All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9869fg01.eps} \end{figure}$ Figure 1: Program stars shown by filled circles on the HR diagram and recent evolutionary tracks (Claret 2004) shown by grey lines. Stellar masses (in unit of solar mass $M_{\odot }$ ) are indicated on some evolutionary tracks.
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg02.eps} \end{figure}$ Figure 2: Some of our model photospheres (solid lines) are compared with those by Plez et al. (1992) (dots). $M/M_{\odot }$ , $T_{\rm eff}$ , log g, and $R/R_{\odot }$ are as follows. A: 1.0/2750/-0.50/295, B: 1.0/3200/0.00/166, and C: 2.0/3600/0.50/132.
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg03.eps} \end{figure}$ Figure 3: a) Logarithmic abundance corrections for the lines of the CO first overtone bands of $\alpha$ Her plotted against the observed log $W/\nu$ values for assumed values of $\xi _{\rm micro} = 3.0$ , 3.5, and 4.0 km s^-1. The analysis outlined in Sect. 3 is applied to the lines of log $W/\nu < -4.5$ (filled circles) with our model b/2.0/150/3200. b) Confirmation of the null logarithmic abundance corrections for log $A_{\rm C} = 8.08$ and $\xi _{\rm micro} = 3.81$ km s^-1, which are the solution of the line-by-line analysis of $\alpha$ Her in a).
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg04.eps} \end{figure}$ Figure 4: a) Logarithmic abundance corrections for the lines of the CO first and second overtone bands observed in $\alpha$ Her plotted against the observed ${\rm log} W/\nu$ values for assumed values of $\xi _{\rm micro} = 2.4$ , 3.0, and 3.6 km s^-1. The CO lines of the first and second overtone bands are shown by circles and triangles, respectively (model photosphere: b/2.0/150/3300). b) Confirmation of the null logarithmic abundance corrections for log $A_{\rm C} = 8.40$ and $\xi _{\rm micro} = 2.82$ km s^-1, which are the solution of the line-by-line analysis of the weak lines (filled symbols) in a).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{9869fg06.eps} \end{figure}$ Figure 6: a) Logarithmic abundance corrections for the lines of the CO first and second overtone bands observed in $\beta$ Peg plotted against the observed ${\rm log} W/\nu$ values for assumed values of $\xi _{\rm micro} = 1.6$ , 2.0, and 2.4 km s^-1 (model: a/2.0/100/3600). b) Confirmation of the null logarithmic abundance corrections for log $A_{\rm C} = 8.27$ and $\xi _{\rm micro} = 2.04$ km s^-1, which are the solution of the line-by-line analysis of the weak lines (filled symbols) in a).
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg08.eps} \end{figure}$ Figure 8: a) Logarithmic abundance corrections for the lines of the CO first and second overtone bands observed in $\rho$ Per plotted against the observed ${\rm log}~W/\nu$ values for assumed values of $\xi _{\rm micro} = 3.0$ , 3.5, and 4.0 km s^-1 (model: b/2.0/100/3500). b) Confirmation of the null logarithmic abundance corrections for log $A_{\rm C} = 8.27$ and $\xi _{\rm micro} = 3.59$ km s^-1, which are the solution of the line-by-line analysis of the weak lines (filled symbols) in a).
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg10.eps} \end{figure}$ Figure 10: a) Logarithmic abundance corrections for the lines of OH fundamental bands observed in $\alpha$ Her plotted against the observed ${\rm log}~W/\nu$ values for assumed values of $\xi _{\rm micro} = 2.0$ , 3.0, and 4.0 km s^-1 (model: b/2.0/150/3300). b) Confirmation of the null logarithmic abundance corrections for log $A_{\rm O} = 8.85$ and $\xi _{\rm micro} = 2.92$ km s^-1, which are the solution of the line-by-line analysis of the weak lines (filled circles) in a).
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg12.eps} \end{figure}$ Figure 12: Lower excitation potentials (LEPs) of the lines plotted against ${\rm log}~W/\nu$ values. a) CO first overtone bands observed in $\alpha$ Her. b) OH fundamental bands observed in $\alpha$ Her.
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg13.eps} \end{figure}$ Figure 13: a) Logarithmic abundance corrections for the lines of the OH first overtone bands observed in $\rho$ Per plotted against the observed ${\rm log}~W/\nu$ values for assumed values of $\xi _{\rm micro} = 2.0$ , 3.0, and 4.0 km s^-1 (model: b/2.0/100/3500). b) Confirmation of the null logarithmic abundance corrections for log $A_{\rm O} = 8.87$ and $\xi _{\rm micro} = 3.11$ km s^-1, which are the solution of the line-by-line analysis of the weak lines (filled circles) in a).
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In the text

$\begin{figure} \par\includegraphics[width=13.5cm]{9869fg15.eps} \end{figure}$ Figure 15: The ordinate scale shows abundances of ¹²C¹⁶O (first and second overtones by filled circles and triangles, respectively), ¹³C¹⁶O (open squares), and ¹²C¹⁷O (open diamonds) derived from the observed values of log $W/\nu$ in the abscissa. a) 10 Dra. Note that there are three lines of ¹³C¹⁶O and ¹²C¹⁷O, of which two are overlapping in the plot. b) RZ Ari. c) $\delta$ Oph. d) $\mu$ Gem.
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In the text

$\begin{figure} \par\includegraphics[width=16.0cm,clip]{9869fg16.eps} \end{figure}$ Figure 16: Observed spectra are shown by dots. Some ¹²C¹⁶O and ¹²C¹⁷O features are indicated by open and filled triangles, respectively. Synthetic spectra with assumed ¹⁶O/¹⁷O ratios are shown by heavy solid lines while those with null ¹⁷O value by light solid lines. a) Observed spectrum of 10 Dra compared with the synthetic one with ¹⁶O/¹⁷O = 151. b) Observed spectrum of RZ Ari compared with the synthetic one with ¹⁶O/¹⁷O = 607. c) Observed spectrum of $\lambda$ Aqr compared with the synthetic one with ¹⁶O/¹⁷O = 1000. d) Observed spectrum of RR UMi compared with the synthetic one with ¹⁶O/¹⁷O = 2000.
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In the text

$\begin{figure} \par\includegraphics[width=16.0cm,clip]{9869fg17.eps} \end{figure}$ Figure 17: Observed abundances of a) carbon (Table 6), b) nitrogen (Aoki & Tsuji 1997; Table 6), c) oxygen (Table 6; if the results derived from the H and L band spectra are available, mean values are used), and d) C + N + O, compared with the predictions of evolutionary models (Claret 2004). The results of FDU and SDU for the case of Z = 0.02 are shown by solid and dash-dotted lines, respectively, in each panel. The observed C + N + O abundances are smaller by about 0.16 dex compared with the predictions based on Z = 0.02 as can be seen in panel d). This initial metallicity correction of -0.16 dex is applied to the predicted C, N, and O abundances in panels a), b), and c), respectively, and the corrected results are shown by dashed lines. In each panel, the solar abundances are shown by open square (Anders & Grevesse 1989; Ayres et al. 2006) and by open diamond (Allende Prieto et al. 2002).
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg18.eps} \end{figure}$ Figure 18: a) The observed ¹⁶O/¹⁷O ratios are plotted against stellar mass by filled circles and by the filled triangles if only lower limits can be estimated. Predicted ¹⁶O/¹⁷O ratios by FDU and SDU are shown by solid and dash-dotted lines, respectively. b) the observed ¹²C/¹³C ratios are plotted by filled circles against stellar mass. Dashed curve is the predicted ¹²C/¹³C ratios by the ``Compulsory Deep Mixing (CDM: Eggleton et al. 2008)''.
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg05.eps} \end{figure}$ Figure 5: a) Confirmation of the null logarithmic abundance corrections for log $A_{\rm C} = 8.22$ and $\xi _{\rm micro} = 2.86$ km s^-1, resulting from the line-by-line analysis of the weak lines of CO in $\delta ^{2}$ Lyr (model: b/2.0/150/3400). b) The same as a) but for log $A_{\rm C} = 8.35$ and $\xi _{\rm micro} = 2.61$ km s^-1 in 30g Her (model: b/2.0/150/3300). c) The same as a) but for log $A_{\rm C} = 8.32$ and $\xi _{\rm micro} = 3.41$ km s^-1 in RX Boo (model: b/2.0/250/2900).
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg07.eps} \end{figure}$ Figure 7: a) Confirmation of the null logarithmic abundance corrections for log $A_{\rm C} = 8.38$ and $\xi _{\rm micro} = 2.20$ km s^-1, resulting from the line-by-line analysis of the weak lines of CO in $\alpha$ Tau (model: a/2.0/50/3900). b) The same as a) but for log $A_{\rm C} = 8.13$ and $\xi _{\rm micro} = 2.14$ km s^-1 in $\nu$ Vir (model: a/2.0/75/3800). c) the same as a) but for log $A_{\rm C} = 8.64$ and $\xi _{\rm micro} = 1.95$ km s^-1 in $\alpha$ Cet (model: a/2.0/50/3900).
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg09.eps} \end{figure}$ Figure 9: a) Confirmation of the null logarithmic abundance corrections for log $A_{\rm C} = 8.41$ and $\xi _{\rm micro} = 3.57$ km s^-1, resulting from the line-by-line analysis of the weak lines of CO in $\tau ^4$ Eri (model: a/2.0/75/3700). b) The same as a) but for log $A_{\rm C} = 8.26$ and $\xi _{\rm micro} = 2.95$ km s^-1 in R Lyr (model: b/2.0/150/3300). c) The same as a) but for log $A_{\rm C} = 8.26$ and $\xi _{\rm micro} = 4.21$ km s^-1 in SW Vir (model: b/2.0/250/2900).
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg11.eps} \end{figure}$ Figure 11: a) Confirmation of the null logarithmic abundance corrections for log $A_{\rm O} = 8.79$ and $\xi _{\rm micro} = 3.85$ km s^-1, resulting from the line-by-line analysis of the weak lines of OH in $\alpha$ Tau (model: a/2.0/50/3900). b) The same as a) but for log $A_{\rm O} = 8.61$ and $\xi _{\rm micro} = 2.99$ km s^-1 in R Lyr (model: b/2.0/150/3300). c) The same as a) but for log $A_{\rm O} = 8.54$ and $\xi _{\rm micro} = 1.83$ km s^-1 in SW Vir (model: b/2.0/250/2900).
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg14.eps} \end{figure}$ Figure 14: a) Confirmation of the null logarithmic abundance corrections for log $A_{\rm O} = 8.76$ and $\xi _{\rm micro} = 3.81$ km s^-1, resulting from the line-by-line analysis of the weak lines of OH in $\alpha$ Tau (model: a/2.0/50/3900). b) The same as a) but for log $A_{\rm O} = 8.82$ and $\xi _{\rm micro} = 2.03$ km s^-1 in $\sigma$ Lib (model: a/2.0/100/3600). c) the same as a) but for log $A_{\rm O} = 8.62$ and $\xi _{\rm micro} = 6.53$ km^-1 in R Lyr (model: b/2.0/150/3300).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9869fg01.eps} \end{figure}$	Figure 1: Program stars shown by filled circles on the HR diagram and recent evolutionary tracks (Claret 2004) shown by grey lines. Stellar masses (in unit of solar mass $M_{\odot }$ ) are indicated on some evolutionary tracks.
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$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg02.eps} \end{figure}$	Figure 2: Some of our model photospheres (solid lines) are compared with those by Plez et al. (1992) (dots). $M/M_{\odot }$ , $T_{\rm eff}$ , log g, and $R/R_{\odot }$ are as follows. A: 1.0/2750/-0.50/295, B: 1.0/3200/0.00/166, and C: 2.0/3600/0.50/132.
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$\begin{figure} \par\includegraphics[width=8.0cm,clip]{9869fg12.eps} \end{figure}$	Figure 12: Lower excitation potentials (LEPs) of the lines plotted against ${\rm log}~W/\nu$ values. a) CO first overtone bands observed in $\alpha$ Her. b) OH fundamental bands observed in $\alpha$ Her.
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