$\begin{figure} \par\mbox{\resizebox{6cm}{!}{\includegraphics{3862f1a.ps}} {\larg... ...tarrow$ } \resizebox{6cm}{!}{\includegraphics{3862f1d.ps}} } \par\end{figure}$ Figure 1: Pipeline-processing in comparison with re-reduced asteroid images. Top: Itokawa measurement #12 (Table 1), N1-filter, 7.5 min integration time, left: pipeline-product, right: the 60 raw images were shifted by 1.0 pixels per minute in x-direction and by -1.0 pixels per minute in y-direction and then co-added. Bottom: Itokawa measurement #20 (Table 1), Q1-filter, 25.8 min integration time, left: pipeline-product, right: the 234 raw images were shifted by 0.8 pixels per minute in x-direction and by 0.2 pixels per minute in y-direction and then co-added.
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In the text

$\begin{figure} { \rotatebox{90}{\resizebox{!}{8cm}{\includegraphics{3862f3.ps}}} } \end{figure}$ Figure 3: Thermal inertia optimisation process for the individual TPM albedos and their standard deviation, using all 20 individual observations (dashed line), a subset with 15 observations (solid line) and a subset of 9 observations (dotted line).
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In the text

$\begin{figure} { \rotatebox{90}{\resizebox{!}{8cm}{\includegraphics{3862f4.ps}}} } \end{figure}$ Figure 4: Thermal inertia optimisation process for the individual TPM diameters and their standard deviation, using all 20 individual observations (dashed line), a subset with 15 observations (solid line) and a subset of 9 observations (dotted line).
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In the text

$\begin{figure} { \rotatebox{90}{\resizebox{!}{8cm}{\includegraphics{3862f5.ps}}} } \end{figure}$ Figure 5: Predicted thermal lightcurve at 10.0 $\mu$ m for the time period around the July 1st, 2004 observations. The original measurements were "transported'' to the 10.0 $\mu$ m wavelength via our TPM solution. Predictions and measurements are shown with their absolute values, no shifting or scaling in time or flux have been done.
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In the text

$\begin{figure} { \rotatebox{90}{\resizebox{!}{7.5cm}{\includegraphics{3862f6a.p... ...atebox{90}{\resizebox{!}{7.5cm}{\includegraphics{3862f6b.ps}}} } \end{figure}$ Figure 6: The observation/TPM ratios for a thermal inertia of 0 ( top) and 750 ( bottom). The high thermal inertia values eliminate the trend with phase angle and reduce the scatter significantly.
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In the text

$\begin{figure} {\rotatebox{90}{\resizebox{!}{7.5cm}{\includegraphics{3862f7a.ps}... ...atebox{90}{\resizebox{!}{7.5cm}{\includegraphics{3862f7b.ps}}} } \end{figure}$ Figure 7: The observation/TPM ratios for a thermal inertia of 0 ( top) and 750 ( bottom). The high thermal inertia values eliminate the trend with wavelength and reduce the scatter significantly.
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In the text

$\begin{figure} { \resizebox{8.8cm}{!}{\includegraphics{3862f2a.ps}} } {\resizebox{8.8cm}{!}{\includegraphics{3862f2b.ps}} } \end{figure}$	Figure 2: Equatorial edge-on ( top) and pole-on ( bottom) images of the shape model.
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$\begin{figure} { \rotatebox{90}{\resizebox{!}{8cm}{\includegraphics{3862f3.ps}}} } \end{figure}$	Figure 3: Thermal inertia optimisation process for the individual TPM albedos and their standard deviation, using all 20 individual observations (dashed line), a subset with 15 observations (solid line) and a subset of 9 observations (dotted line).
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$\begin{figure} { \rotatebox{90}{\resizebox{!}{8cm}{\includegraphics{3862f4.ps}}} } \end{figure}$	Figure 4: Thermal inertia optimisation process for the individual TPM diameters and their standard deviation, using all 20 individual observations (dashed line), a subset with 15 observations (solid line) and a subset of 9 observations (dotted line).
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$\begin{figure} { \rotatebox{90}{\resizebox{!}{8cm}{\includegraphics{3862f5.ps}}} } \end{figure}$	Figure 5: Predicted thermal lightcurve at 10.0 $\mu$ m for the time period around the July 1st, 2004 observations. The original measurements were "transported'' to the 10.0 $\mu$ m wavelength via our TPM solution. Predictions and measurements are shown with their absolute values, no shifting or scaling in time or flux have been done.
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$\begin{figure} { \rotatebox{90}{\resizebox{!}{7.5cm}{\includegraphics{3862f6a.p... ...atebox{90}{\resizebox{!}{7.5cm}{\includegraphics{3862f6b.ps}}} } \end{figure}$	Figure 6: The observation/TPM ratios for a thermal inertia of 0 ( top) and 750 ( bottom). The high thermal inertia values eliminate the trend with phase angle and reduce the scatter significantly.
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$\begin{figure} {\rotatebox{90}{\resizebox{!}{7.5cm}{\includegraphics{3862f7a.ps}... ...atebox{90}{\resizebox{!}{7.5cm}{\includegraphics{3862f7b.ps}}} } \end{figure}$	Figure 7: The observation/TPM ratios for a thermal inertia of 0 ( top) and 750 ( bottom). The high thermal inertia values eliminate the trend with wavelength and reduce the scatter significantly.
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