J/A+A/564/A133 Gaia FGK benchmark stars: metallicity (Jofre+, 2014)
Gaia FGK benchmark stars: Metallicity.
Jofre P., Heiter U., Soubiran C., Blanco-Cuaresma S., Pancino E.,
Bergemann M., Cantat-Gaudin T., Gonzalez Hernandez J.I., Hill V.,
Lardo C., de Laverny P., Lind K., Magrini L., Masseron T., Montes D.,
Mucciarelli A., Nordlander T., Recio Blanco A., Sobeck J., Sordo R.,
Sousa S.G., Tabernero H., Vallenari A., Van Eck S.
<Astron. Astrophys. 564, A133 (2014)>
=2014A&A...564A.133J 2014A&A...564A.133J
ADC_Keywords: Stars, standard ; Spectroscopy ; Abundances, [Fe/H] ;
Equivalent widths
Keywords: standards - techniques: spectroscopic - surveys -
stars: fundamental parameters
Abstract:
To calibrate automatic pipelines that determine atmospheric parameters
of stars, one needs a sample of stars, or "benchmark stars", with
well-defined parameters to be used as a reference.
We provide detailed documentation of the iron abundance determination
of the 34 FGK-type benchmark stars that are selected to be the pillars
for calibration of the one billion Gaia stars. They cover a wide range
of temperatures, surface gravities, and metallicities.
Description:
The metallicity of the Gaia FGK benchmark stars is determined by
combining 6 methods. The Tables indicate the iron abundance and
equivalent width determined for each star, iron line and method.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 86 34 List of studied stars
table6.dat 81 242 Overview table of lines that were included for
each star
ew.dat 94 4252 Equivalent width measurements for different
methods for each iron line for each star
abund.dat 94 4252 Iron abundance measurements for different
methods for each iron line for each star
files/* . 68 *Tables with EW and A(Fe) by stars
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Note on files/* : headers indicate the name of the star.
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See also:
III/281 : Gaia FGK benchmark stars v2.1 (Jofre+, 2018)
J/MNRAS/426/1767 : Gaia Preliminary results (Pancino+, 2012)
J/A+A/552/A64 : Gaia-RVS standards (Soubiran+, 2013)
Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Star name
11- 12 I2 h RAh ? Simbad Hour of Right Ascension (J2000.0)
14- 15 I2 min RAm ? Simbad Minute of Right Ascension (J2000.0)
17- 21 F5.2 s RAs ? Simbad Second of Right Ascension (J2000.0)
23 A1 --- DE- Simbad Sign of the Declination (J2000.0)
24- 25 I2 deg DEd ? Simbad Degree of Declination (J2000.0)
27- 28 I2 arcmin DEm ? Simbad Arcminute of Declination (J2000.0)
30- 33 F4.1 arcsec DEs ? Simbad Arcsecond of Declination (J2000.0)
35- 39 F5.3 mag Bmag ? Simbad B band magnitude
41- 46 F6.3 mag Vmag ? Simbad V band magnitude
48- 62 A15 --- SpType Simbad MK spectral type
64- 74 A11 --- EW Name of the file with equivalent widths data
in subdirectory files (1)
76- 86 A11 --- Abund Name of the file with abundances data in
subdirectory files (2)
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Note (1): All files are compiled in ew.dat file.
Note (2): All files are compiled in abunddat file.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- Line Line (FeI or FeII)
6- 11 F6.1 0.1nm lambda [4787/6821] Wavelength
13 A1 --- golden-flag [Y,N] Golden line flag (Y: yes, N: no) (1)
15 I1 --- 18Sco [0/1] Usage flag (1=used) for 18 Sco
17 I1 --- 61CygA [0/1] Usage flag (1=used) for 61 CygA
19 I1 --- 61CygB [0/1] Usage flag (1=used) for 61 CygB
21 I1 --- alfCenA [0/1] Usage flag (1=used) for α CenA
23 I1 --- alfCenB [0/1] Usage flag (1=used) for α CenB
25 I1 --- alfCet [0/1] Usage flag (1=used) for α Cet
27 I1 --- alfTau [0/1] Usage flag (1=used) for α Tau
29 I1 --- Arcturus [0/1] Usage flag (1=used) for Arcturus
31 I1 --- betAra [0/1] Usage flag (1=used) for β Ara
33 I1 --- betGem [0/1] Usage flag (1=used) for β Gem
35 I1 --- betHyi [0/1] Usage flag (1=used) for β Hyi
37 I1 --- betVir [0/1] Usage flag (1=used) for β Vir
39 I1 --- delEri [0/1] Usage flag (1=used) for δ Eri
41 I1 --- epsEri [0/1] Usage flag (1=used) for ε Eri
43 I1 --- epsFor [0/1] Usage flag (1=used) for ε For
45 I1 --- epsVir [0/1] Usage flag (1=used) for ε Vir
47 I1 --- etaBoo [0/1] Usage flag (1=used) for η Boo
49 I1 --- gamSge [0/1] Usage flag (1=used) for γ Sge
51 I1 --- Gmb1830 [0/1] Usage flag (1=used) for Gmb 1830
53 I1 --- HD107328 [0/1] Usage flag (1=used) for HD 107328
55 I1 --- HD122563 [0/1] Usage flag (1=used) for HD 122563
57 I1 --- HD140283 [0/1] Usage flag (1=used) for HD 140283
59 I1 --- HD220009 [0/1] Usage flag (1=used) for HD 220009
61 I1 --- HD22879 [0/1] Usage flag (1=used) for HD 22879
63 I1 --- HD49933 [0/1] Usage flag (1=used) for HD 49933
65 I1 --- HD84937 [0/1] Usage flag (1=used) for HD 84937
67 I1 --- ksiHya [0/1] Usage flag (1=used) for ξ Hya
69 I1 --- muAra [0/1] Usage flag (1=used) for µ Ara
71 I1 --- muCasA [0/1] Usage flag (1=used) for µ CasA
73 I1 --- muLeo [0/1] Usage flag (1=used) for µ Leo
75 I1 --- Procyon [0/1] Usage flag (1=used) for Procyon
77 I1 --- psiPhe [0/1] Usage flag (1=used) for ψ Phe
79 I1 --- Sun [0/1] Usage flag (1=used) for Sun
81 I1 --- tauCet [0/1] Usage flag (1=used) for τ Cet
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Note (1): Lines commonly used in many stars were selected as golden lines
(see Sect.6.3 of the paper).
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Byte-by-byte Description of file: ew.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Star name
11- 14 A4 --- Line Line (FeI or FeII)
18- 24 F7.2 0.1nm lambda [4787/6821] Wavelength of iron line used
30- 34 F5.2 eV Ex.P Excitation potential
38- 44 F7.2 0.1pm EW1 ?=-999.00 Equivalent width obtained by
the EPINARBO method (G1)
48- 54 F7.2 0.1pm EW2 ?=-999.00 Equivalent width obtained by
the UCM method (G1)
58- 64 F7.2 0.1pm EW3 ?=-999.00 Equivalent width obtained by
the Porto method (G1)
68- 74 F7.2 0.1pm EW4 ?=-999.00 Equivalent width obtained by
the Bologna method (G1)
78- 84 F7.2 0.1pm EW5 ?=-999.00 Equivalent width obtained by
the ULB method (G1)
88- 94 F7.2 0.1pm EW6 ?=-999.00 Equivalent width obtained by
the LUMBA method (G1)
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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- 9 A9 --- Name Star name
11- 14 A4 --- Line Line (FeI or FeII)
18- 24 F7.2 0.1nm lambda [4787/6821] Wavelength of iron line used
30- 34 F5.2 eV Ex.P Excitation potential
38- 44 F7.2 [-] Ab1 [4/9.9]?=-999.00 Iron abundances (A(Fe))
obtained by the EPINARBO method (G1)
48- 54 F7.2 [-] Ab2 [4/9.9]?=-999.00 Iron abundances (A(Fe))
obtained by the UCM method (G1)
58- 64 F7.2 [-] Ab3 [4/9.9]?=-999.00 Iron abundances (A(Fe))
obtained by the Porto method (G1)
68- 74 F7.2 [-] Ab4 [4/9.9]?=-999.00 Iron abundances (A(Fe))
obtained by the Bologna method (G1)
78- 84 F7.2 [-] Ab5 [4/9.9]?=-999.00 Iron abundances (A(Fe))
obtained by the ULB method (G1)
88- 94 F7.2 [-] Ab6 [4/9.9]?=-999.00 Iron abundances (A(Fe))
obtained by the LUMBA method (G1)
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Global notes:
Note (G1): if a method had no measurement available for a given line,
the value was set to -999.00.
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Acknowledgements:
Paula Jofre, pjofre(at)ast.cam.ac.uk
Institute of Astronomy, University of Cambridge
References:
Heiter et al., Paper I 2015A&A...582A..49H 2015A&A...582A..49H
Blanco-Cuaresma et al., Paper II 2014A&A...566A..98B 2014A&A...566A..98B, Cat. J/A+A/566/A98
Jofre et al., Paper III 2014A&A...564A.133J 2014A&A...564A.133J, Cat. J/A+A/564/A133
Jofre et al., Paper IV 2015A&A...582A..81J 2015A&A...582A..81J, Cat. J/A+A/582/A81
Hawkins et al., Paper V 2016A&A...592A..70H 2016A&A...592A..70H, Cat. J/A+A/592/A70
Jofre et al., 2017A&A...601A..38J 2017A&A...601A..38J
(End) Paula Jofre [Cambridge Univ. ], Patricia Vannier [CDS] 25-Feb-2014