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 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:
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FileName Lrecl Records Explanations
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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/* . 160 Individual abundances (from tablee3)
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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/
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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
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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)
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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
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Byte-by-byte Description of file: kinepara.dat
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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)
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Note (1): From HIP catalog
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Byte-by-byte Description of file: starpara.dat
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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
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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
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Byte-by-byte Description of file: xhtable.dat
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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
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Byte-by-byte Description of file: mgsabund.dat
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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)
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Byte-by-byte Description of file: lgf.dat
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Bytes Format Units Label Explanations
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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)
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Note (1): 21.01, 23.00, 25.00, 27.00 for ScII, VI, MnI, CoI respectively
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Byte-by-byte Description of file: dif.dat
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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)
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Note (1): 21.01, 23.00, 25.00, 27.00 for ScII, VI, MnI, CoI respectively
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Byte-by-byte Description of file: xhcor.dat
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Bytes Format Units Label Explanations
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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))
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Note (1): 21.01, 23.00, 25.00, 27.00 for ScII, VI, MnI, CoI respectively
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Byte-by-byte Description of file: mabund.dat
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Bytes Format Units Label Explanations
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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
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Byte-by-byte Description of file: cmb/*
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Bytes Format Units Label Explanations
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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
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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.
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History:
From electronic version of the journal
References:
Takeda et al., Paper I 2005PASJ...57...13T 2005PASJ...57...13T, Cat. J/PASJ/57/13
Takeda et al., Paper II 2005PASJ...57...27T 2005PASJ...57...27T, Cat. J/PASJ/57/27
Takeda et al., Paper III 2005PASJ...57...45T 2005PASJ...57...45T, Cat. J/PASJ/57/45
Takeda et al., Paper IV 2005PASJ...57...65T 2005PASJ...57...65T, Cat. J/PASJ/57/65
(End) Patricia Vannier [CDS] 20-May-2008