Subjects
Astrophysics - Solar and Stellar Astrophysics
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
2014
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3. 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., Jimenez-Esteban, F., Maiorca, E., Geisler, D., San, I., Villanova, S., Gilmore, G., Randich, S., Bensby, T., Flaccomio, E., Lanzafame, A., Recio-Blanco, A., Damiani, F., Hourihane, A., Jofre, P., deLaverny, P., Masseron, T., Morbidelli, L., Prisinzano, L., Sacco, G. G., Sbordone, L., and Worley, C. C.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

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. Studying the chemical homogeneity of the most massive open clusters is necessary to better understand the mechanism of their formation and determine the mass limit under which clusters cannot host multiple populations. Here we studied NGC6705, that 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. This study makes use of BVI and ri photometry and comparisons with theoretical isochrones to derive the age of NGC6705. 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. The estimated ages range from 250 to 316Myr, 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$_{\odot}$ and 11 000 M$_{\odot}$. After selecting the cluster members from their radial velocities, we obtain a metallicity of [Fe/H]=0.10$\pm$0.06 based on 21 candidate members. Moreover, NGC6705 shows no sign of the typical correlations or anti-correlations between Al, Mg, Si, and Na, that are expected in multiple populations. This is consistent with our cluster mass estimate, which is lower than the required mass limit proposed in literature to develop multiple populations.

Published
2014
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4. Red clump stars of the Milky Way - laboratories of extra-mixing

Author

Tautvaišienė, G., Barisevičius, G., Chorniy, Y., Ilyin, I., and Puzeras, E.

Subjects
Astrophysics - Galaxy Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

In this work we present the main atmospheric parameters, carbon, nitrogen and oxygen abundances, and 12C/13C ratios determined in a sample of 28 Galactic clump stars. Abundances of carbon were studied using the C2 band at 5086.2 {\AA}. The wavelength interval 7980-8130 {\AA} with strong CN features was analysed in order to determine nitrogen abundances and 12C/13C isotope ratios. The oxygen abundances were determined from the [O I] line at 6300 {\AA}. The mean abundances of C, N and O abundances in the investigated clump stars support our previous estimations that, compared to the Sun and dwarf stars of the Galactic disc, carbon is depleted by about 0.2 dex, nitrogen is enhanced by 0.2 dex and oxygen is close to abundances in dwarfs. The 12C/13C and C/N ratios for galactic red clump stars analysed were compared to the evolutionary models of extra-mixing. The steeper drop of 12C/13C ratio in the model of thermohaline mixing by Charbonnel & Lagarde better reflects the observational data at low stellar masses than the more shallow model of cool bottom processing by Boothroyd & Sackmann. For stars of about 2 Msun masses a modelling of rotationally induced mixing should be considered with rotation of about 250 km s-1 at the time when a star was at the hydrogen-core-burning stage., Comment: 8 pages, 7 figures, published in MNRAS 03/2013. arXiv admin note: substantial text overlap with arXiv:1007.4064

Published
2013
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5. C, N and O abundances in red clump stars of the Milky Way

Author

Tautvaisiene, G., Edvardsson, B., Puzeras, E., Barisevicius, G., and Ilyin, I.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

The Hipparcos orbiting observatory has revealed a large number of helium-core-burning "clump" stars in the Galactic field. These low-mass stars exhibit signatures of extra-mixing processes that require modeling beyond the first dredge-up of standard models. The 12C/13C ratio is the most robust diagnostic of deep mixing, because it is insensitive to the adopted stellar parameters. In this work we present 12C/13C determinations in a sample of 34 Galactic clump stars as well as abundances of nitrogen, carbon and oxygen. Abundances of carbon were studied using the C2 Swan (0,1) band head at 5635.5 A. The wavelength interval 7980-8130 A with strong CN features was analysed in order to determine nitrogen abundances and 12C/13C isotope ratios. The oxygen abundances were determined from the [O I] line at 6300 A. Compared with the Sun and dwarf stars of the Galactic disk, mean abundances in the investigated clump stars suggest that carbon is depleted by about 0.2 dex, nitrogen is enhanced by 0.2 dex and oxygen is close to abundances in dwarfs. Comparisons to evolutionary models show that the stars fall into two groups: the one is of first ascent giants with carbon isotope ratios altered according to the first dredge-up prediction, and the other one is of helium-core-burning stars with carbon isotope ratios altered by extra mixing. The stars investigated fall to these groups in approximately equal numbers., Comment: 8 pages 6 figures Accepted for publication in MNRAS

Published
2010
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6. High resolution spectroscopic study of red clump stars in the Galaxy: iron group elements

Author

Puzeras, E., Tautvaisiene, G., Cohen, J. G., Gray, D. F., Adelman, S. J., Ilyin, I., and Chorniy, Y.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

The main atmospheric parameters and abundances of the iron group elements (vanadium, chromium, iron, cobalt and nickel) are determined for 62 red giant "clump" stars revealed in the Galactic field by the Hipparcos orbiting observatory. The stars form a homogeneous sample with the mean value of temperature T=4750 +- 160K, of surface gravity log g = 2.41 +- 0.26 and the mean value of metallicity [Fe/H] = -0.04 +- 0.15 dex. A Gaussian fit to the [Fe/H] distribution produces the mean [Fe/H] = -0.01 dex and dispersion of [Fe/H] = 0.08 dex. The near-solar metallicity and small dispersion of [Fe/H] of clump stars of the Galaxy obtained in this work confirm the theoretical model of the Hipparcos clump by Girardi & Salaris (2001). This suggests that nearby clump stars are (in the mean) relatively young objects, reflecting mainly the near-solar metallicities developed in the local disk during the last few Gyrs of its history. We find iron group element to iron abundance ratios in clump giants to be close to solar., Comment: 9 pages, 7 figures, accepted for publication in MNRAS

Published
2010
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7. 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

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

Author

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, Thomas, Flaccomio, E., Recio-Blanco, A., Costado, M. T., Hill, V., Jofre, P., Lardo, C., de laverny, P., Masseron, T., Moribelli, L., Sousa, S. G., Zaggia, S., 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, Thomas, 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.

Abstract

Context. The Gaia-ESO Public Spectroscopic Survey will observe a large sample of clusters and cluster stars, covering a wide age-distance-metallicity-position-density parameter space. Aims. We aim 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. Methods. High-resolution spectra, observed with the FLAMES-UVES spectrograph on the ESO VLT, were analysed using a differential model atmosphere method. Abundances of carbon were derived using the C-2 band heads at 5135 and 5635.5 angstrom. The wavelength interval 6470-6490 angstrom, with CN features, was analysed to determine nitrogen abundances. Oxygen abundances were determined from the [O I] line at 6300 angstrom. Results. 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 NGC4815: [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 NGC6705: [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 M-circle dot, 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. They are not decreased as much as predicted by the recent model in which the thermohaline-and rotation-induced extra-mixing act together. The average [O/H] abundance ratios of NGC4815 and NGC6705 are compa

Published
2015

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

Author

Smiljanic, R., Korn, Andreas J., Bergemann, M., Frasca, A., Magrini, L., Masseron, T., Pancino, E., Ruchti, G., San Roman, I., Sbordone, L., Sousa, S. G., Tabernero, H., Tautvaisiene, G., Valentini, M., Weber, M., Worley, C. C., Adibekyan, V. Zh., Allende Prieto, C., Barisevicius, 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., Gonzalez Hernandez, J. I., Gruyters, Pieter, Guiglion, G., Hansen, C. J., Heiter, Ulrike, Hill, V., Jacobson, H. R., Jofre, P., Jonsson, H., Lanzafame, A. C., Lardo, C., Ludwig, H. -G, Maiorca, E., Mikolaitis, S., Montes, D., Morel, T., Mucciarelli, A., Munoz, C., Nordlander, Thomas, 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., Francois, P., Irwin, M., Koposov, S., Walton, N., Bayo, A., Carraro, G., Costado, M. T., Damiani, F., Edvardsson, Bengt, Hourihane, A., Jackson, R., Lewis, J., Lind, K., Marconi, G., Martayan, C., Monaco, L., Morbidelli, L., Prisinzano, L., Zaggia, S., Smiljanic, R., Korn, Andreas J., Bergemann, M., Frasca, A., Magrini, L., Masseron, T., Pancino, E., Ruchti, G., San Roman, I., Sbordone, L., Sousa, S. G., Tabernero, H., Tautvaisiene, G., Valentini, M., Weber, M., Worley, C. C., Adibekyan, V. Zh., Allende Prieto, C., Barisevicius, 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., Gonzalez Hernandez, J. I., Gruyters, Pieter, Guiglion, G., Hansen, C. J., Heiter, Ulrike, Hill, V., Jacobson, H. R., Jofre, P., Jonsson, H., Lanzafame, A. C., Lardo, C., Ludwig, H. -G, Maiorca, E., Mikolaitis, S., Montes, D., Morel, T., Mucciarelli, A., Munoz, C., Nordlander, Thomas, 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., Francois, P., Irwin, M., Koposov, S., Walton, N., Bayo, A., Carraro, G., Costado, M. T., Damiani, F., Edvardsson, Bengt, Hourihane, A., Jackson, R., Lewis, J., Lind, K., Marconi, G., Martayan, C., Monaco, L., Morbidelli, L., Prisinzano, L., and Zaggia, S.

Abstract

Context. The ongoing Gaia-ESO Public Spectroscopic Survey is using FLAMES at the VLT to obtain high-quality medium-resolution Giraffe spectra for about 10(5) stars and high-resolution UVES spectra for about 5000 stars. With UVES, the Survey has already observed 1447 FGK-type stars. Aims. 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 second internal release and will be part of its first public release of advanced data products. Methods. The final parameter scale is tied to the scale defined by the Gaia benchmark stars, a set of stars with fundamental atmospheric parameters. In addition, a set of open and globular clusters is used to evaluate the physical soundness of the results. Each of the implemented methodologies 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. Results. The recommended results successfully reproduce the atmospheric parameters of the benchmark stars and the expected T-eff-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 55K for T-eff, 0.13dex for log g and 0.07 dex for [Fe/H]. Systematic biases are estimated to be between 50-100 K for T-eff, 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

Published
2014
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10. The Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Smiljanic, R., Korn, A., Bergemann, M., Frasca, A., Magrini, L., Masseron, T., Pancino, E., Ruchti, G., San Roman, I., Sbordone, L., Sousa, S.G., Drew, J., Feltzing, S., Ferguson, A., Jeffries, R., Micela, G., Negueruela, Ignacio, Prusti, T., Rix, H.-W., Alfaro, Emilio J., Babusiaux, C., Bensby, T., Blomme, Ronny, Flaccomio, E., Francois, P., Irwin, M., Koposov, S., Walton, N., Bayo, A., Carraro, G., Costado, M.T., Damiani, F., Edvardsson, B., Hourihane, A., Jackson, R.J., Lewis, J., Lind, K., Marconi, G., Martayan, C., Monaco, L., Morbidelli, L., Prisinzano, L., Zaggia, S., Tabernero, Hugo M., 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., Laverny, P. de, Delgado-Mena, E., Donati, P., Duffau, S., Franciosini, E., Friel, E., Geisler, Douglas, 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, David, Morel, Thierry, Mucciarelli, A., Muñoz, C., Nordlander, T., Pasquini, L., Puzeras, E., Recio-Blanco, A., Ryde, N., Sacco, G.G., Santos, N.C., Serenelli, A.M., Sordo, R., Soubiran, C., Spina, L., Steffen, M., Vallenari, A., Van Eck, S., Villanova, S., Gilmore, Gerard, Randich, Sofia, Asplund, M., Binney, J., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Smiljanic, R., Korn, A., Bergemann, M., Frasca, A., Magrini, L., Masseron, T., Pancino, E., Ruchti, G., San Roman, I., Sbordone, L., Sousa, S.G., Drew, J., Feltzing, S., Ferguson, A., Jeffries, R., Micela, G., Negueruela, Ignacio, Prusti, T., Rix, H.-W., Alfaro, Emilio J., Babusiaux, C., Bensby, T., Blomme, Ronny, Flaccomio, E., Francois, P., Irwin, M., Koposov, S., Walton, N., Bayo, A., Carraro, G., Costado, M.T., Damiani, F., Edvardsson, B., Hourihane, A., Jackson, R.J., Lewis, J., Lind, K., Marconi, G., Martayan, C., Monaco, L., Morbidelli, L., Prisinzano, L., Zaggia, S., Tabernero, Hugo M., 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., Laverny, P. de, Delgado-Mena, E., Donati, P., Duffau, S., Franciosini, E., Friel, E., Geisler, Douglas, 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, David, Morel, Thierry, Mucciarelli, A., Muñoz, C., Nordlander, T., Pasquini, L., Puzeras, E., Recio-Blanco, A., Ryde, N., Sacco, G.G., Santos, N.C., Serenelli, A.M., Sordo, R., Soubiran, C., Spina, L., Steffen, M., Vallenari, A., Van Eck, S., Villanova, S., Gilmore, Gerard, Randich, Sofia, Asplund, M., and Binney, J.

Abstract

Context. The ongoing Gaia-ESO Public Spectroscopic Survey is using FLAMES at the VLT to obtain high-quality medium-resolution Giraffe spectra for about 105 stars and high-resolution UVES spectra for about 5000 stars. With UVES, the Survey has already observed 1447 FGK-type stars. Aims. 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 second internal release and will be part of its first public release of advanced data products. Methods. The final parameter scale is tied to the scale defined by the Gaia benchmark stars, a set of stars with fundamental atmospheric parameters. In addition, a set of open and globular clusters is used to evaluate the physical soundness of the results. Each of the implemented methodologies 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. Results. The recommended results successfully reproduce the atmospheric parameters of the benchmark stars 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

Published
2014

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

Author

Naval Postgraduate School (U.S.), Center for Interdisciplinary Remotely-Piloted Aircraft Studies (CIRPAS), Bragaglia, A., Lanzafame, A.C., Ferguson, A., Frasca, A., Hourihane, A., Serenelli, A.M., Mucciarelli, A., Recio-Blanco, A., Vallenari, A., Bayo, A., Korn, A.J., Edvardsson, B., Allende Prieto, C., Babusiaux, C., Worley, C.C., Hansen, C.J., Lardo, C., Martayan, C., Muñoz, C., Soubiran, C., Geisler, D., Montes, D., Caffau, E., Delgado-Mena, E., Flaccomio. E., Pancino, E., Puzeras, E., Alfaro, E., Franciosini, E., Friel, E., Maiorca, E., Damiani, F., Barisevicius, G., Carraro, G., Gilmore, G., Guiglion, G., Micela, G., Ruchti, G., Sacco, G., Tautvaišien, G., Marconi, G., Rix, H.-W., Jönsson, H., Tabernero, H., Ludwig, H.-G., Jacobson, H.R., Negueruela, I., San Roman, I., Binney, J., González Hernández, J. I., Drew, J., Lewis, J., Biazzo, K., Lind, K, Magrini, L., Monaco, L., Morbidelli, L., Pasquini, L., Prisinzano, L., Sbordone, L., Spina. L., Asplund, M., Bergemann, M., Irwin, M., Valentini, M., Steffen, M., Costado, M.T., Weber, M., Ryde, N., Walton, N., Santos, N.C., Bonifacio, P., Donati, P., Gruyters, P., deLaverny, P., François, P., Jofre, P., Blomme, R., Jackson, R., Smiljanic, R., Jeffries, R., Sordo, R., Blanco-Cuaresma, S., Feltzing, S., Koposov, S., Mikolaitis, Š., Randich, S., Villanova, S., Zaggia, S., Duffau, S., Sousa, S.G., VanEck, S., Bensby, T., Cantat-Gaudin, T., Masseron, T., Nordlander, T., Morel, T., Prusti, T., Heiter, U., Adibekyan, V. Zh., Hill, V., Chorniy, Y., Naval Postgraduate School (U.S.), Center for Interdisciplinary Remotely-Piloted Aircraft Studies (CIRPAS), Bragaglia, A., Lanzafame, A.C., Ferguson, A., Frasca, A., Hourihane, A., Serenelli, A.M., Mucciarelli, A., Recio-Blanco, A., Vallenari, A., Bayo, A., Korn, A.J., Edvardsson, B., Allende Prieto, C., Babusiaux, C., Worley, C.C., Hansen, C.J., Lardo, C., Martayan, C., Muñoz, C., Soubiran, C., Geisler, D., Montes, D., Caffau, E., Delgado-Mena, E., Flaccomio. E., Pancino, E., Puzeras, E., Alfaro, E., Franciosini, E., Friel, E., Maiorca, E., Damiani, F., Barisevicius, G., Carraro, G., Gilmore, G., Guiglion, G., Micela, G., Ruchti, G., Sacco, G., Tautvaišien, G., Marconi, G., Rix, H.-W., Jönsson, H., Tabernero, H., Ludwig, H.-G., Jacobson, H.R., Negueruela, I., San Roman, I., Binney, J., González Hernández, J. I., Drew, J., Lewis, J., Biazzo, K., Lind, K, Magrini, L., Monaco, L., Morbidelli, L., Pasquini, L., Prisinzano, L., Sbordone, L., Spina. L., Asplund, M., Bergemann, M., Irwin, M., Valentini, M., Steffen, M., Costado, M.T., Weber, M., Ryde, N., Walton, N., Santos, N.C., Bonifacio, P., Donati, P., Gruyters, P., deLaverny, P., François, P., Jofre, P., Blomme, R., Jackson, R., Smiljanic, R., Jeffries, R., Sordo, R., Blanco-Cuaresma, S., Feltzing, S., Koposov, S., Mikolaitis, Š., Randich, S., Villanova, S., Zaggia, S., Duffau, S., Sousa, S.G., VanEck, S., Bensby, T., Cantat-Gaudin, T., Masseron, T., Nordlander, T., Morel, T., Prusti, T., Heiter, U., Adibekyan, V. Zh., Hill, V., and Chorniy, Y.

Abstract

Context. The ongoing Gaia-ESO Public Spectroscopic Survey is using FLAMES at the VLT to obtain high-quality medium-resolution Giraffe spectra for about 10(5) stars and high-resolution UVES spectra for about 5000 stars. With UVES, the Survey has already observed 1447 FGK-type stars. Aims. 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 second internal release and will be part of its first public release of advanced data products. Methods. The final parameter scale is tied to the scale defined by the Gaia benchmark stars, a set of stars with fundamental atmospheric parameters. In addition, a set of open and globular clusters is used to evaluate the physical soundness of the results. Each of the implemented methodologies 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. Results. The recommended results successfully reproduce the atmospheric parameters of the benchmark stars and the expected T(eff)-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 55K for T(eff), 0.13 dex for log g and 0.07 dex for [Fe/H]. Systematic biases are estimated to be between 50−100 K for T(eff), 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-me

Published
2014

12. TheGaia-ESO Survey: CNO abundances in the open clusters Trumpler 20, NGC 4815, and NGC 6705

Author

Tautvaišienė, G., primary, Drazdauskas, A., additional, Mikolaitis, Š., additional, Barisevičius, G., additional, Puzeras, E., additional, Stonkut*error*ė, E., additional, Chorniy, Y., additional, Magrini, L., additional, Romano, D., additional, Smiljanic, R., additional, Bragaglia, A., additional, Carraro, G., additional, Friel, E., additional, Morel, T., additional, Pancino, E., additional, Donati, P., additional, Jiménez-Esteban, F., additional, Gilmore, G., additional, Randich, S., additional, Jeffries, R. D., additional, Vallenari, A., additional, Bensby, T., additional, Flaccomio, E., additional, Recio-Blanco, A., additional, Costado, M. T., additional, Hill, V., additional, Jofré, P., additional, Lardo, C., additional, de Laverny, P., additional, Masseron, T., additional, Moribelli, L., additional, Sousa, S. G., additional, and Zaggia, S., additional

Published
2014
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13. TheGaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars

Author

Smiljanic, R., primary, Korn, A. J., additional, Bergemann, M., additional, Frasca, A., additional, Magrini, L., additional, Masseron, T., additional, Pancino, E., additional, Ruchti, G., additional, San Roman, I., additional, Sbordone, L., additional, Sousa, S. G., additional, Tabernero, H., additional, Tautvaišienė, G., additional, Valentini, M., additional, Weber, M., additional, Worley, C. C., additional, Adibekyan, V. Zh., additional, Allende Prieto, C., additional, Barisevičius, G., additional, Biazzo, K., additional, Blanco-Cuaresma, S., additional, Bonifacio, P., additional, Bragaglia, A., additional, Caffau, E., additional, Cantat-Gaudin, T., additional, Chorniy, Y., additional, de Laverny, P., additional, Delgado-Mena, E., additional, Donati, P., additional, Duffau, S., additional, Franciosini, E., additional, Friel, E., additional, Geisler, D., additional, González Hernández, J. I., additional, Gruyters, P., additional, Guiglion, G., additional, Hansen, C. J., additional, Heiter, U., additional, Hill, V., additional, Jacobson, H. R., additional, Jofre, P., additional, Jönsson, H., additional, Lanzafame, A. C., additional, Lardo, C., additional, Ludwig, H.-G., additional, Maiorca, E., additional, Mikolaitis, Š., additional, Montes, D., additional, Morel, T., additional, Mucciarelli, A., additional, Muñoz, C., additional, Nordlander, T., additional, Pasquini, L., additional, Puzeras, E., additional, Recio-Blanco, A., additional, Ryde, N., additional, Sacco, G., additional, Santos, N. C., additional, Serenelli, A. M., additional, Sordo, R., additional, Soubiran, C., additional, Spina, L., additional, Steffen, M., additional, Vallenari, A., additional, Van Eck, S., additional, Villanova, S., additional, Gilmore, G., additional, Randich, S., additional, Asplund, M., additional, Binney, J., additional, Drew, J., additional, Feltzing, S., additional, Ferguson, A., additional, Jeffries, R., additional, Micela, G., additional, Negueruela, I., additional, Prusti, T., additional, Rix, H-W., additional, Alfaro, E., additional, Babusiaux, C., additional, Bensby, T., additional, Blomme, R., additional, Flaccomio, E., additional, François, P., additional, Irwin, M., additional, Koposov, S., additional, Walton, N., additional, Bayo, A., additional, Carraro, G., additional, Costado, M. T., additional, Damiani, F., additional, Edvardsson, B., additional, Hourihane, A., additional, Jackson, R., additional, Lewis, J., additional, Lind, K., additional, Marconi, G., additional, Martayan, C., additional, Monaco, L., additional, Morbidelli, L., additional, Prisinzano, L., additional, and Zaggia, S., additional

Published
2014
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14. TheGaia-ESO Survey: Stellar content and elemental abundances in the massive cluster NGC 6705

Author

Cantat-Gaudin, T., primary, Vallenari, A., additional, Zaggia, S., additional, Bragaglia, A., additional, Sordo, R., additional, Drew, J. E., additional, Eisloeffel, J., additional, Farnhill, H. J., additional, Gonzalez-Solares, E., additional, Greimel, R., additional, Irwin, M. J., additional, Kupcu-Yoldas, A., additional, Jordi, C., additional, Blomme, R., additional, Sampedro, L., additional, Costado, M. T., additional, Alfaro, E., additional, Smiljanic, R., additional, Magrini, L., additional, Donati, P., additional, Friel, E. D., additional, Jacobson, H., additional, Abbas, U., additional, Hatzidimitriou, D., additional, Spagna, A., additional, Vecchiato, A., additional, Balaguer-Nunez, L., additional, Lardo, C., additional, Tosi, M., additional, Pancino, E., additional, Klutsch, A., additional, Tautvaisiene, G., additional, Drazdauskas, A., additional, Puzeras, E., additional, Jiménez-Esteban, F., additional, Maiorca, E., additional, Geisler, D., additional, San Roman, I., additional, Villanova, S., additional, Gilmore, G., additional, Randich, S., additional, Bensby, T., additional, Flaccomio, E., additional, Lanzafame, A., additional, Recio-Blanco, A., additional, Damiani, F., additional, Hourihane, A., additional, Jofré, P., additional, de Laverny, P., additional, Masseron, T., additional, Morbidelli, L., additional, Prisinzano, L., additional, Sacco, G. G., additional, Sbordone, L., additional, and Worley, C. C., additional

Published
2014
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18. The Gaia-ESO Survey: CNO abundances in the open clusters Trumpler 20, NGC4815, and NGC6705.

Author

Tautvaišienė, G., Drazdauskas, A., Mikolaitis, Š., Bariseviçius, G., Puzeras, E., Stonkutė, E., Chorniy, Y., Magrini, L., Romano, D., Smiljanic, R., Bragaglia, A., Carraro, G., Friel, E., Morel, T., Pancino, E., Donati, P., Jiménez-Esteban, F., Gilmore, G., Randich, S., and Jeffries, R. D.

Subjects
ASTRONOMICAL surveys, OPEN clusters of stars, DENSITY of stars, GALACTIC evolution, SPECTROGRAPHS, HIGH resolution spectroscopy
Abstract

Context. The Gaia-ESO Public Spectroscopic Survey will observe a large sample of clusters and cluster stars, covering a wide age-distancemetallicity-position-density parameter space. Aims. We aim 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. Methods. High-resolution spectra, observed with the FLAMES-UVES spectrograph on the ESO VLT, were analysed using a differential model atmosphere method. Abundances of carbon were derived using the C2 band heads at 5135 and 5635.5 Å. The wavelength interval 6470-6490 Å, with CN features, was analysed to determine nitrogen abundances. Oxygen abundances were determined from the [O i] line at 6300 Å. Results. 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 NGC4815. [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 NGC6705. [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 M⊙, 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. They are not decreased as much as predicted by the recent model in which the thermohaline- and rotation-induced extra-mixing act together. The average [O/H] abundance ratios of NGC4815 and NGC6705 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. Conclusions. The first results of CNO determinations in open clusters show the potential of the Gaia-ESO Survey to judge stellar and Galactic chemical evolution models and the validity of their physical assumptions through a homogeneous and detailed spectral analysis. [ABSTRACT FROM AUTHOR]

Published
2015
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20. 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

21. 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

22. 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 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.

Published
2014

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