Table 6: Carbon and oxygen abundances and micro-turbulent velocities (with probable errors(PEs) in 23 red giant stars.

Star		 NHa $N_{H}^{\rm wk}$ NKb $ N_{K}^{\rm wk}$ log $A_{\rm C}$ $\xi_{\rm micro}$ NHc $N_{H}^{\rm wk}$ NLd $N_{L}^{\rm wk}$ log $A_{\rm O}$ $\xi_{\rm micro}$ log $A_{\rm N}^{f} $
             km s-1              km s-1  

$\alpha $ Tau		 13 13 25 9 8.38 $\pm$ 0.04 2.20$\pm$ 0.09 ... ... 28 25 8.79 $\pm$ 0.04 3.85 $\pm$ 0.13 8.05
              23 21 ... ... 8.76 $\pm$ 0.09 3.81 $\pm$ 0.94  
$\delta $ Oph 5 5 21 6 8.27 $\pm$ 0.08 2.46$\pm$ 0.16 42 27 ... ... 8.83 $\pm$ 0.14 2.84 $\pm$ 0.54 8.58
$\nu $ Vir 6 6 22 10 8.13 $\pm$ 0.08 2.14$\pm$ 0.15 55 20 ... ... 8.84 $\pm$ 0.05 2.67 $\pm$ 0.24 8.11
$\alpha $ Cet 6 6 11 3 8.64 $\pm$ 0.05 1.95$\pm$ 0.08 38 18 ... ... 8.98 $\pm$ 0.14 4.25 $\pm$ 1.03 7.73
$\sigma $ Lib 12 12 14 2 8.23 $\pm$ 0.03 2.09$\pm$ 0.13 51 19 ... ... 8.82 $\pm$ 0.10 2.03 $\pm$ 0.20 8.15
$\lambda $ Aqr 5 5 13 4 8.56 $\pm$ 0.11 1.97 $\pm$ 0.15 30 7 ... ... 8.92 $\pm$ 0.15 6.24 $\pm$ 6.01 7.88
$\beta $ Peg 12 12 29 7 8.27 $\pm$ 0.05 2.04 $\pm$ 0.07 53 16 ... ... 8.77 $\pm$ 0.12 3.12 $\pm$ 0.72 8.11
$\tau ^4$ Eri 6 5 20 1 8.41 $\pm$ 0.04 3.57 $\pm$ 0.46 25 9 ... ... 8.87 $\pm$ 0.19 3.38 $\pm$ 1.32 7.94
$\mu $ Gem 19 19 34 9 8.32 $\pm$ 0.06 2.00 $\pm$ 0.11 36 16 ... ... 8.81 $\pm$ 0.13 2.58 $\pm$ 0.33 ...
$\delta $ Vir 16 16 19 4 8.50 $\pm$ 0.06 2.20 $\pm$ 0.11 36 11 ... ... 8.84 $\pm$ 0.15 2.47 $\pm$ 0.45 7.90
10 Dra 5 5 15 3 8.43 $\pm$ 0.14 2.69 $\pm$ 0.26 30 15 ... ... 8.92 $\pm$ 0.18 2.44 $\pm$ 0.41 8.11
$\rho $ Per 13 13 22 2 8.27 $\pm$ 0.07 3.59 $\pm$ 0.64 43 7 ... ... 8.87 $\pm$ 0.07 3.11 $\pm$ 0.98 8.15
BS6861 5 4 12 2 8.38 $\pm$ 0.13 4.91 $\pm$ 1.29 ... ... ... ... ... ... ...
$\delta ^{2}$ Lyr 5 5 13 1 8.22 $\pm$ 0.18 2.86 $\pm$ 0.40 19   3 e ... ... ... ... 8.41
RR UMi 15 15 15 4 8.26 $\pm$ 0.12 2.48 $\pm$ 0.23 34 5 ... ... 8.76 $\pm$ 1.05 2.66 $\pm$ 2.60 8.07
$\alpha $ Her 11 10 17 3 8.40 $\pm$ 0.13 2.82 $\pm$ 0.23 22 0 42 16 8.85 $\pm$ 0.05 2.92 $\pm$ 0.09 8.14
OP Her ... ... 21 4 8.27 $\pm$ 0.60 2.53 $\pm$ 0.72 ... ... ... ... ... ... ...
XY Lyr ... ... 14 4 8.15 $\pm$ 0.15 2.96 $\pm$ 0.24 ... ... ... ... ... ... ...
R Lyr 14 14 17 2 8.26 $\pm$ 0.08 2.95 $\pm$ 0.24 ... ... 52 31 8.61 $\pm$ 0.04 2.99 $\pm$ 0.10 8.06
              25 4 ... ... 8.62 $\pm$ 0.05 6.53 $\pm$ 3.20  
RZ Ari 12 12 26 7 8.10 $\pm$ 0.09 2.54 $\pm$ 0.15 ... ... 28 15 8.57 $\pm$ 0.14 3.35 $\pm$ 0.28 8.44
              52 21 ... ... 8.67 $\pm$ 0.07 3.49 $\pm$ 0.50  
30g Her 6 5 24 3 8.35 $\pm$ 0.11 2.61 $\pm$ 0.26 23 0 38 26 8.75 $\pm$ 0.09 2.49 $\pm$ 0.16 7.92
SW Vir 11 6 15 1 8.26 $\pm$ 0.20 4.21 $\pm$ 2.38 ... ... 29 16 8.54 $\pm$ 0.11 1.83 $\pm$ 0.71 8.46
RX Boo 6 2 13 1 8.32 $\pm$ 1.62 3.41 $\pm$ 2.38 ... ... 13 12 8.55 $\pm$ 0.10 2.04 $\pm$ 0.18 8.26
a The number of CO lines measured in the H band region, of which the number of weak lines (log  ${W/\nu} \la -4.75$) is given in the next column; b the same as a but in the K band region; c the same as a but for OH lines in the H band region; d the same as a but for OH lines in the L band region; e with only 3 weak lines of similar intensities, the micro-turbulent velocity cannot be fixed by our line-by-line analysis; f N abundances based on CN (Aoki & Tsuji 1997) corrected for the effect of the revised C abundances.


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