Author: "Damiani F." / Publisher: edp sciences - Searchworks@Jio Institute Digital Library Search Results

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164 results on '"Damiani F."'

1. The magnetosphere of the close accreting PMS binary V4046 Sgr

Author: Gregory S. G., Holzwarth V. R., Donati J.-F., Hussain G. A. J., Montmerle T., Alecian E., Alencar S. H. P., Argiroffi C., Audard M., Bouvier J., Damiani F., Güdel M., Huenemoerder D. P., Kastner J. H., Maggio A., Sacco G. G., and Wade G. A.
Subjects: Physics, QC1-999
Abstract: V4046 Sagittarii AB is a close short-period classical T Tauri binary. It is a circularised and synchronised system accreting from a circumbinary disk. In 2009 it was observed as part of a coordinated program involving near-simultaneous spectropolarimetric observations with ESPaDOnS at the Canada-France-Hawai’i Telescope and high-resolution X-ray observations with XMM-Newton. Magnetic maps of each star were derived from Zeeman-Doppler imaging. After briefly highlighting the most significant observational findings, we present a preliminary 3D model of the binary magnetosphere constructed from the magnetic maps using a newly developed binary magnetic field extrapolation code. The large-scale fields (the dipole components) of both stars are highly tilted with respect to their rotation axes, and their magnetic fields are linked.
Published: 2014
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2. EWOCS-I: The catalog of X-ray sources in Westerlund 1 from the Extended Westerlund 1 and 2 Open Clusters Survey

Author: Universidad de Alicante. Departamento de Física Aplicada, Guarcello, Mario Giuseppe, Flaccomio, E., Albacete-Colombo, J. F., Almendros-Abad, Víctor, Anastasopoulou, Konstantina, Andersen, M., Argiroffi, C., Bayo, A., Bartlett, Elizabeth S., Bastian, N., De Becker, Michaël, Best, William, Bonito, R., Borghese, Alice, Calzetti, D., Castellanos, Raul, Cecchi-Pestellini, C., Clark, J. Simon, Clarke, C.J., Coti Zelati, Francesco, Damiani, F., Drake, J.J., Gennaro, Mario, Ginsburg, A., Grebel, E.K., Hora, Joseph L., Israel, Gian Luca, Lawrence, Grace, Locci, D., Mapelli, M., Martinez-Galarza, J.R., Micela, G., Miceli, M., Moraux, E., Muzic, K., Najarro de la Parra, Francisco, Negueruela, Ignacio, Nota, A., Pallanca, C., Prisinzano, L., Ritchie, Benedict, Robberto, M., Rom, Tamara, Sabbi, Elena, Scholz, A., Sciortino, Salvatore, Trigilio, Corrado, Umana, G., Winter, A., Wright, N.J., Zeidler, Peter, Universidad de Alicante. Departamento de Física Aplicada, Guarcello, Mario Giuseppe, Flaccomio, E., Albacete-Colombo, J. F., Almendros-Abad, Víctor, Anastasopoulou, Konstantina, Andersen, M., Argiroffi, C., Bayo, A., Bartlett, Elizabeth S., Bastian, N., De Becker, Michaël, Best, William, Bonito, R., Borghese, Alice, Calzetti, D., Castellanos, Raul, Cecchi-Pestellini, C., Clark, J. Simon, Clarke, C.J., Coti Zelati, Francesco, Damiani, F., Drake, J.J., Gennaro, Mario, Ginsburg, A., Grebel, E.K., Hora, Joseph L., Israel, Gian Luca, Lawrence, Grace, Locci, D., Mapelli, M., Martinez-Galarza, J.R., Micela, G., Miceli, M., Moraux, E., Muzic, K., Najarro de la Parra, Francisco, Negueruela, Ignacio, Nota, A., Pallanca, C., Prisinzano, L., Ritchie, Benedict, Robberto, M., Rom, Tamara, Sabbi, Elena, Scholz, A., Sciortino, Salvatore, Trigilio, Corrado, Umana, G., Winter, A., Wright, N.J., and Zeidler, Peter
Abstract: Context. With a mass exceeding several 104 M⊙ and a rich and dense population of massive stars, supermassive young star clusters represent the most massive star-forming environment that is dominated by the feedback from massive stars and gravitational interactions among stars. Aims. In this paper we present the Extended Westerlund 1 and 2 Open Clusters Survey (EWOCS) project, which aims to investigate the influence of the starburst environment on the formation of stars and planets, and on the evolution of both low and high mass stars. The primary targets of this project are Westerlund 1 and 2, the closest supermassive star clusters to the Sun. Methods. The project is based primarily on recent observations conducted with the Chandra and JWST observatories. Specifically, the Chandra survey of Westerlund 1 consists of 36 new ACIS-I observations, nearly co-pointed, for a total exposure time of 1 Msec. Additionally, we included 8 archival Chandra/ACIS-S observations. This paper presents the resulting catalog of X-ray sources within and around Westerlund 1. Sources were detected by combining various existing methods, and photon extraction and source validation were carried out using the ACIS-Extract software. Results. The EWOCS X-ray catalog comprises 5963 validated sources out of the 9420 initially provided to ACIS-Extract, reaching a photon flux threshold of approximately 2 × 10−8 photons cm−2 s−1. The X-ray sources exhibit a highly concentrated spatial distribution, with 1075 sources located within the central 1 arcmin. We have successfully detected X-ray emissions from 126 out of the 166 known massive stars of the cluster, and we have collected over 71 000 photons from the magnetar CXO J164710.20-455217.
Published: 2024

3. EWOCS-I: The catalog of X-ray sources in Westerlund 1 from the Extended Westerlund 1 and 2 Open Clusters Survey

Author: Guarcello, M. G., primary, Flaccomio, E., additional, Albacete-Colombo, J. F., additional, Almendros-Abad, V., additional, Anastasopoulou, K., additional, Andersen, M., additional, Argiroffi, C., additional, Bayo, A., additional, Bartlett, E. S., additional, Bastian, N., additional, De Becker, M., additional, Best, W., additional, Bonito, R., additional, Borghese, A., additional, Calzetti, D., additional, Castellanos, R., additional, Cecchi-Pestellini, C., additional, Clark, J. S., additional, Clarke, C. J., additional, Zelati, F. Coti, additional, Damiani, F., additional, Drake, J. J., additional, Gennaro, M., additional, Ginsburg, A., additional, Grebel, E. K., additional, Hora, J. L., additional, Israel, G. L., additional, Lawrence, G., additional, Locci, D., additional, Mapelli, M., additional, Martinez-Galarza, J. R., additional, Micela, G., additional, Miceli, M., additional, Moraux, E., additional, Muzic, K., additional, Najarro, F., additional, Negueruela, I., additional, Nota, A., additional, Pallanca, C., additional, Prisinzano, L., additional, Ritchie, B., additional, Robberto, M., additional, Rom, T., additional, Sabbi, E., additional, Scholz, A., additional, Sciortino, S., additional, Trigilio, C., additional, Umana, G., additional, Winter, A., additional, Wright, N. J., additional, and Zeidler, P., additional
Published: 2024
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4. The Gaia-ESO Survey: Calibrating the lithium–age relation with open clusters and associations: II. Expanded cluster sample and final membership selection.

Author: Gutiérrez Albarrán, M. L., Montes, D., Tabernero, H. M., González Hernández, J. I., Marfil, E., Frasca, A., Lanzafame, A. C., Klutsch, A., Franciosini, E., Randich, S., Smiljanic, R., Korn, A. J., Gilmore, G., Alfaro, E. J., Bensby, T., Biazzo, K., Casey, A., Carraro, G., Damiani, F., and Feltzing, S.
Subjects: OPEN clusters of stars, MAIN sequence (Astronomy), STAR clusters, CLUSTER sampling, STELLAR rotation, STARS, AGE of stars
Abstract: Context. The Li abundance observed in pre-main sequence and main sequence late-type stars is strongly age-dependent, but also shows a complex pattern depending on several parameters, such as rotation, chromospheric activity, and metallicity. The best way to calibrate these effects, and with the aim of studying Li as an age indicator for FGK stars, is to calibrate coeval groups of stars, such as open clusters (OCs) and associations. Aims. We present a considerable target sample of 42 OCs and associations – with an age range from 1 Myr to 5 Gyr – observed within the Gaia-ESO survey (GES), and using the latest data provided by GES iDR6 and the most recent release of Gaia that was then available, EDR3. As part of this study, we update and improve the membership analysis for all 20 OCs presented in our previous article. Methods. We perform detailed membership analyses for all target clusters to identify likely candidates, using all available parameters provided by GES, complemented with detailed bibliographical searches, and based on numerous criteria: from radial velocity distributions, to the astrometry (proper motions and parallaxes) and photometry provided by Gaia, to gravity indicators (log g and the γ index), [Fe/H] metallicity, and Li content in diagrams of (Li equivalent widths) EW(Li) versus Teff. Results. We obtain updated lists of cluster members for the whole target sample, as well as a selection of Li-rich giant contaminants obtained as an additional result of the membership process. Each selection of cluster candidates was thoroughly contrasted with numerous existing membership studies using data from Gaia to ensure the most robust results. Conclusions. These final cluster selections will be used in the third and last paper of this series, which reports the results of a comparative study characterising the observable Li dispersion in each cluster and analysing its dependence on several parameters, allowing us to calibrate a Li–age relation and obtain a series of empirical Li envelopes for key ages in our sample. [ABSTRACT FROM AUTHOR]
Published: 2024
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5. The Gaia-ESO Survey: Homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., primary, François, P., additional, Worley, C. C., additional, Magrini, L., additional, Gonneau, A., additional, Casey, A. R., additional, Gilmore, G., additional, Randich, S., additional, Sacco, G. G., additional, Recio-Blanco, A., additional, Korn, A. J., additional, Allende Prieto, C., additional, Smiljanic, R., additional, Blomme, R., additional, Bragaglia, A., additional, Walton, N. A., additional, Van Eck, S., additional, Bensby, T., additional, Lanzafame, A., additional, Frasca, A., additional, Franciosini, E., additional, Damiani, F., additional, Lind, K., additional, Bergemann, M., additional, Bonifacio, P., additional, Hill, V., additional, Lobel, A., additional, Montes, D., additional, Feuillet, D. K., additional, Tautvaišienė, G., additional, Guiglion, G., additional, Tabernero, H. M., additional, González Hernández, J. I., additional, Gebran, M., additional, Van der Swaelmen, M., additional, Mikolaitis, Š., additional, Daflon, S., additional, Merle, T., additional, Morel, T., additional, Lewis, J. R., additional, González Solares, E. A., additional, Murphy, D. N. A., additional, Jeffries, R. D., additional, Jackson, R. J., additional, Feltzing, S., additional, Prusti, T., additional, Carraro, G., additional, Biazzo, K., additional, Prisinzano, L., additional, Jofré, P., additional, Zaggia, S., additional, Drazdauskas, A., additional, Stonkuté, E., additional, Marfil, E., additional, Jiménez-Esteban, F., additional, Mahy, L., additional, Gutiérrez Albarrán, M. L., additional, Berlanas, S. R., additional, Santos, W., additional, Morbidelli, L., additional, Spina, L., additional, and Minkevičiūtė, R., additional
Published: 2023
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6. The Gaia-ESO Survey: Homogenisation of stellar parameters and elemental abundances

Author: Universidad de Alicante. Departamento de Física Aplicada, Hourihane, A., François, P., Worley, C.C., Magrini, L., Gonneau, A., Casey, A.R., Gilmore, Gerard, Randich, Sofia, Sacco, G.G., Recio-Blanco, A., Korn, A., Allende Prieto, C., Smiljanic, R., Blomme, Ronny, Bragaglia, A., Walton, N., Van Eck, S., Bensby, T., Lanzafame, A.C., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, Alex, Montes, David, Feuillet, D.K., Tautvaišienė, G., Guiglion, G., Tabernero, Hugo M., González Hernández, J.I., Gebran, M., Van der Swaelmen, M., Mikolaitis, Š., Daflon, Simone, Merle, T., Morel, Thierry, Lewis, J., González Solares, E.A., Murphy, D.N.A., Jeffries, R., Jackson, R.J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkuté, E., Marfil, E., Jiménez Esteban, Francisco M., Mahy, Laurent, Gutiérrez Albarrán, M.L., Berlanas, Sara R., Santos, W., Morbidelli, L., Spina, L., Minkevičiūtė, R., Universidad de Alicante. Departamento de Física Aplicada, Hourihane, A., François, P., Worley, C.C., Magrini, L., Gonneau, A., Casey, A.R., Gilmore, Gerard, Randich, Sofia, Sacco, G.G., Recio-Blanco, A., Korn, A., Allende Prieto, C., Smiljanic, R., Blomme, Ronny, Bragaglia, A., Walton, N., Van Eck, S., Bensby, T., Lanzafame, A.C., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, Alex, Montes, David, Feuillet, D.K., Tautvaišienė, G., Guiglion, G., Tabernero, Hugo M., González Hernández, J.I., Gebran, M., Van der Swaelmen, M., Mikolaitis, Š., Daflon, Simone, Merle, T., Morel, Thierry, Lewis, J., González Solares, E.A., Murphy, D.N.A., Jeffries, R., Jackson, R.J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkuté, E., Marfil, E., Jiménez Esteban, Francisco M., Mahy, Laurent, Gutiérrez Albarrán, M.L., Berlanas, Sara R., Santos, W., Morbidelli, L., Spina, L., and Minkevičiūtė, R.
Abstract: The Gaia-ESO Survey is a public spectroscopic survey that targeted ≳105 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 (Teff ~ 30 000–52 000 K) all the way to K-M (≳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

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

Author: Randich, S., primary, Gilmore, G., additional, Magrini, L., additional, Sacco, G. G., additional, Jackson, R. J., additional, Jeffries, R. D., additional, Worley, C. C., additional, Hourihane, A., additional, Gonneau, A., additional, Viscasillas Vazquez, C., additional, Franciosini, E., additional, Lewis, J. R., additional, Alfaro, E. J., additional, Allende Prieto, C., additional, Bensby, T., additional, Blomme, R., additional, Bragaglia, A., additional, Flaccomio, E., additional, François, P., additional, Irwin, M. J., additional, Koposov, S. E., additional, Korn, A. J., additional, Lanzafame, A. C., additional, Pancino, E., additional, Recio-Blanco, A., additional, Smiljanic, R., additional, Van Eck, S., additional, Zwitter, T., additional, Asplund, M., additional, Bonifacio, P., additional, Feltzing, S., additional, Binney, J., additional, Drew, J., additional, Ferguson, A. M. N., additional, Micela, G., additional, Negueruela, I., additional, Prusti, T., additional, Rix, H.-W., additional, Vallenari, A., additional, Bayo, A., additional, Bergemann, M., additional, Biazzo, K., additional, Carraro, G., additional, Casey, A. R., additional, Damiani, F., additional, Frasca, A., additional, Heiter, U., additional, Hill, V., additional, Jofré, P., additional, de Laverny, P., additional, Lind, K., additional, Marconi, G., additional, Martayan, C., additional, Masseron, T., additional, Monaco, L., additional, Morbidelli, L., additional, Prisinzano, L., additional, Sbordone, L., additional, Sousa, S. G., additional, Zaggia, S., additional, Adibekyan, V., additional, Bonito, R., additional, Caffau, E., additional, Daflon, S., additional, Feuillet, D. K., additional, Gebran, M., additional, Gonzalez Hernandez, J. I., additional, Guiglion, G., additional, Herrero, A., additional, Lobel, A., additional, Maiz Apellaniz, J., additional, Merle, T., additional, Mikolaitis, Š., additional, Montes, D., additional, Morel, T., additional, Soubiran, C., additional, Spina, L., additional, Tabernero, H. M., additional, Tautvaišiene, G., additional, Traven, G., additional, Valentini, M., additional, Van der Swaelmen, M., additional, Villanova, S., additional, Wright, N. J., additional, Abbas, U., additional, Aguirre Børsen-Koch, V., additional, Alves, J., additional, Balaguer-Nunez, L., additional, Barklem, P. S., additional, Barrado, D., additional, Berlanas, S. R., additional, Binks, A. S., additional, Bressan, A., additional, Capuzzo-Dolcetta, R., additional, Casagrande, L., additional, Casamiquela, L., additional, Collins, R. S., additional, D'Orazi, V., additional, Dantas, M. L. L., additional, Debattista, V. P., additional, Delgado-Mena, E., additional, Di Marcantonio, P., additional, Drazdauskas, A., additional, Evans, N. W., additional, Famaey, B., additional, Franchini, M., additional, Frémat, Y., additional, Friel, E. D., additional, Fu, X., additional, Geisler, D., additional, Gerhard, O., additional, Gonzalez Solares, E. A., additional, Grebel, E. K., additional, Gutierrez Albarran, M. L., additional, Hatzidimitriou, D., additional, Held, E. V., additional, Jiménez-Esteban, F., additional, Jönsson, H., additional, Jordi, C., additional, Khachaturyants, T., additional, Kordopatis, G., additional, Kos, J., additional, Lagarde, N., additional, Mahy, L., additional, Mapelli, M., additional, Marfil, E., additional, Martell, S. L., additional, Messina, S., additional, Miglio, A., additional, Minchev, I., additional, Moitinho, A., additional, Montalban, J., additional, Monteiro, M. J. P. F. G., additional, Morossi, C., additional, Mowlavi, N., additional, Mucciarelli, A., additional, Murphy, D. N. A., additional, Nardetto, N., additional, Ortolani, S., additional, Paletou, F., additional, Palouš, J., additional, Paunzen, E., additional, Pickering, J. C., additional, Quirrenbach, A., additional, Re Fiorentin, P., additional, Read, J. I., additional, Romano, D., additional, Ryde, N., additional, Sanna, N., additional, Santos, W., additional, Seabroke, G. M., additional, Spagna, A., additional, Steinmetz, M., additional, Stonkuté, E., additional, Sutorius, E., additional, Thévenin, F., additional, Tosi, M., additional, Tsantaki, M., additional, Vink, J. S., additional, Wright, N., additional, Wyse, R. F. G., additional, Zoccali, M., additional, Zorec, J., additional, Zucker, D. B., additional, and Walton, N. A., additional
Published: 2022
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8. The Gaia-ESO Public Spectroscopic Survey: Motivation, implementation, GIRAFFE data processing, analysis, and final data products

Author: Gilmore, G., primary, Randich, S., additional, Worley, C. C., additional, Hourihane, A., additional, Gonneau, A., additional, Sacco, G. G., additional, Lewis, J. R., additional, Magrini, L., additional, François, P., additional, Jeffries, R. D., additional, Koposov, S. E., additional, Bragaglia, A., additional, Alfaro, E. J., additional, Allende Prieto, C., additional, Blomme, R., additional, Korn, A. J., additional, Lanzafame, A. C., additional, Pancino, E., additional, Recio-Blanco, A., additional, Smiljanic, R., additional, Van Eck, S., additional, Zwitter, T., additional, Bensby, T., additional, Flaccomio, E., additional, Irwin, M. J., additional, Franciosini, E., additional, Morbidelli, L., additional, Damiani, F., additional, Bonito, R., additional, Friel, E. D., additional, Vink, J. S., additional, Prisinzano, L., additional, Abbas, U., additional, Hatzidimitriou, D., additional, Held, E. V., additional, Jordi, C., additional, Paunzen, E., additional, Spagna, A., additional, Jackson, R. J., additional, Maíz Apellániz, J., additional, Asplund, M., additional, Bonifacio, P., additional, Feltzing, S., additional, Binney, J., additional, Drew, J., additional, Ferguson, A. M. N., additional, Micela, G., additional, Negueruela, I., additional, Prusti, T., additional, Rix, H.-W., additional, Vallenari, A., additional, Bergemann, M., additional, Casey, A. R., additional, de Laverny, P., additional, Frasca, A., additional, Hill, V., additional, Lind, K., additional, Sbordone, L., additional, Sousa, S. G., additional, Adibekyan, V., additional, Caffau, E., additional, Daflon, S., additional, Feuillet, D. K., additional, Gebran, M., additional, Gonzalez Hernandez, J. I., additional, Guiglion, G., additional, Herrero, A., additional, Lobel, A., additional, Merle, T., additional, Mikolaitis, Š., additional, Montes, D., additional, Morel, T., additional, Ruchti, G., additional, Soubiran, C., additional, Tabernero, H. M., additional, Tautvaišienė, G., additional, Traven, G., additional, Valentini, M., additional, Van der Swaelmen, M., additional, Villanova, S., additional, Viscasillas Vázquez, C., additional, Bayo, A., additional, Biazzo, K., additional, Carraro, G., additional, Edvardsson, B., additional, Heiter, U., additional, Jofré, P., additional, Marconi, G., additional, Martayan, C., additional, Masseron, T., additional, Monaco, L., additional, Walton, N. A., additional, Zaggia, S., additional, Aguirre Børsen-Koch, V., additional, Alves, J., additional, Balaguer-Nunez, L., additional, Barklem, P. S., additional, Barrado, D., additional, Bellazzini, M., additional, Berlanas, S. R., additional, Binks, A. S., additional, Bressan, A., additional, Capuzzo-Dolcetta, R., additional, Casagrande, L., additional, Casamiquela, L., additional, Collins, R. S., additional, D'Orazi, V., additional, Dantas, M. L. L., additional, Debattista, V. P., additional, Delgado-Mena, E., additional, Di Marcantonio, P., additional, Drazdauskas, A., additional, Evans, N. W., additional, Famaey, B., additional, Franchini, M., additional, Frémat, Y., additional, Fu, X., additional, Geisler, D., additional, Gerhard, O., additional, González Solares, E. A., additional, Grebel, E. K., additional, Gutiérrez Albarrán, M. L., additional, Jiménez-Esteban, F., additional, Jönsson, H., additional, Khachaturyants, T., additional, Kordopatis, G., additional, Kos, J., additional, Lagarde, N., additional, Ludwig, H.-G., additional, Mahy, L., additional, Mapelli, M., additional, Marfil, E., additional, Martell, S. L., additional, Messina, S., additional, Miglio, A., additional, Minchev, I., additional, Moitinho, A., additional, Montalban, J., additional, Monteiro, M. J. P. F. G., additional, Morossi, C., additional, Mowlavi, N., additional, Mucciarelli, A., additional, Murphy, D. N. A., additional, Nardetto, N., additional, Ortolani, S., additional, Paletou, F., additional, Palouš, J., additional, Pickering, J. C., additional, Quirrenbach, A., additional, Re Fiorentin, P., additional, Read, J. I., additional, Romano, D., additional, Ryde, N., additional, Sanna, N., additional, Santos, W., additional, Seabroke, G. M., additional, Spina, L., additional, Steinmetz, M., additional, Stonkuté, E., additional, Sutorius, E., additional, Thévenin, F., additional, Tosi, M., additional, Tsantaki, M., additional, Wright, N., additional, Wyse, R. F. G., additional, Zoccali, M., additional, Zorec, J., additional, and Zucker, D. B., additional
Published: 2022
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9. TheGaia-ESO survey: A spectroscopic study of the young open cluster NGC 3293

Author: Morel, T., primary, Blazère, A., additional, Semaan, T., additional, Gosset, E., additional, Zorec, J., additional, Frémat, Y., additional, Blomme, R., additional, Daflon, S., additional, Lobel, A., additional, Nieva, M. F., additional, Przybilla, N., additional, Gebran, M., additional, Herrero, A., additional, Mahy, L., additional, Santos, W., additional, Tautvaišienė, G., additional, Gilmore, G., additional, Randich, S., additional, Alfaro, E. J., additional, Bergemann, M., additional, Carraro, G., additional, Damiani, F., additional, Franciosini, E., additional, Morbidelli, L., additional, Pancino, E., additional, Worley, C. C., additional, and Zaggia, S., additional
Published: 2022
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10. Low-mass young stars in the Milky Way unveiled by DBSCAN and Gaia EDR3: Mapping the star forming regions within 1.5 kpc

Author: Prisinzano, L., primary, Damiani, F., additional, Sciortino, S., additional, Flaccomio, E., additional, Guarcello, M. G., additional, Micela, G., additional, Tognelli, E., additional, Jeffries, R. D., additional, and Alcalá, J. M., additional
Published: 2022
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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: Implementation, data products, open cluster survey, science, and legacy

Author: Universidad de Alicante. Departamento de Física Aplicada, Randich, Sofia, Gilmore, Gerard, Magrini, L., Sacco, G.G., Jackson, R.J., Jeffries, R., Worley, C.C., Hourihane, A., Gonneau, A., Viscasillas Vázquez, C., Franciosini, E., Sbordone, L., Sousa, S.G., Zaggia, S., Adibekyan, V.Zh., Bonito, R., Caffau, E., Daflon, Simone, Feuillet, D.K., Drazdauskas, A., Gebran, M., Lagarde, N., González Hernández, J.I., Guiglion, G., Herrero, Artemio, Lobel, Alex, Maíz Apellániz, Jesús, Merle, T., Mikolaitis, Š., Montes, David, Morel, Thierry, Evans, N.W., Mahy, Laurent, Soubiran, C., Spina, L., Tabernero, Hugo M., Tautvaišienė, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Wright, N.J., Abbas, U., Mapelli, M., Famaey, B., Aguirre Børsen-Koch, V., Alves, J., Balaguer-Nunez, L., Barklem, P.S., Barrado, D., Berlanas, Sara R., Binks, A.S., Bressan, A., Capuzzo-Dolcetta, R., Marfil, E., Casagrande, L., Franchini, M., Casamiquela, L., Collins, R.S., D'Orazi, V., Dantas, M.L.L., Debattista, V.P., Frémat, Y., Friel, E., Fu, X., Martell, S.L., Geisler, Douglas, Lewis, J., Gerhard, Ortwin, González Solares, E.A., Grebel, E.K., Gutiérrez Albarran, M.L., Hatzidimitriou, D., Held, E.V., Jiménez Esteban, Francisco M., Jönsson, H., Messina, S., Jordi, C., Khachaturyants, T., Alfaro, Emilio J., Kordopatis, G., Kos, J., Miglio, A., Minchev, I., Allende Prieto, C., Moitinho, A., Negueruela, Ignacio, Montalban, J., Monteiro, M.J.P.F.G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D.N.A., Nardetto, N., Ortolani, S., Paletou, F., Bensby, T., Prusti, T., Palouš, J., Paunzen, E., Pickering, J.C., Quirrenbach, A., Re Fiorentin, P., Read, J.I., Romano, D., Ryde, N., Sanna, N., Santos, W., Rix, H.-W., Blomme, Ronny, Seabroke, G.M., Spagna, A., Steinmetz, M., Stonkuté, E., Sutorius, E., Thévenin, F., Tosi, M., Tsantaki, M., Vink, Jorick S., Vallenari, A., Wright, N., Bragaglia, A., Wyse, R.F.G., Zoccali, M., Zorec, J., Zucker, D.B., Walton, N., Flaccomio, E., François, P., Irwin, M., Bayo, A., Koposov, S., Korn, A., Lanzafame, A.C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Asplund, M., Bonifacio, P., Bergemann, M., Feltzing, S., Binney, J., Drew, J., Ferguson, A., Micela, G., Biazzo, K., Carraro, G., Casey, A.R., Damiani, F., Delgado-Mena, E., Frasca, A., Heiter, U., Hill, V., Jofre, P., Laverny, P. de, Lind, K., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Di Marcantonio, P., Morbidelli, L., Prisinzano, L., Universidad de Alicante. Departamento de Física Aplicada, Randich, Sofia, Gilmore, Gerard, Magrini, L., Sacco, G.G., Jackson, R.J., Jeffries, R., Worley, C.C., Hourihane, A., Gonneau, A., Viscasillas Vázquez, C., Franciosini, E., Sbordone, L., Sousa, S.G., Zaggia, S., Adibekyan, V.Zh., Bonito, R., Caffau, E., Daflon, Simone, Feuillet, D.K., Drazdauskas, A., Gebran, M., Lagarde, N., González Hernández, J.I., Guiglion, G., Herrero, Artemio, Lobel, Alex, Maíz Apellániz, Jesús, Merle, T., Mikolaitis, Š., Montes, David, Morel, Thierry, Evans, N.W., Mahy, Laurent, Soubiran, C., Spina, L., Tabernero, Hugo M., Tautvaišienė, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Wright, N.J., Abbas, U., Mapelli, M., Famaey, B., Aguirre Børsen-Koch, V., Alves, J., Balaguer-Nunez, L., Barklem, P.S., Barrado, D., Berlanas, Sara R., Binks, A.S., Bressan, A., Capuzzo-Dolcetta, R., Marfil, E., Casagrande, L., Franchini, M., Casamiquela, L., Collins, R.S., D'Orazi, V., Dantas, M.L.L., Debattista, V.P., Frémat, Y., Friel, E., Fu, X., Martell, S.L., Geisler, Douglas, Lewis, J., Gerhard, Ortwin, González Solares, E.A., Grebel, E.K., Gutiérrez Albarran, M.L., Hatzidimitriou, D., Held, E.V., Jiménez Esteban, Francisco M., Jönsson, H., Messina, S., Jordi, C., Khachaturyants, T., Alfaro, Emilio J., Kordopatis, G., Kos, J., Miglio, A., Minchev, I., Allende Prieto, C., Moitinho, A., Negueruela, Ignacio, Montalban, J., Monteiro, M.J.P.F.G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D.N.A., Nardetto, N., Ortolani, S., Paletou, F., Bensby, T., Prusti, T., Palouš, J., Paunzen, E., Pickering, J.C., Quirrenbach, A., Re Fiorentin, P., Read, J.I., Romano, D., Ryde, N., Sanna, N., Santos, W., Rix, H.-W., Blomme, Ronny, Seabroke, G.M., Spagna, A., Steinmetz, M., Stonkuté, E., Sutorius, E., Thévenin, F., Tosi, M., Tsantaki, M., Vink, Jorick S., Vallenari, A., Wright, N., Bragaglia, A., Wyse, R.F.G., Zoccali, M., Zorec, J., Zucker, D.B., Walton, N., Flaccomio, E., François, P., Irwin, M., Bayo, A., Koposov, S., Korn, A., Lanzafame, A.C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Asplund, M., Bonifacio, P., Bergemann, M., Feltzing, S., Binney, J., Drew, J., Ferguson, A., Micela, G., Biazzo, K., Carraro, G., Casey, A.R., Damiani, F., Delgado-Mena, E., Frasca, A., Heiter, U., Hill, V., Jofre, P., Laverny, P. de, Lind, K., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Di Marcantonio, P., Morbidelli, L., and Prisinzano, L.
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

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

Author: Universidad de Alicante. Departamento de Física Aplicada, Gilmore, Gerard, Randich, Sofia, Worley, C.C., Hourihane, A., Gonneau, A., Sacco, G.G., Lewis, J., Magrini, L., François, P., Jeffries, R., Koposov, S., 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., Bragaglia, A., Di Marcantonio, P., Drazdauskas, A., Evans, N.W., Famaey, B., Franchini, M., Frémat, Y., Fu, X., Geisler, Douglas, Gerhard, Ortwin, González Solares, E.A., Alfaro, Emilio J., Grebel, E.K., Gutiérrez Albarrán, M.L., Jiménez Esteban, Francisco M., Jönsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H.-G., Mahy, Laurent, Allende Prieto, C., 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., Blomme, Ronny, Mowlavi, N., Mucciarelli, A., Murphy, D.N.A., Nardetto, N., Ortolani, S., Paletou, F., Palouš, J., Pickering, J.C., Quirrenbach, A., Re Fiorentin, P., Korn, A., Read, J.I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G.M., Spina, L., Steinmetz, M., Stonkuté, E., Sutorius, E., Lanzafame, A.C., Thévenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R.F.G., Zoccali, M., Zorec, J., Zucker, D.B., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E., Vink, Jorick S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E.V., Jordi, C., Paunzen, E., Spagna, A., Jackson, R.J., Maíz Apellániz, Jesús, Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A., Micela, G., Negueruela, Ignacio, Prusti, T., Rix, H.-W., Vallenari, A., Bergemann, M., Casey, A.R., Laverny, P. de, Frasca, A., Hill, V., Lind, K., Sbordone, L., Sousa, S.G., Adibekyan, V.Zh., Caffau, E., Daflon, Simone, Feuillet, D.K., Gebran, M., González Hernández, J.I., Guiglion, G., Herrero, Artemio, Lobel, Alex, Merle, T., Mikolaitis, Š., Montes, David, Morel, Thierry, Ruchti, G., Soubiran, C., Tabernero, Hugo M., Tautvaišienė, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Viscasillas Vázquez, C., Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N., Zaggia, S., Aguirre Børsen-Koch, V., Alves, J., Balaguer-Nunez, L., Barklem, P.S., Barrado, D., Bellazzini, M., Berlanas, Sara R., Universidad de Alicante. Departamento de Física Aplicada, Gilmore, Gerard, Randich, Sofia, Worley, C.C., Hourihane, A., Gonneau, A., Sacco, G.G., Lewis, J., Magrini, L., François, P., Jeffries, R., Koposov, S., 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., Bragaglia, A., Di Marcantonio, P., Drazdauskas, A., Evans, N.W., Famaey, B., Franchini, M., Frémat, Y., Fu, X., Geisler, Douglas, Gerhard, Ortwin, González Solares, E.A., Alfaro, Emilio J., Grebel, E.K., Gutiérrez Albarrán, M.L., Jiménez Esteban, Francisco M., Jönsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H.-G., Mahy, Laurent, Allende Prieto, C., 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., Blomme, Ronny, Mowlavi, N., Mucciarelli, A., Murphy, D.N.A., Nardetto, N., Ortolani, S., Paletou, F., Palouš, J., Pickering, J.C., Quirrenbach, A., Re Fiorentin, P., Korn, A., Read, J.I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G.M., Spina, L., Steinmetz, M., Stonkuté, E., Sutorius, E., Lanzafame, A.C., Thévenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R.F.G., Zoccali, M., Zorec, J., Zucker, D.B., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E., Vink, Jorick S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E.V., Jordi, C., Paunzen, E., Spagna, A., Jackson, R.J., Maíz Apellániz, Jesús, Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A., Micela, G., Negueruela, Ignacio, Prusti, T., Rix, H.-W., Vallenari, A., Bergemann, M., Casey, A.R., Laverny, P. de, Frasca, A., Hill, V., Lind, K., Sbordone, L., Sousa, S.G., Adibekyan, V.Zh., Caffau, E., Daflon, Simone, Feuillet, D.K., Gebran, M., González Hernández, J.I., Guiglion, G., Herrero, Artemio, Lobel, Alex, Merle, T., Mikolaitis, Š., Montes, David, Morel, Thierry, Ruchti, G., Soubiran, C., Tabernero, Hugo M., Tautvaišienė, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Viscasillas Vázquez, C., Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N., Zaggia, S., Aguirre Børsen-Koch, V., Alves, J., Balaguer-Nunez, L., Barklem, P.S., Barrado, D., Bellazzini, M., and Berlanas, Sara R.
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

14. The Gaia-ESO Survey: Target selection of open cluster stars

Author: Ministerio de Ciencia e Innovación (España), Junta de Andalucía, European Commission, Bragaglia, A., Alfaro, Emilio J., Flaccomio, E., Blomme, R., Donati, P., Costado, M. T., Damiani, F., Franciosini, E., Prisinzano, L., Randich, S., Friel, E. D., Hatztidimitriou, D., Vallenari, A., Spagna, A., Balaguer-Nuñez, Lola, Bonito, R., Cantat-Gaudin, Tristan, Casamiquela, Laia, Jeffries, R.D., Jordi, Carme, Magrini, Laura, Drew, J. E., Jackson, R. J., Abbas, U., Caramazza, M., Hayes, C., Jiménez-Esteban, Francisco M., Re Fiorentin, P., Wright, N., Bayo, A., Bensby, T., Bergemann, Maria, Gilmore, Gerry, Gonneau, A., Heiter, Ulrike, Hourihane, A., Pancino, E., Sacco, G., Smiljanic, R., Zaggia, S., Vink, J. S., Ministerio de Ciencia e Innovación (España), Junta de Andalucía, European Commission, Bragaglia, A., Alfaro, Emilio J., Flaccomio, E., Blomme, R., Donati, P., Costado, M. T., Damiani, F., Franciosini, E., Prisinzano, L., Randich, S., Friel, E. D., Hatztidimitriou, D., Vallenari, A., Spagna, A., Balaguer-Nuñez, Lola, Bonito, R., Cantat-Gaudin, Tristan, Casamiquela, Laia, Jeffries, R.D., Jordi, Carme, Magrini, Laura, Drew, J. E., Jackson, R. J., Abbas, U., Caramazza, M., Hayes, C., Jiménez-Esteban, Francisco M., Re Fiorentin, P., Wright, N., Bayo, A., Bensby, T., Bergemann, Maria, Gilmore, Gerry, 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

15. The Gaia-ESO survey: A spectroscopic study of the young open cluster NGC 3293

Author: Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, Morel, T., Blazère, A., Semaan, T., Gosset, E., Zorec, J., Frémat, Y., Blomme, R., Daflon, S., Lobel, A., Nieva, M. F., Przybilla, N., Gebran, M., Herrero, A., Mahy, L., Santos, W., Tautvaišienė, G., Gilmore, Gerry, Randich, S., Alfaro, Emilio J., Bergemann, Maria, Carraro, G., Damiani, F., Franciosini, E., Morbidelli, L., Pancino, E., Worley, C. C., Zaggia, S., Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, Morel, T., Blazère, A., Semaan, T., Gosset, E., Zorec, J., Frémat, Y., Blomme, R., Daflon, S., Lobel, A., Nieva, M. F., Przybilla, N., Gebran, M., Herrero, A., Mahy, L., Santos, W., Tautvaišienė, G., Gilmore, Gerry, Randich, S., Alfaro, Emilio J., Bergemann, Maria, Carraro, G., Damiani, F., Franciosini, E., Morbidelli, L., Pancino, E., Worley, C. C., and Zaggia, S.
Abstract: We present a spectroscopic analysis of the GIRAFFE and UVES data collected by the Gaia-ESO survey for the young open cluster NGC 3293. Archive spectra from the same instruments obtained in the framework of the ‘VLT-FLAMES survey of massive stars’ are also analysed. Atmospheric parameters, non-local thermodynamic equilibrium (LTE) chemical abundances for six elements (He, C, N, Ne, Mg, and Si), or variability information are reported for a total of about 160 B stars spanning a wide range in terms of spectral types (B1 to B9.5) and rotation rate (up to 350 km s−1). Our analysis leads to about a five-fold increase in the number of cluster members with an abundance determination and it characterises the late B-star population in detail for the first time. We take advantage of the multi-epoch observations on various timescales and a temporal baseline, sometimes spanning ∼15 years, to detect several binary systems or intrinsically line-profile variables. A deconvolution algorithm is used to infer the current, true (deprojected) rotational velocity distribution. We find a broad, Gaussian-like distribution peaking around 200–250 km s−1. Although some stars populate the high-velocity tail, most stars in the cluster appear to rotate far from critical. We discuss the chemical properties of the cluster, including the low occurrence of abundance peculiarities in the late B stars and the paucity of objects showing CN-cycle burning products at their surface. We argue that the former result can largely be explained by the inhibition of diffusion effects because of fast rotation, while the latter is generally in accord with the predictions of single-star evolutionary models under the assumption of a wide range of initial spin rates at the onset of main-sequence evolution. However, we find some evidence for a less efficient mixing in two quite rapidly rotating stars that are among the most massive objects in our sample. Finally, we obtain a cluster age of ∼20 Myr through a detailed
Published: 2022

16. The Gaia-ESO Survey: Target selection of open cluster stars

Author: Bragaglia, A., primary, Alfaro, E. J., additional, Flaccomio, E., additional, Blomme, R., additional, Donati, P., additional, Costado, M., additional, Damiani, F., additional, Franciosini, E., additional, Prisinzano, L., additional, Randich, S., additional, Friel, E. D., additional, Hatztidimitriou, D., additional, Vallenari, A., additional, Spagna, A., additional, Balaguer-Nunez, L., additional, Bonito, R., additional, Cantat Gaudin, T., additional, Casamiquela, L., additional, Jeffries, R. D., additional, Jordi, C., additional, Magrini, L., additional, Drew, J. E., additional, Jackson, R. J., additional, Abbas, U., additional, Caramazza, M., additional, Hayes, C., additional, Jiménez-Esteban, F. M., additional, Re Fiorentin, P., additional, Wright, N., additional, Bayo, A., additional, Bensby, T., additional, Bergemann, M., additional, Gilmore, G., additional, Gonneau, A., additional, Heiter, U., additional, Hourihane, A., additional, Pancino, E., additional, Sacco, G., additional, Smiljanic, R., additional, Zaggia, S., additional, and Vink, J. S., additional
Published: 2022
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17. Gaia-ESO Survey: Role of magnetic activity and starspots on pre-main-sequence lithium evolution

Author: Franciosini, E., primary, Tognelli, E., additional, Degl’Innocenti, S., additional, Prada Moroni, P. G., additional, Randich, S., additional, Sacco, G. G., additional, Magrini, L., additional, Pancino, E., additional, Lanzafame, A. C., additional, Smiljanic, R., additional, Prisinzano, L., additional, Sanna, N., additional, Roccatagliata, V., additional, Bonito, R., additional, de Laverny, P., additional, Gutiérrez Albarrán, M. L., additional, Montes, D., additional, Jiménez-Esteban, F., additional, Gilmore, G., additional, Bergemann, M., additional, Carraro, G., additional, Damiani, F., additional, Gonneau, A., additional, Hourihane, A., additional, Morbidelli, L., additional, Worley, C. C., additional, and Zaggia, S., additional
Published: 2022
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18. The Gaia-ESO Survey: Galactic evolution of lithium from iDR6

Author: Romano, D., primary, Magrini, L., additional, Randich, S., additional, Casali, G., additional, Bonifacio, P., additional, Jeffries, R. D., additional, Matteucci, F., additional, Franciosini, E., additional, Spina, L., additional, Guiglion, G., additional, Chiappini, C., additional, Mucciarelli, A., additional, Ventura, P., additional, Grisoni, V., additional, Bellazzini, M., additional, Bensby, T., additional, Bragaglia, A., additional, de Laverny, P., additional, Korn, A. J., additional, Martell, S. L., additional, Tautvaišienė, G., additional, Carraro, G., additional, Gonneau, A., additional, Jofré, P., additional, Pancino, E., additional, Smiljanic, R., additional, Vallenari, A., additional, Fu, X., additional, Gutiérrez Albarrán, M. L., additional, Jiménez-Esteban, F. M., additional, Montes, D., additional, Damiani, F., additional, Bergemann, M., additional, and Worley, C., additional
Published: 2021
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19. Dispersal timescale of protoplanetary disks in the low-metallicity young cluster Dolidze 25

Author: Guarcello, M. G., primary, Biazzo, K., additional, Drake, J. J., additional, Micela, G., additional, Prisinzano, L., additional, Sciortino, S., additional, Damiani, F., additional, Flaccomio, E., additional, Neiner, C., additional, and Wright, N. J., additional
Published: 2021
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20. Atomic data for the Gaia-ESO Survey

Author: Heiter, U., primary, Lind, K., additional, Bergemann, M., additional, Asplund, M., additional, Mikolaitis, Š., additional, Barklem, P. S., additional, Masseron, T., additional, de Laverny, P., additional, Magrini, L., additional, Edvardsson, B., additional, Jönsson, H., additional, Pickering, J. C., additional, Ryde, N., additional, Bayo Arán, A., additional, Bensby, T., additional, Casey, A. R., additional, Feltzing, S., additional, Jofré, P., additional, Korn, A. J., additional, Pancino, E., additional, Damiani, F., additional, Lanzafame, A., additional, Lardo, C., additional, Monaco, L., additional, Morbidelli, L., additional, Smiljanic, R., additional, Worley, C., additional, Zaggia, S., additional, Randich, S., additional, and Gilmore, G. F., additional
Published: 2021
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21. The Gaia-ESO Survey: A new diagnostic for accretion and outflow activity in the young cluster NGC 2264

Author: Bonito, R., primary, Prisinzano, L., additional, Venuti, L., additional, Damiani, F., additional, Micela, G., additional, Sacco, G., additional, Traven, G., additional, Biazzo, K., additional, Sbordone, L., additional, Masseron, T., additional, Zwitter, T., additional, Gonneau, A., additional, Bayo, A., additional, Roccatagliata, V., additional, Randich, S., additional, Vink, J. S., additional, Jofre, P., additional, Flaccomio, E., additional, Magrini, L., additional, Carraro, G., additional, Morbidelli, L., additional, Frasca, A., additional, Monaco, L., additional, Rigliaco, E., additional, Worley, C., additional, Hourihane, A., additional, Gilmore, G., additional, Franciosini, E., additional, Lewis, J., additional, and Koposov, S., additional
Published: 2020
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22. TheGaia-ESO Survey: detection and characterisation of single-line spectroscopic binaries

Author: Merle, T., primary, Van der Swaelmen, M., additional, Van Eck, S., additional, Jorissen, A., additional, Jackson, R. J., additional, Traven, G., additional, Zwitter, T., additional, Pourbaix, D., additional, Klutsch, A., additional, Sacco, G., additional, Blomme, R., additional, Masseron, T., additional, Gilmore, G., additional, Randich, S., additional, Badenes, C., additional, Bayo, A., additional, Bensby, T., additional, Bergemann, M., additional, Biazzo, K., additional, Damiani, F., additional, Feuillet, D., additional, Frasca, A., additional, Gonneau, A., additional, Jeffries, R. D., additional, Jofré, P., additional, Morbidelli, L., additional, Mowlavi, N., additional, Pancino, E., additional, and Prisinzano, L., additional
Published: 2020
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23. The Gaia-ESO Survey: Structural and dynamical properties of the young cluster Chamaeleon i

Author: Sacco, G. G., Spina, L., Randich, S., Palla, F., Parker, J., Jeffries, D., Jackson, R., Meyer, R., Mapelli, M., Lanzafame, C., Bonito, R., Damiani, F., Franciosini, E., Frasca, A., Klutsch, A., Prisinzano, L., Tognelli, E., Degl’Innocenti, S., Prada Moroni, P. G., Alfaro, J., Micela, G., Prusti, T., Barrado, D., Biazzo, K., Bouy, H., Bravi, L., Lopez-Santiago, J., Wright, J., Bayo, A., Gilmore, G., Bragaglia, A., Flaccomio, E., Koposov, S. E., Pancino, E., Casey, A. R., Costado, M. T., Donati, P., Hourihane, A., Jofré, P., Lardo, C., Lewis, J., Magrini, L., Monaco, L., Morbidelli, L., Sousa, S. G., Worley, C. C., Zaggia, S., Parker, R. J., Jeffries, R. D., Meyer, M. R., Lanzafame, A. C., Degl'Innocenti, S., Alfaro, E. J., Wright, N. J., Gilmore, Gerard [0000-0003-4632-0213], Koposov, Sergey [0000-0003-2644-135X], Worley, Clare [0000-0001-9310-2898], Apollo - University of Cambridge Repository, Sacco G.G., Spina L., Randich S., Palla F., Parker R.J., Jeffries R.D., Jackson R., Meyer M.R., Mapelli M., Lanzafame A.C., Bonito R., Damiani F., Franciosini E., Frasca A., Klutsch A., Prisinzano L., Tognelli E., Degl'Innocenti S., Prada Moroni P.G., Alfaro E.J., Micela G., Prusti T., Barrado D., Biazzo K., Bouy H., Bravi L., Lopez-Santiago J., Wright N.J., Bayo A., Gilmore G., Bragaglia A., Flaccomio E., Koposov S.E., Pancino E., Casey A.R., Costado M.T., Donati P., Hourihane A., Jofre P., Lardo C., Lewis J., Magrini L., Monaco L., Morbidelli L., Sousa S.G., Worley C.C., Zaggia S., Ministero dell'Istruzione, dell'Università e della Ricerca, Istituto Nazionale di Astrofisica, European Research Council, Fundação para a Ciência e a Tecnologia (Portugal), Pôle Gérontologie, Centre Hospitalier Universitaire de Nice (CHU Nice), Muséum national d'Histoire naturelle (MNHN), Watershed Associates Ltd, Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), Istituto Nazionale di Astrofisica (INAF), University of Turin, INAF - Osservatorio Astrofisico di Catania (OACT), Economía Política y Hacienda Pública, Estadística Económica y Empresarial y Política Económica, Universidad de Castilla-La Mancha (UCLM), INAF - Osservatorio Astronomico di Palermo (OAPa), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), INAF - Osservatorio Astrofisico di Arcetri (OAA), M2A 2017, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Synchrotron Radiation Facility (ESRF), Focas Research Institute, Dublin Institute of Technology, Institut national de recherche et de sécurité (Vandoeuvre lès Nancy) (INRS ( Vandoeuvre lès Nancy)), Hitotsubashi University, Department of Physiology and Pharmacology, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome]-Réseau International des Instituts Pasteur (RIIP)-Institut Pasteur, Fondation Cenci Bolognetti - Istituto Pasteur Italia, Fondazione Cenci Bolognetti, Réseau International des Instituts Pasteur (RIIP), Universidade de Sao Paulo, Instituto Ocenografico, Department of Microbiology and Molecular Genetics, Michigan State University [East Lansing], Michigan State University System-Michigan State University System, Université libre de Bruxelles (ULB), and Newcastle University [Newcastle]
Subjects: astro-ph.SR, Stellar population, open clustersand associations: individual: Chamaeleon I, Individual: Chamaeleon I [Open clusters and associations], Open clusters and associations: Individual: Chamaeleon I, Stars: Kinematics and dynamics, Stars: Pre-main sequence, Techniques: Spectroscopic, astro-ph.GA, stars: kinematics and dynamics, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, stars: pre-main sequence, 01 natural sciences, Virial theorem, Kinematics and dynamics [Stars], Stars: Kinematics and dynamic, 0103 physical sciences, Cluster (physics), Mass segregation, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Stellar evolution, QC, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, QB, Physics, Pre-main sequence [Stars], open clusters and associations: individual: Chamaeleon I, 010308 nuclear & particles physics, Velocity dispersion, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], techniques: spectroscopic, Star cluster, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Spectroscopic [Techniques], Equivalent width, QB799
Abstract: Investigating the physical mechanisms driving the dynamical evolution of young star clusters is fundamental to our understanding of the star formation process and the properties of the Galactic field stars. The young (~2 Myr) and partially embedded cluster Chamaeleon I is one of the closest laboratories for the study of the early stages of star cluster dynamics in a low-density environment. The aim of this work is to study the structural and kinematical properties of this cluster combining parameters from the high-resolution spectroscopic observations of the Gaia-ESO Survey with data from the literature. Our main result is the evidence of a large discrepancy between the velocity dispersion (σ = 1.14 ± 0.35 km s) of the stellar population and the dispersion of the pre-stellar cores (~0.3 km s) derived from submillimeter observations. The origin of this discrepancy, which has been observed in other young star clusters, is not clear. It has been suggested that it may be due to either the effect of the magnetic field on the protostars and the filaments or to the dynamical evolution of stars driven by two-body interactions. Furthermore, the analysis of the kinematic properties of the stellar population puts in evidence a significant velocity shift (~1 km s) between the two subclusters located around the north and south main clouds of the cluster. This result further supports a scenario where clusters form from the evolution of multiple substructures rather than from a monolithic collapse. Using three independent spectroscopic indicators (the gravity indicator γ, the equivalent width of the Li line at 6708 Å, and the Hα 10% width), we performed a new membership selection. We found six new cluster members all located in the outer region of the cluster, proving that Chamaeleon I is probably more extended than previously thought. Starting from the positions and masses of the cluster members, we derived the level of substructure Q, the surface density Σ, and the level of mass segregation Λ of the cluster. The comparison between these structural properties and the results of N-body simulations suggests that the cluster formed in a low-density environment, in virial equilibrium or a supervirial state, and highly substructured.© 2017 ESO., This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR) in the form of the grant >Premiale VLT 2012>. This work has been partially supported by PRIN-INAF-2014. The results presented here benefited from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. M.M. acknowledges financial support from the Italian Ministry of Education, University and Research (MIUR) through grant FIRB 2012 RBFR12PM1F, from INAF through grant PRIN-2014-14, and from the MERAC Foundation. S.G.S. acknowledges the support by Fundacao para a Ciencia e Tecnologia (FCT) through national funds and a research grant (project Ref. UID/FIS/04434/2013, and PTDC/FIS-AST/7073/2014). S.G.S. also acknowledge the support from FCT through Investigador FCT contract of reference IF/00028/2014 and POPH/FSE (EC) by FEDER funding through the program Programa Operacional de Factores de Competitividade COMPETE.
Published: 2017
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24. The gaia -ESO survey: calibration strategy

Author: Pancino, E., Lardo, C., Altavilla, G., Marinoni, S., Ragaini, S., Cocozza, G., Bellazzini, M., Sabbi, E., Zoccali, M., Donati, P., Heiter, U., Koposov, S. E., Blomme, R., Morel, T., Símon-Díaz, S., Lobel, A., Soubiran, C., Montalban, J., Valentini, M., Casey, A. R., Blanco-Cuaresma, S., Jofré, P., Worley, C. C., Magrini, L., Hourihane, A., François, P., Feltzing, S., Gilmore, G., Randich, S., Asplund, M., Bonifacio, P., Drew, J. E., Jeffries, R. D., Micela, G., Vallenari, A., Alfaro, E. J., Allende Prieto, C., Babusiaux, C., Bensby, T., angela Bragaglia, Flaccomio, E., Hambly, N., Korn, A. J., Lanzafame, A. C., Smiljanic, R., Eck, S., Walton, N. A., Bayo, A., Carraro, G., Costado, M. T., Damiani, F., Edvardsson, B., Franciosini, E., Frasca, A., Lewis, J., Monaco, L., Morbidelli, L., Prisinzano, L., Sacco, G. G., Sbordone, L., Sousa, S. G., Zaggia, S., Koch, A., Ministero dell'Istruzione, dell'Università e della Ricerca, Knut and Alice Wallenberg Foundation, European Research Council, Swedish National Space Board, Belgian Science Policy Office, National Science Centre (Poland), European Science Foundation, Ministerio de Economía y Competitividad (España), Pancino E., Lardo C., Altavilla G., Marinoni S., Ragaini S., Cocozza G., Bellazzini M., Sabbi E., Zoccali M., Donati P., Heiter U., Koposov S.E., Blomme R., Morel T., Simon-Diaz S., Lobel A., Soubiran C., Montalban J., Valentini M., Casey A.R., Blanco-Cuaresma S., Jofre P., Worley C.C., Magrini L., Hourihane A., Francois P., Feltzing S., Gilmore G., Randich S., Asplund M., Bonifacio P., Drew J.E., Jeffries R.D., Micela G., Vallenari A., Alfaro E.J., Allende Prieto C., Babusiaux C., Bensby T., Bragaglia A., Flaccomio E., Hambly N., Korn A.J., Lanzafame A.C., Smiljanic R., Van Eck S., Walton N.A., Bayo A., Carraro G., Costado M.T., Damiani F., Edvardsson B., Franciosini E., Frasca A., Lewis J., Monaco L., Morbidelli L., Prisinzano L., Sacco G.G., Sbordone L., Sousa S.G., Zaggia S., Koch A., Institut national de recherche et de sécurité (Vandoeuvre lès Nancy) (INRS ( Vandoeuvre lès Nancy)), Royal Observatory of Belgium [Brussels] (ROB), Science et Ingénierie des Matériaux et Procédés (SIMaP ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), M2A 2017, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Leibniz-Institut für Astrophysik Potsdam (AIP), Focas Research Institute, Dublin Institute of Technology, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), School of Physics, Astronomy and Mathematics [Hatfield], University of Hertfordshire [Hatfield] (UH), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Economía Política y Hacienda Pública, Estadística Económica y Empresarial y Política Económica, Universidad de Castilla-La Mancha (UCLM), Department of Astronomy and Space Physics [Uppsala], Uppsala University, INAF - Osservatorio Astrofisico di Catania (OACT), Institut d'Astronomie et d'Astrophysique, Université libre de Bruxelles (ULB), University of Turin, Department of Physiology and Pharmacology, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome]-Réseau International des Instituts Pasteur (RIIP)-Institut Pasteur, Fondation Cenci Bolognetti - Istituto Pasteur Italia, Fondazione Cenci Bolognetti, Réseau International des Instituts Pasteur (RIIP), Pôle Gérontologie, and Centre Hospitalier Universitaire de Nice (CHU Nice)
Subjects: Stars: abundance, Milky Way, FOS: Physical sciences, Techniques: spectroscopic, Astrophysics, Parameter space, Surveys, 01 natural sciences, Spectral line, surveys, 0103 physical sciences, Calibration, Emission spectrum, Survey, 010303 astronomy & astrophysics, Galaxy: general, Solar and Stellar Astrophysics (astro-ph.SR), QC, general [Galaxy], QB, Physics, [PHYS]Physics [physics], Observational error, 010308 nuclear & particles physics, Techniques: radial velocitie, Stars: abundances, Astronomy and Astrophysics, Ranging, radial velocities [techniques], [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, abundances [stars], Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Techniques: radial velocities, stars: abundances, techniques: spectroscopic, techniques: radial velocities, spectroscopic [techniques], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The Gaia-ESO survey (GES) is now in its fifth and last year of observations and has produced tens of thousands of high-quality spectra of stars in all Milky Way components. This paper presents the strategy behind the selection of astrophysical calibration targets, ensuring that all GES results on radial velocities, atmospheric parameters, and chemical abundance ratios will be both internally consistent and easily comparable with other literature results, especially from other large spectroscopic surveys and from Gaia. The calibration of GES is particularly delicate because of (i) the large space of parameters covered by its targets, ranging from dwarfs to giants, from O to M stars; these targets have a large wide of metallicities and also include fast rotators, emission line objects, and stars affected by veiling; (ii) the variety of observing setups, with different wavelength ranges and resolution; and (iii) the choice of analyzing the data with many different state-of-the-art methods, each stronger in a different region of the parameter space, which ensures a better understanding of systematic uncertainties. An overview of the GES calibration and homogenization strategy is also given, along with some examples of the usage and results of calibrators in GES iDR4, which is the fourth internal GES data release and will form the basis of the next GES public data release. The agreement between GES iDR4 recommended values and reference values for the calibrating objects are very satisfactory. The average offsets and spreads are generally compatible with the GES measurement errors, which in iDR4 data already meet the requirements set by the main GES scientific goals.© ESO, 2017., This work was partly supported by the European Union FP7 program through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR) in the form of the grant >Premiale VLT 2012>. The results presented here benefit from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. S.F. and T.B. acknowledge the support from the New Milky Way project funded by a grant from the Knut and Alice Wallenberg foundation. C.L. gratefully acknowledges financial support from the European Research Council (ERC-CoG-646928, Multi-Pop, PI: N. Bastian). U.H. and A.J.K acknowledge support from the Swedish National Space Board (Rymdstyrelsen). The research of A.L. has been subsidized by the Belgian Federal Science Policy Office under contract No. BR/143/A2/BRASS. R.S. acknowledges support by the National Science Center of Poland through grant 2014/15/B/ST9/03981. C.A.P. is thankful for support from the Spanish Ministry of Economy and Competitiveness (MINECO) through grant AYA2014-56359-P.J.M. acknowledges support from the ERC Consolidator Grant funding scheme (project STARKEY, G.A. No. 615604). T.M. acknowledges financial support from Belspo for contract PRODEX Gaia-DPAC. S.G.S acknowledges the support by Fundacao para a Ciencia e Tecnologia (FCT) through national funds and a research grant (project ref. UID/FIS/04434/2013, and PTDC/FIS-AST/7073/2014). S.G.S. also acknowledge the support from FCT through Investigador FCT contract of reference IF/00028/2014 and POPH/FSE (EC) by FEDER funding through the program >Programa Operacional de Factores de Competitividade - COMPETE>. L.S. acknowledges support by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics (MAS). M.Z. acknowledges support by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics (MAS), by Fondecyt Regular 1150345 and by the BASAL CATA PFB-06. E.J.A. and M.T.C acknowledge the financial support from the Spanish Ministerio de Economia y Competitividad, through grant AYA2013-40611-P.S.Z. acknowledge the support from the INAF grant >PRIN INAF 2014>, >Star won't tell their ages to Gaia, Galactic Archaelogy with wide-area asterosismic>.
Published: 2017
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25. The Gaia-ESO survey: Calibrating a relationship between age and the [C/N] abundance ratio with open clusters

Author: Casali, G., primary, Magrini, L., additional, Tognelli, E., additional, Jackson, R., additional, Jeffries, R. D., additional, Lagarde, N., additional, Tautvaišienė, G., additional, Masseron, T., additional, Degl’Innocenti, S., additional, Prada Moroni, P. G., additional, Kordopatis, G., additional, Pancino, E., additional, Randich, S., additional, Feltzing, S., additional, Sahlholdt, C., additional, Spina, L., additional, Friel, E., additional, Roccatagliata, V., additional, Sanna, N., additional, Bragaglia, A., additional, Drazdauskas, A., additional, Mikolaitis, Š., additional, Minkevičiūtė, R., additional, Stonkutė, E., additional, Chorniy, Y., additional, Bagdonas, V., additional, Jimenez-Esteban, F., additional, Martell, S., additional, Van der Swaelmen, M., additional, Gilmore, G., additional, Vallenari, A., additional, Bensby, T., additional, Koposov, S. E., additional, Korn, A., additional, Worley, C., additional, Smiljanic, R., additional, Bergemann, M., additional, Carraro, G., additional, Damiani, F., additional, Prisinzano, L., additional, Bonito, R., additional, Franciosini, E., additional, Gonneau, A., additional, Hourihane, A., additional, Jofre, P., additional, Lewis, J., additional, Morbidelli, L., additional, Sacco, G., additional, Sousa, S. G., additional, Zaggia, S., additional, Lanzafame, A. C., additional, Heiter, U., additional, Frasca, A., additional, and Bayo, A., additional
Published: 2019
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26. The Gaia-ESO Survey: The inner disc, intermediate-age open cluster Pismis 18

Author: Hatzidimitriou, D., primary, Held, E. V., additional, Tognelli, E., additional, Bragaglia, A., additional, Magrini, L., additional, Bravi, L., additional, Gazeas, K., additional, Dapergolas, A., additional, Drazdauskas, A., additional, Delgado-Mena, E., additional, Friel, E. D., additional, Minkevičiūtė, R., additional, Sordo, R., additional, Tautvaišienė, G., additional, Gilmore, G., additional, Randich, S., additional, Feltzing, S., additional, Vallenari, A., additional, Alfaro, E. J., additional, Flaccomio, E., additional, Lanzafame, A. C., additional, Pancino, E., additional, Smiljanic, R., additional, Bayo, A., additional, Bergemann, M., additional, Carraro, G., additional, Casey, A. R., additional, Costado, M. T., additional, Damiani, F., additional, Franciosini, E., additional, Gonneau, A., additional, Jofré, P., additional, Lewis, J., additional, Monaco, L., additional, Morbidelli, L., additional, Worley, C. C., additional, and Zaggia, S., additional
Published: 2019
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27. The Gaia-ESO Survey: Age spread in the star forming region NGC 6530 from the HR diagram and gravity indicators

Author: Prisinzano, L., primary, Damiani, F., additional, Kalari, V., additional, Jeffries, R., additional, Bonito, R., additional, Micela, G., additional, Wright, N. J., additional, Jackson, R. J., additional, Tognelli, E., additional, Guarcello, M. G., additional, Vink, J. S., additional, Klutsch, A., additional, Jiménez-Esteban, F. M., additional, Roccatagliata, V., additional, Tautvaišienė, G., additional, Gilmore, G., additional, Randich, S., additional, Alfaro, E. J., additional, Flaccomio, E., additional, Koposov, S., additional, Lanzafame, A., additional, Pancino, E., additional, Bergemann, M., additional, Carraro, G., additional, Franciosini, E., additional, Frasca, A., additional, Gonneau, A., additional, Hourihane, A., additional, Jofré, P., additional, Lewis, J., additional, Magrini, L., additional, Monaco, L., additional, Morbidelli, L., additional, Sacco, G. G., additional, Worley, C. C., additional, and Zaggia, S., additional
Published: 2019
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28. Stellar population of Sco OB2 revealed by Gaia DR2 data

Author: Damiani, F., primary, Prisinzano, L., additional, Pillitteri, I., additional, Micela, G., additional, and Sciortino, S., additional
Published: 2019
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29. Wide-area photometric and astrometric (Gaia DR2) study of the young cluster NGC 6530

Author: Damiani, F., primary, Prisinzano, L., additional, Micela, G., additional, and Sciortino, S., additional
Published: 2019
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30. The Gaia-ESO Survey: A lithium-rotation connection at 5 Myr?

Author: Delgado Mena, E., Carraro, G., Lanzafame, A., Zwitter, T., Zaggia, S., Worley, C., Vallenari, A., Sousa, S., Sbordone, L., Sacco, G., Prisinzano, L., Morbidelli, L., Monaco, L., Magrini, L., Lewis, J., Lardo, C., Koposov, S., Hourihane, A., Franciosini, E., Donati, P., Mena, E., Damiani, F., Costado, M., Casey, A., Carraro, C., Bragaglia, A., Bensby, T., Bayo, A., Gilmore, G., Flaccomio, E., Cody, A., Stauffer, J., Randich, S., Micela, G., Messina, S., Biazzo, K., Moraux, E., Frasca, A., Jeffries, R., Klutsch, A., Venuti, L., Bouvier, J., Bouvier J., Lanzafame A.C., Venuti L., Klutsch A., Jeffries R., Frasca A., Moraux E., Biazzo K., Messina S., Micela G., Randich S., Stauffer J., Cody A.M., Flaccomio E., Gilmore G., Bayo A., Bensby T., Bragaglia A., Carraro G., Casey A., Costado M.T., Damiani F., Delgado Mena E., Donati P., Franciosini E., Hourihane A., Koposov S., Lardo C., Lewis J., Magrini L., Monaco L., Morbidelli L., Prisinzano L., Sacco G., Sbordone L., Sousa S.G., Vallenari A., Worley C.C., Zaggia S., Zwitter T., Gilmore, Gerard [0000-0003-4632-0213], Casey, Andrew [0000-0003-0174-0564], Koposov, Sergey [0000-0003-2644-135X], Worley, Clare [0000-0001-9310-2898], and Apollo - University of Cambridge Repository
Subjects: stars: abundances / stars: pre-main sequence / stars: rotation / open clusters and associations: individual: NGC 2264, Stars: abundance, astro-ph.SR, stars: abundances, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Rotation, 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Stellar evolution, Open clusters and associations: individual: NGC 2264, Stars: abundances, Stars: pre-main sequence, Stars: rotation, Astronomy and Astrophysics, Space and Planetary Science, Solar and Stellar Astrophysics (astro-ph.SR), QC, Astrophysics::Galaxy Astrophysics, QB, Physics, 010308 nuclear & particles physics, Radius, Accretion (astrophysics), Stars, Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Pleiades, Equivalent width, QB799
Abstract: We investigate here the lithium content of young low-mass stars in the 5~Myr-old star forming region NGC~2264 and its relationship with rotation. We combine lithium equivalent width measurements, EW(Li), from the Gaia-ESO Survey with the determination of rotational periods from the CSI~2264 survey. We consider only bona fide non accreting cluster members in order to minimize uncertainties on EW(Li). We report the existence of a relationship between lithium content and rotation in NGC~2264 at an age of 5~Myr. The Li-rotation connection is seen over a restricted temperature range, Teff=3800--4400K, where fast rotators are Li-rich compared to slow ones. This correlation is similar to, albeit of lower amplitude than, the Li-rotation connection previously reported for K dwarfs in the 125 Myr-old Pleiades cluster. We investigate whether the non-standard pre-main sequence models developed so far to explain the Pleiades results, which are based on episodic accretion, pre-main sequence core-envelope decoupling, and/or radius inflation due to enhanced magnetic activity, can account for an early development of the Li-rotation connection. While radius inflation appears to be the most promising possibility, each of these models has issues. We therefore also discuss external causes that might operate during the first few Myr of pre-main sequence evolution, such as planet engulfment and/or steady disk accretion, as possible candidates for the common origin for Li-excess and fast rotation in young low-mass pre-main sequence stars. The emergence of a connection between lithium content and rotation rate at such an early age as 5~Myr suggests a complex link between accretion processes, early angular momentum evolution, and possibly planet formation, which likely impacts early stellar evolution and still is to be fully deciphered., Comment: 9 pages, 5 figures, Astronomy & Astrophysics, in press
Published: 2016
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31. The Gaia-ESO Survey: The origin and evolution of s-process elements

Author: European Research Council, Leverhulme Trust, Istituto Nazionale di Astrofisica, European Science Foundation, Ministerio de Economía y Competitividad (España), European Commission, Fundação para a Ciência e a Tecnologia (Portugal), Science and Technology Facilities Council (UK), Ministerio de Economía, Fomento y Turismo (Chile), Ministry of Science and Higher Education (Poland), Knut and Alice Wallenberg Foundation, Magrini, L., Spina, Lorenzo, Randich, S., Friel, E., Kordopatis, G., Worley, C., Pancino, E., Bragaglia, A., Donati, P., Tautvaišienė, G., Bagdonas, V., Delgado-Mena, E., Adibekyan, V., Sousa, S. G., Jiménez-Esteban, Francisco M., Sanna, N., Roccatagliata, V., Bonito, R., Sbordone, L., Duffau, S., Gilmore, Gerry, Feltzing, S., Jeffries, R.D., Vallenari, A., Alfaro, Emilio J., Bensby, T., Francois, P., Koposov, S., Korn, A.J., Recio-Blanco, A., Smiljanic, R., Bayo, A., Carraro, G., Casey, A. R., Costado, M. T., Damiani, F., Franciosini, E., Frasca, A., Hourihane, A., Jofré, P., de Laverny, P., Lewis, J., Masseron, T., Monaco, L., Morbidelli, L., Prisinzano, L., Sacco, G., Zaggia, S., European Research Council, Leverhulme Trust, Istituto Nazionale di Astrofisica, European Science Foundation, Ministerio de Economía y Competitividad (España), European Commission, Fundação para a Ciência e a Tecnologia (Portugal), Science and Technology Facilities Council (UK), Ministerio de Economía, Fomento y Turismo (Chile), Ministry of Science and Higher Education (Poland), Knut and Alice Wallenberg Foundation, Magrini, L., Spina, Lorenzo, Randich, S., Friel, E., Kordopatis, G., Worley, C., Pancino, E., Bragaglia, A., Donati, P., Tautvaišienė, G., Bagdonas, V., Delgado-Mena, E., Adibekyan, V., Sousa, S. G., Jiménez-Esteban, Francisco M., Sanna, N., Roccatagliata, V., Bonito, R., Sbordone, L., Duffau, S., Gilmore, Gerry, Feltzing, S., Jeffries, R.D., Vallenari, A., Alfaro, Emilio J., Bensby, T., Francois, P., Koposov, S., Korn, A.J., Recio-Blanco, A., Smiljanic, R., Bayo, A., Carraro, G., Casey, A. R., Costado, M. T., Damiani, F., Franciosini, E., Frasca, A., Hourihane, A., Jofré, P., de Laverny, P., Lewis, J., Masseron, T., Monaco, L., Morbidelli, L., Prisinzano, L., Sacco, G., and Zaggia, S.
Abstract: Context. Several works have found an increase of the abundances of the s-process neutron-capture elements in the youngest Galactic stellar populations. These trends provide important constraints on stellar and Galactic evolution and they need to be confirmed with large and statistically significant samples of stars spanning wide age and distance intervals. Aims. We aim to trace the abundance patterns and the time evolution of five s-process elements - two belonging to the first peak, Y and Zr, and three belonging to the second peak, Ba, La, and Ce - using the Gaia-ESO IDR5 results for open clusters and disc stars. Methods. From the UVES spectra of cluster member stars, we determined the average composition of clusters with ages >0.1 Gyr. We derived statistical ages and distances of field stars, and we separated them into thin and thick disc populations. We studied the time-evolution and dependence on metallicity of abundance ratios using open clusters and field stars whose parameters and abundances were derived in a homogeneous way. Results. Using our large and homogeneous sample of open clusters, thin and thick disc stars, spanning an age range larger than 10 Gyr, we confirm an increase towards young ages of s-process abundances in the solar neighbourhood. These trends are well defined for open clusters and stars located nearby the solar position and they may be explained by a late enrichment due to significant contribution to the production of these elements from long-living low-mass stars. At the same time, we find a strong dependence of the s-process abundance ratios on the Galactocentric distance and on the metallicity of the clusters and field stars. Conclusions. Our results, derived from the largest and most homogeneous sample of s-process abundances in the literature, confirm the growth with decreasing stellar ages of the s-process abundances in both field and open cluster stars. At the same time, taking advantage of the abundances of open clusters located i
Published: 2018

32. The Gaia-ESO Survey and CSI 2264: Substructures, disks, and sequential star formation in the young open cluster NGC 2264

Author: European Research Council, Leverhulme Trust, Istituto Nazionale di Astrofisica, Ministero dell'Istruzione, dell'Università e della Ricerca, European Science Foundation, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Ministerio de Economía y Competitividad (España), European Commission, Venuti, L., Prisinzano, L., Sacco, G. G., Flaccomio, E., Bonito, R., Damiani, F., Micela, Giusi, Guarcello, M.G., Randich, S., Stauffer, J. R., Cody, A. M., Jeffries, R.D., Alencar, S. H. P., Alfaro, Emilio J., Lanzafame, A.C., Pancino, E., Bayo, A., Carraro, G., Costado, M. T., Frasca, A., Jofré, P., Morbidelli, L., Sousa, S. G., Zaggia, S., European Research Council, Leverhulme Trust, Istituto Nazionale di Astrofisica, Ministero dell'Istruzione, dell'Università e della Ricerca, European Science Foundation, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Ministerio de Economía y Competitividad (España), European Commission, Venuti, L., Prisinzano, L., Sacco, G. G., Flaccomio, E., Bonito, R., Damiani, F., Micela, Giusi, Guarcello, M.G., Randich, S., Stauffer, J. R., Cody, A. M., Jeffries, R.D., Alencar, S. H. P., Alfaro, Emilio J., Lanzafame, A.C., Pancino, E., Bayo, A., Carraro, G., Costado, M. T., Frasca, A., Jofré, P., Morbidelli, L., Sousa, S. G., and Zaggia, S.
Abstract: Context. Reconstructing the structure and history of young clusters is pivotal to understanding the mechanisms and timescales of early stellar evolution and planet formation. Recent studies suggest that star clusters often exhibit a hierarchical structure, possibly resulting from several star formation episodes occurring sequentially rather than a monolithic cloud collapse. Aims. We aim to explore the structure of the open cluster and star-forming region NGC 2264 (∼3 Myr), which is one of the youngest, richest and most accessible star clusters in the local spiral arm of our Galaxy; we link the spatial distribution of cluster members to other stellar properties such as age and evolutionary stage to probe the star formation history within the region. Methods. We combined spectroscopic data obtained as part of the Gaia-ESO Survey (GES) with multi-wavelength photometric data from the Coordinated Synoptic Investigation of NGC 2264 (CSI 2264) campaign. We examined a sample of 655 cluster members, with masses between 0.2 and 1.8 M and including both disk-bearing and disk-free young stars. We used T estimates from GES and g,r,i photometry from CSI 2264 to derive individual extinction and stellar parameters. Results. We find a significant age spread of 4-5 Myr among cluster members. Disk-bearing objects are statistically associated with younger isochronal ages than disk-free sources. The cluster has a hierarchical structure, with two main blocks along its latitudinal extension. The northern half develops around the O-type binary star S Mon; the southern half, close to the tip of the Cone Nebula, contains the most embedded regions of NGC 2264, populated mainly by objects with disks and ongoing accretion. The median ages of objects at different locations within the cluster, and the spatial distribution of disked and non-disked sources, suggest that star formation began in the north of the cluster, over 5 Myr ago, and was ignited in its southern region a few Myr later. Star for
Published: 2018

33. The $\textit{Gaia}$-ESO Survey: the inner disk, intermediate-age open cluster Trumpler 23

Author: Overbeek, JC, Friel, ED, Donati, P, Smiljanic, R, Jacobson, HR, Hatzidimitriou, D, Held, EV, Magrini, L, Bragaglia, A, Randich, S, Vallenari, A, Cantat-Gaudin, T, Tautvaišienė, G, Jiménez-Esteban, F, Frasca, A, Geisler, D, Villanova, S, Tang, B, Muñoz, C, Marconi, G, Carraro, G, San Roman, I, Drazdauskas, A, Ženovienė, R, Gilmore, G, Jeffries, RD, Flaccomio, E, Pancino, E, Bayo, A, Costado, MT, Damiani, F, Jofré, P, Monaco, L, Prisinzano, L, Sousa, SG, Zaggia, S, Gilmore, Gerard [0000-0003-4632-0213], and Apollo - University of Cambridge Repository
Subjects: open clusters and associations: individual: Trumpler 23, stars: abundances, Galaxy: formation, Astrophysics::Solar and Stellar Astrophysics, Galaxy: abundances, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy: disk
Abstract: $\textit{Context}$. Trumpler 23 is a moderately populated, intermediate-age open cluster within the solar circle at a $R_\text{GC}$ ~ 6 kpc. It is in a crowded field very close to the Galactic plane and the color–magnitude diagram shows significant field contamination and possible differential reddening; it is a relatively understudied cluster for these reasons, but its location makes it a key object for determining Galactic abundance distributions. $\textit{Aims}$. New data from the $\textit{Gaia}$-ESO Survey enable the first ever radial velocity and spectroscopic metallicity measurements for this cluster. We aim to use velocities to isolate cluster members, providing more leverage for determining cluster parameters. $\textit{Methods}$. $\textit{Gaia}$-ESO Survey data for 167 potential members have yielded radial velocity measurements, which were used to determine the systemic velocity of the cluster and membership of individual stars. Atmospheric parameters were also used as a check on membership when available. Literature photometry was used to re-determine cluster parameters based on radial velocity member stars only; theoretical isochrones are fit in the $V$, $V$ − $I$ diagram. Cluster abundance measurements of ten radial-velocity member stars with high-resolution spectroscopy are presented for 24 elements. These abundances have been compared to local disk stars, and where possible placed within the context of literature gradient studies. $\textit{Results}$. We find Trumpler 23 to have an age of 0.80 ± 0.10 Gyr, significant differential reddening with an estimated mean cluster $E$($V$ − $I$) of 1.02$^{+0.14}_{−0.09}$, and an apparent distance modulus of 14.15 ± 0.20. We find an average cluster metallicity of [Fe/H] = 0.14 ± 0.03 dex, a solar [$\alpha$/Fe] abundance, and notably subsolar [$s$-process/Fe] abundances., Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell’ Istruzione, dell’ Università’ e della Ricerca (MIUR) in the form of the grant “Premiale VLT 2012”. The results presented here benefit from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. The research leading to these results has received funding from the European Community’s Seventh Framework Programme (FP7-SPACE-2013-1) under grant agreement No. 606740. D.G., S.V., B.T., and C.M. gratefully acknowledge support from the Chilean BASAL Centro de Excelencia en Astrofísica y Tecnologías Afines (CATA) grant PFB-06/2007.
Published: 2017

34. The $\textit{Gaia}$-ESO Survey: Calibration strategy

Author: Pancino, E, Lardo, C, Altavilla, G, Marinoni, S, Ragaini, S, Cocozza, G, Bellazzini, M, Sabbi, E, Zoccali, M, Donati, P, Heiter, U, Koposov, SE, Blomme, R, Morel, T, Símon-Díaz, S, Lobel, A, Soubiran, C, Montalban, J, Valentini, M, Casey, AR, Blanco-Cuaresma, S, Jofré, P, Worley, CC, Magrini, L, Hourihane, A, François, P, Feltzing, S, Gilmore, G, Randich, S, Asplund, M, Bonifacio, P, Drew, JE, Jeffries, RD, Micela, G, Vallenari, A, Alfaro, EJ, Allende Prieto, C, Babusiaux, C, Bensby, T, Bragaglia, A, Flaccomio, E, Hambly, N, Korn, AJ, Lanzafame, AC, Smiljanic, R, Van Eck, S, Walton, NA, Bayo, A, Carraro, G, Costado, MT, Damiani, F, Edvardsson, B, Franciosini, E, Frasca, A, Lewis, J, Monaco, L, Morbidelli, L, Prisinzano, L, Sacco, GG, Sbordone, L, Sousa, SG, Zaggia, S, Koch, A, Koposov, Sergey [0000-0003-2644-135X], Worley, Clare [0000-0001-9310-2898], Gilmore, Gerard [0000-0003-4632-0213], Walton, Nicholas [0000-0003-3983-8778], and Apollo - University of Cambridge Repository
Subjects: surveys, stars: abundances, techniques: radial velocities, Condensed Matter::Disordered Systems and Neural Networks, Galaxy: general, Astrophysics::Galaxy Astrophysics, techniques: spectroscopic
Abstract: The $\textit{Gaia}$-ESO survey (GES) is now in its fifth and last year of observations and has produced tens of thousands of high-quality spectra of stars in all Milky Way components. This paper presents the strategy behind the selection of astrophysical calibration targets, ensuring that all GES results on radial velocities, atmospheric parameters, and chemical abundance ratios will be both internally consistent and easily comparable with other literature results, especially from other large spectroscopic surveys and from $\textit{Gaia}$. The calibration of GES is particularly delicate because of (i) the large space of parameters covered by its targets, ranging from dwarfs to giants, from O to M stars; these targets have a large wide of metallicities and also include fast rotators, emission line objects, and stars affected by veiling; (ii) the variety of observing setups, with different wavelength ranges and resolution; and (iii) the choice of analyzing the data with many different state-of-the-art methods, each stronger in a different region of the parameter space, which ensures a better understanding of systematic uncertainties. An overview of the GES calibration and homogenization strategy is also given, along with some examples of the usage and results of calibrators in GES iDR4, which is the fourth internal GES data release and will form the basis of the next GES public data release. The agreement between GES iDR4 recommended values and reference values for the calibrating objects are very satisfactory. The average offsets and spreads are generally compatible with the GES measurement errors, which in iDR4 data already meet the requirements set by the main GES scientific goals., Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under program ID 188.B-3002 and 193.B-0936. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF–Osservatorio Astrofisico di Arcetri. These data have been obtained from the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 program through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell’Istruzione, dell’Università e della Ricerca (MIUR) in the form of the grant “Premiale VLT 2012”. The results presented here benefit from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. S.F. and T.B. acknowledge the support from the New Milky Way project funded by a grant from the Knut and Alice Wallenberg foundation. C.L. gratefully acknowledges financial support from the European Research Council (ERC-CoG-646928, Multi-Pop, PI: N. Bastian). U.H. and A.J.K acknowledge support from the Swedish National Space Board (Rymdstyrelsen). The research of A.L. has been subsidized by the Belgian Federal Science Policy Office under contract No. BR/143/A2/BRASS. R.S. acknowledges support by the National Science Center of Poland through grant 2014/15/B/ST9/03981. C.A.P. is thankful for support from the Spanish Ministry of Economy and Competitiveness (MINECO) through grant AYA2014- 56359-P. J.M. acknowledges support from the ERC Consolidator Grant funding scheme (project STARKEY, G.A. No. 615604). T.M. acknowledges financial support from Belspo for contract PRODEX Gaia-DPAC. S.G.S acknowledges the support by Fundação para a Ciência e Tecnologia (FCT) through national funds and a research grant (project ref. UID/FIS/04434/2013, and PTDC/FISAST/7073/2014). S.G.S. also acknowledge the support from FCT through Investigador FCT contract of reference IF/00028/2014 and POPH/FSE (EC) by FEDER funding through the program “Programa Operacional de Factores de Competitividade – COMPETE”. L.S. acknowledges support by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics (MAS). M.Z. acknowledges support by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics (MAS), by Fondecyt Regular 1150345 and by the BASAL CATA PFB-06. E.J.A. and M.T.C acknowledge the financial support from the Spanish Ministerio de Economía y Competitividad, through grant AYA2013-40611-P. S.Z. acknowledge the support from the INAF grant “PRIN INAF 2014”, “Star won’t tell their ages to Gaia, Galactic Archaelogy with wide-area asterosismic”. This research has made use of the WEBDA database, operated at the Department of Theoretical Physics and Astrophysics of the Masaryk University; of the TOPCAT catalogue handling and plotting tool (Taylor 2005); of the Simbad database and the VizieR catalog access tool, CDS, Strasbourg, France (Ochsenbein et al. 2000); and of NASA’s Astrophysics Data System.
Published: 2017

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

Author: Merle, T., Van der Swaelmen, M., Van Eck, S., Jorissen, A., Jackson, R. J., Traven, G., Zwitter, T., Pourbaix, D., Klutsch, A., Sacco, G., Blomme, R., Masseron, T., Gilmore, G., Randich, S., Badenes, C., Bayo, A., Bensby, T., Bergemann, M., Biazzo, K., and Damiani, F.
Subjects: GIANT stars, STELLAR populations, STAR formation, STELLAR evolution, SIGNAL-to-noise ratio, RED giants, GALACTIC bulges
Abstract: Context. Multiple stellar systems play a fundamental role in the formation and evolution of stellar populations in galaxies. Recent and ongoing large ground-based multi-object spectroscopic surveys significantly increase the sample of spectroscopic binaries (SBs) allowing analyses of their statistical properties. Aims. We investigate the repeated spectral observations of the Gaia-ESO Survey internal data release 5 (GES iDR5) to identify and characterise SBs with one visible component (SB1s) in fields covering mainly the discs, the bulge, the CoRot fields, and some stellar clusters and associations. Methods. A statistical X²-test is performed on spectra of the iDR5 subsample of approximately 43 500 stars characterised by at least two observations and a signal-to-noise ratio larger than three. In the GES iDR5, most stars have four observations generally split into two epochs. A careful estimation of the radial velocity (RV) uncertainties is performed. Our sample of RV variables is cleaned from contamination by pulsation- and/or convection-induced variables using Gaia DR2 parallaxes and photometry. Monte-Carlo simulations using the SB9 catalogue of spectroscopic orbits allow to estimate our detection efficiency and to correct the SB1 rate to evaluate the GES SB1 binary fraction and its relation to effective temperature and metallicity. Results. We find 641 (resp., 803) FGK SB1 candidates at the 5σ (resp., 3σ) level. The maximum RV differences range from 2.2 km s-1 at the 5σ confidence level (1.6 km s-1 at 3σ) to 133 km s-1 (in both cases). Among them a quarter of the primaries are giant stars and can be located as far as 10 kpc. The orbital-period distribution is estimated from the RV standard-deviation distribution and reveals that the detected SB1s probe binaries with log P[d] / 4. We show that SB1s with dwarf primaries tend to have shorter orbital periods than SB1s with giant primaries. This is consistent with binary interactions removing shorter period systems as the primary ascends the red giant branch. For two systems, tentative orbital solutions with periods of 4 and 6 d are provided. After correcting for detection efficiency, selection biases, and the present-day mass function, we estimate the global GES SB1 fraction to be in the range 7-14% with a typical uncertainty of 4%. A small increase of the SB1 frequency is observed from K- towards F-type stars, in agreement with previous studies. The GES SB1 frequency decreases with metallicity at a rate of (-9 ± 3)% dex-1 in the metallicity range -2.7 ≤ [Fe=H] ≤ +0.6. This anticorrelation is obtained with a confidence level higher than 93% on a homogeneous sample covering spectral types FGK and a large range of metallicities. When the present-day mass function is accounted for, this rate turns to (-4 ± 2)% dex-1 with a confidence level higher than 88%. In addition we provide the variation of the SB1 fraction with metallicity separately for F, G, and K spectral types, as well as for dwarf and giant primaries. [ABSTRACT FROM AUTHOR]
Published: 2020
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36. Deep, multiband photometry of low-mass stars to reveal young clusters: A blind study of the NGC2264 region

Author: Venuti, L., primary, Damiani, F., additional, and Prisinzano, L., additional
Published: 2018
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37. Low-mass star formation and subclustering in the H II regions RCW 32, 33, and 27 of the Vela Molecular Ridge

Author: Prisinzano, L., primary, Damiani, F., additional, Guarcello, M. G., additional, Micela, G., additional, Sciortino, S., additional, Tognelli, E., additional, and Venuti, L., additional
Published: 2018
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38. The Gaia-ESO Survey: the origin and evolution of s-process elements

Author: Magrini, L., primary, Spina, L., additional, Randich, S., additional, Friel, E., additional, Kordopatis, G., additional, Worley, C., additional, Pancino, E., additional, Bragaglia, A., additional, Donati, P., additional, Tautvaišienė, G., additional, Bagdonas, V., additional, Delgado-Mena, E., additional, Adibekyan, V., additional, Sousa, S. G., additional, Jiménez-Esteban, F. M., additional, Sanna, N., additional, Roccatagliata, V., additional, Bonito, R., additional, Sbordone, L., additional, Duffau, S., additional, Gilmore, G., additional, Feltzing, S., additional, Jeffries, R. D., additional, Vallenari, A., additional, Alfaro, E. J., additional, Bensby, T., additional, Francois, P., additional, Koposov, S., additional, Korn, A. J., additional, Recio-Blanco, A., additional, Smiljanic, R., additional, Bayo, A., additional, Carraro, G., additional, Casey, A. R., additional, Costado, M. T., additional, Damiani, F., additional, Franciosini, E., additional, Frasca, A., additional, Hourihane, A., additional, Jofré, P., additional, de Laverny, P., additional, Lewis, J., additional, Masseron, T., additional, Monaco, L., additional, Morbidelli, L., additional, Prisinzano, L., additional, Sacco, G., additional, and Zaggia, S., additional
Published: 2018
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39. The Gaia DR2 view of the Gamma Velorum cluster: resolving the 6D structure

Author: Franciosini, E., primary, Sacco, G. G., additional, Jeffries, R. D., additional, Damiani, F., additional, Roccatagliata, V., additional, Fedele, D., additional, and Randich, S., additional
Published: 2018
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40. TheGaia-ESO Survey: a kinematical and dynamical study of four young open clusters

Author: Bravi, L., primary, Zari, E., additional, Sacco, G. G., additional, Randich, S., additional, Jeffries, R. D., additional, Jackson, R. J., additional, Franciosini, E., additional, Moraux, E., additional, López-Santiago, J., additional, Pancino, E., additional, Spina, L., additional, Wright, N. J., additional, Jiménez-Esteban, F. M., additional, Klutsch, A., additional, Roccatagliata, V., additional, Gilmore, G., additional, Bragaglia, A., additional, Flaccomio, E., additional, Francois, P., additional, Koposov, S. E., additional, Bayo, A., additional, Carraro, G., additional, Costado, M. T., additional, Damiani, F., additional, Frasca, A., additional, Hourihane, A., additional, Jofré, P., additional, Lardo, C., additional, Lewis, J., additional, Magrini, L., additional, Morbidelli, L., additional, Prisinzano, L., additional, Sousa, S. G., additional, Worley, C. C., additional, and Zaggia, S., additional
Published: 2018
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41. The Gaia-ESO Survey: Lithium enrichment histories of the Galactic thick and thin disc

Author: Fu, X., primary, Romano, D., additional, Bragaglia, A., additional, Mucciarelli, A., additional, Lind, K., additional, Delgado Mena, E., additional, Sousa, S. G., additional, Randich, S., additional, Bressan, A., additional, Sbordone, L., additional, Martell, S., additional, Korn, A. J., additional, Abia, C., additional, Smiljanic, R., additional, Jofré, P., additional, Pancino, E., additional, Tautvaišienė, G., additional, Tang, B., additional, Magrini, L., additional, Lanzafame, A. C., additional, Carraro, G., additional, Bensby, T., additional, Damiani, F., additional, Alfaro, E. J., additional, Flaccomio, E., additional, Morbidelli, L., additional, Zaggia, S., additional, Lardo, C., additional, Monaco, L., additional, Frasca, A., additional, Donati, P., additional, Drazdauskas, A., additional, Chorniy, Y., additional, Bayo, A., additional, and Kordopatis, G., additional
Published: 2018
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42. Gaia-ESO Survey: Global properties of clusters Trumpler 14 and 16 in the Carina nebula

Author: European Research Council, Leverhulme Trust, Damiani, F., Klutsch, A., Jeffries, R.D., Randich, S., Prisinzano, L., Maíz Apellániz, Jesús, Micela, Giusi, Kalari, V., Frasca, A., Zwitter, T., Bonito, R., Gilmore, Gerry, Flaccomio, E., Francois, P., Koposov, S., Lanzafame, A.C., Sacco, G. G., Bayo, A., Carraro, G., Casey, A. R., Alfaro, Emilio J., Costado, M. T., Donati, P., Franciosini, E., Hourihane, A., Jofré, P., Lardo, C., Lewis, J., Magrini, L., Monaco, L., Morbidelli, L., Worley, C. C., Vink, J. S., Zaggia, S., European Research Council, Leverhulme Trust, Damiani, F., Klutsch, A., Jeffries, R.D., Randich, S., Prisinzano, L., Maíz Apellániz, Jesús, Micela, Giusi, Kalari, V., Frasca, A., Zwitter, T., Bonito, R., Gilmore, Gerry, Flaccomio, E., Francois, P., Koposov, S., Lanzafame, A.C., Sacco, G. G., Bayo, A., Carraro, G., Casey, A. R., Alfaro, Emilio J., Costado, M. T., Donati, P., Franciosini, E., Hourihane, A., Jofré, P., Lardo, C., Lewis, J., Magrini, L., Monaco, L., Morbidelli, L., Worley, C. C., Vink, J. S., and Zaggia, S.
Abstract: Aims: We present the first extensive spectroscopic study of the global population in star clusters Trumpler 16, Trumpler 14, and Collinder 232 in the Carina nebula, using data from the Gaia-ESO Survey, down to solar-mass stars. Methods: In addition to the standard homogeneous survey data reduction, a special processing was applied here because of the bright nebulosity surrounding Carina stars. Results: We find about 400 good candidate members ranging from OB types down to slightly subsolar masses. About 100 heavily reddened early-type Carina members found here were previously unrecognized or poorly classified, including two candidate O stars and several candidate Herbig Ae/Be stars. Their large brightness makes them useful tracers of the obscured Carina population. The spectroscopically derived temperatures for nearly 300 low-mass members enables the inference of individual extinction values and the study of the relative placement of stars along the line of sight. Conclusions: We find a complex spatial structure with definite clustering of low-mass members around the most massive stars and spatially variable extinction. By combining the new data with existing X-ray data, we obtain a more complete picture of the three-dimensional spatial structure of the Carina clusters and of their connection to bright and dark nebulosity and UV sources. The identification of tens of background giants also enables us to determine the total optical depth of the Carina nebula along many sightlines. We are also able to put constraints on the star formation history of the region with Trumpler 14 stars found to be systematically younger than stars in other subclusters. We find a large percentage of fast-rotating stars among Carina solar-mass members, which provide new constraints on the rotational evolution of pre-main-sequence stars in this mass range.© 2017 ESO.
Published: 2017

43. The Gaia-ESO Survey and CSI 2264: Substructures, disks, and sequential star formation in the young open cluster NGC 2264

Author: Venuti, L., primary, Prisinzano, L., additional, Sacco, G. G., additional, Flaccomio, E., additional, Bonito, R., additional, Damiani, F., additional, Micela, G., additional, Guarcello, M. G., additional, Randich, S., additional, Stauffer, J. R., additional, Cody, A. M., additional, Jeffries, R. D., additional, Alencar, S. H. P., additional, Alfaro, E. J., additional, Lanzafame, A. C., additional, Pancino, E., additional, Bayo, A., additional, Carraro, G., additional, Costado, M. T., additional, Frasca, A., additional, Jofré, P., additional, Morbidelli, L., additional, Sousa, S. G., additional, and Zaggia, S., additional
Published: 2017
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44. TheGaia-ESO Survey: double-, triple-, and quadruple-line spectroscopic binary candidates

Author: Merle, T., primary, Van Eck, S., additional, Jorissen, A., additional, Van der Swaelmen, M., additional, Masseron, T., additional, Zwitter, T., additional, Hatzidimitriou, D., additional, Klutsch, A., additional, Pourbaix, D., additional, Blomme, R., additional, Worley, C. C., additional, Sacco, G., additional, Lewis, J., additional, Abia, C., additional, Traven, G., additional, Sordo, R., additional, Bragaglia, A., additional, Smiljanic, R., additional, Pancino, E., additional, Damiani, F., additional, Hourihane, A., additional, Gilmore, G., additional, Randich, S., additional, Koposov, S., additional, Casey, A., additional, Morbidelli, L., additional, Franciosini, E., additional, Magrini, L., additional, Jofre, P., additional, Costado, M. T., additional, Jeffries, R. D., additional, Bergemann, M., additional, Lanzafame, A. C., additional, Bayo, A., additional, Carraro, G., additional, Flaccomio, E., additional, Monaco, L., additional, and Zaggia, S., additional
Published: 2017
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45. TheGaia-ESO Survey: dynamics of ionized and neutral gas in the Lagoon nebula (M 8)

Author: Damiani, F., primary, Bonito, R., additional, Prisinzano, L., additional, Zwitter, T., additional, Bayo, A., additional, Kalari, V., additional, Jiménez-Esteban, F. M., additional, Costado, M. T., additional, Jofré, P., additional, Randich, S., additional, Flaccomio, E., additional, Lanzafame, A. C., additional, Lardo, C., additional, Morbidelli, L., additional, and Zaggia, S., additional
Published: 2017
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46. TheGaia-ESO Survey: Galactic evolution of sulphur and zinc

Author: Duffau, S., primary, Caffau, E., additional, Sbordone, L., additional, Bonifacio, P., additional, Andrievsky, S., additional, Korotin, S., additional, Babusiaux, C., additional, Salvadori, S., additional, Monaco, L., additional, François, P., additional, Skúladóttir, Á., additional, Bragaglia, A., additional, Donati, P., additional, Spina, L., additional, Gallagher, A. J., additional, Ludwig, H.-G., additional, Christlieb, N., additional, Hansen, C. J., additional, Mott, A., additional, Steffen, M., additional, Zaggia, S., additional, Blanco-Cuaresma, S., additional, Calura, F., additional, Friel, E., additional, Jiménez-Esteban, F. M., additional, Koch, A., additional, Magrini, L., additional, Pancino, E., additional, Tang, B., additional, Tautvaišienė, G., additional, Vallenari, A., additional, Hawkins, K., additional, Gilmore, G., additional, Randich, S., additional, Feltzing, S., additional, Bensby, T., additional, Flaccomio, E., additional, Smiljanic, R., additional, Bayo, A., additional, Carraro, G., additional, Casey, A. R., additional, Costado, M. T., additional, Damiani, F., additional, Franciosini, E., additional, Hourihane, A., additional, Jofré, P., additional, Lardo, C., additional, Lewis, J., additional, Morbidelli, L., additional, Sousa, S. G., additional, and Worley, C. C., additional
Published: 2017
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47. Gaia-ESO Survey: Global properties of clusters Trumpler 14 and 16 in the Carina nebula

Author: Damiani, F., primary, Klutsch, A., additional, Jeffries, R. D., additional, Randich, S., additional, Prisinzano, L., additional, Maíz Apellániz, J., additional, Micela, G., additional, Kalari, V., additional, Frasca, A., additional, Zwitter, T., additional, Bonito, R., additional, Gilmore, G., additional, Flaccomio, E., additional, Francois, P., additional, Koposov, S., additional, Lanzafame, A. C., additional, Sacco, G. G., additional, Bayo, A., additional, Carraro, G., additional, Casey, A. R., additional, Alfaro, E. J., additional, Costado, M. T., additional, Donati, P., additional, Franciosini, E., additional, Hourihane, A., additional, Jofré, P., additional, Lardo, C., additional, Lewis, J., additional, Magrini, L., additional, Monaco, L., additional, Morbidelli, L., additional, Worley, C. C., additional, Vink, J. S., additional, and Zaggia, S., additional
Published: 2017
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48. TheGaia-ESO Survey: radial distribution of abundances in the Galactic disc from open clusters and young-field stars

Author: Magrini, L., primary, Randich, S., additional, Kordopatis, G., additional, Prantzos, N., additional, Romano, D., additional, Chieffi, A., additional, Limongi, M., additional, François, P., additional, Pancino, E., additional, Friel, E., additional, Bragaglia, A., additional, Tautvaišienė, G., additional, Spina, L., additional, Overbeek, J., additional, Cantat-Gaudin, T., additional, Donati, P., additional, Vallenari, A., additional, Sordo, R., additional, Jiménez-Esteban, F. M., additional, Tang, B., additional, Drazdauskas, A., additional, Sousa, S., additional, Duffau, S., additional, Jofré, P., additional, Gilmore, G., additional, Feltzing, S., additional, Alfaro, E., additional, Bensby, T., additional, Flaccomio, E., additional, Koposov, S., additional, Lanzafame, A., additional, Smiljanic, R., additional, Bayo, A., additional, Carraro, G., additional, Casey, A. R., additional, Costado, M. T., additional, Damiani, F., additional, Franciosini, E., additional, Hourihane, A., additional, Lardo, C., additional, Lewis, J., additional, Monaco, L., additional, Morbidelli, L., additional, Sacco, G., additional, Sbordone, L., additional, Worley, C. C., additional, and Zaggia, S., additional
Published: 2017
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49. Multiple kinematical populations in Vela OB2 from Gaia DR1 data

Author: Damiani, F., primary, Prisinzano, L., additional, Jeffries, R. D., additional, Sacco, G. G., additional, Randich, S., additional, and Micela, G., additional
Published: 2017
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50. TheGaia-ESO Survey

Author: Pancino, E., primary, Romano, D., additional, Tang, B., additional, Tautvaišienė, G., additional, Casey, A. R., additional, Gruyters, P., additional, Geisler, D., additional, San Roman, I., additional, Randich, S., additional, Alfaro, E. J., additional, Bragaglia, A., additional, Flaccomio, E., additional, Korn, A. J., additional, Recio-Blanco, A., additional, Smiljanic, R., additional, Carraro, G., additional, Bayo, A., additional, Costado, M. T., additional, Damiani, F., additional, Jofré, P., additional, Lardo, C., additional, de Laverny, P., additional, Monaco, L., additional, Morbidelli, L., additional, Sbordone, L., additional, Sousa, S. G., additional, and Villanova, S., additional
Published: 2017
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