J/A+A/668/A168 MINCE. I. Abundances for 35 giant stars (Cescutti+, 2022)
MINCE. I. Presentation of the project and of the first year sample.
Cescutti G., Bonifacio P., Caffau E., Monaco L., Franchini M., Lombardo L.,
Matas Pinto A.M., Lucertini F., Francois P., Spitoni E., Lallement R.,
Sbordone L., Mucciarelli A., Spite M., Hansen C.J., Di Marcantonio P.,
Kucinskas A., Dobrovolskas V., Korn A., Valentini M., Magrini L.,
Cristallo S., Matteucci F.
<Astron. Astrophys. 668, A168 (2022)>
=2022A&A...668A.168C 2022A&A...668A.168C (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Stars, giant ; Spectroscopy ; Optical ; Abundances
Keywords: Galaxy: evolution - Galaxy: formation - Galaxy: halo -
stars: abundances - stars: atmospheres -
nuclear reactions, nucleosynthesis, abundances
Abstract:
In recent years, Galactic archaeology has become a particularly
vibrant field of astronomy, with its main focus set on the oldest
stars of our Galaxy. In most cases, these stars have been identified
as the most metal-poor. However, the struggle to find these ancient
fossils has produced an important bias in the observations - in
particular, the intermediate metal-poor stars (-2.5<[Fe/H]←1.5) have
been frequently overlooked. The missing information has consequences
for the precise study of the chemical enrichment of our Galaxy, in
particular for what concerns neutron capture elements and it will be
only partially covered by future multi object spectroscopic surveys
such as WEAVE and 4MOST.
Measuring at Intermediate Metallicity Neutron Capture Elements (MINCE)
is gathering the first high-quality spectra (high signal-to-noise
ratio, S/N, and high resolution) for several hundreds of bright and
metal-poor stars, mainly located in our Galactic halo. Methods. We
compiled our selection mainly on the basis of Gaia data and determined
the stellar atmospheres of our sample and the chemical abundances of
each star.
In this paper, we present the first sample of 59 spectra of 46 stars.
We measured the radial velocities and computed the Galactic orbits for
all stars. We found that 8 stars belong to the thin disc, 15 to
disrupted satellites, and the remaining cannot be associated to the
mentioned structures, and we call them halo stars. For 33 of these
stars, we provide abundances for the elements up to zinc. We also show
the chemical evolution results for eleven chemical elements, based on
recent models.
Our observational strategy of using multiple telescopes and
spectrographs to acquire high S/N and high-resolution spectra for
intermediate-metallicity stars has proven to be very efficient, since
the present sample was acquired over only about one year of
observations. Finally, our target selection strategy, after an initial
adjustment, proved satisfactory for our purposes.
Description:
We present a homogeneous set of chemical abundance analysis of
elements from O to Zn for a sample of 35 stellar spectra of giant
stars. For two stars, we have measured the spctrum with two different
spectrographs. For each spectrum, we also present the line list used
to determine the chemical abundances. The solar abundances considered
are in the manuscript (Table 7), as well as details of the
observations (Tables A1-A4) and of stellar atmospheres (Table 2).
-99 stands for no blank field.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
abund.dat 298 35 Chemical abundances (tables C1-C3)
lines.dat 52 19836 Stellar atmospheres (table B1)
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Byte-by-byte Description of file: abund.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- Star Stellar name
16 A1 --- Flag [abc] Instrument flag (G1)
18- 25 A8 --- Inst Name of the Spectrograph
27- 33 A7 --- S/N Signal to Noise
35- 40 F6.2 --- [OI/H] ?=-99.0 Abundance relative to the Sun for OI
42- 45 F4.2 --- sigma-OI Line-to-line scatter for OI
47 I1 --- o_OI Number of lines used for OI
49- 54 F6.2 --- [NaI/H] ?=-99.0 Abundance relative to the Sun for NaI
56- 59 F4.2 --- sigma-NaI Line-to-line scatter for NaI
61 I1 --- o_NaI Number of lines used for NaI
63- 67 F5.2 --- [MgI/H] Abundance relative to the Sun for MgI
69- 72 F4.2 --- sigma-MgI Line-to-line scatter for MgI
74 I1 --- o_MgI Number of lines used for MgI
76- 81 F6.2 --- [AlI/H] ?=-99.0 Abundance relative to the Sun for AlI
83- 86 F4.2 --- sigma-AlI Line-to-line scatter for AlI
88 I1 --- o_AlI Number of lines used for AlI
90- 94 F5.2 --- [SiI/H] Abundance relative to the Sun for SiI
96- 99 F4.2 --- sigma-SiI Line-to-line scatter for SiI
101-102 I2 --- o_SiI Number of lines used for SiI
104-108 F5.2 --- [CaI/H] Abundance relative to the Sun for CaI
110-113 F4.2 --- sigma-CaI Line-to-line scatter for CaI
115-116 I2 --- o_CaI Number of lines used for CaI
118-122 F5.2 --- [ScII/H] Abundance relative to the Sun for ScII
124-127 F4.2 --- sigma-ScII Line-to-line scatter for ScII
129-130 I2 --- o_ScII Number of lines used for ScII
132-136 F5.2 --- [TiI/H] Abundance relative to the Sun for TiI
138-141 F4.2 --- sigma-TiI Line-to-line scatter for TiI
143-144 I2 --- o_TiI Number of lines used for TiI
146-150 F5.2 --- [TiII/H] Abundance relative to the Sun for TiII
152-155 F4.2 --- sigma-TiII Line-to-line scatter for TiII
157-158 I2 --- o_TiII Number of lines used for TiII
160-164 F5.2 --- [VI/H] Abundance relative to the Sun for VI
166-169 F4.2 --- sigma-VI Line-to-line scatter for VI
171-172 I2 --- o_VI Number of lines used for VI
174-178 F5.2 --- [CrI/H] Abundance relative to the Sun for CrI
180-183 F4.2 --- sigma-CrI Line-to-line scatter for CrI
185-186 I2 --- o_CrI Number of lines used for CrI
188-192 F5.2 --- [CrII/H] Abundance relative to the Sun for CrII
194-197 F4.2 --- sigma-CrII Line-to-line scatter for CrII
199 I1 --- o_CrII Number of lines used for CrII
201-205 F5.2 --- [MnI/H] Abundance relative to the Sun for MnI
207-210 F4.2 --- sigma-MnI Line-to-line scatter for MnI
212-213 I2 --- o_MnI Number of lines used for MnI
215-219 F5.2 --- [FeI/H] Abundance relative to the Sun for FeI
221-224 F4.2 --- sigma-FeI Line-to-line scatter for FeI
226-228 I3 --- o_FeI Number of lines used for FeI
230-234 F5.2 --- [FeII/H] Abundance relative to the Sun for FeII
236-239 F4.2 --- sigma-FeII Line-to-line scatter for FeII
241-242 I2 --- o_FeII Number of lines used for FeII
244-248 F5.2 --- [CoI/H] Abundance relative to the Sun for CoI
250-253 F4.2 --- sigma-CoI Line-to-line scatter for CoI
255-256 I2 --- o_CoI Number of lines used for CoI
258-262 F5.2 --- [NiI/H] Abundance relative to the Sun for NiI
264-267 F4.2 --- sigma-NiI Line-to-line scatter for NiI
269-270 I2 --- o_NiI Number of lines used for NiI
272-277 F6.2 --- [CuI/H] ?=-99.0 Abundance relative to the Sun for CuI
279-282 F4.2 --- sigma-CuI Line-to-line scatter for CuI
284 I1 --- o_CuI Number of lines used for CuI
286-291 F6.2 --- [ZnI/H] ?=-99.0 Abundance relative to the Sun for ZnI
293-296 F4.2 --- sigma-ZnI Line-to-line scatter for ZnI
298 I1 --- o_ZnI Number of lines used for ZnI
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Byte-by-byte Description of file: lines.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- El Chemical element
4- 5 I2 --- Z Atomic number
7 I1 --- ion Ionization state
9- 23 A15 --- Star Stellar name
24 A1 --- Flag [abc] Instrument flag (G1)
26- 33 F8.4 nm lambda Wavelength
35- 41 F7.3 [-] loggf loggf
43- 52 F10.3 cm-1 Elow Energy of the lower state
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Global notes:
Note (G1): Instrument flag as follows:
a = FIES spectrum
b = SOPHIE spectrum
c = HARPS-N spectrum
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Acknowledgements:
Gabriele Cescutti, gabriele.cescutti(at)inaf.it
(End) Gabriele Cescutti [INAF], Patricia Vannier [CDS] 30-Oct-2022