All Figures

$\begin{figure} \par\includegraphics[width=6.65cm,clip]{5647fig1.eps} \end{figure}$ Figure 1: Distribution of the $T_{{\rm eff}}$ , ${\rm [Fe/H]}$ , and $\log g$ values found in the literature for the star BD +17 4708, as given in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=12.4cm,clip]{5647fig2.eps} \end{figure}$ Figure 2: Upper panel: the spectral energy distribution measured by Bohlin & Gilliland (2004b) is shown with the filled circles. Alpha-element enhanced ([ $\alpha$ /Fe] = +0.4) no-overshoot [no] Kurucz's models of ${\rm [Fe/H]}=-1.74$ , $\log g=3.87$ , reddened by E(B-V)=0.01 according to the Fitzpatrick (1999) parameterization, and two effective temperatures: $T_{{\rm eff}}=6141$ K and 5950 K, are shown with the solid and dot-dashed lines, respectively. An overshoot [ov] Kurucz model of $T_{{\rm eff}}=6222$ K is shown with the dotted line ( $\log g$ and ${\rm [Fe/H]}$ for this model are slightly different to make them consistent with the higher $T_{{\rm eff}}$ ). Lower panel: as in the upper panel for the difference (percentile) between observed and theoretical fluxes. The hydrogen lines have been excluded.
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In the text

$\begin{figure} \par\includegraphics[width=12.75cm,clip]{5647fig3.eps} \end{figure}$ Figure 3: The observed spectral region around the Na D lines for BD +17 4708, uncorrected for the radial velocity of the star, is shown with the histogram (these observational data are described in Sect. 3.1). The dotted line is the model for telluric water vapor, open circles correspond to the model fit to the stellar lines (see Sect. 3.5), and the thick solid line is the model fit to the interstellar Na D lines (including blends with telluric lines).
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In the text

$\begin{figure} \par\includegraphics[width=6.95cm,clip]{5647fig4.eps} \end{figure}$ Figure 4: Top panel: mean $T_{{\rm eff}}$ obtained from the $T_{{\rm eff}}$ -color calibrations by Ramírez & Meléndez (2005b) as a function of E(B-V) using all colors (14, open circles), and blue-visible colors only (7, filled circles). Bottom panel: as in the top panel for the standard error $\sigma _N=\sigma T_{{\rm eff}}/\sqrt {N}$ , where $\sigma$ is the standard deviation and N the number of colors used.
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In the text

$\begin{figure} \par\includegraphics[width=7.05cm,clip]{5647fig5.eps} \end{figure}$ Figure 5: Upper panel: mean value of the ratio of observed ( $f_{\rm obs}$ ) to scaled theoretical ( $f_{\rm kur}$ ) fluxes (see Fig. 2) as a function of $T_{{\rm eff}}$ . Bottom panel: the quality of the fit, as given by $\chi '=\sqrt {\chi ^2/(n-1)}$ where $\chi ^2=\sum _{i=1}^n[(f_{\rm obs}-f_{\rm kur})_i^2/\sigma _i^2]$ , as a function of $T_{{\rm eff}}$ ( $\sigma$ is the error in $f_{\rm obs}$ only).
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In the text

$\begin{figure} \par\includegraphics[width=7.05cm,clip]{5647fig6.eps} \end{figure}$ Figure 6: Top panel: the observed H $\alpha$ profile (points) is shown along with model line profiles of $T_{{\rm eff}}=5950,6050,6150,6250,6350,6450$ K (solid lines). The bars on top show the regions excluded from the $\chi ^2$ calculation. Bottom panel: quality of the fits in the top panel, as measured by $\chi '=\sqrt {\chi ^2/(n-1)}$ where $\chi ^2=\sum _{i=1}^n[(f_{\rm obs}-f_{\rm kur})_i^2/\sigma _i^2]$ ( $\sigma$ is the error in $f_{\rm obs}$ only), as a function of $T_{{\rm eff}}$ (filled circles). The solid line is a cubic fit to the filled circles.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{5647fig7.eps} \end{figure}$ Figure 7: Top panel: the region around the strong Mg I b triplet as given by the observations (open circles), and as predicted by models of $T_{{\rm eff}}=6141$ K, ${\rm [Fe/H]}=-1.74$ , $A_{\rm Mg}=6.19$ , and three different values of the surface gravity ( $\log g=3.5,3.87,4.5$ ). Residuals of the fit are also shown. Bottom panel: zoom into the 5183.6 Å line.
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In the text

$\begin{figure} \par\includegraphics[width=12.2cm,clip]{5647fig8.eps} \end{figure}$ Figure 8: Abundance of iron from Fe I (open circles) and Fe II lines (filled circles), as determined using different combinations of $T_{{\rm eff}}$ , $\log g$ , and v_t; as a function of excitation potential and reduced equivalent width. The solid lines are linear fits to the Fe I data only.
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{5647fig9.eps} \end{figure}$ Figure 9: Mean abundance of iron from Fe I (open symbols) and Fe II (filled symbols) lines as a function of $T_{{\rm eff}}$ and $\log g$ . Here ${\rm [Fe/H]}={A}_{\rm Fe}-7.51$ , i.e., we used $A_{\rm Fe}=7.51$ for the Sun.
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In the text

$\begin{figure} \par\includegraphics[width=7.95cm,clip]{5647fig10.eps} \end{figure}$ Figure 10: Locus of the $T_{{\rm eff}}$ and $\log g$ values for which ionization equilibrium of Fe lines is satisfied. The circle with the error bars correspond to our best estimates of $T_{{\rm eff}}$ from the flux distribution and $\log g$ from the fit of the Mg I b lines.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5647fig11.eps} \end{figure}$ Figure 11: Observed profile of the O I triplet in BD +17 4708 (filled circles). Non-LTE model fits to the data (solid lines) are shown for $S_{\rm H}=0,1$ , and 10. LTE fits are also shown. The abundances adopted in each case, given in each panel, have been chosen to fit the reddest line of the triplet. Residuals, shifted by +0.80, are show at the bottom of each panel.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{5647figA1.eps} \end{figure}$ Figure A.1: Top panel: abundance of iron as a function of excitation potential for two different effective temperatures as inferred using the Fulbright (2000) line list. Open circles: Fe I lines, filled circles: Fe II lines. The solid lines are linear fits to the Fe I data only. Bottom panel: slope of the $A_{\rm Fe}$ vs. EP trend as a function of $T_{{\rm eff}}$ using the Fulbright (2000) line list (squares and solid line) and our line list (triangles and dotted line). One-sigma ( $1\sigma$ ) errors for the slopes are also shown.

In the text

$\begin{figure} \par\includegraphics[width=6.65cm,clip]{5647fig1.eps} \end{figure}$	Figure 1: Distribution of the $T_{{\rm eff}}$ , ${\rm [Fe/H]}$ , and $\log g$ values found in the literature for the star BD +17 4708, as given in Table 1.
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$\begin{figure} \par\includegraphics[width=12.5cm,clip]{5647fig7.eps} \end{figure}$	Figure 7: Top panel: the region around the strong Mg I b triplet as given by the observations (open circles), and as predicted by models of $T_{{\rm eff}}=6141$ K, ${\rm [Fe/H]}=-1.74$ , $A_{\rm Mg}=6.19$ , and three different values of the surface gravity ( $\log g=3.5,3.87,4.5$ ). Residuals of the fit are also shown. Bottom panel: zoom into the 5183.6 Å line.
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$\begin{figure} \par\includegraphics[width=12.2cm,clip]{5647fig8.eps} \end{figure}$	Figure 8: Abundance of iron from Fe I (open circles) and Fe II lines (filled circles), as determined using different combinations of $T_{{\rm eff}}$ , $\log g$ , and v_t; as a function of excitation potential and reduced equivalent width. The solid lines are linear fits to the Fe I data only.
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$\begin{figure} \par\includegraphics[width=6.4cm,clip]{5647fig9.eps} \end{figure}$	Figure 9: Mean abundance of iron from Fe I (open symbols) and Fe II (filled symbols) lines as a function of $T_{{\rm eff}}$ and $\log g$ . Here ${\rm [Fe/H]}={A}_{\rm Fe}-7.51$ , i.e., we used $A_{\rm Fe}=7.51$ for the Sun.
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$\begin{figure} \par\includegraphics[width=7.95cm,clip]{5647fig10.eps} \end{figure}$	Figure 10: Locus of the $T_{{\rm eff}}$ and $\log g$ values for which ionization equilibrium of Fe lines is satisfied. The circle with the error bars correspond to our best estimates of $T_{{\rm eff}}$ from the flux distribution and $\log g$ from the fit of the Mg I b lines.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{5647fig11.eps} \end{figure}$	Figure 11: Observed profile of the O I triplet in BD +17 4708 (filled circles). Non-LTE model fits to the data (solid lines) are shown for $S_{\rm H}=0,1$ , and 10. LTE fits are also shown. The abundances adopted in each case, given in each panel, have been chosen to fit the reddest line of the triplet. Residuals, shifted by +0.80, are show at the bottom of each panel.
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