J/A+A/660/A135 62 Galactic open clusters abundances (Viscasillas Vazquez+ 2022)
The Gaia-ESO Survey:
Age-chemical-clock relations spatially resolved in the Galactic disc.
Viscasillas Vazquez C., Magrini L., Casali G., Tautvaisiene G., Spina L.,
Van der Swaelmen M., Randich S., Bensby T., Bragaglia A., Friel E.,
Feltzing S., Sacco G.G., Turchi A., Jimenez-Esteban F., D'Orazi V.,
Delgado-Mena E., Mikolaitis S., Drazdauskas A., Minkeviciute R.,
Stonkute E., Bagdonas V., Montes D., Guiglion G., Baratella M.,
Tabernero H.M., Gilmore G., Alfaro E., Francois P., Korn A., Smiljanic R.,
Bergemann M., Franciosini E., Gonneau A., Hourihane A., Worley C.C.,
Zaggia S.
<Astron. Astrophys. 660, A135 (2022)>
=2022A&A...660A.135V 2022A&A...660A.135V (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Clusters, open ; Abundances ; Optical
Keywords: Galaxy: abundances - Galaxy: disc -
Galaxy: open clusters and associations: general - stars: abundances
Abstract:
The last decade has seen a revolution in our knowledge of the Galaxy
thanks to the Gaia and asteroseismic space missions and the
ground-based spectroscopic surveys. To complete this picture, it is
necessary to map the ages of its stellar populations. During recent
years, the dependence on time of abundance ratios involving slow (s)
neutron-capture and α elements (called chemical-clocks) has been
used to provide estimates of stellar ages, usually in a limited volume
close to the Sun. We aim to analyse the relations of chemical clocks
in the Galactic disc extending the range to Rgc∼6-20kpc. Using the
sixth internal data release of the Gaia-ESO survey, we calibrated
several relations between stellar ages and abundance ratios[s/α]
using a sample of open clusters, the largest one so far used with this
aim (62 clusters). Thanks to their wide galactocentric coverage, we
investigated the radial variations of the shape of these relations,
confirming their non-universality. The multi-variate relations allowed
us to infer stellar ages for field stars. We estimated our accuracy
(ranging from 0.0 to -0.9Gyr) and precision (from 0.4 to 2.3Gyr) in
recovering the global ages of open clusters, and the ages of their
individual members. We applied the relations with the highest
correlation coefficients to the field star population, finding an
older population at lower metallicity and higher [α/Fe] in the
thin disc, and a younger one at higher [Fe/H] and low [α/Fe], as
expected. We confirm that there is no single age-chemical clock
relationship valid for the whole disc, but that there is a dependence
on the galactocentric position, which is related to the radial
variation of the star formation history combined with the
non-monotonic dependence on metallicity of the yields of the s-process
elements from low- and intermediate-mass stars. Finally, the abundance
ratios [Ba/α] are more sensitive to age than those with
[Y/α] for young disc stars, and their slopes vary less with
galactocentric distance. We remind the reader that the application of
such relationships to field stars is only of statistical value.
Description:
Abundances of 62 open clusters obtained from the spectral analysis
from the UVES spectra using data from the idr6 Gaia-ESO Survey.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 97 62 Metallicity of each cluster, galactocentric distance,
age and abundance ratios (average ratios [s/H] and
[s/Fe] of open clusters)
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See also:
J/A+A/640/A1 : Portrait Galactic disc (Cantat-Gaudin+, 2020)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- GESField Gaia ESO Field (cluster Name in the
Gaia ESO catalogue)
14- 18 F5.2 --- [Fe/H] Metallicity of each cluster from
Randich et al. (2022, A&A, in prep.)
20- 23 F4.2 Gyr Age Cluster age from Cantat-Gaudin et al.
(2020, Cat. J/A+A/640/A1)
25- 29 F5.2 kpc Rgc Cluster galactocentric distance from
Cantat-Gaudin et al. (2020, Cat. J/A+A/640/A1)
31- 35 F5.2 --- [YII/H] Solar scaled abundance [YII/H]
38- 42 F5.2 --- [ZrI/H] ?=- Solar scaled abundance [ZrI/H]
45- 49 F5.2 --- [BaII/H] ?=- Solar scaled abundance [BaII/H]
52- 56 F5.2 --- [LaII/H] ?=- Solar scaled abundance [LaII/H]
59- 63 F5.2 --- [CeII/H] ?=- Solar scaled abundance [CeII/H]
65- 69 F5.2 --- [YII/Fe] ?=- Solar scaled abundance ratio [YII/Fe]
72- 76 F5.2 --- [ZrI/Fe] ?=- Solar scaled abundance ratio [ZrI/Fe]
79- 83 F5.2 --- [BaII/Fe] ?=- Solar scaled abundance ratio [BaII/Fe]
86- 90 F5.2 --- [LaII/Fe] ?=- Solar scaled abundance ratio [LaII/Fe]
93- 97 F5.2 --- [CeII/Fe] ?=- Solar scaled abundance ratio [CeII/Fe]
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Acknowledgements:
Carlos Viscasillas Vazquez, carlos.viscasillas(at)ff.vu.lt
(End) Patricia Vannier [CDS] 15-Feb-2022