J/A+A/665/A10 CERES I. Abundances for 52 star (Lombardo+, 2022)
Chemical Evolution of R-process Elements in Stars (CERES).
I. Stellar parameters and chemical abundances from Na to Zr.
Lombardo L., Bonifacio P., Francois P., Hansen C.J., Caffau E., Hanke M.,
Skuladottir A., Arcones A., Eichler M., Reichert M., Psaltis A.,
Koch Hansen A.J., Sbordone L.
<Astron. Astrophys. 665, A10 (2022)>
=2022A&A...665A..10L 2022A&A...665A..10L (SIMBAD/NED BibCode)
ADC_Keywords: Stars, giant ; Abundances ; Optical
Keywords: Galaxy: abundances - Galaxy: evolution - stars: abundances -
stars: Population II - stars: Population III -
nuclear reactions, nucleosynthesis
Abstract:
The Chemical Evolution of R-process Elements in Stars (CERES) project
aims at providing a homogeneous analysis of a sample of metal poor
stars ([Fe/H]←1.5). We present the stellar parameters and the
chemical abundances of elements up to Zr for a sample of 52 giant
stars.
We relied on a sample of high signal-to-noise UVES spectra. We
determined stellar parameters from Gaia photometry and parallaxes.
Chemical abundances were derived using spectrum synthesis and model
atmospheres.
We determined chemical abundances of 26 species of 18 elements: Na,
Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Sr, Y, and Zr.
For several stars, we could measure both neutral and ionised species
including Si, Sc, Mn and Zr. We have roughly doubled the number of
measurements of Cu for stars at [Fe/H]≤2.5. The homogeneity of the
sample made it possible to highlight the presence of two Zn rich stars
([Zn/Fe]~+0.7), one r-rich and the other r-poor. We report the
existence of two branches in the [Zn/Fe] vs. [Ni/Fe] plane and suggest
that the high [Zn/Fe] branch is the result of hypernova
nucleosynthesis. We discovered two stars with peculiar light neutron
capture abundance patterns: CES1237+1922 (also known as BS
16085-0050), which is ∼1 dex underabundant in Sr, Y, and Zr with
respect to the other stars in the sample, and CES2250-4057 (also known
as HE 2247-4113), which shows a ∼1 dex overabundance of Sr with
respect to Y and Zr.
The high quality of our dataset allowed us to measure hardly
detectable ions. This can provide guidance in the development of line
formation computations that take into account deviations from local
thermodynamic equilibrium and hydrodynamical effects.
Description:
The target stars were observed with the Ultraviolet and Visual Echelle
Spectrograph (UVES) of the Very Large Telescope (VLT) at the European
Southern Observatory (ESO) during two runs (November 2019 and March
2020) with differing exposures to reach a S/N of 50 to 120 per pixel
at 390nm for most stars.
Our own observations were complemented with archival data of
comparable quality. All the archival data used were acquired prior to
2019.
We present a homogeneous set of stellar parameters and a chemical
abundance analysis of elements from Na to Zr for a sample of 52
Galactic halo giant stars with -3:58≤[Fe/H]≤-1.79.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 53 52 Sample stars
table3.dat 748 52 Abundances
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Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name Star name
18- 29 A12 --- Star Stellar name (CESHHMM+DDMM)
31- 32 I2 h RAh Right ascension (J2000)
34- 35 I2 min RAm Right ascension (J2000)
37- 41 F5.2 s RAs Right ascension (J2000)
43 A1 --- DE- Declination sign (J2000)
44- 45 I2 deg DEd Declination (J2000)
47- 48 I2 arcmin DEm Declination (J2000)
50- 53 F4.1 arcsec DEs Declination (J2000)
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Star Stellar name (CESHHMM+DDMM)
14- 16 I3 --- o_FeI Number of FeI lines used
18- 21 F4.2 --- A(FeI) FeI abundance from FeI lines
23- 26 F4.2 --- s(FeI) Line-to-line scatter for FeI lines
28- 32 F5.2 --- [FeI/H] FeI abundance relative to the Sun
34- 35 I2 --- o_FeII Number of FeII lines used
37- 40 F4.2 --- A(FeII) FeII abundance from FeI lines
42- 45 F4.2 --- s(FeII) Line-to-line scatter for FeII lines
47- 51 F5.2 --- [FeII/H] FeII abundance relative to the Sun
53 A1 --- f_FeII Flag on FeII (1)
55 I1 --- o_NaI ? Number of NaI lines used
57- 61 F5.2 --- A(NaI)LTE ? NaI LTE abundance from NaI lines
63- 67 F5.2 --- s(NaI)LTE ? Line-to-line scatter for NaI lines
69- 73 F5.2 --- [NaI/H]LTE ? NaI LTE abundance relative to the Sun
75- 79 F5.2 --- [NaI/FeI]LTE ? NaI LTE over FeI abundance ratio
81- 85 F5.2 --- A(NaI)NLTE ? NaI NLTE abundance from NaI lines
87- 91 F5.2 --- s(NaI)NLTE ? line-to-line scatter for NaI lines
93- 97 F5.2 --- [NaI/H]NLTE ? NaI NLTE abundance relative to the Sun
99-103 F5.2 --- [NaI/FeI]NLTE ? NaI NLTE over FeI abundance ratio
105 A1 --- f_NaI Flag on NaI (1)
107 I1 --- o_MgI Number of MgI lines used
109-112 F4.2 --- A(MgI) MgI abundance from MgI lines
114-117 F4.2 --- s(MgI) Line-to-line scatter for MgI lines
119-123 F5.2 --- [MgI/H] MgI abundance relative to the Sun
125-128 F4.2 --- [MgI/FeI] MgI over FeI abundance ratio
130 A1 --- f_MgI Flag on MgI (1)
132 I1 --- o_AlI ? Number of AlI lines used
134-138 F5.2 --- A(AlI)LTE ? AlI LTE abundance from AlI lines
140-144 F5.2 --- s(AlI)LTE ? Line-to-line scatter for AlI lines
146-150 F5.2 --- [AlI/H]LTE ? AlI LTE abundance relative to the Sun
152-156 F5.2 --- [AlI/FeI]LTE ? AlI LTE over FeI abundance ratio
158-162 F5.2 --- [AlI/H]NLTE ? AlI NLTE abundance relative to the Sun
164-168 F5.2 --- [AlI/FeI]NLTE ? AlI NLTE over FeI abundance ratio
170 A1 --- f_AlI Flag on AlI (1)
172-173 I2 --- o_SiI ? Number of SiI lines used
175-179 F5.2 --- A(SiI) ? SiI abundance from SiI lines
181-185 F5.2 --- s(SiI) ? Line-to-line scatter for SiI lines
187-191 F5.2 --- [SiI/H] ? SiI abundance relative to the Sun
193-197 F5.2 --- [SiI/FeI] ? SiI over FeI abundance ratio
199 A1 --- f_SiI Flag on SiI (1)
201 I1 --- o_SiII ? Number of SiII lines used
203-207 F5.2 --- A(SiII) ? SiII abundance from SiII lines
209-213 F5.2 --- s(SiII) ? Line-to-line scatter for SiII lines
215-219 F5.2 --- [SiII/H] ? SiII abundance relative to the Sun
221-225 F5.2 --- [SiII/FeII] ? SiII over FeII abundance ratio
227-228 A2 --- f_SiII Flag on SiII (1)
230-231 I2 --- o_CaI ? Number of CaI lines used
233-237 F5.2 --- A(CaI) ? CaI abundance from CaI lines
239-243 F5.2 --- s(CaI) ? Line-to-line scatter for CaI lines
245-249 F5.2 --- [CaI/H] ? CaI abundance relative to the Sun
251-255 F5.2 --- [CaI/FeI] ? CaI over FeI abundance ratio
257 I1 --- o_ScI ? Number of ScI lines used
259-263 F5.2 --- A(ScI) ? ScI abundance from ScI lines
265-269 F5.2 --- s(ScI) ? Line-to-line scatter for ScI lines
271-275 F5.2 --- [ScI/H] ? ScI abundance relative to the Sun
277-281 F5.2 --- [ScI/FeI] ? ScI over FeI abundance ratio
283-284 A2 --- f_ScI Flag on ScI (1)
286-287 I2 --- o_ScII ? Number of ScII lines used
289-293 F5.2 --- A(ScII) ? ScII abundance from ScII lines
295-299 F5.2 --- s(ScII) ? Line-to-line scatter for ScII lines
301-305 F5.2 --- [ScII/H] ? ScII abundance relative to the Sun
307-311 F5.2 --- [ScII/FeII] ? ScII over FeII abundance ratio
313-314 I2 --- o_TiI Number of TiI lines used
316-319 F4.2 --- A(TiI) TiI abundance from TiI lines
321-324 F4.2 --- s(TiI) Line-to-line scatter for TiI lines
326-330 F5.2 --- [TiI/H] TiI abundance relative to the Sun
332-335 F4.2 --- [TiI/FeI] TiI over FeI abundance ratio
337-338 I2 --- o_TiII Number of TiII lines used
340-343 F4.2 --- A(TiII) TiII abundance from TiII lines
345-348 F4.2 --- s(TiII) Line-to-line scatter for TiII lines
350-354 F5.2 --- [TiII/H] TiII abundance relative to the Sun
356-359 F4.2 --- [TiII/FeII] TiII over FeII abundance ratio
361-362 I2 --- o_VI ? Number of VI lines used
364-368 F5.2 --- A(VI) ? VI abundance from VI lines
370-374 F5.2 --- s(VI) ? Line-to-line scatter for VI lines
376-380 F5.2 --- [VI/H] ? VI abundance relative to the Sun
382-386 F5.2 --- [VI/FeI] ? VI over FeI abundance ratio
388 A1 --- f_VI Flag on VI (1)
390 I1 --- o_VII Number of VII lines used
392-395 F4.2 --- A(VII) VII abundance from VII lines
397-400 F4.2 --- s(VII) Line-to-line scatter for VII lines
402-406 F5.2 --- [VII/H] VII abundance relative to the Sun
408-412 F5.2 --- [VII/FeII] VII over FeII abundance ratio
414 A1 --- f_VII Flag on VII (1)
416-417 I2 --- o_CrI ? Number of CrI lines used
419-423 F5.2 --- A(CrI) ? CrI abundance from CrI lines
425-429 F5.2 --- s(CrI) ? Line-to-line scatter for CrI lines
431-435 F5.2 --- [CrI/H] ? CrI abundance relative to the Sun
437-441 F5.2 --- [CrI/FeI] ? CrI over FeI abundance ratio
443 A1 --- f_CrI Flag on CrI (1)
445 I1 --- o_CrII ? Number of CrII lines used
447-451 F5.2 --- A(CrII) ? CrII abundance from CrII lines
453-457 F5.2 --- s(CrII) ? Line-to-line scatter for CrII lines
459-463 F5.2 --- [CrII/H] ? CrII abundance relative to the Sun
465-469 F5.2 --- [CrII/FeII] ? CrII over FeII abundance ratio
471 A1 --- f_CrII Flag on CrII (1)
473-474 I2 --- o_MnI ? Number of MnI lines used
476-479 F4.2 --- A(MnI) ? MnI abundance from MnI lines
481-484 F4.2 --- s(MnI) ? Line-to-line scatter for MnI lines
486-490 F5.2 --- [MnI/H] ? MnI abundance relative to the Sun
492-496 F5.2 --- [MnI/FeI] ? MnI over FeI abundance ratio
498 A1 --- f_MnI Flag on MnI (1)
500 I1 --- o_MnII ? Number of MnII lines used
502-506 F5.2 --- A(MnII) ? MnII abundance from MnII lines
508-511 F4.1 --- s(MnII) ? Line-to-line scatter for MnII lines
513-517 F5.2 --- [MnII/H] ? MnII abundance relative to the Sun
519-523 F5.2 --- [MnII/FeII] ? MnII over FeII abundance ratio
525-526 A2 --- f_MnII Flag on MnII (1)
528-529 I2 --- o_CoI Number of CoI lines used
531-534 F4.2 --- A(CoI) CoI abundance from CoI lines
536-539 F4.2 --- s(CoI) Line-to-line scatter for CoI lines
541-545 F5.2 --- [CoI/H] CoI abundance relative to the Sun
547-551 F5.2 --- [CoI/FeI] CoI over FeI abundance ratio
553 A1 --- f_CoI Flag on CoI (1)
555-556 I2 --- o_NiI Number of NiI lines used
558-561 F4.2 --- A(NiI) NiI abundance from NiI lines
563-566 F4.2 --- s(NiI) Line-to-line scatter for NiI lines
568-572 F5.2 --- [NiI/H] NiI abundance relative to the Sun
574-578 F5.2 --- [NiI/FeI] NiI over FeI abundance ratio
580 A1 --- f_NiI Flag on NiI (1)
582 I1 --- o_CuI ? Number of CuI lines used
584-588 F5.2 --- A(CuI) ? CuI abundance from CuI lines
590-594 F5.2 --- s(CuI) ? Line-to-line scatter for CuI lines
596-600 F5.2 --- [CuI/H] ? CuI abundance relative to the Sun
602-606 F5.2 --- [CuI/FeI] ? CuI over FeI abundance ratio
608 A1 --- f_CuI Flag on CuI (1)
610 I1 --- o_ZnI ? Number of ZnI lines used
612-616 F5.2 --- A(ZnI) ? ZnI abundance from ZnI lines
618-622 F5.2 --- s(ZnI) ? Line-to-line scatter for ZnI lines
624-628 F5.2 --- [ZnI/H] ? ZnI abundance relative to the Sun
630-634 F5.2 --- [ZnI/FeI] ? ZnI over FeI abundance ratio
636 A1 --- f_ZnI Flag on ZnI (1)
638 I1 --- o_SrII ? Number of SrII lines used
640-644 F5.2 --- A(SrII) ? SrII abundance from SrII lines
646-650 F5.2 --- s(SrII) ? Line-to-line scatter for SrII lines
652-656 F5.2 --- [SrII/H] ? SrII abundance relative to the Sun
658-662 F5.2 --- [SrII/FeII] ? SrII over FeII abundance ratio
664 A1 --- f_SrII Flag on SrII (1)
666-667 I2 --- o_YII Number of YII lines used
669-673 F5.2 --- A(YII) YII abundance from YII lines
675-678 F4.2 --- s(YII) Line-to-line scatter for YII lines
680-684 F5.2 --- [YII/H] YII abundance relative to the Sun
686-690 F5.2 --- [YII/FeII] YII over FeII abundance ratio
692 I1 --- o_ZrI ? Number of ZrI lines used
694-698 F5.2 --- A(ZrI) ? ZrI abundance from ZrI lines
700-704 F5.2 --- s(ZrI) ? Line-to-line scatter for ZrI lines
706-710 F5.2 --- [ZrI/H] ? ZrI abundance relative to the Sun
712-716 F5.2 --- [ZrI/FeI] ? ZrI over FeI abundance ratio
718-719 A2 --- f_ZrI Flag on ZrI (1)
721-722 I2 --- o_ZrII ? Number of ZrII lines used
724-728 F5.2 --- A(ZrII) ? ZrII abundance from ZrII lines
730-734 F5.2 --- s(ZrII) ? Line-to-line scatter for ZrII lines
736-740 F5.2 --- [ZrII/H] ? ZrII abundance relative to the Sun
742-746 F5.2 --- [ZrII/FeII] ? ZrII over FeII abundance ratio
748 A1 --- f_ZrII Flag on ZrII (1)
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Note (1): Flag as follows:
* = abundance derived from only one line. For these stars we adopted as
s(X) the mean line-to-line scatter over the stars with ≥ 2 lines
of the same element X
** = for SiII, ScI, MnII, and ZrI abundances. We adopted as s(X) the mean
line-to-line scatter of the other ionisation state
D = only for Na. Na abundance derived from NaI D line(s)
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Acknowledgements:
Linda Lombardo, Linda.Lombardo(at)obspm.fr
(End) Patricia Vannier [CDS] 02-Aug-2022