J/A+A/647/A162 AMBRE catalogue of sulfur abundances (Perdigon+, 2021)
The AMBRE Project: Origin and evolution of sulfur in the Milky Way.
Perdigon J., de Laverny P., Recio-Blanco A., Fernandez-Alvar E.,
Santos-Peral P., Kordopatis G., Alvarez M.A.
<Astron. Astrophys. 647, A162 (2021)>
=2021A&A...647A.162P 2021A&A...647A.162P (SIMBAD/NED BibCode)
ADC_Keywords: Stars, late-type ; Abundances, [Fe/H] ; Spectroscopy
Keywords: Galaxy: abundances - Galaxy: evolution - stars: abundances
Abstract:
Sulfur is a volatile chemical element that plays an important role in
tracing the chemical evolution of the Milky Way and external galaxies.
However, its nucleosynthesis origin and abundance variations in the
Galaxy are still unclear because the number of available stellar
sulfur abundance measurements is currently rather small.
The goal of the present article is to accurately and precisely study
the sulfur content of large number of stars located in the solar
neighbourhood. We use the parametrisation of thousands of
high-resolution stellar spectra provided by the AMBRE Project, and
combine it with the automated abundance determination GAUGUIN to
derive local thermodynamic equilibrium (LTE) sulfur abundances for
1855 slow-rotating FGK-type stars.
This is the largest and most precise catalogue of sulfur abundances
published to date. It covers a metallicity domain as high as ∼2.5dex
starting at [M/H]≲-2.0dex.
We find that the sulfur-to-iron abundances ratio is compatible with a
plateau-like distribution in the metal-poor regime, and then starts to
decrease continuously at [M/H]~-1.0dex. This decrease continues
towards negative values for supersolar metallicity stars as recently
reported for magnesium and as predicted by Galactic chemical evolution
models. Moreover, sulfur-rich stars having metallicities in the range
[-1.0,-0.5] have very different kinematical and orbital properties
with respect to more metal-rich and sulfur-poor ones. Two disc
components, associated with the thin and thick discs, are thus seen
independently in kinematics and sulfur abundances. The sulfur radial
gradients in the Galactic discs have also been estimated. Finally, the
enrichment in sulfur with respect to iron is nicely correlated with
stellar ages: older metal-poor stars have higher [S/M] ratios than
younger metal-rich ones.
This work has confirmed that sulfur is an α-element that could
be considered to explore the Galactic populations properties. For the
first time, a chemo-dynamical study from the sulfur abundance point of
view, as a stand-alone chemical element, is performed.
Description:
We present LTE sulfur abundances derived from the three main
components of the multiplet 8 system lines found around 675nm, which
are known to be poorly affected by NLTE effects. This study analysed
100,000 spectra (including several repeats per stars) retrieved from
the ESO archives of the HARPS, FEROS, and UVES instruments. These
sulfur abundances have been homogeneously measured at a spectral
resolution of 40,000 thanks to (i) stellar atmospheric parameters
previously determined within the AMBRE Project (de Laverny et al.,
2013, The Messenger, 153, 18); (ii) GAUGUIN, an optimisation method
based on the Gauss-Newton algorithm; and (iii) a precomputed grid of
synthetic spectra with [S/H] abundances varying from -3.0 to +2.0dex.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table5.dat 86 1855 AMBRE catalogue of LTE sulfur abundances
table6.dat 111 13 AMBRE LTE sulfur abundances of the Gaia
benchmarks stars adopting their recommended
atmospheric parameters
--------------------------------------------------------------------------------
See also:
J/A+A/542/A48 : AMBRE project. FEROS archived spectra (Worley+, 2012)
J/A+A/595/A18 : Lithium abundances in AMBRE stars (Guiglion+, 2016)
J/A+A/600/A22 : Iron-peak elements in solar neighbourhood (Mikolaitis+, 2017)
J/A+A/619/A130 : Solar sibling candidates chemical abundances (Adibekyan+,2018)
J/A+A/619/A143 : r-process abundances in AMBRE stars (Guiglion+, 2018)
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- GaiaDR2 ? Gaia DR2 ID
21- 28 A8 --- Name HD name for six very bright stars not present
in the Gaia second data release
31- 35 F5.1 --- S/N Signal-to-noise ratio
37- 42 F6.1 K Teff Effective temperature
44- 48 F5.2 [cm/s2] logg Surface gravity (log scale)
50- 54 F5.2 [-] [M/H] Mean stellar metallicity
56- 60 E5.2 [-] [alpha/Fe] Ratio between alpha-elements and Fe abundances
62- 65 I4 --- N6743 Number of S-6743 analysed
67- 70 I4 --- N6748 Number of S-6748 analysed
72- 75 I4 --- N6757 Number of S-6757 analysed
77- 81 F5.2 [-] [S/H] LTE sulfur abundance
83- 86 F4.2 [-] s_[S/H] ? Dispersion associated to [S/H]
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Star Star Name
13- 20 A8 --- HD HD name
22- 40 I19 --- GaiaDR2 ? Gaia DR2 ID
42 A1 --- l_S/N Limit flag on S/N
43- 46 I4 --- S/N Signal-to-noise ratio
48- 51 I4 K Teff Effective temperature
53- 56 F4.2 [cm/s] logg Surface gravity (log scale)
58- 62 F5.2 [-] [M/H] Mean stellar metallicity
64- 68 F5.2 [-] [alpha/Fe] Ratio between alpha-elements and Fe abundances
70- 73 I4 --- N6743 Number of S-6743 analysed
75- 78 I4 --- N6748 Number of S-6748 analysed
80- 83 I4 --- N6757 Number of S-6757 analysed
85- 89 F5.2 [-] [S/H] LTE sulfur abundance
91- 94 F4.2 [-] s_[S/H] ? Dispersion associated to [S/H]
96-111 A16 --- Type Type of stars
--------------------------------------------------------------------------------
Acknowledgements:
Patrick de Laverny, laverny(at)oca.eu
(End) Patrick de Laverny [Obs. Cote d'Azur], Patricia Vannier [CDS] 12-Feb-2021