All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.0cm]{0639fig1.eps} \end{figure}$ Figure 1: The chromium image of theta Aur based on the same dataset as was used for plate 2 of Hatzes (1991a). This was generously provided by Hatzes to allow for more convenient comparison of the chromium and the oxygen image of this paper. The phases have been adjusted so that the images are displayed here on the basis of the ephemeris used in this paper and these images can be compared directly with Fig. 2. Note that the dark areas represent weaker chromium local equivalent width and the light regions represent stronger local line strength.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{0639fig2.ps} \end{figure}$ Figure 2: Eight phases of the abundance map of the oxygen distribution over the surface of $\theta$ Aur. The upper left image is phase 0.0 with successive phases at intervals of 0.125.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[angle=-90,width=8.8cm]{0639fg3a.ps} \includegraphics[angle=-90,width=8.8cm]{0639fg3b.ps} } \end{figure}$ Figure 3: Two Mercator style projections of the oxygen map of $\theta$ Aur, each based on half of the line profiles. The figure on the left is made from every other line profile listed in Table 1 beginning with the first (the odd profiles) and the figure on the right is made from every other line profile observation listed in Table 1 starting with the second profile (the even profile set). The two images represent images formed from two completely separate data sets. These alternative projections are provided for convenience in locating features by latitude and longitude and also to provide visual evidence of the errors that can be expected in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=14cm]{0639fg4a.ps} \includegraphics[angle=-90,width=14cm]{0639fg4b.ps} \end{figure}$ Figure 4: Fit of predicted O I $\lambda$ 7775 line profiles based on the Doppler image to the observed line profiles at half of the observed phases. Only every other spectrum and its fit is shown to allow for more detail in the display of the individual spectra. The spikes in the data at phases 212 and 215 have been removed from the Doppler Image reconstruction by having a weighting of zero applied to those data points.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0639fig5.eps} \end{figure}$ Figure 5: Eight phases of the abundance map of the oxygen distribution over the surface of $\epsilon$ UMa from Rice et al. (1997). This old image is included here for convenience in making the comparison with the $\theta$ Aur map. You will note here that for $\epsilon$ UMa there is just one clear belt of normal oxygen abundance at roughly the magnetic equator of the star and that oxygen is depleted by many orders of magnitude at the magnetic poles.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{0639fig2.ps} \end{figure}$	Figure 2: Eight phases of the abundance map of the oxygen distribution over the surface of $\theta$ Aur. The upper left image is phase 0.0 with successive phases at intervals of 0.125.
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