Author: "Jeffries, R. D." / Publisher: max planck inst astron, konigstuhl 17, d-69117 heidelberg, germany. - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Jeffries, R. D."' showing total 22 results

Start Over Author "Jeffries, R. D." Publisher max planck inst astron, konigstuhl 17, d-69117 heidelberg, germany.

22 results on '"Jeffries, R. D."'

1. The Gaia-ESO Survey : The DR5 analysis of the medium-resolution GIRAFFE and high-resolution UVES spectra of FGK-type stars

Author: Worley, C. C., Smiljanic, R., Magrini, L., Frasca, A., Franciosini, E., Montes, D., Feuillet, D. K., Tabernero, H. M., González Hernandez, J. I., Villanova, S., Mikolaitis, S., Lind, K., Tautvaisiene, G., Casey, A. R., Korn, Andreas J., Bonifacio, P., Soubiran, C., Caffau, E., Guiglion, G., Merle, T., Hourihane, A., Gonneau, A., François, P., Randich, S., Gilmore, G., Lewis, J. R., Murphy, D. N. A., Jeffries, R. D., Koposov, S. E., Blomme, R., Lanzafame, A. C., Bensby, T., Bragaglia, A., Alfaro, E. J., Walton, N. A., Vallenari, A., Prusti, T., Biazzo, K., Jofré, P., Zaggia, S., Heiter, Ulrike, Marfil, E., Jiménez-Esteban, F., Gutiérrez Albarran, M. L., Morbidelli, L., Worley, C. C., Smiljanic, R., Magrini, L., Frasca, A., Franciosini, E., Montes, D., Feuillet, D. K., Tabernero, H. M., González Hernandez, J. I., Villanova, S., Mikolaitis, S., Lind, K., Tautvaisiene, G., Casey, A. R., Korn, Andreas J., Bonifacio, P., Soubiran, C., Caffau, E., Guiglion, G., Merle, T., Hourihane, A., Gonneau, A., François, P., Randich, S., Gilmore, G., Lewis, J. R., Murphy, D. N. A., Jeffries, R. D., Koposov, S. E., Blomme, R., Lanzafame, A. C., Bensby, T., Bragaglia, A., Alfaro, E. J., Walton, N. A., Vallenari, A., Prusti, T., Biazzo, K., Jofré, P., Zaggia, S., Heiter, Ulrike, Marfil, E., Jiménez-Esteban, F., Gutiérrez Albarran, M. L., and Morbidelli, L.
Abstract: The Gaia-ESO Survey is an European Southern Observatory (ESO) public spectroscopic survey that targeted 105 stars in the Milky Way covering the major populations of the disk, bulge and halo. The observations were made using FLAMES on the VLT obtaining both UVES high (R ~ 47 000) and GIRAFFE medium (R ~ 20 000) resolution spectra. The analysis of the Gaia-ESO spectra was the work of multiple analysis teams (nodes) within five working groups (WG). The homogenisation of the stellar parameters within WG11 (high resolution observations of FGK stars) and the homogenisation of the stellar parameters within WG10 (medium resolution observations of FGK stars) is described here. In both cases, the homogenisation was carried out using a Bayesian Inference method developed specifically for the Gaia-ESO Survey by WG11. The method was also used for the chemical abundance homogenisation within WG11, however, the WG10 chemical abundance data set was too sparsely populated so basic corrections for each node analysis were employed for the homogenisation instead. The WG10 homogenisation primarily used the cross-match of stars with WG11 as the reference set in both the stellar parameter and chemical abundance homogenisation. In this way the WG10 homogenised results have been placed directly onto the WG11 stellar parameter and chemical abundance scales. The reference set for the metal-poor end was sparse which limited the effectiveness of the homogenisation in that regime. For WG11, the total number of stars for which stellar parameters were derived was 6 231 with typical uncertainties for Teff, log g and [Fe/H] of 32 K, 0.05 and 0.05 respectively. One or more chemical abundances out of a possible 39 elements were derived for 6 188 of the stars. For WG10, the total number of stars for which stellar parameters were derived was 76 675 with typical uncertainties for Teff, log g and [Fe/H] of 64 K, 0.15 and 0.07 respectively. One or more chemical abundances out of a possible 30 elements were
Published: 2024
Full Text: View/download PDF

2. The Gaia-ESO Survey : The DR5 analysis of the medium-resolution GIRAFFE and high-resolution UVES spectra of FGK-type stars

Author: Worley, C. C., Smiljanic, R., Magrini, L., Frasca, A., Franciosini, E., Montes, D., Feuillet, D. K., Tabernero, H. M., González Hernandez, J. I., Villanova, S., Mikolaitis, S., Lind, K., Tautvaisiene, G., Casey, A. R., Korn, Andreas J., Bonifacio, P., Soubiran, C., Caffau, E., Guiglion, G., Merle, T., Hourihane, A., Gonneau, A., François, P., Randich, S., Gilmore, G., Lewis, J. R., Murphy, D. N. A., Jeffries, R. D., Koposov, S. E., Blomme, R., Lanzafame, A. C., Bensby, T., Bragaglia, A., Alfaro, E. J., Walton, N. A., Vallenari, A., Prusti, T., Biazzo, K., Jofré, P., Zaggia, S., Heiter, Ulrike, Marfil, E., Jiménez-Esteban, F., Gutiérrez Albarran, M. L., Morbidelli, L., Worley, C. C., Smiljanic, R., Magrini, L., Frasca, A., Franciosini, E., Montes, D., Feuillet, D. K., Tabernero, H. M., González Hernandez, J. I., Villanova, S., Mikolaitis, S., Lind, K., Tautvaisiene, G., Casey, A. R., Korn, Andreas J., Bonifacio, P., Soubiran, C., Caffau, E., Guiglion, G., Merle, T., Hourihane, A., Gonneau, A., François, P., Randich, S., Gilmore, G., Lewis, J. R., Murphy, D. N. A., Jeffries, R. D., Koposov, S. E., Blomme, R., Lanzafame, A. C., Bensby, T., Bragaglia, A., Alfaro, E. J., Walton, N. A., Vallenari, A., Prusti, T., Biazzo, K., Jofré, P., Zaggia, S., Heiter, Ulrike, Marfil, E., Jiménez-Esteban, F., Gutiérrez Albarran, M. L., and Morbidelli, L.
Abstract: The Gaia-ESO Survey is an European Southern Observatory (ESO) public spectroscopic survey that targeted 105 stars in the Milky Way covering the major populations of the disk, bulge and halo. The observations were made using FLAMES on the VLT obtaining both UVES high (R ~ 47 000) and GIRAFFE medium (R ~ 20 000) resolution spectra. The analysis of the Gaia-ESO spectra was the work of multiple analysis teams (nodes) within five working groups (WG). The homogenisation of the stellar parameters within WG11 (high resolution observations of FGK stars) and the homogenisation of the stellar parameters within WG10 (medium resolution observations of FGK stars) is described here. In both cases, the homogenisation was carried out using a Bayesian Inference method developed specifically for the Gaia-ESO Survey by WG11. The method was also used for the chemical abundance homogenisation within WG11, however, the WG10 chemical abundance data set was too sparsely populated so basic corrections for each node analysis were employed for the homogenisation instead. The WG10 homogenisation primarily used the cross-match of stars with WG11 as the reference set in both the stellar parameter and chemical abundance homogenisation. In this way the WG10 homogenised results have been placed directly onto the WG11 stellar parameter and chemical abundance scales. The reference set for the metal-poor end was sparse which limited the effectiveness of the homogenisation in that regime. For WG11, the total number of stars for which stellar parameters were derived was 6 231 with typical uncertainties for Teff, log g and [Fe/H] of 32 K, 0.05 and 0.05 respectively. One or more chemical abundances out of a possible 39 elements were derived for 6 188 of the stars. For WG10, the total number of stars for which stellar parameters were derived was 76 675 with typical uncertainties for Teff, log g and [Fe/H] of 64 K, 0.15 and 0.07 respectively. One or more chemical abundances out of a possible 30 elements were
Published: 2024
Full Text: View/download PDF

3. The Gaia-ESO Survey : The DR5 analysis of the medium-resolution GIRAFFE and high-resolution UVES spectra of FGK-type stars

Author: Worley, C. C., Smiljanic, R., Magrini, L., Frasca, A., Franciosini, E., Montes, D., Feuillet, D. K., Tabernero, H. M., González Hernandez, J. I., Villanova, S., Mikolaitis, S., Lind, K., Tautvaisiene, G., Casey, A. R., Korn, Andreas J., Bonifacio, P., Soubiran, C., Caffau, E., Guiglion, G., Merle, T., Hourihane, A., Gonneau, A., François, P., Randich, S., Gilmore, G., Lewis, J. R., Murphy, D. N. A., Jeffries, R. D., Koposov, S. E., Blomme, R., Lanzafame, A. C., Bensby, T., Bragaglia, A., Alfaro, E. J., Walton, N. A., Vallenari, A., Prusti, T., Biazzo, K., Jofré, P., Zaggia, S., Heiter, Ulrike, Marfil, E., Jiménez-Esteban, F., Gutiérrez Albarran, M. L., Morbidelli, L., Worley, C. C., Smiljanic, R., Magrini, L., Frasca, A., Franciosini, E., Montes, D., Feuillet, D. K., Tabernero, H. M., González Hernandez, J. I., Villanova, S., Mikolaitis, S., Lind, K., Tautvaisiene, G., Casey, A. R., Korn, Andreas J., Bonifacio, P., Soubiran, C., Caffau, E., Guiglion, G., Merle, T., Hourihane, A., Gonneau, A., François, P., Randich, S., Gilmore, G., Lewis, J. R., Murphy, D. N. A., Jeffries, R. D., Koposov, S. E., Blomme, R., Lanzafame, A. C., Bensby, T., Bragaglia, A., Alfaro, E. J., Walton, N. A., Vallenari, A., Prusti, T., Biazzo, K., Jofré, P., Zaggia, S., Heiter, Ulrike, Marfil, E., Jiménez-Esteban, F., Gutiérrez Albarran, M. L., and Morbidelli, L.
Abstract: The Gaia-ESO Survey is an European Southern Observatory (ESO) public spectroscopic survey that targeted 105 stars in the Milky Way covering the major populations of the disk, bulge and halo. The observations were made using FLAMES on the VLT obtaining both UVES high (R ~ 47 000) and GIRAFFE medium (R ~ 20 000) resolution spectra. The analysis of the Gaia-ESO spectra was the work of multiple analysis teams (nodes) within five working groups (WG). The homogenisation of the stellar parameters within WG11 (high resolution observations of FGK stars) and the homogenisation of the stellar parameters within WG10 (medium resolution observations of FGK stars) is described here. In both cases, the homogenisation was carried out using a Bayesian Inference method developed specifically for the Gaia-ESO Survey by WG11. The method was also used for the chemical abundance homogenisation within WG11, however, the WG10 chemical abundance data set was too sparsely populated so basic corrections for each node analysis were employed for the homogenisation instead. The WG10 homogenisation primarily used the cross-match of stars with WG11 as the reference set in both the stellar parameter and chemical abundance homogenisation. In this way the WG10 homogenised results have been placed directly onto the WG11 stellar parameter and chemical abundance scales. The reference set for the metal-poor end was sparse which limited the effectiveness of the homogenisation in that regime. For WG11, the total number of stars for which stellar parameters were derived was 6 231 with typical uncertainties for Teff, log g and [Fe/H] of 32 K, 0.05 and 0.05 respectively. One or more chemical abundances out of a possible 39 elements were derived for 6 188 of the stars. For WG10, the total number of stars for which stellar parameters were derived was 76 675 with typical uncertainties for Teff, log g and [Fe/H] of 64 K, 0.15 and 0.07 respectively. One or more chemical abundances out of a possible 30 elements were
Published: 2024
Full Text: View/download PDF

4. The Gaia-ESO Survey : The DR5 analysis of the medium-resolution GIRAFFE and high-resolution UVES spectra of FGK-type stars

Author: Worley, C. C., Smiljanic, R., Magrini, L., Frasca, A., Franciosini, E., Montes, D., Feuillet, D. K., Tabernero, H. M., González Hernandez, J. I., Villanova, S., Mikolaitis, S., Lind, K., Tautvaisiene, G., Casey, A. R., Korn, Andreas J., Bonifacio, P., Soubiran, C., Caffau, E., Guiglion, G., Merle, T., Hourihane, A., Gonneau, A., François, P., Randich, S., Gilmore, G., Lewis, J. R., Murphy, D. N. A., Jeffries, R. D., Koposov, S. E., Blomme, R., Lanzafame, A. C., Bensby, T., Bragaglia, A., Alfaro, E. J., Walton, N. A., Vallenari, A., Prusti, T., Biazzo, K., Jofré, P., Zaggia, S., Heiter, Ulrike, Marfil, E., Jiménez-Esteban, F., Gutiérrez Albarran, M. L., Morbidelli, L., Worley, C. C., Smiljanic, R., Magrini, L., Frasca, A., Franciosini, E., Montes, D., Feuillet, D. K., Tabernero, H. M., González Hernandez, J. I., Villanova, S., Mikolaitis, S., Lind, K., Tautvaisiene, G., Casey, A. R., Korn, Andreas J., Bonifacio, P., Soubiran, C., Caffau, E., Guiglion, G., Merle, T., Hourihane, A., Gonneau, A., François, P., Randich, S., Gilmore, G., Lewis, J. R., Murphy, D. N. A., Jeffries, R. D., Koposov, S. E., Blomme, R., Lanzafame, A. C., Bensby, T., Bragaglia, A., Alfaro, E. J., Walton, N. A., Vallenari, A., Prusti, T., Biazzo, K., Jofré, P., Zaggia, S., Heiter, Ulrike, Marfil, E., Jiménez-Esteban, F., Gutiérrez Albarran, M. L., and Morbidelli, L.
Abstract: The Gaia-ESO Survey is an European Southern Observatory (ESO) public spectroscopic survey that targeted 105 stars in the Milky Way covering the major populations of the disk, bulge and halo. The observations were made using FLAMES on the VLT obtaining both UVES high (R ~ 47 000) and GIRAFFE medium (R ~ 20 000) resolution spectra. The analysis of the Gaia-ESO spectra was the work of multiple analysis teams (nodes) within five working groups (WG). The homogenisation of the stellar parameters within WG11 (high resolution observations of FGK stars) and the homogenisation of the stellar parameters within WG10 (medium resolution observations of FGK stars) is described here. In both cases, the homogenisation was carried out using a Bayesian Inference method developed specifically for the Gaia-ESO Survey by WG11. The method was also used for the chemical abundance homogenisation within WG11, however, the WG10 chemical abundance data set was too sparsely populated so basic corrections for each node analysis were employed for the homogenisation instead. The WG10 homogenisation primarily used the cross-match of stars with WG11 as the reference set in both the stellar parameter and chemical abundance homogenisation. In this way the WG10 homogenised results have been placed directly onto the WG11 stellar parameter and chemical abundance scales. The reference set for the metal-poor end was sparse which limited the effectiveness of the homogenisation in that regime. For WG11, the total number of stars for which stellar parameters were derived was 6 231 with typical uncertainties for Teff, log g and [Fe/H] of 32 K, 0.05 and 0.05 respectively. One or more chemical abundances out of a possible 39 elements were derived for 6 188 of the stars. For WG10, the total number of stars for which stellar parameters were derived was 76 675 with typical uncertainties for Teff, log g and [Fe/H] of 64 K, 0.15 and 0.07 respectively. One or more chemical abundances out of a possible 30 elements were
Published: 2024
Full Text: View/download PDF

5. The Gaia-ESO Survey : The DR5 analysis of the medium-resolution GIRAFFE and high-resolution UVES spectra of FGK-type stars

Author: Worley, C. C., Smiljanic, R., Magrini, L., Frasca, A., Franciosini, E., Montes, D., Feuillet, D. K., Tabernero, H. M., González Hernandez, J. I., Villanova, S., Mikolaitis, S., Lind, K., Tautvaisiene, G., Casey, A. R., Korn, Andreas J., Bonifacio, P., Soubiran, C., Caffau, E., Guiglion, G., Merle, T., Hourihane, A., Gonneau, A., François, P., Randich, S., Gilmore, G., Lewis, J. R., Murphy, D. N. A., Jeffries, R. D., Koposov, S. E., Blomme, R., Lanzafame, A. C., Bensby, T., Bragaglia, A., Alfaro, E. J., Walton, N. A., Vallenari, A., Prusti, T., Biazzo, K., Jofré, P., Zaggia, S., Heiter, Ulrike, Marfil, E., Jiménez-Esteban, F., Gutiérrez Albarran, M. L., Morbidelli, L., Worley, C. C., Smiljanic, R., Magrini, L., Frasca, A., Franciosini, E., Montes, D., Feuillet, D. K., Tabernero, H. M., González Hernandez, J. I., Villanova, S., Mikolaitis, S., Lind, K., Tautvaisiene, G., Casey, A. R., Korn, Andreas J., Bonifacio, P., Soubiran, C., Caffau, E., Guiglion, G., Merle, T., Hourihane, A., Gonneau, A., François, P., Randich, S., Gilmore, G., Lewis, J. R., Murphy, D. N. A., Jeffries, R. D., Koposov, S. E., Blomme, R., Lanzafame, A. C., Bensby, T., Bragaglia, A., Alfaro, E. J., Walton, N. A., Vallenari, A., Prusti, T., Biazzo, K., Jofré, P., Zaggia, S., Heiter, Ulrike, Marfil, E., Jiménez-Esteban, F., Gutiérrez Albarran, M. L., and Morbidelli, L.
Abstract: The Gaia-ESO Survey is an European Southern Observatory (ESO) public spectroscopic survey that targeted 105 stars in the Milky Way covering the major populations of the disk, bulge and halo. The observations were made using FLAMES on the VLT obtaining both UVES high (R ~ 47 000) and GIRAFFE medium (R ~ 20 000) resolution spectra. The analysis of the Gaia-ESO spectra was the work of multiple analysis teams (nodes) within five working groups (WG). The homogenisation of the stellar parameters within WG11 (high resolution observations of FGK stars) and the homogenisation of the stellar parameters within WG10 (medium resolution observations of FGK stars) is described here. In both cases, the homogenisation was carried out using a Bayesian Inference method developed specifically for the Gaia-ESO Survey by WG11. The method was also used for the chemical abundance homogenisation within WG11, however, the WG10 chemical abundance data set was too sparsely populated so basic corrections for each node analysis were employed for the homogenisation instead. The WG10 homogenisation primarily used the cross-match of stars with WG11 as the reference set in both the stellar parameter and chemical abundance homogenisation. In this way the WG10 homogenised results have been placed directly onto the WG11 stellar parameter and chemical abundance scales. The reference set for the metal-poor end was sparse which limited the effectiveness of the homogenisation in that regime. For WG11, the total number of stars for which stellar parameters were derived was 6 231 with typical uncertainties for Teff, log g and [Fe/H] of 32 K, 0.05 and 0.05 respectively. One or more chemical abundances out of a possible 39 elements were derived for 6 188 of the stars. For WG10, the total number of stars for which stellar parameters were derived was 76 675 with typical uncertainties for Teff, log g and [Fe/H] of 64 K, 0.15 and 0.07 respectively. One or more chemical abundances out of a possible 30 elements were
Published: 2024
Full Text: View/download PDF

6. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., Minkeviciute, R., Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., and Minkeviciute, R.
Abstract: The Gaia-ESO Survey is a public spectroscopic survey that targeted greater than or similar to 10(5) stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (T-eff similar to 30 000-52 000 K) all the way to K-M (greater than or similar to 3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
Published: 2023
Full Text: View/download PDF

7. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., Minkeviciute, R., Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., and Minkeviciute, R.
Abstract: The Gaia-ESO Survey is a public spectroscopic survey that targeted greater than or similar to 10(5) stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (T-eff similar to 30 000-52 000 K) all the way to K-M (greater than or similar to 3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
Published: 2023
Full Text: View/download PDF

8. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., Minkeviciute, R., Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., and Minkeviciute, R.
Abstract: The Gaia-ESO Survey is a public spectroscopic survey that targeted greater than or similar to 10(5) stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (T-eff similar to 30 000-52 000 K) all the way to K-M (greater than or similar to 3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
Published: 2023
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9. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., Minkeviciute, R., Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., and Minkeviciute, R.
Abstract: The Gaia-ESO Survey is a public spectroscopic survey that targeted greater than or similar to 10(5) stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (T-eff similar to 30 000-52 000 K) all the way to K-M (greater than or similar to 3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
Published: 2023
Full Text: View/download PDF

10. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., Minkeviciute, R., Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., and Minkeviciute, R.
Abstract: The Gaia-ESO Survey is a public spectroscopic survey that targeted greater than or similar to 10(5) stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (T-eff similar to 30 000-52 000 K) all the way to K-M (greater than or similar to 3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
Published: 2023
Full Text: View/download PDF

11. The Gaia-ESO Survey : Target selection of open cluster stars & x22c6

Author: Bragaglia, A., Alfaro, E. J., Flaccomio, E., Blomme, R., Donati, P., Costado, M., Damiani, F., Franciosini, E., Prisinzano, L., Randich, S., Friel, E. D., Hatztidimitriou, D., Vallenari, A., Spagna, A., Balaguer-Nunez, L., Bonito, R., Gaudin, T. Cantat, Casamiquela, L., Jeffries, R. D., Jordi, C., Magrini, L., Drew, J. E., Jackson, R. J., Abbas, U., Caramazza, M., Hayes, C., Jimenez-Esteban, F. M., Fiorentin, P. Re, Wright, N., Bayo, A., Bensb, T., Bergemann, M., Gilmore, G., Gonneau, A., Heiter, Ulrike, Hourihane, A., Pancino, E., Sacco, G., Smiljanic, R., Zaggia, S., Vink, J. S., Bragaglia, A., Alfaro, E. J., Flaccomio, E., Blomme, R., Donati, P., Costado, M., Damiani, F., Franciosini, E., Prisinzano, L., Randich, S., Friel, E. D., Hatztidimitriou, D., Vallenari, A., Spagna, A., Balaguer-Nunez, L., Bonito, R., Gaudin, T. Cantat, Casamiquela, L., Jeffries, R. D., Jordi, C., Magrini, L., Drew, J. E., Jackson, R. J., Abbas, U., Caramazza, M., Hayes, C., Jimenez-Esteban, F. M., Fiorentin, P. Re, Wright, N., Bayo, A., Bensb, T., Bergemann, M., Gilmore, G., Gonneau, A., Heiter, Ulrike, Hourihane, A., Pancino, E., Sacco, G., Smiljanic, R., Zaggia, S., and Vink, J. S.
Abstract: Context. The Gaia-ESO Survey (GES) is a public, high-resolution spectroscopic survey, conducted with the multi-object spectrograph Fibre Large Array Multi Element Spectrograph (FLAMES) on the Very Large Telescope (European Southern Observatory, ESO, Cerro Paranal, Chile) from December 2011 to January 2018. Gaia-ESO has targeted all the main stellar components of the Milky Way, including thin and thick disc, bulge, and halo. In particular, a large sample of open clusters has been observed, from very young ones, just out of the embedded phase, to very old ones. Aims. The different kinds of clusters and stars targeted in them are useful to reach the main science goals of the open cluster part of GES, which are the study of the open cluster structure and dynamics, the use of open clusters to constrain and improve stellar evolution models, and the definition of Galactic disc properties (e.g., metallicity distribution). Methods. The Gaia-ESO Survey is organised in 19 working groups (WGs), each one being responsible for a task. We describe here the work of three of them, one in charge of the selection of the targets within each cluster or association (WG4), one responsible for defining the most probable candidate member stars (WG1), and another one in charge of the preparation of the observations (WG6). As the entire GES has been conducted before the second Gaia data release, we could not make use of the Gaia astrometry to define cluster member candidates. We made use of public and private photometry to select the stars to be observed with FLAMES, once brought on a common astrometric system (the one defined by 2MASS). Candidate target selection was based on ground-based proper motions, radial velocities, and X-ray properties when appropriate, for example, and it was mostly used to define the position of the clusters' evolutionary sequences in the colour-magnitude diagrams. Targets for GIRAFFE were then selected near the sequences in an unbiased way. We used known informati
Published: 2022
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12. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022
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13. The Gaia-ESO Public Spectroscopic Survey : Implementation, data products, open cluster survey, science, and legacy

Author: Randich, S., Gilmore, G., Magrini, L., Sacco, G. G., Jackson, R. J., Jeffries, R. D., Worley, C. C., Hourihane, A., Gonneau, A., Vazquez, C. Viscasillas, Franciosini, E., Lewis, J. R., Alfaro, E. J., Allende Prieto, C., Bensby, T., Blomme, R., Bragaglia, A., Flaccomio, E., Francois, P., Irwin, M. J., Koposov, S. E., Korn, Andreas, Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bayo, A., Bergemann, M., Biazzo, K., Carraro, G., Casey, A. R., Damiani, F., Frasca, A., Heiter, Ulrike, Hill, V, Jofre, P., de Laverny, P., Lind, K., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Morbidelli, L., Prisinzano, L., Sbordone, L., Sousa, S. G., Zaggia, S., Adibekyan, V, Bonito, R., Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Maiz Apellaniz, J., Montes, D., Morel, T., Soubiran, C., Spina, L., Tabernero, H. M., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Wright, N. J., Abbas, U., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Friel, E. D., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Hatzidimitriou, D., Held, E. , V, Jimenez-Esteban, F., Jonsson, H., Jordi, C., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Paunzen, E., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. , I, Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spagna, A., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Vink, J. S., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Walton, N. A., Randich, S., Gilmore, G., Magrini, L., Sacco, G. G., Jackson, R. J., Jeffries, R. D., Worley, C. C., Hourihane, A., Gonneau, A., Vazquez, C. Viscasillas, Franciosini, E., Lewis, J. R., Alfaro, E. J., Allende Prieto, C., Bensby, T., Blomme, R., Bragaglia, A., Flaccomio, E., Francois, P., Irwin, M. J., Koposov, S. E., Korn, Andreas, Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bayo, A., Bergemann, M., Biazzo, K., Carraro, G., Casey, A. R., Damiani, F., Frasca, A., Heiter, Ulrike, Hill, V, Jofre, P., de Laverny, P., Lind, K., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Morbidelli, L., Prisinzano, L., Sbordone, L., Sousa, S. G., Zaggia, S., Adibekyan, V, Bonito, R., Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Maiz Apellaniz, J., Montes, D., Morel, T., Soubiran, C., Spina, L., Tabernero, H. M., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Wright, N. J., Abbas, U., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Friel, E. D., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Hatzidimitriou, D., Held, E. , V, Jimenez-Esteban, F., Jonsson, H., Jordi, C., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Paunzen, E., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. , I, Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spagna, A., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Vink, J. S., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., and Walton, N. A.
Abstract: Context. In the last 15 years different ground-based spectroscopic surveys have been started (and completed) with the general aim of delivering stellar parameters and elemental abundances for large samples of Galactic stars, complementing Gaia astrometry. Among those surveys, the Gaia-ESO Public Spectroscopic Survey, the only one performed on a 8m class telescope, was designed to target 100 000 stars using FLAMES on the ESO VLT (both Giraffe and UVES spectrographs), covering all the Milky Way populations, with a special focus on open star clusters. Aims. This article provides an overview of the survey implementation (observations, data quality, analysis and its success, data products, and releases), of the open cluster survey, of the science results and potential, and of the survey legacy. A companion article reviews the overall survey motivation, strategy, Giraffe pipeline data reduction, organisation, and workflow. Methods. We made use of the information recorded and archived in the observing blocks; during the observing runs; in a number of relevant documents; in the spectra and master catalogue of spectra; in the parameters delivered by the analysis nodes and the working groups; in the final catalogue; and in the science papers. Based on these sources, we critically analyse and discuss the output and products of the Survey, including science highlights. We also determined the average metallicities of the open clusters observed as science targets and of a sample of clusters whose spectra were retrieved from the ESO archive. Results. The Gaia-ESO Survey has determined homogeneous good-quality radial velocities and stellar parameters for a large fraction of its more than 110 000 unique target stars. Elemental abundances were derived for up to 31 elements for targets observed with UVES. Lithium abundances are delivered for about 1/3 of the sample. The analysis and homogenisation strategies have proven to be successful; several science topics have been addressed by t
Published: 2022
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14. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022
Full Text: View/download PDF

15. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, A. J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, P. S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jönsson, Henrik, Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. , I, Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, A. J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, P. S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jönsson, Henrik, Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. , I, Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022
Full Text: View/download PDF

16. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022
Full Text: View/download PDF

17. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022
Full Text: View/download PDF

18. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, A. J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, P. S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jönsson, Henrik, Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. , I, Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, A. J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, P. S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jönsson, Henrik, Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. , I, Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022
Full Text: View/download PDF

19. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022
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20. The Gaia-ESO survey : a lithium depletion boundary age for NGC 2232

Author: Binks, A. S., Jeffries, R. D., Jackson, R. J., Franciosini, E., Sacco, G. G., Bayo, A., Magrini, L., Randich, S., Arancibia-Silva, J., Bergemann, M., Bragaglia, A., Gilmore, G., Gonneau, A., Hourihane, A., Jofre, P., Korn, Andreas, Morbidelli, L., Prisinzano, L., Worley, C. C., Zaggia, S., Binks, A. S., Jeffries, R. D., Jackson, R. J., Franciosini, E., Sacco, G. G., Bayo, A., Magrini, L., Randich, S., Arancibia-Silva, J., Bergemann, M., Bragaglia, A., Gilmore, G., Gonneau, A., Hourihane, A., Jofre, P., Korn, Andreas, Morbidelli, L., Prisinzano, L., Worley, C. C., and Zaggia, S.
Abstract: Astrometry and photometry from Gaia and spectroscopic data from the Gaia-ESO Survey (GES) are used to identify the lithium depletion boundary (LDB) in the young cluster NGC 2232. A specialized spectral line analysis procedure was used to recover the signature of undepleted lithium in very low luminosity cluster members. An age of 38 +/- 3 Myr is inferred by comparing the LDB location in absolute colour-magnitude diagrams (CMDs) with the predictions of standard models. This is more than twice the age derived from fitting isochrones to low-mass stars in the CMD with the same models. Much closer agreement between LDB and CMD ages is obtained from models that incorporate magnetically suppressed convection or flux-blocking by dark, magnetic starspots. The best agreement is found at ages of 45-50 Myr for models with high levels of magnetic activity and starspot coverage fractions >50 percent, although a uniformly high spot coverage does not match the CMD well across the full luminosity range considered.
Published: 2021
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21. The Gaia-ESO Survey : the present-day radial metallicity distribution of the Galactic disc probed by pre-main-sequence clusters

Author: Spina, L., Randich, S., Magrini, L., Jeffries, R. D., Friel, E. D., Sacco, G. G., Pancino, E., Bonito, R., Bravi, L., Franciosini, E., Klutsch, A., Montes, D., Gilmore, G., Vallenari, A., Bensby, T., Bragaglia, A., Flaccomio, E., Koposov, S. E., Korn, Andreas J., Lanzafame, A. C., Smiljanic, R., Bayo, A., Carraro, G., Casey, A. R., Costado, M. T., Damiani, F., Donati, P., Frasca, A., Hourihane, A., Jofre, P., Lewis, J., Lind, K., Monaco, L., Morbidelli, L., Prisinzano, L., Sousa, S. G., Worley, C. C., Zaggia, S., Spina, L., Randich, S., Magrini, L., Jeffries, R. D., Friel, E. D., Sacco, G. G., Pancino, E., Bonito, R., Bravi, L., Franciosini, E., Klutsch, A., Montes, D., Gilmore, G., Vallenari, A., Bensby, T., Bragaglia, A., Flaccomio, E., Koposov, S. E., Korn, Andreas J., Lanzafame, A. C., Smiljanic, R., Bayo, A., Carraro, G., Casey, A. R., Costado, M. T., Damiani, F., Donati, P., Frasca, A., Hourihane, A., Jofre, P., Lewis, J., Lind, K., Monaco, L., Morbidelli, L., Prisinzano, L., Sousa, S. G., Worley, C. C., and Zaggia, S.
Abstract: Context. The radial metallicity distribution in the Galactic thin disc represents a crucial constraint for modelling disc formation and evolution. Open star clusters allow us to derive both the radial metallicity distribution and its evolution over time. Aims. In this paper we perform the first investigation of the present-day radial metallicity distribution based on [Fe/H] determinations in late type members of pre-main-sequence clusters. Because of their youth, these clusters are therefore essential for tracing the current interstellar medium metallicity. Methods. We used the products of the Gaia-ESO Survey analysis of 12 young regions (age < 100 Myr), covering Galactocentric distances from 6.67 to 8.70 kpc. For the first time, we derived the metal content of star forming regions farther than 500 pc from the Sun. Median metallicities were determined through samples of reliable cluster members. For ten clusters the membership analysis is discussed in the present paper, while for other two clusters (i.e. Chamaeleon I and Gamma Velorum) we adopted the members identified in our previous works. Results. All the pre-main-sequence clusters considered in this paper have close-to-solar or slightly sub-solar metallicities. The radial metallicity distribution traced by these clusters is almost flat, with the innermost star forming regions having [Fe/H] values that are 0.10-0.15 dex lower than the majority of the older clusters located at similar Galactocentric radii. Conclusions. This homogeneous study of the present-day radial metallicity distribution in the Galactic thin disc favours models that predict a flattening of the radial gradient over time. On the other hand, the decrease of the average [Fe/H] at young ages is not easily explained by the models. Our results reveal a complex interplay of several processes (e.g. star formation activity, initial mass function, supernova yields, gas flows) that controlled the recent evolution of the Milky Way.
Published: 2017
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22. The Gaia-ESO Survey : revisiting the Li-rich giant problem

Author: Casey, A. R., Ruchti, G., Masseron, T., Randich, S., Gilmore, G., Lind, Karin, Kennedy, G. M., Koposov, S. E., Hourihane, A., Franciosini, E., Lewis, J. R., Magrini, L., Morbidelli, L., Sacco, G. G., Worley, C. C., Feltzing, S., Jeffries, R. D., Vallenari, A., Bensby, T., Bragaglia, A., Flaccomio, E., Francois, P., Korn, Andreas J., Lanzafame, A., Pancino, E., Recio-Blanco, A., Smiljanic, R., Carraro, G., Costado, M. T., Damiani, F., Donati, P., Frasca, A., Jofre, P., Lardo, C., de Laverny, P., Monaco, L., Prisinzano, L., Sbordone, L., Sousa, S. G., Tautvaisiene, G., Zaggia, S., Zwitter, T., Delgado Mena, E., Chorniy, Y., Martell, S. L., Aguirre, V. Silva, Miglio, A., Chiappini, C., Montalban, J., Morel, T., Valentini, M., Casey, A. R., Ruchti, G., Masseron, T., Randich, S., Gilmore, G., Lind, Karin, Kennedy, G. M., Koposov, S. E., Hourihane, A., Franciosini, E., Lewis, J. R., Magrini, L., Morbidelli, L., Sacco, G. G., Worley, C. C., Feltzing, S., Jeffries, R. D., Vallenari, A., Bensby, T., Bragaglia, A., Flaccomio, E., Francois, P., Korn, Andreas J., Lanzafame, A., Pancino, E., Recio-Blanco, A., Smiljanic, R., Carraro, G., Costado, M. T., Damiani, F., Donati, P., Frasca, A., Jofre, P., Lardo, C., de Laverny, P., Monaco, L., Prisinzano, L., Sbordone, L., Sousa, S. G., Tautvaisiene, G., Zaggia, S., Zwitter, T., Delgado Mena, E., Chorniy, Y., Martell, S. L., Aguirre, V. Silva, Miglio, A., Chiappini, C., Montalban, J., Morel, T., and Valentini, M.
Abstract: The discovery of lithium-rich giants contradicts expectations from canonical stellar evolution. Here we report on the serendipitous discovery of 20 Li-rich giants observed during the Gaia-ESO Survey, which includes the first nine Li-rich giant stars known towards the CoRoT fields. Most of our Li-rich giants have near-solar metallicities and stellar parameters consistent with being before the luminosity bump. This is difficult to reconcile with deep mixing models proposed to explain lithium enrichment, because these models can only operate at later evolutionary stages: at or past the luminosity bump. In an effort to shed light on the Li-rich phenomenon, we highlight recent evidence of the tidal destruction of close-in hot Jupiters at the sub-giant phase. We note that when coupled with models of planet accretion, the observed destruction of hot Jupiters actually predicts the existence of Li-rich giant stars, and suggests that Li-rich stars should be found early on the giant branch and occur more frequently with increasing metallicity. A comprehensive review of all known Li-rich giant stars reveals that this scenario is consistent with the data. However, more evolved or metal-poor stars are less likely to host close-in giant planets, implying that their Li-rich origin requires an alternative explanation, likely related to mixing scenarios rather than external phenomena.
Published: 2016
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22 results on '"Jeffries, R. D."'

1. The Gaia-ESO Survey : The DR5 analysis of the medium-resolution GIRAFFE and high-resolution UVES spectra of FGK-type stars

2. The Gaia-ESO Survey : The DR5 analysis of the medium-resolution GIRAFFE and high-resolution UVES spectra of FGK-type stars

3. The Gaia-ESO Survey : The DR5 analysis of the medium-resolution GIRAFFE and high-resolution UVES spectra of FGK-type stars

4. The Gaia-ESO Survey : The DR5 analysis of the medium-resolution GIRAFFE and high-resolution UVES spectra of FGK-type stars

5. The Gaia-ESO Survey : The DR5 analysis of the medium-resolution GIRAFFE and high-resolution UVES spectra of FGK-type stars

6. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

7. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

8. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

9. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

10. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

11. The Gaia-ESO Survey : Target selection of open cluster stars & x22c6

12. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

13. The Gaia-ESO Public Spectroscopic Survey : Implementation, data products, open cluster survey, science, and legacy

14. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

15. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

16. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

17. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

18. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

19. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

20. The Gaia-ESO survey : a lithium depletion boundary age for NGC 2232

21. The Gaia-ESO Survey : the present-day radial metallicity distribution of the Galactic disc probed by pre-main-sequence clusters

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

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