J/A+A/600/A22 Iron-peak elements in solar neighbourhood (Mikolaitis+, 2017)
The AMBRE project:
Iron-peak elements in the solar neighbourhood internal data release.
Mikolaitis S., de Laverny P., Recio-Blanco A., Hill V., Worley C.C.,
de Pascale M.
<Astron. Astrophys. 600, A22 (2017)>
=2017A&A...600A..22M 2017A&A...600A..22M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, nearby ; Stars, normal ; Spectroscopy ; Abundances
Keywords: Galaxy - stars: abundances - Galaxy: stellar content
Abstract:
The aim of this paper is to characterise the abundance patterns of
five iron-peak elements (Mn, Fe, Ni, Cu, and Zn) for which the stellar
origin and chemical evolution are still debated. We automatically
derived iron peak (Mn, Fe, Ni, Cu, and Zn) and alpha element (Mg)
chemical abundances for 4666 stars. We used the bimodal distribution
of [Mg/Fe] to chemically classify sample stars into different Galactic
substructures: thin disc, metal-poor and high-alpha metal rich,
high-alpha and low-alpha metal-poor populations. High-alpha and
low-alpha metal-poor populations are fully distinct in Mg, Cu, and Zn.
Thin disc trends of [Ni/Fe] and [Cu/Fe] are very similar and show a
small increase at supersolar metallicities. Thin and thick disc trends
of Ni and Cu are very similar and indistinguishable. Mn looks
different from Ni and Cu. [Mn/Fe] trends of thin and thick discs
actually have noticeable differences: the thin disc is slightly Mn
richer than the thick disc. [Zn/Fe] trends look very similar to those
of [alpha/Fe] trends. The dispersion of results in both discs is low
(∼0.05dex for [Mg, Mn, and Cu/Fe]) and is even much lower for [Ni/Fe]
(∼0.035dex). Zn is an alpha-like element and could be used to separate
thin and thick disc stars. [Mn/Mg] ratio could also be a very good
tool for tagging Galactic substructures. Some models can partially
reproduce the observed Mg, Zn, and, Cu behaviours. Models mostly fail
to reproduce Mn and Ni in all metallicity domains, however, models
adopting yields normalised from solar chemical properties reproduce Mn
and Ni better, suggesting that there is still a lack of realistic
theoretical yields of some iron-peak elements. Very low scatter
(∼0.05dex) in thin and thick disc sequences could provide an
observational constrain for Galactic evolutionary models that study
the efficiency of stellar radial migration.
Description:
Table 5 contains Chemical abundances of iron-peak elements and
magnesium in the solar neighbourhood.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table5.dat 118 4666 Abundances of 4666 stars
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See also:
J/A+A/595/A18 : Lithium abundances in AMBRE stars (Guiglion+, 2016)
Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right ascension (J2000)
11- 20 F10.5 deg DEdeg Declination (J2000)
23- 27 A5 --- Spect Sepctrograph identification name,
HARPS or FEROS
29- 33 F5.2 [Sun] [MgI/Fe] Abundance [MgI/Fe] (Z=12)
36- 39 F4.2 [Sun] e_[MgI/Fe] rms uncertainty of Mg1 abundance
41- 45 F5.2 [Sun] [MnI/Fe] ? Abundance [MnI/Fe] (Z=25)
47- 51 F5.2 [Sun] e_[MnI/Fe] ? rms uncertainty of Mn1 abundance
53- 57 F5.2 [Sun] [FeI/H] Abundance [Fe1/H] (Z=26)
59- 63 F5.2 [Sun] e_[FeI/H] rms uncertainty of Fe1 abundance
65- 69 F5.2 [Sun] [FeII/H] ? Abundance [FeII/H] (Z=26)
71- 75 F5.2 [Sun] e_[FeII/H] ? rms uncertainty of Fe2 abundance
77- 81 F5.2 [Sun] [NiI/Fe] ? Abundance [NiI/Fe] (Z=28)
83- 87 F5.2 [Sun] e_[NiI/Fe] ? rms uncertainty of Ni1 abundance
89- 93 F5.2 [Sun] [CuI/Fe] ? Abundance [CuI/Fe] (Z=29)
95- 99 F5.2 [Sun] e_[CuI/Fe] ? rms uncertainty of Cu1 abundance
101-105 F5.2 [Sun] [ZnI/Fe] ? Abundance [ZnI/Fe] (Z=30)
107-111 F5.2 [Sun] e_[ZnI/Fe] ? rms uncertainty of Zn1 abundance
113-118 A6 --- GC ID of the Galactic component (1)
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Note (1): ID of the Galactic component as follows:
THICK = thick disc
THIN = thin disc
MP_HA = high-alpha metal-poor population
MP_LA = low-alpha metal-poor population
MR_HA = high-alpha metal-rich population
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Acknowledgements:
Sarunas Mikolaitis, Sarunas.Mikolaitis(at)tfai.vu.lt
ITPA VU, Vilnius, Lithuania and OCA, Nice, France
(End) Sarunas Mikolaitis [ITPA VU, and OCA], Patricia Vannier [CDS] 10-Jan-2017