All Figures

$\begin{figure} \includegraphics[angle=-90,width=13cm,clip]{5242F1.eps} \end{figure}$ Figure 1: New high-precision photometry of PW And in 2004. a) Periodogram from the combined V and y data. The x-axis is in units of cycles per day. b) V (pluses) and y (dots) photometry. The x-axis is in fractional days from JD 2 453 000. c) Phased light and color curves with the ephemeris in Eq. (1). Note that the b-y curve is differential with respect to HD 1440. The spectroscopic observations were obtained during the interval 2 453 243-50.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{5242F2.eps} \end{figure}$ Figure 2: A lithium spectrum of PW And at R=120 000 ( top). The Li I 670.8 nm line is the strong line in the center. Its equivalent width is 278 mÅ corrected for the contribution from an inactive star $\epsilon$ Eri (middle spectrum) or 70 Oph A (not shown). As a comparison, a R=600 000 spectrum of the Sun is shown at the bottom (Kurucz et al. 1984). Notice the line-core asymmetries in PW And. All spectra are on the same intensity scale but $\epsilon$ Eri and the Sun are shifted for plotting purposes.
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In the text

$\begin{figure} \par\includegraphics[origin=rb,angle=0,width=10.6cm,clip]{5242F3.eps} \end{figure}$ Figure 3: Averaged Doppler image of PW And for August 26-31, 2004 (JD 2 453 243-249). Maps are plotted in a spherical projection at eight equidistant rotational phases. The temperature scale is indicated and is the same for all projections. The image is an average from seven spectral regions, see text. Note that the photospheric temperature is $\approx$ 5000 K.
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In the text

$\begin{figure} \par\includegraphics[origin=rb,angle=0,width=10.6cm,clip]{5242F4.eps} \end{figure}$ Figure 4: Doppler image of PW And from the full-spectrum approach. Otherwise as in Fig. 3.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=0,width=8cm]{5242F5a.eps}\hspace{5mm} \includegraphics[angle=0,width=8cm]{5242F5b.eps} }\end{figure}$ Figure 5: Example line-profile fits. Shown is only the (simultaneous) inversion of the Fe I 642.1 and Fe I 641.9 line pair for all 27 phases. Phase is indicated in degrees (0-360 $^\circ$ ) on the right side of the individual graphs. Crosses are the data, the lines are the fits. The points between the two lines where the fit is poor were given zero weight in order not to influence the solution.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{5242F6.eps} \end{figure}$ Figure 6: Latitudinally averaged surface temperatures. Shown is the average temperature per 5-degree latitude bin between the surface visibility limit at $-44\hbox {$^\circ $ }$ and close to the visible pole for the individual spectral lines images (the thick line is the average from the combined image). The surface pixels around the geometric pole between 85-90 $^\circ$ are not plotted. The main spot activity seems to occur at a latitude of below $\approx$ +40 $^\circ$ while the warm features seem to reside at a latitude of $\approx$ +60 $^\circ$ , especially well seen in the Ca I 643.9-nm line.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=8cm,clip]{5242F7.eps} \end{figure}$ Figure 7: The expected latitude distribution of emerging flux tubes for PW And. Shown is as a radial cross section with the trajectories of the summit of rising flux loops (lines; left panel). Its surfacing probability as a function of latitude between zero and 90 $^\circ$ is shown in the right panel (a larger width means a higher surfacing probability). Most magnetic flux would be expected to surface at a latitude of +45-55 $^\circ$ .
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=0,width=8cm]{5242AF1a.eps}\hspace{5mm} \includegraphics[angle=0,width=8cm]{5242AF1b.eps} }\end{figure}$ Figure A.1: Fe I 639.3-nm line profile data and fits for all 27 phases. Phase is indicated in degrees (0-360 $^\circ$ ) on the right side of the individual graphs. Crosses are the data, the lines are the fits.

In the text

$\begin{figure} \par\mbox{\includegraphics[angle=0,width=8cm]{5242AF2a.eps}\hspace{5mm} \includegraphics[angle=0,width=8cm]{5242AF2b.eps} }\end{figure}$ Figure A.2: Fe I 640.8-nm line profile data and fits for all 27 phases. Phase is indicated in degrees (0-360 $^\circ$ ) on the right side of the individual graphs. Crosses are the data, the lines are the fits.

In the text

$\begin{figure} \mbox{\includegraphics[angle=0,width=8cm]{5242AF3a.eps}\hspace{5mm} \includegraphics[angle=0,width=8cm]{5242AF3b.eps} }\end{figure}$ Figure A.3: Fe I 641.1-nm line profile data and fits for all 27 phases. Phase is indicated in degrees (0-360 $^\circ$ ) on the right side of the individual graphs. Crosses are the data, the lines are the fits.

In the text

$\begin{figure} \mbox{\includegraphics[angle=0,width=8cm]{5242AF4a.eps}\hspace{5mm} \includegraphics[angle=0,width=8cm]{5242AF4b.eps} }\end{figure}$ Figure A.4: Fe I 643.0-nm line profile data and fits for all 27 phases. Phase is indicated in degrees (0-360 $^\circ$ ) on the right side of the individual graphs. Crosses are the data, the lines are the fits.

In the text

$\begin{figure} \mbox{\includegraphics[angle=0,width=8cm]{5242AF5a.eps}\hspace{5mm} \includegraphics[angle=0,width=8cm]{5242AF5b.eps} }\end{figure}$ Figure A.5: Ca I 643.9-nm line profile data and fits for all 27 phases. Phase is indicated in degrees (0-360 $^\circ$ ) on the right side of the individual graphs. Crosses are the data, the lines are the fits.

In the text

$\begin{figure} \par\includegraphics[origin=rb,angle=0,width=10.6cm,clip]{5242F3.eps} \end{figure}$	Figure 3: Averaged Doppler image of PW And for August 26-31, 2004 (JD 2 453 243-249). Maps are plotted in a spherical projection at eight equidistant rotational phases. The temperature scale is indicated and is the same for all projections. The image is an average from seven spectral regions, see text. Note that the photospheric temperature is $\approx$ 5000 K.
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$\begin{figure} \par\includegraphics[origin=rb,angle=0,width=10.6cm,clip]{5242F4.eps} \end{figure}$	Figure 4: Doppler image of PW And from the full-spectrum approach. Otherwise as in Fig. 3.
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