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J/PASJ/59/335   Properties of 160 F-K disk dwarfs/subgiants      (Takeda+, 2007)

Fundamental parameters and elemental abundances of 160 F-G-K stars based on OAO spectrum database. Takeda Y. <Publ. Astron. Soc. Jap., 59, 335-356 (2007)> =2007PASJ...59..335T
ADC_Keywords: Stars, late-type ; Stars, dwarfs ; Abundances ; Equivalent widths ; Stars, masses ; Stars, ages Keywords: stars: abundances - stars: atmospheres - stars: fundamental parameters - stars: late-type Abstract: The properties of 160 F, G, and K disk dwarfs/subgiants (including 27 planet-host stars) mostly within -0.6≲[Fe/H]≲+0.4, the Okayama Astrophysical Observatory spectrum collection of which had been made open to the public recently, were extensively investigated with particular attention to determining (1) the mass and the age with the help of theoretical stellar evolution calculations, (2) the kinematic parameters of orbital motions in the Galaxy, and (3) the abundances of 15 elements (Na, Mg, Al, Si, S, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Cu, and Zn) by analyzing the spectra in this database. The resulting characteristics are discussed in terms of several relevant topics of interest, such as a validity check for assuming LTE, the [X/Fe] vs. [Fe/H] diagram containing information on the chemical evolution of the Galactic disk, the age-metallicity-kinematics relation, and the difference/similarity between stars with and without planets. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 87 160 Fundamental stellar parameters of program stars kinepara.dat 109 160 Kinematic parameters of program stars (tablee1) starpara.dat 105 160 Fundamental stellar parameters of 160 stars (tablee2) xhtable.dat 141 160 [X/H] (relative-to-Sun abundance for 19 species) (from tablee3) mgsabund.dat 61 161 Profile-fit abundance for Mg and S and computed equivalence widhts (from tablee3) lgf.dat 35 365 *Wavelength and the loggf data of each hyper-fine splitting (hfs) component (from tablee4) dif.dat 74 2824 Results of abundance corrections caused by inclusion of the hyper-fine splitting (hfs) effect for the relevant line (from tablee4) xhcor.dat 66 569 Corrections on the final (line-averaged) results of [ScII/H], [VI/H], [MnI/H] and [CoI/H] caused by inclusion of the hyper-fine splitting effect for each of the relevant lines (from tablee4) mabund.dat 45 2552 Average abundances (from tablee3) cmb/* 79 160 Individual abundances (from tablee3)
Note on lgf.dat: all of which were exclusively taken from the database of R.L. Kurucz available at http://kurucz.harvard.edu/LINELISTS/GFHYPERALL/
See also: J/PASJ/57/13 : High-dispersion spectra of nearby F-K stars (Takeda+, 2005) J/PASJ/57/27 : Atmospheric parameters of nearby F-K stars (Takeda+, 2005) J/PASJ/57/45 : Lithium abundances of F-K stars (Takeda+, 2005) J/PASJ/57/65 : CNO abundances of solar-type stars (Takeda+, 2005) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 6 I06 --- HD HD number of the star 8- 11 I4 --- HR ? HR number of the star 13- 18 I6 --- HIP ? HIP number of the star 20- 30 A11 --- Name Star name 32- 39 A8 --- SpType MK spectral type 41- 44 I4 K Teff Effective temperature (1) 46- 49 F4.2 [cm/s2] logg Surface gravity (1) 51- 54 F4.2 km/s vt Microturbulent velocity (1) 56- 60 F5.2 [Sun] [Fe/H] Metallicity (1) 62- 66 F5.2 [solLum] logL Stellar luminosity derived as -0.4(Mbol-4.75) 68- 71 F4.2 solMass Mass Mass (2) 73- 77 F5.2 [yr] logAge Age (2) 79 A1 --- q_logAge [ABC] Quality flag showing the reliability of age (see Sect. 2.1 for more details) (3) 81- 85 F5.1 km/s V(LSR) Space speed relative to the LSR (G1) 87 A1 --- n_HD [P] 'P' when star harbors planet(s)
Note (1): Determined from FeI and FeII lines taken from table 1 of Paper II. Note (2): Mass and age derived by comparing the (logTeff, logL) position on the HR diagram with Girardi et al.'s (2000, Cat. J/A+AS/141/371) theoretical evolutionary tracks Note (3): Quality flag as follows: A = high B = moderate C = poor
Byte-by-byte Description of file: kinepara.dat
Bytes Format Units Label Explanations
1 A1 --- n_HD [P] 'P' when star harbors planet(s) 3- 8 I06 --- HD HD number 10- 11 I2 h RAh Right ascension (J2000, Ep=1991.25, HIP) 13- 14 I2 min RAm Right ascension (J2000, Ep=1991.25, HIP) 16- 20 F5.2 s RAs Right ascension (J2000, Ep=1991.25, HIP) 22 A1 --- DE- Declination sign (J2000, Ep=1991.25, HIP 23- 24 I2 deg DEd Declination (J2000, Ep=1991.25, HIP) 26- 27 I2 arcmin DEm Declination (J2000, Ep=1991.25, HIP) 29- 32 F4.1 arcsec DEs Declination (J2000, Ep=1991.25, HIP) 34- 39 F6.2 mas plx Parallax (1) 41- 48 F8.2 mas/yr pmRA Proper motion in alpha direction (1) 50- 57 F8.2 mas/yr pmDE Proper motion in delta direction (1) 59- 64 F6.1 km/s HRV Heliocentric radial velocity (from table 2 of Paper I, Cat. J/PASJ/57/13) 66- 71 F6.3 kpc Rm Mean galactocentric distance 73- 77 F5.3 kpc zm Maximum separation from the galactic plane 79- 83 F5.3 --- e Galactocentric orbital eccentricity 85- 90 F6.1 km/s Ulsr Space velocity in radial direction relative to LSR 92- 97 F6.1 km/s Vlsr Space velocity in tangential direction relative to LSR 99-103 F5.1 km/s Wlsr Space velocity in vertical direction relative to LSR 105-109 F5.1 km/s V(LSR) speed relative to LSR (G1)
Note (1): From HIP catalog
Byte-by-byte Description of file: starpara.dat
Bytes Format Units Label Explanations
1 A1 --- n_HD [P] 'P' when star harbors planet(s) 3- 8 I06 --- HD HD number 10- 15 F6.1 K Teff2 Effective temperature (1) 17- 21 F5.3 [cm/s+2] logg2 logarithmic surface gravity (1) 23- 26 F4.2 km/s vt2 microturbulent velocity (1) 28- 33 F6.3 [Sun] [Fe/H]2 Fe abundance relative to the Sun (1) 35- 38 F4.2 mag VMAG2 Absolute visual magnitude (2) 40- 44 F5.2 mag BC2 Bolometric correction (2) 46- 49 F4.2 mag Mbol2 Bolometric magnitude (2) 51- 56 F6.3 [solLum] logL2 logarithmic luminosity 58- 61 F4.2 solMass M(trk) Stellar mass derived from evolutionary track (3) 63- 66 F4.2 solMass E_M(trk) Possible error in M(trk) on the upper side 68- 71 F4.2 solMass e_M(trk) Possible error in M(trk) on the lower side 73- 76 F4.2 solMass M(iso) Stellar mass derived from isochrones 78- 81 F4.2 [cm/s+2] logg(TLM) Theorerical logg derived from Teff, L, and M(trk) 83- 87 F5.2 [yr] logAge(trk) log(stellar age) derived from evolutionary track (3) 89- 92 F4.2 [yr] E_logAge(trk) Possible error in logAge(trk) on the upper side 94- 97 F4.2 [yr] e_logAge(trk) Possible error in logAge(trk) on the lower side 99 A1 --- q_logAge(trk) Reliability of age(trk) (4) 101-105 F5.2 [yr] logAge(iso) log(stellar age) derived from isochrones
Note (1): Teff, log g, vt, and [Fe/H]) spectroscopically established in Paper II, Cat. J/PASJ/57/27 Note (2): From table1 of paper II, Cat. J/PASJ/57/27 Note (3): Age and mass revisited in this paper by comparing the positions on the HR diagram with theoretically evolutionary tracks/isochrones. Note (4): Quality flag as follows: A = high B = moderate C = poor
Byte-by-byte Description of file: xhtable.dat
Bytes Format Units Label Explanations
1- 6 I06 --- HD HD number 8- 11 I4 K Teff Effective temperature 13- 16 F4.2 [cm/s2] logg logarithmic surface gravity 18- 21 F4.2 km/s vt Microturbulent velocity 23- 27 F5.2 [Sun] [Fe/H] Fe abundance relative to the Sun 29- 33 F5.2 [Sun] [Na/H] Na abundance relative to the Sun 35- 39 F5.2 [Sun] [Mg/H] Mg abundance relative to the Sun (MgI 8806 fit) 41- 45 F5.2 [Sun] [Al/H] ?=99.99 Al abundance relative to the Sun 47- 51 F5.2 [Sun] [Si/H] Si abundance relative to the Sun 53- 57 F5.2 [Sun] [S/H] ?=99.99 S abundance relative to the Sun (SI 8684 fit) 59- 63 F5.2 [Sun] [Ca/H] Ca abundance relative to the Sun 65- 69 F5.2 [Sun] [ScI/H] ?=99.99 Sc abundance relative to the Sun (from ScI) 71- 75 F5.2 [Sun] [ScII/H] Sc abundance relative to the Sun (from ScII) 77- 81 F5.2 [Sun] [TiI/H] Ti abundance relative to the Sun (from TiI) 83- 87 F5.2 [Sun] [TiII/H] Ti abundance relative to the Sun (from TiII) 89- 93 F5.2 [Sun] [VI/H] ?=99.99 V abundance relative to the Sun (from VI) 95- 99 F5.2 [Sun] [VII/H] ?=99.99 V abundance relative to the Sun (from VII) 101-105 F5.2 [Sun] [CrI/H] Cr abundance relative to the Sun (from CrI) 107-111 F5.2 [Sun] [CrII/H] Cr abundance relative to the Sun (from CrII) 113-117 F5.2 [Sun] [Mn/H] ?=99.99 Mn abundance relative to the Sun 119-123 F5.2 [Sun] [Co/H] Co abundance relative to the Sun 125-129 F5.2 [Sun] [Ni/H] Ni abundance relative to the Sun 131-135 F5.2 [Sun] [Cu/H] ?=99.99 Cu abundance relative to the Sun 137-141 F5.2 [Sun] [Zn/H] ?=99.99 Zn abundance relative to the Sun
Byte-by-byte Description of file: mgsabund.dat
Bytes Format Units Label Explanations
1- 6 I06 --- HD HD number (999999 for the Sun) 8- 11 I4 K Teff Effective temperature 13- 16 F4.2 [cm/s2] logg logarithmic surface gravity 18- 21 F4.2 km/s vt Microturbulent velocity 23- 27 F5.2 [Sun] [Fe/H] Fe abundance relative to the Sun 29- 32 F4.2 --- A(Mg) Mg abundance from 8806 fit (normalisation of H=12.00) 34- 38 F5.1 0.1pm EW(Mg) EW(MgI 8806.8) inversely computed from A(Mg) 40- 43 F4.2 --- A(S) S abundance from 8693-5 fit (normalisation of H=12.00) 45- 49 F5.1 0.1pm EW(S1) ?=-99.9 EW(SI 8693.1) inversely computed from A(S) 51- 55 F5.1 0.1pm EW(S2) ?=-99.9 EW(SI 8693.9) inversely computed from A(S) 57- 61 F5.1 0.1pm EW(S3) ?=-99.9 EW(SI 8694.6) inversely computed from A(S)
Byte-by-byte Description of file: lgf.dat
Bytes Format Units Label Explanations
1- 4 I4 0.1nm lambda Line wavelength 6- 7 I2 --- o_Ion Number of hyperfine components 9- 13 F5.2 --- Ion Ion code (G2) (1) 15- 22 F8.3 0.1nm lam.hf Wavelength of the hyperfine components 24- 28 F5.3 eV chi ? lower excitation potential 30- 35 F6.3 --- loggf log of (statistical weight times oscillator strength)
Note (1): 21.01, 23.00, 25.00, 27.00 for ScII, VI, MnI, CoI respectively
Byte-by-byte Description of file: dif.dat
Bytes Format Units Label Explanations
1- 5 F5.2 --- Ion Ion code (G2) (1) 7- 10 I4 0.1nm lambda Line wavelength 12- 17 I06 --- HD HD number (0 for Sun) 20- 25 F6.1 K Teff Effective temperature 28- 32 F5.3 [m/s2] logg Logarithmic surface gravity 35- 38 F4.2 km/s vt Microturbulent velocity 40- 45 F6.3 --- [Fe/H] Fe abundance relative to the Sun 48- 52 F5.1 0.1pm EW Equivalent width of the line 54- 59 F6.3 --- A(hfs) Abundance obtained with hyperfine splitting 61- 66 F6.3 --- A(nohf) Abundance obtained without hyperfine splitting 69- 74 F6.3 --- delta hfs correction defined as A(hfs)-A(nohf)
Note (1): 21.01, 23.00, 25.00, 27.00 for ScII, VI, MnI, CoI respectively
Byte-by-byte Description of file: xhcor.dat
Bytes Format Units Label Explanations
1- 6 I06 --- HD HD number 9- 14 F6.1 K Teff Effective temperature 17- 21 F5.3 [cm/s2] logg logarithmic surface gravity 24- 27 F4.2 km/s vt Microturbulent velocity 29- 34 F6.3 [Sun] [Fe/H] Fe abundance relative to the Sun 37- 41 F5.2 --- Ion Ion code (G2) (1) 45- 50 F6.3 --- [X/H](hfs) final [X/H] value obtained with hfs 52- 57 F6.3 --- [X/H](nohf) final [X/H] value obtained without hfs 61- 66 F6.3 --- delta hfs correction ([X/H](hfs)-[X/H](nohf))
Note (1): 21.01, 23.00, 25.00, 27.00 for ScII, VI, MnI, CoI respectively
Byte-by-byte Description of file: mabund.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [HD] 4- 9 I06 --- HD HD number 12- 13 I2 --- Nline Number of lines for the species 15- 16 I2 --- o_<delA> Number of lines actually adopted for computing the averaged abundances 18- 22 F5.2 --- Ion Ion code (G2) 24- 28 F5.2 --- <delA> Average differential abundance (star-Sun) 30- 33 F4.2 --- e_<delA> rms uncertainty on <delA> 35- 45 A11 --- FileName Name of the file with individual measurements in subdirectory cmb
Byte-by-byte Description of file: cmb/*
Bytes Format Units Label Explanations
2- 6 F5.2 --- Ion Ion code (G2) 7- 15 F9.3 0.1nm lambda Wavelength 18- 22 F5.3 eV chi Lower excitation potential 24- 29 F6.3 --- loggf log(gf) value 32- 36 F5.1 0.1pm EW(star) Equivalent width of the star 39- 42 F4.2 km/s vt(star) Adopted microturbulence of the star 45- 49 F5.3 --- A(star) Abundance of the ion in the star 53- 56 F4.1 0.1pm EW(Sun) Solar flux equivalent width 59- 62 F4.2 km/s vt(Sun) Adopted microturbulence of the Sun 65- 69 F5.3 --- A(Sun) Abundance of the ion in the Sun 73- 77 F5.2 --- delA Differential abundance (star-Sun) 79 A1 --- Note [x] x for rejection of inadequate data according to Chauvenet's criterion
Global notes: Note (G1): V(LSR)= sqrt(U(LSR)2+V(LSR)2+W(LSR)2)] Note (G2): Species code used in the WIDTH9 program (e.g., 11.00 for NaI, 22.01 for Ti II) 21.01, 23.00, 25.00, 27.00 for ScII, VI, MnI, CoI, respectively.
History: From electronic version of the journal References: Takeda et al., Paper I 2005PASJ...57...13T, Cat. J/PASJ/57/13 Takeda et al., Paper II 2005PASJ...57...27T, Cat. J/PASJ/57/27 Takeda et al., Paper III 2005PASJ...57...45T, Cat. J/PASJ/57/45 Takeda et al., Paper IV 2005PASJ...57...65T, Cat. J/PASJ/57/65
(End) Patricia Vannier [CDS] 20-May-2008
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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