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Table 6

Input parameters for the marcs code from Decin et al. (2003a) unless indicated otherwise.

α Boo ι Aur β UMi γ Dra α Tau

Sp. Type K2 IIIp K3 II K4 III K5 III K5 III
T eff 4320 ± 140 4160 ± 1301 4085 ± 140 3960 ± 140 3850 ± 140
log g 1.5 ± 0.15 1.74 ± 0.361 1.6 ± 0.02 1.30 ± 0.25 1.50 ± 0.15
ξ t 1.7 ± 0.5 3.00 ± 0.51 2 ± 0.5 2.0 ± 0.5 1.7 ± 0.5
[Fe/H] −0.50 ± 0.20 −0.11 ± 0.221 −0.15 ± 0.2 0.00 ± 0.20 −0.15 ± 0.20
ϵ(C) 7.96 ± 0.20 8.35 8.25 ± 0.2 8.15 ± 0.25 8.35 ± 0.20
ϵ(N) 7.61 ± 0.25 8.35 8.16 ± 0.25 8.26 ± 0.25 8.35 ± 0.25
ϵ(O) 8.68 ± 0.20 8.93 8.83 ± 0.2 8.93 ± 0.20 8.93 ± 0.20
12C/13C 7 ± 2 10 9 ± 2 10 ± 2 10 ± 2
θ d 20.74 ± 0.10 7.05 ± 0.03 10.15 ± 0.42 9.94 ± 0.05 20.89 ± 0.10
distance 11.26 ± 0.09 166.56 ± 33.315 39.87 ± 7.975 45.25 ± 0.94 19.96 ± 0.38
M g 0.73 ± 0.27 3.6 2.49 ± 0.92 1.72 ± 1.02 2.30 ± 0.85
A v 0.01 ± 0.15 0.00 ± 0.15 0.00 ± 0.5 0.03 ± 0.15 0.03 ± 0.15
K –3.076 –0.6866 -1.457 –1.3706 –2.9406

β And α Cet β Peg σ Lib

Sp. Type M0 III M2 III M2.5 III M3/M4 III
T eff 3880 ± 140 3740 ± 140 3600 ± 300 3634 ± 1102
log g 0.95 ± 0.25 0.95 ± 0.25 0.65 ± 0.40 0.9 ± 0.31 2
ξ t 2.0 ± 0.5 2.3 ± 0.5 2.0 ± 0.3 3.1 ± 0.53
[Fe/H] 0.00 ± 0.30 0.00 ± 0.30 0.00 0.00
ϵ(C) 8.12 ± 0.30 8.20 ± 0.30 8.20 ± 0.40 8.23 ± 0.043
ϵ(N) 8.37 ± 0.40 8.26 ± 0.40 8.18 ± 0.40 8.15 ± 0.054
ϵ(O) 9.08 ± 0.30 8.93 ± 0.30 8.93 ± 0.40 8.93
12C/13C 9 ± 2 10 ± 2 5 ± 3 10
θ d 13.03 ± 0.06 12.34 ± 0.06 16.43 ± 0.24 11.00 ± 0.05
distance 61.12 ± 2.84 67.48 ± 3.78 61.08 ± 2.69 90.80 ± 18.165
M g 2.49 ± 1.48 2.69 ± 1.61 1.5
A v 0.06 ± 0.15 0.06 ± 0.16 0.03 ± 0.15 0.20 ± 0.17
K –1.9306 –1.7606 –2.3306 –1.4716

Notes. The parameters are the effective temperature Teff in K, the gravity log g in cm/s2, the microturbulent velocity ξt in km s-1, the metallicity [Fe/H], the abundances of carbon, nitrogen, and oxygen, the 12C/13C-ratio and the photospheric stellar angular diameter θd in milliarcseconds. The calculation of the angular diameter is discussed in Sect. 4. The table also contains the distances (in pc) and the values of the interstellar extinction Av as derived from the model of Arenou et al. (1992) and the K-band magnitude used for the absolute calibration of the SEDs. Values, for which no literature values have been found, have been assumed on the basis of analogue objects, and are listed in italics.

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