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

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

doi:10.1051/0004-6361/201423937

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

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

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

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 dispersion of the abundances varies between 0.10 and 0.20 dex. Conclusions: The Gaia-ESO sample of high-resolution spectra of FGK-type stars will be among the largest of its kind analyzed in a homogeneous way. The extensive list of elemental abundances derived in these stars will enable significant advances in the areas of stellar evolution and Milky Way formation and evolution. Based on observations made with the ESO/VLT, at Paranal Observatory, under program 188.B-3002 (The Gaia-ESO Public Spectroscopic Survey, PIs Gilmore and Randich). Appendices are available in electronic form at http://www.aanda.org

Original language	English
Article number	A122
Number of pages	38
Journal	Astronomy & Astrophysics
Volume	570
DOIs	https://doi.org/10.1051/0004-6361/201423937
Publication status	Published - 1 Oct 2014

Keywords

methods: data analysis
surveys
stars: abundances
stars: fundamental parameters
stars: late-type

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10.1051/0004-6361/201423937

Cite this

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. Z., Allende Prieto, C., Barisevičius, G., ... Zaggia, S. (2014). The Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars. Astronomy & Astrophysics, 570, [A122]. https://doi.org/10.1051/0004-6361/201423937

@article{4d8f8d1729c147238029e08475181357,

title = "The Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars",

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 dispersion of the abundances varies between 0.10 and 0.20 dex. Conclusions: The Gaia-ESO sample of high-resolution spectra of FGK-type stars will be among the largest of its kind analyzed in a homogeneous way. The extensive list of elemental abundances derived in these stars will enable significant advances in the areas of stellar evolution and Milky Way formation and evolution. Based on observations made with the ESO/VLT, at Paranal Observatory, under program 188.B-3002 (The Gaia-ESO Public Spectroscopic Survey, PIs Gilmore and Randich). Appendices are available in electronic form at http://www.aanda.org",

keywords = "methods: data analysis, surveys, stars: abundances, stars: fundamental parameters, stars: late-type",

author = "R. Smiljanic and Korn, {A. J.} and M. Bergemann and A. Frasca and L. Magrini and T. Masseron and E. Pancino and G. Ruchti and {San Roman}, I. and L. Sbordone and Sousa, {S. G.} and H. Tabernero and G. Tautvai{\v s}ienė and M. Valentini and M. Weber and Worley, {C. C.} and Adibekyan, {V. Zh.} and {Allende Prieto}, C. and G. Barisevi{\v c}ius and K. Biazzo and S. Blanco-Cuaresma and P. Bonifacio and A. Bragaglia and E. Caffau and T. Cantat-Gaudin and Y. Chorniy and {de Laverny}, P. and E. Delgado-Mena and P. Donati and S. Duffau and E. Franciosini and E. Friel and D. Geisler and {Gonz{\'a}lez Hern{\'a}ndez}, {J. I.} and P. Gruyters and G. Guiglion and Hansen, {C. J.} and U. Heiter and V. Hill and Jacobson, {H. R.} and P. Jofre and H. J{\"o}nsson and Lanzafame, {A. C.} and C. Lardo and H.-G. Ludwig and E. Maiorca and {\v S}. Mikolaitis and D. Montes and T. Morel and A. Mucciarelli and C. Mu{\~n}oz and T. Nordlander and L. Pasquini and E. Puzeras and A. Recio-Blanco and N. Ryde and G. Sacco and Santos, {N. C.} and Serenelli, {A. M.} and R. Sordo and C. Soubiran and L. Spina and M. Steffen and A. Vallenari and {Van Eck}, S. and S. Villanova and G. Gilmore and S. Randich and M. Asplund and J. Binney and J. Drew and S. Feltzing and A. Ferguson and R. Jeffries and G. Micela and I. Negueruela and T. Prusti and H.-W. Rix and E. Alfaro and C. Babusiaux and T. Bensby and R. Blomme and E. Flaccomio and P. Fran{\c c}ois and M. Irwin and S. Koposov and N. Walton and A. Bayo and G. Carraro and Costado, {M. T.} and F. Damiani and B. Edvardsson and A. Hourihane and R. Jackson and J. Lewis and K. Lind and G. Marconi and C. Martayan and L. Monaco and L. Morbidelli and L. Prisinzano and S. Zaggia",

year = "2014",

month = oct,

day = "1",

doi = "10.1051/0004-6361/201423937",

language = "English",

volume = "570",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Smiljanic, R, Korn, AJ, Bergemann, M, Frasca, A, Magrini, L, Masseron, T, Pancino, E, Ruchti, G, San Roman, I, Sbordone, L, Sousa, SG, Tabernero, H, Tautvaišienė, G, Valentini, M, Weber, M, Worley, CC, Adibekyan, VZ, 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, JI, Gruyters, P, Guiglion, G, Hansen, CJ, Heiter, U, Hill, V, Jacobson, HR, Jofre, P, Jönsson, H, Lanzafame, AC, 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, NC, Serenelli, AM, 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, MT, Damiani, F, Edvardsson, B, Hourihane, A, Jackson, R, Lewis, J, Lind, K, Marconi, G, Martayan, C, Monaco, L, Morbidelli, L, Prisinzano, L & Zaggia, S 2014, 'The Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars', Astronomy & Astrophysics, vol. 570, A122. https://doi.org/10.1051/0004-6361/201423937

TY - JOUR

T1 - The Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars

AU - Smiljanic, R.

AU - Korn, A. J.

AU - Bergemann, M.

AU - Frasca, A.

AU - Magrini, L.

AU - Masseron, T.

AU - Pancino, E.

AU - Ruchti, G.

AU - San Roman, I.

AU - Sbordone, L.

AU - Sousa, S. G.

AU - Tabernero, H.

AU - Tautvaišienė, G.

AU - Valentini, M.

AU - Weber, M.

AU - Worley, C. C.

AU - Adibekyan, V. Zh.

AU - Allende Prieto, C.

AU - Barisevičius, G.

AU - Biazzo, K.

AU - Blanco-Cuaresma, S.

AU - Bonifacio, P.

AU - Bragaglia, A.

AU - Caffau, E.

AU - Cantat-Gaudin, T.

AU - Chorniy, Y.

AU - de Laverny, P.

AU - Delgado-Mena, E.

AU - Donati, P.

AU - Duffau, S.

AU - Franciosini, E.

AU - Friel, E.

AU - Geisler, D.

AU - González Hernández, J. I.

AU - Gruyters, P.

AU - Guiglion, G.

AU - Hansen, C. J.

AU - Heiter, U.

AU - Hill, V.

AU - Jacobson, H. R.

AU - Jofre, P.

AU - Jönsson, H.

AU - Lanzafame, A. C.

AU - Lardo, C.

AU - Ludwig, H.-G.

AU - Maiorca, E.

AU - Mikolaitis, Š.

AU - Montes, D.

AU - Morel, T.

AU - Mucciarelli, A.

AU - Muñoz, C.

AU - Nordlander, T.

AU - Pasquini, L.

AU - Puzeras, E.

AU - Recio-Blanco, A.

AU - Ryde, N.

AU - Sacco, G.

AU - Santos, N. C.

AU - Serenelli, A. M.

AU - Sordo, R.

AU - Soubiran, C.

AU - Spina, L.

AU - Steffen, M.

AU - Vallenari, A.

AU - Van Eck, S.

AU - Villanova, S.

AU - Gilmore, G.

AU - Randich, S.

AU - Asplund, M.

AU - Binney, J.

AU - Drew, J.

AU - Feltzing, S.

AU - Ferguson, A.

AU - Jeffries, R.

AU - Micela, G.

AU - Negueruela, I.

AU - Prusti, T.

AU - Rix, H.-W.

AU - Alfaro, E.

AU - Babusiaux, C.

AU - Bensby, T.

AU - Blomme, R.

AU - Flaccomio, E.

AU - François, P.

AU - Irwin, M.

AU - Koposov, S.

AU - Walton, N.

AU - Bayo, A.

AU - Carraro, G.

AU - Costado, M. T.

AU - Damiani, F.

AU - Edvardsson, B.

AU - Hourihane, A.

AU - Jackson, R.

AU - Lewis, J.

AU - Lind, K.

AU - Marconi, G.

AU - Martayan, C.

AU - Monaco, L.

AU - Morbidelli, L.

AU - Prisinzano, L.

AU - Zaggia, S.

PY - 2014/10/1

Y1 - 2014/10/1

N2 - 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 dispersion of the abundances varies between 0.10 and 0.20 dex. Conclusions: The Gaia-ESO sample of high-resolution spectra of FGK-type stars will be among the largest of its kind analyzed in a homogeneous way. The extensive list of elemental abundances derived in these stars will enable significant advances in the areas of stellar evolution and Milky Way formation and evolution. Based on observations made with the ESO/VLT, at Paranal Observatory, under program 188.B-3002 (The Gaia-ESO Public Spectroscopic Survey, PIs Gilmore and Randich). Appendices are available in electronic form at http://www.aanda.org

AB - 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 dispersion of the abundances varies between 0.10 and 0.20 dex. Conclusions: The Gaia-ESO sample of high-resolution spectra of FGK-type stars will be among the largest of its kind analyzed in a homogeneous way. The extensive list of elemental abundances derived in these stars will enable significant advances in the areas of stellar evolution and Milky Way formation and evolution. Based on observations made with the ESO/VLT, at Paranal Observatory, under program 188.B-3002 (The Gaia-ESO Public Spectroscopic Survey, PIs Gilmore and Randich). Appendices are available in electronic form at http://www.aanda.org

KW - methods: data analysis

KW - surveys

KW - stars: abundances

KW - stars: fundamental parameters

KW - stars: late-type

U2 - 10.1051/0004-6361/201423937

DO - 10.1051/0004-6361/201423937

M3 - Article

VL - 570

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A122

ER -

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

Abstract

Keywords

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