The Gaia-ESO Survey: Calibrating the lithium-age relation with open clusters and associations. I. Cluster age range and initial membership selections. (arXiv:2009.00610v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Albarran_M/0/1/0/all/0/1">M.L. Gutiérrez Albarrán</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Montes_D/0/1/0/all/0/1">D. Montes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garrido_M/0/1/0/all/0/1">M. Gómez Garrido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tabernero_H/0/1/0/all/0/1">H.M. Tabernero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hernandez_J/0/1/0/all/0/1">J.I. Gónzalez Hernández</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marfil_E/0/1/0/all/0/1">E. Marfil</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frasca_A/0/1/0/all/0/1">A. Frasca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lanzafame_A/0/1/0/all/0/1">A. C. Lanzafame</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klutsch_A/0/1/0/all/0/1">A. Klutsch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Franciosini_E/0/1/0/all/0/1">E. Franciosini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Randich_S/0/1/0/all/0/1">S. Randich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smiljanic_R/0/1/0/all/0/1">R. Smiljanic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Korn_A/0/1/0/all/0/1">A. J. Korn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gilmore_G/0/1/0/all/0/1">G. Gilmore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alfaro_E/0/1/0/all/0/1">E.J. Alfaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baratella_M/0/1/0/all/0/1">M. Baratella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bayo_A/0/1/0/all/0/1">A. Bayo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bensby_T/0/1/0/all/0/1">T. Bensby</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonito_R/0/1/0/all/0/1">R. Bonito</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carraro_G/0/1/0/all/0/1">G. Carraro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mena_E/0/1/0/all/0/1">E. Delgado Mena</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feltzing_S/0/1/0/all/0/1">S. Feltzing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonneau_A/0/1/0/all/0/1">A. Gonneau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heiter_U/0/1/0/all/0/1">U. Heiter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hourihane_A/0/1/0/all/0/1">A. Hourihane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Esteban_F/0/1/0/all/0/1">F. Jiménez Esteban</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jofre_P/0/1/0/all/0/1">P. Jofre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masseron_T/0/1/0/all/0/1">T. Masseron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monaco_L/0/1/0/all/0/1">L. Monaco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morbidelli_L/0/1/0/all/0/1">L. Morbidelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prisinzano_L/0/1/0/all/0/1">L. Prisinzano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roccatagliata_V/0/1/0/all/0/1">V. Roccatagliata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sousa_S/0/1/0/all/0/1">S. Sousa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Swaelmen_M/0/1/0/all/0/1">M. Van der Swaelmen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Worley_C/0/1/0/all/0/1">C.C. Worley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zaggia_S/0/1/0/all/0/1">S. Zaggia</a>
Previous studies of open clusters have shown that lithium depletion is not
only strongly age dependent but also shows a complex pattern with other
parameters that is not yet understood. For pre- and main-sequence late-type
stars, these parameters include metallicity, mixing mechanisms, convection
structure, rotation, and magnetic activity. We perform a thorough membership
analysis for a large number of stars observed within the Gaia-ESO survey (GES)
in the field of 20 open clusters, ranging in age from young clusters and
associations, to intermediate-age and old open clusters. Based on the
parameters derived from the GES spectroscopic observations, we obtained lists
of candidate members for each of the clusters in the sample by deriving RV
distributions and studying the position of the kinematic selections in the
EW(Li) versus Teff plane to obtain lithium members. We used gravity indicators
to discard field contaminants and studied [Fe/H] metallicity to further confirm
the membership of the candidates. We also made use of studies using recent data
from the Gaia DR1 and DR2 releases to assess our member selections. We
identified likely member candidates for the sample of 20 clusters observed in
GES (iDR4) with UVES and GIRAFFE, and conducted a comparative study that
allowed us to characterize the properties of these members, as well as identify
field contaminant stars, both lithium-rich giants and non-giant outliers. This
work is the first step towards the calibration of the lithium-age relation and
its dependence on other GES parameters. During this project we aim to use this
relation to infer the ages of GES field stars, and identify their potential
membership to young associations and stellar kinematic groups of different
ages.
Previous studies of open clusters have shown that lithium depletion is not
only strongly age dependent but also shows a complex pattern with other
parameters that is not yet understood. For pre- and main-sequence late-type
stars, these parameters include metallicity, mixing mechanisms, convection
structure, rotation, and magnetic activity. We perform a thorough membership
analysis for a large number of stars observed within the Gaia-ESO survey (GES)
in the field of 20 open clusters, ranging in age from young clusters and
associations, to intermediate-age and old open clusters. Based on the
parameters derived from the GES spectroscopic observations, we obtained lists
of candidate members for each of the clusters in the sample by deriving RV
distributions and studying the position of the kinematic selections in the
EW(Li) versus Teff plane to obtain lithium members. We used gravity indicators
to discard field contaminants and studied [Fe/H] metallicity to further confirm
the membership of the candidates. We also made use of studies using recent data
from the Gaia DR1 and DR2 releases to assess our member selections. We
identified likely member candidates for the sample of 20 clusters observed in
GES (iDR4) with UVES and GIRAFFE, and conducted a comparative study that
allowed us to characterize the properties of these members, as well as identify
field contaminant stars, both lithium-rich giants and non-giant outliers. This
work is the first step towards the calibration of the lithium-age relation and
its dependence on other GES parameters. During this project we aim to use this
relation to infer the ages of GES field stars, and identify their potential
membership to young associations and stellar kinematic groups of different
ages.
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