All Figures

$\begin{figure} \par\includegraphics[angle=270,width=8.7cm,clip]{4909fig1.eps}\end{figure}$ Figure 1: Examples of normalized spectra in the region of the K I lines. The spectra were shifted vertically by 1.0 units in relative flux. The K I line at 7664.92 Å is blended with the very strong telluric O₂ lines in some cases.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4909fig2.eps}\end{figure}$ Figure 2: Typical example of collision-dominated K I population departure coefficients $b_n = N_n^{\rm NLTE}/N_n^{\rm LTE}$ in the moderately metal-poor star HD 58551. The kinetic equilibrium calculations are described in the text.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{4909fig3.eps}\end{figure}$ Figure 3: Synthetic flux profiles under LTE (dotted line) and NLTE (solid line) conditions compared with the observed spectra (filled circles) of HD 58551.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4909fig4.eps}\end{figure}$ Figure 4: Dependences of NLTE corrections for our sample stars on a) effective temperature, b) gravity and c) metal abundance.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{4909fig5.eps}\end{figure}$ Figure 5: Abundance ratios [K/Fe] for NLTE analysis. Open circles refer to the thin-disk stars, filled circles to the thick-disk stars, asterisks to the halo stars, open triangle to the stars with uncertain population membership. The solid line shows the theoretical predictions of Goswami & Prantzos (2000), the dashed line is the one of Samland (1998), and the dotted line refers to Timmes et al. (1995).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4909fig6.eps}\end{figure}$ Figure 6: [K/Mg] abundances ratios from NLTE analyses as functions of [Fe/H], [Mg/H], and [Mg/Fe]. Symbols are the same as in Fig. 5.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.7cm,clip]{4909fig1.eps}\end{figure}$	Figure 1: Examples of normalized spectra in the region of the K I lines. The spectra were shifted vertically by 1.0 units in relative flux. The K I line at 7664.92 Å is blended with the very strong telluric O₂ lines in some cases.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4909fig2.eps}\end{figure}$	Figure 2: Typical example of collision-dominated K I population departure coefficients $b_n = N_n^{\rm NLTE}/N_n^{\rm LTE}$ in the moderately metal-poor star HD 58551. The kinetic equilibrium calculations are described in the text.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{4909fig3.eps}\end{figure}$	Figure 3: Synthetic flux profiles under LTE (dotted line) and NLTE (solid line) conditions compared with the observed spectra (filled circles) of HD 58551.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4909fig4.eps}\end{figure}$	Figure 4: Dependences of NLTE corrections for our sample stars on a) effective temperature, b) gravity and c) metal abundance.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4909fig6.eps}\end{figure}$	Figure 6: [K/Mg] abundances ratios from NLTE analyses as functions of [Fe/H], [Mg/H], and [Mg/Fe]. Symbols are the same as in Fig. 5.
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