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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 (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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table5.dat 118 4666 Abundances of 4666 stars
See also: J/A+A/595/A18 : Lithium abundances in AMBRE stars (Guiglion+, 2016) Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
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)
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
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
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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