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J/PASJ/57/27  Atmospheric parameters of nearby F-K stars   (Takeda+, 2005)

Spectroscopic study on the atmospheric parameters of nearby F-K dwarfs and subgiants. Takeda Y., Ohkubo M., Sato B., Kambe E., Sadakane K. <Publ. Astron. Soc. Jap., 57, 27-43 (2005)> =2005PASJ...57...27T
ADC_Keywords: Stars, nearby ; Stars, late-type ; Stars, atmospheres ; Abundances ; Effective temperatures Keywords: stars: abundances - stars: atmospheres - stars: late-type Abstract: Based on a collection of high-dispersion spectra obtained at Okayama Astrophysical Observatory, the atmospheric parameters (Teff, logg, vt, and [Fe/H]) of 160 mid-F through early-K stars were extensively determined by the spectroscopic method using the equivalent widths of Fe I and Fe II lines along with the numerical technique of Takeda et al. (2002PASJ...54..451T). The results are comprehensively discussed and compared with the parameter values derived by different approaches (e.g., photometric colors, theoretical evolutionary tracks, Hipparcos parallaxes, etc.) as well as with the published values found in various literature. It has been confirmed that our purely spectroscopic approach yields fairly reliable and consistent results. Description: tablee1.dat: Based on the equivalent widths measured on the solar flux spectrum of Kurucz et al. (1984, Solar FLux Atlas from 296 to 1300nm (Sunspot, New Mexico: National Solar Observatory) for the Fe I and Fe II lines in Meylan et al.'s (1993ApJS...85..163M) list (with additional two lines Fe I 5855.091 and 6297.792 included by us), we derived the solar gf values while using Kurucz's (1993, CD-ROM 13) ATLAS9 solar atmospheric model (Teff=5777K, log g=4.437, [X]=0.0) with the assumption of A(Fe)=7.50 and vt=1.0 km/s. Such established solar gf values are presented with corresponding E.W. data. For comparison purposes, the gf values of Kurucz and Bell (1995, CD-ROM 23) and those of Grevesse and Sauval (1999, Cat. J/A+A/347/348) (if available) are also given. If the solar gf value could not be determined because the line EW was not measured, a dummy value of 99.999 is given with EW=0.0. Note that the data in the first five columns (line, code, lambdaK, chi, and loggfTGV) are the data actually used by the TGVIT program in the present calculation. tablee2.dat: tablee2.dat contains the input data of measured equivalent widths and the abundance results of the Fe I and Fe II lines corresponding to the finally converged solutions of the atmospheric parameters. tablee2a.dat contains the header part of tablee2, which includes the information concerning the final parameter solutions derived by the TGVIT program. The Fe abundances are repeatedly listed twice in columns 7 and 8 with different signs for neutral and ionized species, such as [+A(FeI),-A(FeII)] in column 7 and [-A(FeI),+A(FeII)] in column 8, in order for the convenience of plotting the FeI and FeII data with different symbols. tablee3.dat: The convergence performance of the final solutions is represented by dt, dg, and dv, which are the averaged absolute changes of Teff, logg, and vt solutions (mostly oscillatory) over the last 4 iterations. Regarding the final Fe abundances derived from Fe I and Fe II lines (A1 and A2), A1=A2(=A)is practically accomplished in all cases, from which [Fe/H] is derived as [Fe/H]=A-7.50. The statistical errors involved with the finally adopted solutions in Teff, logg, vt, A1, and A2 were estimated by the procedure described in subsection 5.2 and are given here as errt, errg, errv, erra1, and erra2, respectively. Note, however, that this procedure does not necessarily work well in all cases. (Sometimes zero values are yielded, which does not mean that the solution is error-free, of course.) File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 108 161 Basic data and the parameter solutions of the program stars + the Sun (999999). tablee1.dat 76 330 Solar gf values and EW of FeI/II lines tablee2a.dat 77 161 Initial values of tablee2.dat calculations tablee2.dat 65 27551 EW data and the Fe abundances for the 160 program stars + Sun (999999) etab2/* 0 161 Original files of tableE2 tablee3.dat 106 161 Parameter solutions, errors, convergence performance
See also: J/PASJ/57/45 : Lithium abundances of F-K stars (Takeda+, 2005) J/PASJ/57/65 : CNO abundances of solar-type stars (Takeda+, 2005) J/PASJ/57/109 : Late-G giants abundances (Takeda+, 2005) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1 A1 --- n_HD [*] Individual note (1) 2- 7 I06 --- HD HD number 9- 21 A13 --- Name Name 23- 32 A10 --- SpType MK spectral type 34- 37 F4.2 mag Vmag ? V magnitude 39- 42 I4 K Teff Effective temperature 44- 47 F4.2 [cm/s2] logg log of surface gravity 49- 52 F4.2 km/s vt Microturbulent velocity 54- 58 F5.2 Sun [Fe/H] Metallicity 60- 64 F5.1 mas plx ? Trigonometric Hipparcos parallax 66- 69 F4.2 mag VMAG ? Absolute V magnitude 71- 75 F5.2 mag BC ? Bolometric correction 77- 81 F5.2 [solLum] logL ? log of stellar luminosity 83- 86 F4.2 solMass Mass ? Stellar mass 88- 91 F4.2 [cm/s2] loggTLM ? log of surface gravity from Teff, logL and M 93-106 A14 --- Rem Remarks (2)
Note (1): *: Only the region R spectra were used for this star HD 99491 (i.e., unlike others,region G data were not used) Note (2): T(29), g(0.05) and v(0.1) mean <|δTeff|≥29K, <|δlogg|≥0.05 and <|δvt|≥0.1km/s
Byte-by-byte Description of file: tablee1.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Line Line number used in the TGVIT program 6- 10 F5.2 --- Elem Species code (26.00: Fe I, 26.01: Fe II) 12- 19 F8.3 0.1nm lambdaK Adopted wavelength [from Kurucz and Bell (1995)] 21- 25 F5.3 eV Chi lower excitation potential (=chi_G, otherwise from Kurucz & Bell) 27- 32 F6.3 --- loggfTGV loggf value adopted in the TGVIT program 34 A1 --- n_loggfTGV [SG] source for loggf_TGV (S-->loggfS, G-->loggfG) 36- 41 F6.3 --- loggfK log gf value from Kuruz and Bell (1995) 43- 47 F5.1 0.1pm EWS Equivalent width measured on the solar flux atlas 49- 54 F6.3 --- loggfS ?=99.99 solar gf value determined by us from EWS 56- 61 F6.3 --- loggfG ? log gf value from Grevesse and Sauval (1999, Cat. J/A+A/347/348) 63- 70 F8.3 0.1nm lambdaG ? Wavelength from Grevesse and Sauval (1999, Cat. J/A+A/347/348) 72- 76 F5.3 eV ChiG ? Lower excitation potential from Grevesse and Sauval (1999, Cat. J/A+A/347/348)
Byte-by-byte Description of file: tablee2a.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [HD] 4- 9 I06 --- HD HD number (G1) (1) 11- 16 F6.3 --- xcur xcur parameter 18- 23 F6.1 K Teff(f) Effective temperature 25- 29 F5.3 [cm/s2] logg(f) log of surface gravity 31- 34 F4.2 km/s vt(f) Microturbulent velocity 36- 46 E11.6 --- func func parameter 48- 52 F5.3 --- A1 Initial abundance in Fe I 54- 58 F5.3 --- sig1 Standard deviation of Fe I abundances around A1 60- 64 F5.3 --- A2 Initial abundance in Fe II 66- 70 F5.3 --- sig2 Standard deviation of Fe II abundances around A2 72- 74 I3 --- n1 Number of used Fe I lines 76- 77 I2 --- n2 Number of used Fe II lines
Note (1): Initial values identical for all: met: xxx c1: 1.00000 c2: 1.00000 c3: 0.00000 ftol= E-04
Byte-by-byte Description of file: tablee2.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [HD] 4- 9 I06 --- HD HD number (G1) 11- 14 I4 --- Line line number 15- 20 F6.2 --- Elem FeI: 26.00 FeII: 26.01 21- 29 F9.3 0.1nm lambda wavelength 30- 36 F7.3 eV Chi lower excitation potential 37- 43 F7.3 --- loggf adopted log(gf) value 44- 49 F6.1 0.1pm EW equivalent width 50- 57 F8.3 --- abund1 Fe abundance (sign inversed for Fe II lines) [+A(FeI),-A(FeII)] 58- 65 F8.3 --- abund2 Fe abundance (sign inversed for Fe I lines) [-A(FeI),+A(FeII)]
Byte-by-byte Description of file: tablee3.dat
Bytes Format Units Label Explanations
1- 6 I06 --- HD HD number of the object (G1) 8- 11 F4.1 K DTeff Effective temperature variation (abs. value) averaged over last 4 iterations 13- 17 F5.3 cm/s2 Dlogg Surface gravity variation(abs. value) averaged over last 4 iterations 19- 22 F4.2 km/s Dvt Microturbulent velocity variation (abs. value) averaged over last 4 iterations 24- 29 F6.1 K Teff finally converged (adopted) solution of effective temperature 31- 35 F5.3 cm/s logg finally converged (adopted) solution of surface gravity 37- 40 F4.2 km/s vt finally converged (adopted) solution of microturbulent velocity 42- 47 F6.3 --- [Fe/H] finally converged (adopted) solution of [Fe/H] (=A-7.50) 49- 51 I3 --- n1 Number of used Fe I lines 53- 57 F5.3 --- A1 Averaged Fe abundance derived from Fe I lines 59- 63 F5.3 --- sig1 Standard deviation of Fe I abundances around A1 65- 66 I2 --- n2 Number of used Fe II lines 68- 72 F5.3 --- A2 Averaged Fe abundance derived from Fe II lines 74- 78 F5.3 --- sig2 Standard deviation of Fe II abundances around A2 80- 83 F4.1 K e_Teff Estimated error in Teff 85- 89 F5.3 cm/s e_logg Estimated error in logg 91- 94 F4.2 km/s e_vt Estimated error in vt 96-100 F5.3 --- e_A1 Estimated error in A1 102-106 F5.3 --- e_A2 Estimated error in A2
Global notes: Note (G1): 999999 is the Sun(moon)
History: From PASJ editor, Maho Kuroiwa, maho(at)pasj.asj.or.jp * 27-May-2005: HD number corrected from 733640 into 133640 in tables E2 and E3.
(End) Patricia Vannier [CDS] 06-Apr-2005
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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