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J/AJ/153/21 Abundances in the local region. II. F, G, and K dwarfs (Luck+, 2017)

Abundances in the local region. II. F, G, and K dwarfs and subgiants. Luck R.E. <Astron. J., 153, 21-21 (2017)> =2017AJ....153...21L (SIMBAD/NED BibCode)
ADC_Keywords: Stars, F-type ; Stars, G-type ; Stars, K-type ; Stars, dwarfs ; Abundances ; Stars, masses ; Stars, ages ; Effective temperatures Keywords: Galaxy: abundances - stars: abundances - stars: evolution - stars: fundamental parameters Abstract: Parameters and abundances have been derived for 1002 stars of spectral types F, G, and K, and luminosity classes IV and V. After culling the sample for rotational velocity and effective temperature, 867 stars remain for discussion. Twenty-eight elements are considered in the analysis. The α, iron-peak, and Period 5 transition metal abundances for these stars show a modest enhancement over solar averaging about 0.05dex. The lanthanides are more abundant, averaging about +0.2dex over solar. The question is: Are these stars enhanced, or is the Sun somewhat metal-poor relative to these stars? The consistency of the abundances derived here supports an argument for the latter view. Lithium, carbon, and oxygen abundances have been derived. The stars show the usual lithium astration as a function of mass/temperature. There are more than 100 planet-hosts in the sample, and there is no discernible difference in their lithium content, relative to the remaining stars. The carbon and oxygen abundances show the well-known trend of decreasing [x/Fe] ratio with increasing [Fe/H]. Description: The McDonald Observatory 2.1m Telescope and Sandiford Cassegrain Echelle Spectrograph provided much of the observational data for this study. High-resolution spectra were obtained during numerous observing runs, from 1996 to 2010. The spectra cover a continuous wavelength range from about 484 to 700nm, with a resolving power of about 60000. The wavelength range used demands two separate observations--one centered at about 520nm, and the other at about 630nm. Typical S/N values per pixel for the spectra are more than 150. Spectra of 57 dwarfs were obtained using the Hobby-Eberly telescope and High-Resolution Spectrograph. The spectra have a resolution of 30000, spanning the wavelength range of 400 to 785nm. They also have very high signal-to-noise ratios, >300 per resolution element in numerous cases. The last set of spectra were obtained from the ELODIE Archive (Moultaka et al. 2004PASP..116..693M). These spectra are fully processed, including order co-addition, and have a continuous wavelength span of 400 to 680nm and a resolution of 42000. The ELODIE spectra utilized here all have S/N>75 per pixel. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 106 1002 Program stars table2.dat 109 1002 Temperature, luminosity, mass, age, and gravity table3.dat 106 1041 Parameter and iron data table4.dat 185 1041 Z>10 abundances for mass-derived gravities table5.dat 94 1041 Lithium, carbon, and oxygen data table7.dat 538 1041 [x/H] detail for Z>10: physical parameters
See also: I/274 : Catalog of Components of Double & Multiple stars (Dommanget+ 2002) I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) J/AJ/150/88 : Abundances in local region. I. G and K giants (Luck, 2015) J/A+A/562/A71 : Abundances of solar neighbourhood dwarfs (Bensby+, 2014) J/AJ/147/137 : Atmospheric parameters in luminous stars (Luck, 2014) J/AJ/142/136 : Spectroscopy of Cepheids. l=30-250° (Luck+, 2011) J/AJ/133/2464 : Parameters and abundances of nearby giants (Luck+, 2007) J/AJ/129/1063 : Abundances of stars within 15pc of the Sun (Luck+, 2005) J/MNRAS/349/757 : Masses, ages and metallicities of F-G dwarfs (Lambert+, 2004) J/A+AS/106/275 : Theoretical isochrones (Bertelli+ 1994) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 18 A18 --- Name Name of the primary star 20- 26 A7 --- HD H. Draper identifier (1) 28- 33 I6 --- HIP ? Hipparcos catalogue identifier (Cat. I/239) (1) 35- 38 I4 --- HR ? The Bright Star Catalogue identifier (1) 40- 50 A11 --- CCDM Identifier in the Catalog of Double and Multiple Stars (Dommanget et al. 2002, Cat. I/274) (1) 51- 52 A2 --- m_CCDM CCDM component (either A, AB, AD, B, C, or CD) 54- 68 A15 --- SpT Spectral Type (1) 70- 75 F6.2 mas plx [4.2/311]? Parallax (1) 77- 81 F5.2 mas e_plx [0.1/21.6]? Uncertainty in plx (1) 83- 87 F5.2 mag Vmag [0.3/10.9]? Johnson V band apparent magnitude (1) 89- 93 F5.1 pc Dist [3.2/234.2]? Distance 95- 98 F4.2 mag E(B-V) [0/0.03]? B-V color excess (2) 100-104 F5.2 mag VMag [0.75/11.9]? Johnson V band absolute magnitude 106 A1 --- Host [H] Planet host status (H=known host) (3)
Note (1): Values taken from Simbad. Note (2): Computed from the extinction method of Hakkila et al. 1997AJ....114.2043H. Except for d<75pc, the extinction is set to 0. Note (3): Source is The Extrasolar Planets Encyclopedia (Exoplanets team, 2016, http://exoplanet.eu/).
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 18 A18 --- Name Name of the primary star 20 A1 --- Sce [EHS] Source for spectroscopic material (E=ELODIE, H=HET, or S=Sandiford) (G1) 22- 25 I4 K Teff [3644/7671]? Effective Temperature 27- 29 I3 K e_Teff [2/333]? Standard deviation of the effective temperature 31- 32 I2 --- o_Teff [1/12]? Number of colors used in the effective temperature determination 34- 38 F5.2 [Lsun] logL [-2.42/1.61] Luminosity (logL/L) 40- 43 F4.2 Msun B1Mass [0.6/2.05]? Mass, determined from the Bertelli et al. 1994 (Cat. J/A+AS/106/275) isochrones 45- 49 F5.2 Gyr B1Age [0.63/12.02]? Age, determined from the Bertelli et al. 1994 (Cat. J/A+AS/106/275) isochrones 51- 54 F4.2 Msun DMass [0.48/2.08]? Mass, determined from the Dotter et al. 2008ApJS..178...89D isochrones 56- 60 F5.2 Gyr DAge [0.55/12.5]? Age, determined from the Dotter et al. 2008ApJS..178...89D isochrones 62- 65 F4.2 Msun YMass [0.39/2.16]? Mass, determined from the Demarque et al. 2004ApJS..155..667D isochrones 67- 71 F5.2 Gyr YAge [0.6/12]? Age, determined from the Demarque et al. 2004ApJS..155..667D isochrones 73- 76 F4.2 Msun B2Mass [0.5/2.2]? Mass, determined from the BaSTI Team (2016, BaSTI Ver. 5.0.1: http://basti.oa-teramo.inaf.it/) isochrones (1) 78- 82 F5.2 Gyr B2Age [0.6/12.5]? Age, determined from the BaSTI Team (2016, BaSTI Ver. 5.0.1: http://basti.oa-teramo.inaf.it/) isochrones (1) 84- 87 F4.2 Msun <Mass> [0.39/2.1]? Average mass 89- 92 F4.2 Msun MRange [0/0.75]? Range in mass determination 94- 98 F5.2 Gyr <Age> [0.58/12.5]? Average age 100-104 F5.2 Gyr ARange [0/11.45]? Range in age determination 106-109 F4.2 [cm/s2] logg [3.08/6.88] Log surface gravity (2)
Note (1): BaSTI Team 2016 - BaSTI Ver. 5.0.1: http://basti.oa-teramo.inaf.it/ Note (2): Surface acceleration, computed from average mass, temperature, and luminosity.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 18 A18 --- Name Name of the primary star 20 A1 --- Sce [EHS] Source for spectroscopic material (E=ELODIE, H=HET, or S=Sandiford) (G1) 22- 25 I4 K Teff1 [3644/7671] Effective temperature (1) 27- 30 F4.2 cm/s2 logg1 [3.08/5] Log surface acceleration (gravity), computed from average mass, temperature, and luminosity (1) 32- 35 F4.2 km/s Vt1 [0.15/5.7] Microturbulent velocity (Vt) (1) 37- 40 F4.2 [Sun] [FeI/H]1 [5.15/8.5] Total iron abundance, computed from neutral iron lines (the solar iron abundance is 7.47) (1) 42- 45 F4.2 [Sun] e_[FeI/H]1 [0.04/0.6] Standard deviation of the neutral iron line abundances (σ) (1) 47- 49 I3 --- o_[FeI/H]1 [3/639] Number of neutral iron lines used (1) 51- 55 F5.2 [Sun] [FeII/H]1 [5.2/11.4] Total iron abundance, computed from first ionization stage iron lines (the solar iron abundance is 7.47) (1) 57- 60 F4.2 [Sun] e_[FeII/H]1 [0/1.63] Standard deviation of the first ionization stage iron line abundances (1) 62- 63 I2 --- o_[FeII/H]1 [1/90] Number of first ionization stage iron lines used (1) 65- 68 I4 K Teff2 [3644/7671] Effective temperature (2) 70- 73 F4.2 cm/s2 logg2 [3/5] Log surface acceleration (gravity), computed from ionization balance (2) 75- 78 F4.2 km/s Vt2 [0.1/5.65] Microturbulent velocity (2) 80- 83 F4.2 [Sun] [FeI/H]2 [5.15/8.3] Total iron abundance, computed from neutral iron lines (the solar iron abundance is 7.47) (2) 85- 88 F4.2 [Sun] e_[FeI/H]2 [0.04/0.6] Standard deviation of the neutral iron line abundances (2) 90- 92 I3 --- o_[FeI/H]2 [3/639] Number of neutral iron lines used (2) 94- 98 F5.2 [Sun] [FeII/H]2 [5.15/11.4] Total iron abundance, computed from first ionization stage iron lines (the solar iron abundance is 7.47) (2) 100-103 F4.2 [Sun] e_[FeII/H]2 [0/1.63] Standard deviation of the first ionization stage iron line abundances (2) 105-106 I2 --- o_[FeII/H]2 [1/90] Number of first ionization stage iron lines used (2)
Note (1): Mass-derived gravity results, effective temperature is the same in both cases. Note (2): Ionization balance gravity results, effective temperature is the same in both cases.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 18 A18 --- Name Name of the primary star 20 A1 --- Sce [EHS] Source for spectroscopic material (E=ELODIE, H=HET, or S=Sandiford) (G1) 22- 25 I4 K Teff [3644/7671] Effective temperature 27- 30 F4.2 [cm/s2] logg [3.08/5] Log of the surface acceleration due to gravity 32- 35 F4.2 km/s Vt [0.15/5.68] Microturbulent velocity (Vt) 37- 41 F5.2 [Sun] [Na/H] [-2.5/1.9]? Log abundance of sodium 43- 47 F5.2 [Sun] [Mg/H] [-2.1/2.1]? Log abundance of magnesium 49- 53 F5.2 [Sun] [Al/H] [-1.2/1.3]? Log abundance of aluminum 55- 59 F5.2 [Sun] [Si/H] [-1.7/3.2]? Log abundance of silicon 61- 65 F5.2 [Sun] [S/H] [-0.6/4.7]? Log abundance of sulfur 67- 71 F5.2 [Sun] [Ca/H] [-2.3/2.1]? Log abundance of calcium 73- 77 F5.2 [Sun] [Sc/H] [-1.8/2.4]? Log abundance of scandium 79- 83 F5.2 [Sun] [Ti/H] [-2.2/1.9]? Log abundance of titanium 85- 89 F5.2 [Sun] [V/H] [-2.8/2.1]? Log abundance of vanadium 91- 95 F5.2 [Sun] [Cr/H] [-2.5/1.8]? Log abundance of chromium 97-101 F5.2 [Sun] [Mn/H] [-2.7/1.9]? Log abundance of manganese 103-107 F5.2 [Sun] [Fe/H] [-2.3/1.1]? Log abundance of iron 109-113 F5.2 [Sun] [Co/H] [-1.9/2.1]? Log abundance of cobalt 115-119 F5.2 [Sun] [Ni/H] [-2.2/1.8]? Log abundance of nickel 121-125 F5.2 [Sun] [Cu/H] [-2.1/1.7]? Log abundance of copper 127-131 F5.2 [Sun] [Zn/H] [-2.3/4]? Log abundance of zinc 133-137 F5.2 [Sun] [Sr/H] [-1.7/2.7]? Log abundance of strontium 139-143 F5.2 [Sun] [Y/H] [-1.9/2.4]? Log abundance of yttrium 145-149 F5.2 [Sun] [Zr/H] [-1.1/4.6]? Log abundance of zirconium 151-155 F5.2 [Sun] [Ba/H] [-3.2/1.2]? Log abundance of barium 157-161 F5.2 [Sun] [La/H] [-1.2/2.6]? Log abundance of lanthanum 163-167 F5.2 [Sun] [Ce/H] [-1.1/3.1]? Log abundance of cerium 169-173 F5.2 [Sun] [Nd/H] [-1/3.6]? Log abundance of neodymium 175-179 F5.2 [Sun] [Sm/H] [-0.9/3.4]? Log abundance of samarium 181-185 F5.2 [Sun] [Eu/H] [-2.3/3.3]? Log abundance of europium
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 18 A18 --- Name Name of the primary star 20 A1 --- Sce [EHS] Source for spectroscopic material (E=ELODIE, H=HET, or S=Sandiford) (G1) 22- 25 I4 K Teff [3644/7671] Effective temperature 27- 30 F4.2 [cm/s2] logg [3/5] Log surface gravity 32- 35 F4.2 km/s Vt [0.15/5.7] Microturbulent velocity (Vt) 37- 40 F4.1 km/s vsini [0/97.2] Rotational velocity (Vr) 42- 45 F4.2 [Sun] Fe [5.15/8.5] Iron abundance (1) 47- 51 F5.2 [-] Li [-1.1/3.8]? Lithium abundance (2) 53- 57 F5.2 [-] NLTE [-0.1/0.2]? Correction for Non Local Thermodynamic Equilibrium 59 A1 --- l_Li [L] L=Upper limit flag on lithium abundance 61- 64 F4.2 [-] 505.2 [6.4/8.9]? Carbon abundance from C I 505.2nm line (3) 66- 69 F4.2 [-] 538.0 [6.9/9.1]? Carbon abundance from C I 538.0nm line (3) 71- 74 F4.2 [-] C2 [6.4/9.3]? Carbon abundance from C2 Swan lines (primary indicator at 513.5nm) (3) 76- 79 F4.2 [-] 615.5 [6.5/9.4]? Oxygen abundance from [OI] 630.0nm line (4) 81- 84 F4.2 [-] 630.0 [6.5/9.5]? Oxygen abundance from O I 615.5 triplet (4) 86- 89 F4.2 [-] <C> [6.6/9.3]? Mean carbon abundance (weights discussed in Section 3.3) (3) 91- 94 F4.2 [-] <O> [6.5/9.5]? Mean oxygen abundance (weights discussed in Section 3.3) (4)
Note (1): The solar iron abundance is 7.47 relative to H=12. Note (2): The solar lithium abundance is 1.0dex. Note (3): The individual carbon features are combined as below: For Teff<5250K, only C2 513.5nm is used; At 5250<T<6000K, C I 505.2 and 538.0nm have weight 1 as does C2 513.5; For 6000K<T<6350K, the two C I lines have weight 2, and C2 has weight 1; Above Teff>6350K, the two C2 are not used and the two C I lines have equal weight. Relative strength and blending are the basis for the weights. A typical range in abundance for the features is 0.15 dex. The Asplund et al. 2009ARA&A..47..481A carbon abundance, logεC=8.43, is adopted for the solar reference abundance. Note (4): Oxygen abundance indicators were averaged in the following manner: for Teff<5250K, [O I] only is used. For 5250K<Teff<6000K, O I has weight 1 and [O I] has weight 3. In the regime 6000K<Teff<6350K, O I and [O I] have equal weight. Lastly, for Teff>6350K only O I is used. Near the solar temperature, typical differences between oxygen derived from O I and [O I] are of order 0.15dex. For Teff<5500K, the C-O interlock has been taken into account in the abundance determination.
Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
1- 18 A18 --- Name Name of the primary star 20- 28 A9 --- Tag ID tag for the star 30 A1 --- Sce [EHS] Source for spectroscopic material (E=ELODIE, H=HET, or S=Sandiford) (G1) 32- 35 I4 K Teff [3644/7671] Effective temperature 37- 40 F4.2 [cm/s2] logg [3/5] Log surface gravity 42- 45 F4.2 km/s Vt [0.15/5.7] Microturbulent velocity (Vt) 47- 51 F5.2 [Sun] <[NaI/H]> [-2.5/1.9]? Mean abundance of element [NaI/H] relative to solar 53- 56 F4.2 [Sun] e_<[NaI/H]> [0.02/1.2]? Standard Deviation of <[NaI/H]> 58 I1 --- o_<[NaI/H]> [1/8]? Number of lines used in <[NaI/H]> 60- 64 F5.2 [Sun] <[MgI/H]> [-2.1/2.1]? Mean abundance of element [MgI/H] relative to solar 66- 69 F4.2 [Sun] e_<[MgI/H]> [0/1.4]? Standard Deviation of <[MgI/H]> 71 I1 --- o_<[MgI/H]> [1/8]? Number of lines used in <[MgI/H]> 73- 77 F5.2 [Sun] <[AlI/H]> [-1.2/1.3]? Mean abundance of element [AlI/H] relative to solar 79- 82 F4.2 [Sun] e_<[AlI/H]> [0/0.95]? Standard Deviation of <[AlI/H]> 84 I1 --- o_<[AlI/H]> [1/8]? Number of lines used in <[AlI/H]> 86- 90 F5.2 [Sun] <[SiI/H]> [-1.7/2.5]? Mean abundance of element [SiI/H] relative to solar 92- 95 F4.2 [Sun] e_<[SiI/H]> [0.04/1]? Standard Deviation of <[SiI/H]> 97- 98 I2 --- o_<[SiI/H]> [1/70]? Number of lines used in <[SiI/H]> 100-104 F5.2 [Sun] <[SiII/H]> [-1.7/6.8]? Mean abundance of element [SiII/H] relative to solar 106-109 F4.2 [Sun] e_<[SiII/H]> [0/1.1]? Standard Deviation of <[SiII/H]> 111 I1 --- o_<[SiII/H]> [1/2]? Number of lines used in <[SiII/H]> 113-117 F5.2 [Sun] <[SI/H]> [-0.6/4.7]? Mean abundance of element [SI/H] relative to solar 119-122 F4.2 [Sun] e_<[SI/H]> [0/1.4]? Standard Deviation of <[SI/H]> 124-125 I2 --- o_<[SI/H]> [1/11]? Number of lines used in <[SI/H]> 127-131 F5.2 [Sun] <[CaI/H]> [-2.3/1.1]? Mean abundance of element [CaI/H] relative to solar 133-136 F4.2 [Sun] e_<[CaI/H]> [0.02/1.7]? Standard Deviation of <[CaI/H]> 138-139 I2 --- o_<[CaI/H]> [1/36]? Number of lines used in <[CaI/H]> 141-145 F5.2 [Sun] <[CaII/H]> [-0.7/4.9]? Mean abundance of element [CaII/H] relative to solar 147-150 F4.2 [Sun] e_<[CaII/H]> [0/1.1]? Standard Deviation of <[CaII/H]> 152 I1 --- o_<[CaII/H]> [1/4]? Number of lines used in <[CaII/H]> 154-158 F5.2 [Sun] <[ScI/H]> [-1.5/3.2]? Mean abundance of element [ScI/H] relative to solar 160-163 F4.2 [Sun] e_<[ScI/H]> [0.01/1.2]? Standard Deviation of <[ScI/H]> 165-166 I2 --- o_<[ScI/H]> [1/13]? Number of lines used in <[ScI/H]> 168-172 F5.2 [Sun] <[ScII/H]> [-1.9/2.2]? Mean abundance of element [ScII/H] relative to solar 174-177 F4.2 [Sun] e_<[ScII/H]> [0/1.4]? Standard Deviation of <[ScII/H]> 179-180 I2 --- o_<[ScII/H]> [1/18]? Number of lines used in <[ScII/H]> 182-186 F5.2 [Sun] <[TiI/H]> [-2.1/1.9]? Mean abundance of element [TiI/H] relative to solar 188-191 F4.2 [Sun] e_<[TiI/H]> [0.07/1.5]? Standard Deviation of <[TiI/H]> 193-195 I3 --- o_<[TiI/H]> [3/152]? Number of lines used in <[TiI/H]> 197-201 F5.2 [Sun] <[TiII/H]> [-2.3/2.4]? Mean abundance of element [TiII/H] relative to solar 203-206 F4.2 [Sun] e_<[TiII/H]> [0.03/1.1]? Standard Deviation of <[TiII/H]> 208-209 I2 --- o_<[TiII/H]> [1/48]? Number of lines used in <[TiII/H]> 211-215 F5.2 [Sun] <[VI/H]> [-2.8/2.7]? Mean abundance of element [VI/H] relative to solar 217-220 F4.2 [Sun] e_<[VI/H]> [0.01/1.3]? Standard Deviation of <[VI/H]> 222-223 I2 --- o_<[VI/H]> [1/69]? Number of lines used in <[VI/H]> 225-229 F5.2 [Sun] <[VII/H]> [-1.6/4]? Mean abundance of element [VII/H] relative to solar 231-234 F4.2 [Sun] e_<[VII/H]> [0/2.1]? Standard Deviation of <[VII/H]> 236-237 I2 --- o_<[VII/H]> [1/11]? Number of lines used in <[VII/H]> 239-243 F5.2 [Sun] <[CrI/H]> [-2.6/1.8]? Mean abundance of element [CrI/H] relative to solar 245-248 F4.2 [Sun] e_<[CrI/H]> [0.06/2]? Standard Deviation of <[CrI/H]> 250-252 I3 --- o_<[CrI/H]> [1/142]? Number of lines used in <[CrI/H]> 254-258 F5.2 [Sun] <[CrII/H]> [-2.32/3.68]? Mean abundance of element [CrII/H] relative to solar 260-263 F4.2 [Sun] e_<[CrII/H]> [0.03/1.2]? Standard Deviation of <[CrII/H]> 265-266 I2 --- o_<[CrII/H]> [1/21]? Number of lines used in <[CrII/H]> 268-272 F5.2 [Sun] <[MnI/H]> [-2.7/1.9]? Mean abundance of element [MnI/H] relative to solar 274-277 F4.2 [Sun] e_<[MnI/H]> [0.02/1.5]? Standard Deviation of <[MnI/H]> 279-280 I2 --- o_<[MnI/H]> [1/38]? Number of lines used in <[MnI/H]> 282-286 F5.2 [Sun] <[FeI/H]> [-2.4/1.1]? Mean abundance of element [FeI/H] relative to solar 288-291 F4.2 [Sun] e_<[FeI/H]> [0.04/0.6]? Standard Deviation of <[FeI/H]> 293-295 I3 --- o_<[FeI/H]> [3/639]? Number of lines used in <[FeI/H]> 297-301 F5.2 [Sun] <[FeII/H]> [-2.3/4]? Mean abundance of element [FeII/H] relative to solar 303-306 F4.2 [Sun] e_<[FeII/H]> [0.01/1.7]? Standard Deviation of <[FeII/H]> 308-309 I2 --- o_<[FeII/H]> [1/90]? Number of lines used in <[FeII/H]> 311-315 F5.2 [Sun] <[CoI/H]> [-1.9/2.1]? Mean abundance of element [CoI/H] relative to solar 317-320 F4.2 [Sun] e_<[CoI/H]> [0.05/1.1]? Standard Deviation of <[CoI/H]> 322-323 I2 --- o_<[CoI/H]> [1/96]? Number of lines used in <[CoI/H]> 325-329 F5.2 [Sun] <[NiI/H]> [-2.2/1.8]? Mean abundance of element [NiI/H] relative to solar 331-334 F4.2 [Sun] e_<[NiI/H]> [0.05/1]? Standard Deviation of <[NiI/H]> 336-338 I3 --- o_<[NiI/H]> [1/201]? Number of lines used in <[NiI/H]> 340-344 F5.2 [Sun] <[CuI/H]> [-2.1/1.7]? Mean abundance of element [CuI/H] relative to solar 346-349 F4.2 [Sun] e_<[CuI/H]> [0/1]? Standard Deviation of <[CuI/H]> 351 I1 --- o_<[CuI/H]> [1/4]? Number of lines used in <[CuI/H]> 353-357 F5.2 [Sun] <[ZnI/H]> [-2.3/4]? Mean abundance of element [ZnI/H] relative to solar 359-362 F4.2 [Sun] e_<[ZnI/H]> [0/1]? Standard Deviation of <[ZnI/H]> 364 I1 --- o_<[ZnI/H]> [1/4]? Number of lines used in <[ZnI/H]> 366-370 F5.2 [Sun] <[SrI/H]> [-1.7/2.7]? Mean abundance of element [SrI/H] relative to solar 372-375 F4.2 [Sun] e_<[SrI/H]> [0/0.9]? Standard Deviation of <[SrI/H]> 377 I1 --- o_<[SrI/H]> [1/4]? Number of lines used in <[SrI/H]> 379-383 F5.2 [Sun] <[YI/H]> [-1.6/2.8]? Mean abundance of element [YI/H] relative to solar 385-388 F4.2 [Sun] e_<[YI/H]> [0/2.1]? Standard Deviation of <[YI/H]> 390-391 I2 --- o_<[YI/H]> [1/13]? Number of lines used in <[YI/H]> 393-397 F5.2 [Sun] <[YII/H]> [-1.9/2.9]? Mean abundance of element [YII/H] relative to solar 399-402 F4.2 [Sun] e_<[YII/H]> [0.03/1.4]? Standard Deviation of <[YII/H]> 404-405 I2 --- o_<[YII/H]> [1/18]? Number of lines used in <[YII/H]> 407-411 F5.2 [Sun] <[ZrI/H]> [-1.1/4.6]? Mean abundance of element [ZrI/H] relative to solar 413-416 F4.2 [Sun] e_<[ZrI/H]> [0/1.4]? Standard Deviation of <[ZrI/H]> 418-419 I2 --- o_<[ZrI/H]> [1/20]? Number of lines used in <[ZrI/H]> 421-425 F5.2 [Sun] <[ZrII/H]> [-1.5/4]? Mean abundance of element [ZrII/H] relative to solar 427-430 F4.2 [Sun] e_<[ZrII/H]> [0/1.6]? Standard deviation of <[ZrII/H]> 432-433 I2 --- o_<[ZrII/H]> [1/10]? Number of lines used in <[ZrII/H]> 435-439 F5.2 [Sun] <[BaII/H]> [-3.2/1.2]? Mean abundance of element [BaII/H] relative to solar 441-444 F4.2 [Sun] e_<[BaII/H]> [0/0.8]? Standard Deviation of <[BaII/H]> 446 I1 --- o_<[BaII/H]> [1/4]? Number of lines used in <[BaII/H]> 448-452 F5.2 [Sun] <[LaII/H]> [-1.2/2.6]? Mean abundance of element [LaII/H] relative to solar 454-457 F4.2 [Sun] e_<[LaII/H]> [0/1.4]? Standard Deviation of <[LaII/H]> 459-460 I2 --- o_<[LaII/H]> [1/12]? Number of lines used in <[LaII/H]> 462-466 F5.2 [Sun] <[CeII/H]> [-1.1/3.1]? Mean abundance of element [CeII/H] relative to solar 468-471 F4.2 [Sun] e_<[CeII/H]> [0.01/2]? Standard Deviation of <[CeII/H]> 473-474 I2 --- o_<[CeII/H]> [1/38]? Number of lines used in <[CeII/H]> 476-480 F5.2 [Sun] <[PrII/H]> [-0.8/3.1]? Mean abundance of element [PrII/H] relative to solar 482-485 F4.2 [Sun] e_<[PrII/H]> [0/1.5]? Standard Deviation of <[PrII/H]> 487 I1 --- o_<[PrII/H]> [1/8]? Number of lines used in <[PrII/H]> 489-493 F5.2 [Sun] <[NdII/H]> [-1/3.6]? Mean abundance of element [NdII/H] relative to solar 495-498 F4.2 [Sun] e_<[NdII/H]> [0/2.9]? Standard Deviation of <[NdII/H]> 500-501 I2 --- o_<[NdII/H]> [1/53]? Number of lines used in <[NdII/H]> 503-507 F5.2 [Sun] <[SmII/H]> [-0.9/3.4]? Mean abundance of element [SmII/H] relative to solar 509-512 F4.2 [Sun] e_<[SmII/H]> [0.01/1.7]? Standard Deviation of <[SmII/H]> 514-515 I2 --- o_<[SmII/H]> [1/35]? Number of lines used in <[SmII/H]> 517-521 F5.2 [Sun] <[EuI/H]> [-2.3/2.1]? Mean abundance of element [EuI/H] relative to solar 523 F1.0 [Sun] e_<[EuI/H]> ? Standard Deviation of <[EuI/H]> 525 I1 --- o_<[EuI/H]> [1/1]? Number of lines used in <[EuI/H]> 527-531 F5.2 [Sun] <[EuII/H]> [-1.6/3.22]? Mean abundance of element [EuII/H] relative to solar 533-536 F4.2 [Sun] e_<[EuII/H]> [0/1.11]? Standard Deviation of <[EuII/H]> 538 I1 --- o_<[EuII/H]> [1/4]? Number of lines used in <[EuII/H]>
Global Notes: Note (G1): Source for spectroscopic material is defined as follows: E = ELODIE Archive (Observatoire de Haute Provence, Moultaka et al. 2004PASP..116..693M); H = High-Resolution Spectrograph, Hobby-Eberly Telescope (HET); S = Sandiford Echelle, McDonald Observatory 2.1m Telescope.
History: From electronic version of the journal References: Luck et al., Paper I 2015AJ....150...88L, Cat. J/AJ/150/88
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 16-Jun-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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