All Figures

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{8847f1.eps}\end{figure}$ Figure 1: Upper panel: radial velocities of CS 22876-032 (filled circles: A; open circles: B). Open diamonds: data from Norris et al. (2000). The curves show the orbital solution (P = 425 d, e = 0.14) for Star A (solid) and B (dashed). Dot-dashed horizontal line: centre-of-mass velocity of the system. Lower panel: residuals from the fit.
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In the text

$\begin{figure} \par\includegraphics[clip=true,width=8cm]{8847f2.eps}\end{figure}$ Figure 2: Average temperature profile of 3D $\ensuremath {{\rm CO}^5{\rm BOLD}}$ atmospheric models (solid lines) compared to 1D $_{\rm LHD}$ (dashed) and 1D MARCS models (dotted) in stars A ( bottom panel) and B ( top).
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In the text

$\begin{figure} \par\includegraphics[clip=true,width=8cm]{8847f3.eps}\end{figure}$ Figure 3: The two components of CS 22876-032 on a 14-Gyr isochrone by Chieffi & Limongi (priv. comm.) for Z=10^-6 (solid line). For comparison, isochrones for 14 Gyr and Z=10^-5 (dashed) and 12 Gyr and Z=10^-6 (dotted) are also shown.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8847f4a.eps}\par\vspace*{2mm} \includegraphics[width=8cm,clip]{8847f4b.eps}\end{figure}$ Figure 4: Distribution of effective temperatures for CS 22876-032 A and B obtained by Monte Carlo simulations, comparing the observed colours with those from the isochrone in Fig. 3 for the observed mass ratio. The lowest contour encloses 95.4% of the 10 000 simulations.
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In the text

$\begin{figure} \par\includegraphics[clip=true,width=7cm]{8847f5a.eps}\par\vspace*{2mm} \includegraphics[clip=true,width=8cm]{8847f5b.eps}\end{figure}$ Figure 5: Same as Fig. 4, for the surface gravities.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.4cm,clip]{8847f6.eps}\end{figure}$ Figure 6: Computed H $_\alpha$ profiles for three sets of effective temperatures, 6300+5900, 6500+5900 and 6700+5900, and normalised to the level of the observed UVES spectrum at 645.0 nm.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{8847f7.eps}\end{figure}$ Figure 7: Synthetic spectral fits to the Li line in the co-added UVES spectrum of star A ( top) and B ( bottom). The observed spectra have been corrected for veiling (see Table 5), so the lines appear with their intrinsic strength in each star.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{8847f8.eps} \end{figure}$ Figure 8: Synthetic spectral fits to OH lines in the co-added UVES spectrum of star A ( top) and B ( bottom) in CS 22876-032. The observed spectra have been corrected for veiling factors of 1.30 (A) and 4.36 (B).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{8847f9.eps} \end{figure}$ Figure 9: Same as Fig. 8 for another OH line.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{8847f10.eps} \end{figure}$ Figure 10: Synthetic spectral fits to OH lines in the co-added UVES spectrum of star B. The observed spectra have been corrected for a veiling factor of 4.36.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8847f11.eps}\end{figure}$ Figure 11: Entropy profiles of the $\langle$ 3D $\rangle$ CO⁵BOLD model atmospheres (solid lines), compared to 1D $_{\rm LHD}$ models (dashed) for stars B (5900 K) and A (6500 K). The labelled contours indicate the specific heat at constant pressure in units of 10⁸ erg g^-1 K^-1 (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8847f12.eps}\end{figure}$ Figure 12: 1D-NLTE Li abundances vs. [Fe/H] for the stars in CS 22876-032 (circles) and in other metal-poor dwarfs as reported by Asplund et al. (2006, triangles) and Bonifacio et al. (2007, diamonds). The Li abundances by Asplund et al. (2006) were recomputed using TURBOSPECTRUM as reported by Bonifacio et al. (2007). No 3D-LTE or 3D-NLTE was considered.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8847f13.eps}\end{figure}$ Figure 13: Same as Fig. 12, but in the Li- $T_{\rm eff}\;$ plane.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8847f14.eps}\end{figure}$ Figure 14: 3D [O/Fe] ratios of the stars in CS 22876-032 (circles) and in the metal-poor giants of Paper V. Triangles: ``unmixed'', diamonds ``mixed'' stars; downward triangle with arrow: upper limit for CS 22172-002.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm,clip]{8847f1.eps}\end{figure}$	Figure 1: Upper panel: radial velocities of CS 22876-032 (filled circles: A; open circles: B). Open diamonds: data from Norris et al. (2000). The curves show the orbital solution (P = 425 d, e = 0.14) for Star A (solid) and B (dashed). Dot-dashed horizontal line: centre-of-mass velocity of the system. Lower panel: residuals from the fit.
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$\begin{figure} \par\includegraphics[clip=true,width=8cm]{8847f2.eps}\end{figure}$	Figure 2: Average temperature profile of 3D $\ensuremath {{\rm CO}^5{\rm BOLD}}$ atmospheric models (solid lines) compared to 1D $_{\rm LHD}$ (dashed) and 1D MARCS models (dotted) in stars A ( bottom panel) and B ( top).
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$\begin{figure} \par\includegraphics[clip=true,width=8cm]{8847f3.eps}\end{figure}$	Figure 3: The two components of CS 22876-032 on a 14-Gyr isochrone by Chieffi & Limongi (priv. comm.) for Z=10^-6 (solid line). For comparison, isochrones for 14 Gyr and Z=10^-5 (dashed) and 12 Gyr and Z=10^-6 (dotted) are also shown.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{8847f4a.eps}\par\vspace*{2mm} \includegraphics[width=8cm,clip]{8847f4b.eps}\end{figure}$	Figure 4: Distribution of effective temperatures for CS 22876-032 A and B obtained by Monte Carlo simulations, comparing the observed colours with those from the isochrone in Fig. 3 for the observed mass ratio. The lowest contour encloses 95.4% of the 10 000 simulations.
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$\begin{figure} \par\includegraphics[clip=true,width=7cm]{8847f5a.eps}\par\vspace*{2mm} \includegraphics[clip=true,width=8cm]{8847f5b.eps}\end{figure}$	Figure 5: Same as Fig. 4, for the surface gravities.
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$\begin{figure} \par\includegraphics[angle=90,width=8.4cm,clip]{8847f6.eps}\end{figure}$	Figure 6: Computed H $_\alpha$ profiles for three sets of effective temperatures, 6300+5900, 6500+5900 and 6700+5900, and normalised to the level of the observed UVES spectrum at 645.0 nm.
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$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{8847f7.eps}\end{figure}$	Figure 7: Synthetic spectral fits to the Li line in the co-added UVES spectrum of star A ( top) and B ( bottom). The observed spectra have been corrected for veiling (see Table 5), so the lines appear with their intrinsic strength in each star.
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$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{8847f8.eps} \end{figure}$	Figure 8: Synthetic spectral fits to OH lines in the co-added UVES spectrum of star A ( top) and B ( bottom) in CS 22876-032. The observed spectra have been corrected for veiling factors of 1.30 (A) and 4.36 (B).
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$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{8847f9.eps} \end{figure}$	Figure 9: Same as Fig. 8 for another OH line.
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$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{8847f10.eps} \end{figure}$	Figure 10: Synthetic spectral fits to OH lines in the co-added UVES spectrum of star B. The observed spectra have been corrected for a veiling factor of 4.36.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8847f11.eps}\end{figure}$	Figure 11: Entropy profiles of the $\langle$ 3D $\rangle$ CO⁵BOLD model atmospheres (solid lines), compared to 1D $_{\rm LHD}$ models (dashed) for stars B (5900 K) and A (6500 K). The labelled contours indicate the specific heat at constant pressure in units of 10⁸ erg g^-1 K^-1 (see text).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8847f12.eps}\end{figure}$	Figure 12: 1D-NLTE Li abundances vs. [Fe/H] for the stars in CS 22876-032 (circles) and in other metal-poor dwarfs as reported by Asplund et al. (2006, triangles) and Bonifacio et al. (2007, diamonds). The Li abundances by Asplund et al. (2006) were recomputed using TURBOSPECTRUM as reported by Bonifacio et al. (2007). No 3D-LTE or 3D-NLTE was considered.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8847f13.eps}\end{figure}$	Figure 13: Same as Fig. 12, but in the Li- $T_{\rm eff}\;$ plane.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8847f14.eps}\end{figure}$	Figure 14: 3D [O/Fe] ratios of the stars in CS 22876-032 (circles) and in the metal-poor giants of Paper V. Triangles: ``unmixed'', diamonds ``mixed'' stars; downward triangle with arrow: upper limit for CS 22172-002.
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