All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{6236fig1.ps}}\end{figure}$ Figure 1: Flow diagram summarizing the processing steps of the ISOSS slew data from the raw data streams to the final ISOSS Sky Atlas images and the ISOSS compact source database.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{6236fig2.ps}}\end{figure}$ Figure 2: The distribution of the relative differences of slew brightnesses at slew crossings. The width of the distribution after rescaling is an order of magnitude narrower than the original distribution obtained with the standard processing.
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In the text

$\begin{figure} \par\mbox{\resizebox{8.5cm}{!}{\includegraphics{6236fig3.ps}}\resizebox{8.5cm}{!}{\includegraphics{6236fig4.ps}} } \end{figure}$ Figure 3: A $10 \hbox {$^\circ $ }\times 10 \hbox {$^\circ $ }$ region of the sky around the Draco cloud ( $l \approx 90\hbox {$^\circ $ }$ , $b \approx$ +38 $\hbox {$^\circ $ }$ ), an area with prominent galactic Cirrus structures at high galactic latitude. The map from the uncorrected slew data has a much larger scatter in brightness along individual slews ( left) compared to the result after cross-calibration and rescaling ( right). Surface brightnesses cover a range of 5-10 MJy/sr.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{6236fig5.ps}}\end{figure}$ Figure 4: An example of a map assembled from the rescaled ISOSS slew data. The image shows a typical sky region in the northern galactic hemisphere in Cygnus. Sources appearing in the ISOSS compact source database (Stickel et al. 2003,2002) are encircled. The ellipse ( upper left) indicates a close double source and the rectangular inset the corresponding region from the IRAS 100 $\mu$ m survey, demonstrating the similar angular resolution. Surface brightnesses cover a range of 150-500 MJy/sr. The scale bar indicates $1\hbox {$^\circ $ }$ .
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[origin=c,angle=-90]{6236fig6.ps}}\end{figure}$ Figure 5: Map of M 31 derived from all Serendipity Survey slews crossing the area. The large scale ring structure and the bright knot north-west of the center is apparent. (Cf. the fully sampled ISOPHOT 170 $\mu$ m map by Haas et al. 1998.)
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In the text

$\begin{figure} \par\includegraphics[width=17cm]{6236fig7.ps}\end{figure}$ Figure 6: The overall distribution of the coldest cores (crosses) with ISOSS 170 $\mu$ m - IRAS 100 $\mu$ m color temperatures below 12 K across the Milky Way. For comparison, warmer cores are indicated by filled dots. The largest cluster of very cold cores is found in the Taurus and Cepheus Flare region, both of which are associated with large molecular cloud complexes (Hotzel 2001).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{6236fig8.ps}\end{figure}$ Figure 7: Far-infrared emission from dust in the region of Cassiopeia A. The ISOPHOT 170 $\mu$ m slew covers a $40\hbox {$^\prime $ }\times 80\hbox {$^\prime $ }$ field centered on Cas A. Colours represent the 170 $\mu$ m surface brightness in the range 140-300 MJy/sr (Krause et al. 2004b).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{6236fig1.ps}}\end{figure}$	Figure 1: Flow diagram summarizing the processing steps of the ISOSS slew data from the raw data streams to the final ISOSS Sky Atlas images and the ISOSS compact source database.
Open with DEXTER

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{6236fig2.ps}}\end{figure}$	Figure 2: The distribution of the relative differences of slew brightnesses at slew crossings. The width of the distribution after rescaling is an order of magnitude narrower than the original distribution obtained with the standard processing.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[origin=c,angle=-90]{6236fig6.ps}}\end{figure}$	Figure 5: Map of M 31 derived from all Serendipity Survey slews crossing the area. The large scale ring structure and the bright knot north-west of the center is apparent. (Cf. the fully sampled ISOPHOT 170 $\mu$ m map by Haas et al. 1998.)
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$\begin{figure} \par\includegraphics[width=17cm]{6236fig7.ps}\end{figure}$	Figure 6: The overall distribution of the coldest cores (crosses) with ISOSS 170 $\mu$ m - IRAS 100 $\mu$ m color temperatures below 12 K across the Milky Way. For comparison, warmer cores are indicated by filled dots. The largest cluster of very cold cores is found in the Taurus and Cepheus Flare region, both of which are associated with large molecular cloud complexes (Hotzel 2001).
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{6236fig8.ps}\end{figure}$	Figure 7: Far-infrared emission from dust in the region of Cassiopeia A. The ISOPHOT 170 $\mu$ m slew covers a $40\hbox {$^\prime $ }\times 80\hbox {$^\prime $ }$ field centered on Cas A. Colours represent the 170 $\mu$ m surface brightness in the range 140-300 MJy/sr (Krause et al. 2004b).
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