J/A+A/619/A130 Solar sibling candidates chemical abundances (Adibekyan+, 2018)
The AMBRE project: searching for the closest solar siblings.
Adibekyan V., de Laverny P., Recio-Blanco A., Sousa S.G., Delgado-Mena E.,
Kordopatis G., Ferreira A.C.S., Santos N.C., Hakobyan A.A., Tsantaki M.
<Astron. Astrophys. 619, A130 (2018)>
=2018A&A...619A.130A 2018A&A...619A.130A (SIMBAD/NED BibCode)
ADC_Keywords: Abundances ; Stars, ages ; Sun
Keywords: stars: abundances - stars: kinematics and dynamics -
solar neighborhood
Abstract:
Finding solar siblings, that is, stars that formed in the same cluster
as the Sun, will yield information about the conditions at the Sun's
birthplace. Finding possible solar siblings is difficult since they
are spread widely throughout the Galaxy.
We search for solar sibling candidates in AMBRE, the very large
spectra database of solar vicinity stars.
Since the ages and chemical abundances of solar siblings are very
similar to those of the Sun, we carried out a chemistry- and age-based
search for solar sibling candidates. We used high-resolution spectra
to derive precise stellar parameters and chemical abundances of the
stars. We used these spectroscopic parameters together with Gaia DR2
astrometric data to derive stellar isochronal ages. Gaia data were
also used to study the kinematics of the sibling candidates.
From the about 17000 stars that are characterized within the AMBRE
project, we first selected 55 stars whose metallicities are closest to
the solar value (-0.1≤[Fe/H]≤0.1dex). For these stars we derived
precise chemical abundances of several iron-peak, α- and
neutron-capture elements, based on which we selected 12 solar sibling
candidates with average abundances and metallicities between -0.03 to
0.03dex. Our further selection left us with 4 candidates with stellar
ages that are compatible with the solar age within observational
uncertainties. For the 2 of the hottest candidates, we derived the
carbon isotopic ratios, which are compatible with the solar value.
HD186302 is the most precisely characterized and probably the most
probable candidate of our 4 best candidates.
Very precise chemical characterization and age estimation is necessary
to identify solar siblings. We propose that in addition to typical
chemical tagging, the study of isotopic ratios can give further
important information about the relation of sibling candidates with
the Sun. Ideally, asteroseismic age determinations of the candidates
could solve the problem of imprecise isochronal ages.
Description:
Chemical abundance of 55 solar sibling candidates.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
abund.dat 208 55 Abundances for each star and element (table A1)
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See also:
J/ApJ/787/154 : Solar sibling candidates elemental abundances (Ramirez+, 2014)
J/ApJ/837/15 : WISE IR excesses among main sequence stars (Da Costa+, 2017)
Byte-by-byte Description of file: abund.dat
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Bytes Format Units Label Explanations
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1- 10 A10 ----- Star Star's identifier
12- 16 F5.2 [Sun] [NaI/H] Abundance [NaI/H]
18- 21 F4.2 [Sun] e_[NaI/H] Uncertainty of [NaI/H]
23- 27 F5.2 [Sun] [MgI/H] ? Abundance [MgI/H]
29- 32 F4.2 [Sun] e_[MgI/H] ? Uncertainty of [MgI/H]
34- 38 F5.2 [Sun] [AlI/H] ? Abundance [AlI/H]
40- 43 F4.2 [Sun] e_[AlI/H] ? Uncertainty of [AlI/H]
45- 49 F5.2 [Sun] [SiI/H] Abundance [SiI/H]
51- 54 F4.2 [Sun] e_[SiI/H] Uncertainty of [SiI/H]
56- 60 F5.2 [Sun] [CaI/H] Abundance [CaI/H]
62- 65 F4.2 [Sun] e_[CaI/H] Uncertainty of [CaI/H]
67- 71 F5.2 [Sun] [ScII/H] Abundance [ScII/H]
73- 76 F4.2 [Sun] e_[ScII/H] Uncertainty of [ScII/H]
78- 82 F5.2 [Sun] [TiI/H] Abundance [TiI/H]
84- 87 F4.2 [Sun] e_[TiI/H] Uncertainty of [TiI/H]
89- 93 F5.2 [Sun] [CrI/H] Abundance [CrI/H]
95- 98 F4.2 [Sun] e_[CrI/H] Uncertainty of [CrI/H]
100-104 F5.2 [Sun] [NiI/H] Abundance [NiI/H]
106-109 F4.2 [Sun] e_[NiI/H] Uncertainty of [NiI/H]
111-115 F5.2 [Sun] [BaII/H] ? Abundance [BaII/H]
117-120 F4.2 [Sun] e_[BaII/H] ? Uncertainty of [BaII/H]
122-126 F5.2 [Sun] [CeII/H] ? Abundance [CeII/H]
128-131 F4.2 [Sun] e_[CeII/H] ? Uncertainty of [CeII/H]
133-137 F5.2 [Sun] [CuI/H] ? Abundance [CuI/H]
139-142 F4.2 [Sun] e_[CuI/H] ? Uncertainty of [CuI/H]
144-148 F5.2 [Sun] [EuII/H] ? Abundance [EuII/H]
150-153 F4.2 [Sun] e_[EuII/H] ? Uncertainty of [EuII/H]
155-159 F5.2 [Sun] [NdII/H] ? Abundance [NdII/H]
161-164 F4.2 [Sun] e_[NdII/H] ? Uncertainty of [NdII/H]
166-170 F5.2 [Sun] [SrI/H] ? Abundance [SrI/H]
172-175 F4.2 [Sun] e_[SrI/H] ? Uncertainty of [SrI/H]
177-181 F5.2 [Sun] [YII/H] ? Abundance [YII/H]
183-186 F4.2 [Sun] e_[YII/H] ? Uncertainty of [YII/H]
188-192 F5.2 [Sun] [ZnI/H] ? Abundance [ZnI/H]
194-197 F4.2 [Sun] e_[ZnI/H] ? Uncertainty of [ZnI/H]
199-203 F5.2 [Sun] [ZrII/H] ? Abundance [ZrII/H]
205-208 F4.2 [Sun] e_[ZrII/H] ? Uncertainty of [ZrII/H]
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Acknowledgements:
Vardan Adibekyan, Vardan.Adibekyan(at)astro.up.pt
(End) Vardan Adibekyan [IA], Patricia Vannier [CDS] 11-Oct-2018