The Gaia-ESO Survey: Calibrating the lithium-age relation with open clusters and associations: II. Expanded cluster sample and final membership selection

被引：0

作者：

Albarran, M. L. Gutierrez ^{[1
,2
]}

Montes, D. ^{[1
,2
]}

Tabernero, H. M. ^{[1
,2
,3
]}

Hernandez, J. I. Gonzalez ^{[3
,4
]}

Marfil, E. ^{[1
,2
,5
]}

Frasca, A. ^{[6
]}

Lanzafame, A. C. ^{[6
,7
]}

Klutsch, A. ^{[6
,8
]}

Franciosini, E. ^{[9
]}

Randich, S. ^{[9
]}

Smiljanic, R. ^{[10
]}

Korn, A. J. ^{[11
]}

Gilmore, G. ^{[12
]}

Alfaro, E. J. ^{[13
]}

Bensby, T. ^{[15
]}

Biazzo, K. ^{[16
]}

Casey, A. ^{[19
]}

Carraro, G. ^{[22
]}

Damiani, F. ^{[14
]}

Feltzing, S. ^{[15
]}

Francois, P. ^{[21
]}

Esteban, F. Jimenez ^{[13
]}

Magrini, L. ^{[9
]}

Morbidelli, L. ^{[9
]}

Prisinzano, L. ^{[14
]}

Prusti, T. ^{[20
]}

Worley, C. C. ^{[18
]}

Zaggia, S. ^{[17
]}

机构：

[1] Univ Complutense Madrid, Fac Ciencias Fis, Dept Fis Tierra & Astrofis, Madrid 28040, Spain

[2] Univ Complutense Madrid, Fac Ciencias Fis, IPARCOS UCM, Inst Fis Particulas & Cosmos UCM, Madrid 28040, Spain

[3] INTA, Ctr Astrobiol CSIC INTA, Ctra Ajalvir Km 4, Madrid 28850, Spain

[4] IAC, San Cristobal la Laguna 38205, Spain

[5] Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany

[6] INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy

[7] Univ Catania, Dipartimento Fis & Astron, Sez Astrofis, Via S Sofia 78, I-95123 Catania, Italy

[8] Eberhard Karls Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany

[9] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy

[10] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland

[11] Uppsala Univ, Dept Phys & Astron, Div Astron & Space Phys, Observat Astrophys, Box 516, S-75120 Uppsala, Sweden

[12] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[13] Inst Astrofis Andalucia CSIC, Glorieta Astron S-N, Granada 18008, Spain

[14] INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy

[15] Lund Univ, Dept Phys, Div Astrophys, Lund Observ, Box 43, S-22100 Lund, Sweden

[16] INAF, Osserv Astron Rome, Via Frascati 33, I-00044 Monte Porzio Catone, Italy

[17] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[18] Te Kura Matu Univ Canterbury, Sch Phys & Chem Sci, Private Bag 4800, Christchurch 8140, New Zealand

[19] Monash Univ, Monash Sch Phys & Astron, 114,10 Coll Walk, Clayton, Vic 3800, Australia

[20] European Space Res & Technol Ctr ESTEC, European Space Agcy ESA, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands

[21] Univ Paris Diderot, GEPI, Observ Paris, CNRS, 5 Pl Jules Janssen, F-92190 Meudon, France

[22] Univ Padua, Dipartimento Fis & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 685卷

基金：

瑞典研究理事会; 英国科学技术设施理事会;

关键词：

techniques: spectroscopic; stars: abundances; stars: activity; stars: late-type; stars: rotation; galaxies: clusters: general; LOW-MASS STARS; YOUNG OPEN CLUSTER; SOLAR-TYPE STARS; HIGH-RESOLUTION SPECTROSCOPY; SURVEY GALACTIC EVOLUTION; PROPER-MOTION SURVEY; MAIN-SEQUENCE STARS; CHAMELEON-I; RADIAL-VELOCITIES; INTERMEDIATE-AGE;

D O I：

10.1051/0004-6361/202348438

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 gamma 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.

引用

页数：80

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