J/A+A/683/A72 Gaia RVS benchmark stars. II. (Caffau+, 2024)
The Gaia RVS benchmark stars.
II. A sample of stars selected for their Gaia high radial velocity.
Caffau E., Katz D., Gomez A., Bonifacio P., Lallement R., Sartoretti P.,
Sbordone L., Spite M., Mucciarelli A., Ibata R., Chemin L., Thevenin F.,
Panuzzo P., Leclerc N., Francois P., Ludwig H.-G., Monaco L., Haywood M.,
Soubiran C.
<Astron. Astrophys. 683, A72 (2024)>
=2024A&A...683A..72C 2024A&A...683A..72C (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Stars, late-type ; Abundances
Keywords: stars: abundances - Galaxy: abundances - Galaxy: evolution -
Galaxy: formation
Abstract:
The Gaia satellite has already provided the astronomical community
with three data releases, and the Radial Velocity Spectrometer (RVS)
on board Gaia has provided the radial velocity for 33 million stars.
When deriving the radial velocity from the RVS spectra, several stars
are measured to have large values. To verify the credibility of these
measurements, we selected some bright stars with the modulus of radial
velocity in excess of 500km/s to be observed with SOPHIE at OHP
and UVES at VLT. This paper is devoted to investigating the chemical
composition of the stars observed with UVES.
We derived atmospheric parameters using Gaia photometry and
parallaxes, and we performed a chemical analysis using the MyGIsFOS
code.
We find that the sample consists of metal-poor stars, although none
have extremely low metallicities. The abundance patterns match what
has been found in other samples of metal-poor stars selected
irrespective of their radial velocities. We highlight the presence of
three stars with low Cu and Zn abundances that are likely descendants
of pair-instability supernovae. Two stars are apparently younger than
1 Ga, and their masses exceed twice the turn-off mass of metal-poor
populations. This makes it unlikely that they are blue stragglers
because it would imply they formed from triple or multiple systems. We
suggest instead that they are young metal-poor stars accreted from a
dwarf galaxy. Finally, we find that the star RVS721 is associated with
the Gjoll stream, which itself is associated with the Globular Cluster
NGC 3201.
Description:
A sample of 45 stars was observed in the ESO programme 0109.22XP.001
with UVES at VLT in the setting DIC2 437+760 (wavelength ranges
373-499 and 565-946nm), with slit 0.4" (resolving power 90000) in
the blue arm and 0.3" (resolving power 110000) in the red arm. A single
exposure of about half an hour was taken for each star. A sub-sample
of 19 stars were re-observed in ESO programme 110.23V0.001.
Of the observations in P109, 42 were graded 'A' and three 'B'.
In P110, of the 21 spectra investigated, 17 were graded 'A' and
four 'B'. For the star RVS735, observed in P109, there is no blue
spectrum.
We present the abundances of the stellar sample.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
rvs.dat 779 43 Abundances of the stellar sample
lines.dat 50 34498 List of lines used
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See also:
J/A+A/651/A20 : Gaia RVS benchmark stars. I. (Caffau+, 2021)
Byte-by-byte Description of file: rvs.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Name Name of the star as in the paper (RVSNNN)
8- 26 I19 --- GaiaDR3 GaiaDR3 source_id
28- 36 A9 --- Star Internal star name
38- 43 F6.1 K Teff Effective temperature
45- 48 F4.2 [cm/s2] logg Surface gravity
50- 53 F4.2 km/s micro Microturbulence
55- 60 F6.3 --- [Fe/H] Metallicity
62- 67 F6.3 --- C1fit ? [C/H]=A(C)-A(C)sun derived from fit of
the Gband, with A(C)sun=8.50
69- 73 F5.3 --- s_C1fit Uncertainty in the C abundance
75- 80 F6.3 --- C1fitFe ? [CI/Fe] abundance
82 I1 --- NC1fit [0/1] Number of C lines
84- 89 F6.3 --- O1fit ? [O/H]=A(O)-A(O)sun derived from fit of
the Gband, with A(O)sun=8.76
91- 95 F5.3 --- s_O1fit Line-to-line scatter of O
97-101 F5.3 --- O1fitFe ? [OI/Fe] abundance
103 I1 --- NO1fit [0/2] Number of OI lines
105-110 F6.3 --- Na1nlte ? [Na/H]=A(Na)-A(Na)sun with A(Na)sun=6.30
112-116 F5.3 --- s_Na1nlte Line-to-line scatter of Na
118-123 F6.3 --- Na1nlteFe ? [NaI/Fe] abundance
125 I1 --- NNa1nlte [0/2] Number of NaI lines
127-131 F5.2 --- corNLTENa1 NLTE correction for NaI
133-138 F6.3 --- Mg1 ? [Mg/H]=A(Mg)-A(Mg)sun with A(Mg)sun=7.54
140-144 F5.3 --- s_Mg1 Line-to-line scatter of MgI
146-150 F5.3 --- Mg1Fe ? [MgI/Fe] abundance
152-153 I2 --- NMg1 [0/12] Number of MgI lines
155-160 F6.3 --- Al1 ? [Al/H]=A(Al)-A(Al)sun with A(Al)sun=6.47
162-166 F5.3 --- s_Al1 Line-to-line scatter of AlI
168-173 F6.3 --- Al1Fe ? [AlI/Fe] abundance
175 I1 --- NAl1 [0/6] Number of AlI lines
177-182 F6.3 --- Si1 ? [Si/H]=A(Si)-A(Si)sun with A(Si)sun=7.52
184-188 F5.3 --- s_Si1 Line-to-line scatter of SiI
190-195 F6.3 --- Si1Fe ? [SiI/Fe] abundance
197-198 I2 --- NSi1 [0/27] Number of SiI lines
200-205 F6.3 --- S1nlte ? [S/H]=A(S)-A(S)sun with A(S)sun=7.16
207-211 F5.3 --- s_S1nlte Line-to-line scatter of SI
213-218 F6.3 --- S1nlteFe ? [SI/Fe] abundance
220 I1 --- NS1nlte [0/2] Number of SI lines
222-226 F5.2 --- corNLTES1 NLTE correction for SI
228-233 F6.3 --- K1fit ? [K/H]=A(K)-A(K)sun with A(K)sun=5.11
235-239 F5.3 --- s_K1fit [0/0] Line-to-line scatter of KI
241-245 F5.3 --- K1fitFe ? [KI/Fe] abundance
247 I1 --- NK1fit [0/1] Number of KI lines
249-254 F6.3 --- Ca1nlte ? [Ca/H]=A(Ca)-A(Ca)sun with A(Ca)sun=6.33
256-260 F5.3 --- s_Ca1nlte Line-to-line scatter of CaI
262-266 F5.3 --- Ca1nlteFe ? [CaI/Fe] abundance
268-269 I2 --- NCa1nlte [4/24] Number of CaI lines
271-274 F4.2 --- corNLTECa1 [0.04/0.3] NLTE correction for CaI
276-281 F6.3 --- Sc1 ? [ScI/H]=A(ScI)-A(Sc)sun with
A(Sc)sun=3.10
283-287 F5.3 --- s_Sc1 Line-to-line scatter of ScI
289-294 F6.3 --- Sc1Fe ? [ScI/Fe] abundance
296 I1 --- NSc1 [0/2] Number of ScI lines
298-303 F6.3 --- Sc2 ? [ScII/H]=A(ScII)-A(Sc)sun with
A(Sc)sun=3.10
305-309 F5.3 --- s_Sc2 Line-to-line scatter of ScII
311-316 F6.3 --- Sc2Fe ? [ScII/Fe] abundance
318 I1 --- NSc2 [0/4] Number of ScII lines
320-325 F6.3 --- Ti1 ? [TiI/H]=A(TiI)-A(Ti)sun with
A(Ti)sun=4.90
327-331 F5.3 --- s_Ti1 Line-to-line scatter of TiI
333-337 F5.3 --- Ti1Fe ? [TiI/Fe] abundance
339-340 I2 --- NTi1 [0/48] Number of TiI lines
342-347 F6.3 --- Ti2 ? [TiII/H]=A(TiII)-A(Ti)sun with
A(Ti)sun=4.90
349-353 F5.3 --- s_Ti2 Line-to-line scatter of TiII
355-359 F5.3 --- Ti2Fe ? [TiII/Fe] abundance
361-362 I2 --- NTi2 [1/33] Number of TiII lines
364-369 F6.3 --- V1 ? [VI/H]=A(VI)-A(V)sun with A(V)sun=4.00
371-375 F5.3 --- s_V1 Line-to-line scatter of VI
377-382 F6.3 --- V1Fe ? [VI/Fe] abundance
384-385 I2 --- NV1 [0/19] Number of VI lines
387-392 F6.3 --- V2 ? [VII/H]=A(VII)-A(Vc)sun with A(V)sun=4.00
394-398 F5.3 --- s_V2 Line-to-line scatter of VII
400-405 F6.3 --- V2Fe ? [V/Fe] abundance
407 I1 --- NV2 [0/5] Number of VII lines
409-414 F6.3 --- Cr1 ? [CrI/H]=A(CrI)-A(Cr)sun
with A(Cr)sun=5.64
416-420 F5.3 --- s_Cr1 Line-to-line scatter of CrI
422-427 F6.3 --- Cr1Fe ? [CrI/Fe] abundance
429-430 I2 --- NCr1 [1/18] Number of CrI lines
432-437 F6.3 --- Cr2 ? [CrII/H]=A(CrII)-A(Cr)sun
with A(Cr)sun=5.64
439-443 F5.3 --- s_Cr2 Line-to-line scatter of CrII
445-450 F6.3 --- Cr2Fe ? [CrII/Fe] abundance
452 I1 --- NCr2 [0/4] Number of CrII lines
454-459 F6.3 --- Mn1nlte3d ? [MnI/H]=A(MnI)-A(Mn)sun
with A(Mn)sun=5.37
461-465 F5.3 --- s_Mn1nlte3d Line-to-line scatter of MnI
467-472 F6.3 --- Mn1nlte3dFe ? [Mn/Fe] abundance
474-475 I2 --- NMn1nlte3d [0/14] Number of MnI lines
477-481 A5 --- corNLTEMn13d NLTE correction for MnI
483-488 F6.3 --- Mn2 ? [MnII/H]=A(MnII)-A(Mn)sun
with A(Mn)sun=5.37
490-494 F5.3 --- s_Mn2 Line-to-line scatter of MnII
496-501 F6.3 --- Mn2Fe ? [MnII/Fe] abundance
503 I1 --- NMn2 [0/1] Number of MnII lines
505-510 F6.3 --- Fe1 ? [FeI/H]=A(FeI)-A(Fe)sun
with A(Fe)sun=8.52
512-516 F5.3 --- s_Fe1 Line-to-line scatter of FeI
518-522 F5.3 --- Fe1Fe [0/0] [FeI/Fe] abundance
524-526 I3 --- NFe1 [9/263] Number of FeI lines
528-533 F6.3 --- Fe2 ? FeII/H]=A(FeII)-A(Fe)sun
with A(Fe)sun=8.52
535-539 F5.3 --- s_Fe2 Line-to-line scatter of FeII
541-546 F6.3 --- Fe2Fe ? [FeII/Fe] abundance
548-549 I2 --- NFe2 [0/24] Number of FeII lines
551-556 F6.3 --- Co1 ? [CoI/H]=A(CoI)-A(Co)sun
with A(Fe)sun=4.92
558-562 F5.3 --- s_Co1 Line-to-line scatter of CoI
564-569 F6.3 --- Co1Fe ? [CoI/Fe] abundance
571-572 I2 --- NCo1 [0/15] Number of CoI lines
574-579 F6.3 --- Ni1 ? [NiI/H]=A(NiI)-A(Ni)sun
with A(Ni)sun=6.23
581-585 F5.3 --- s_Ni1 Line-to-line scatter of NiI
587-592 F6.3 --- Ni1Fe ? [NiI/Fe] abundance
594-595 I2 --- NNi1 [0/45] Number of NiI lines
597-602 F6.3 --- Cu1 ? [CuI/H]=A(CuI)-A(Cu)sun
with A(Cu)sun=4.21
604-608 F5.3 --- s_Cu1 Line-to-line scatter of CuI
610-615 F6.3 --- Cu1Fe ? [CuI/Fe] abundance
617 I1 --- NCu1 [0/2] Number of CuI lines
619-624 F6.3 --- Zn1nlte ? [ZnI/H]=A(ZnI)-A(Zn)sun
with A(Zn)sun=4.62
626-630 F5.3 --- s_Zn1nlte Line-to-line scatter of ZnI
632-637 F6.3 --- Zn1nlteFe ? [ZnI/Fe] abundance
639 I1 --- NZn1nlte [0/2] Number of ZnI lines
641-646 F6.3 --- corNLTEZn1 NLTE correction for ZnI
648-653 F6.3 --- Sr1 ? [SrI/H]=A(SrI)-A(Sr)sun
with A(Sr)sun=2.92
655-659 F5.3 --- s_Sr1 Line-to-line scatter of SrI
661-665 F5.3 --- Sr1Fe ? [SrI/Fe] abundance
667 I1 --- NSr1 [0/1] Number of SrI lines
669-674 F6.3 --- Y2 ? [YII/H]=A(YII)-A(Y)sun
with A(Y)sun=2.21
676-680 F5.3 --- s_Y2 Line-to-line scatter of YII
682-687 F6.3 --- Y2Fe ? [YII/Fe] abundance
689-690 I2 --- NY2 [0/10] Number of YII lines
692-697 F6.3 --- Zr1 ? [ZrI/H]=A(ZrI)-A(Zr)sun
with A(Zr)sun=2.62
699-703 F5.3 --- s_Zr1 Line-to-line scatter of ZrII
705-710 F6.3 --- Zr1Fe ? [ZrI/Fe] abundance
712-713 I2 --- NZr1 [0/10] Number of ZrI lines
715-720 F6.3 --- Zr2 ? [ZrII/H]=A(ZrII)-A(Zr)sun
with A(Zr)sun=2.62
722-726 F5.3 --- s_Zr2 Line-to-line scatter of ZrII
728-733 F6.3 --- Zr2Fe ? [ZrII//Fe] abundance
735-736 I2 --- NZr2 [0/10] Number of ZrII lines
738-743 F6.3 --- Ba2fit ? [BaII/H]=A(BaII)-A(Ba)sun
with A(Ba)sun=2.17
745-749 F5.3 --- s_Ba2fit Line-to-line scatter of BaII
751-756 F6.3 --- Ba2fitFe ? [BaII/Fe] abundance
758 I1 --- NBa2fit [0/2] Number of BaII lines
760-765 F6.3 --- Eu2fit ? [EuII/H]=A(EuII)-A(Eu)sun
with A(Eu)sun=0.52
767-771 F5.3 --- s_Eu2fit Line-to-line scatter of EuII
773-777 F5.3 --- Eu2fitFe ? [EuII/Fe] abundance
779 I1 --- NEu2fit [0/3] Number of EuII lines
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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- 10 A10 --- El Element
12- 22 A11 --- Star Star name (STAR_RVSNNN)
24- 31 F8.4 nm lambda Wavelength
33- 39 F7.3 [-] loggf Oscillator strength
41- 50 F10.3 eV Elow Lower energy
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Acknowledgements:
Elisabetta Caffau, Elisabetta.Caffau(at)obspm.fr
(End) Patricia Vannier [CDS] 31-Jan-2024