All Figures

$\begin{figure} {\epsfig{figure=0226f01,height=10cm} } \end{figure}$ Figure 1: Artist view of the PRONAOS/SPM gondola in flight. The front side of the telescope is not represented in order to show the primary mirror structure and the focal plane instrument.
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In the text

$\begin{figure} \par\epsfig{figure=0226f02.eps,width=8.8cm,height=6.5cm} \end{figure}$ Figure 2: Design of the warm optics of the SPM instrument located behind the primary mirror M 1.
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In the text

$\begin{figure} \par\epsfig{figure=0226f03.ps,width=8.4cm,height=5.7cm} \end{figure}$ Figure 3: Measurements of the PRONAOS/SPM spectral response. The vertical lines correspond to the effective wavelength positions for each band (Sect. 3.1.2).
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In the text

$\begin{figure} \par\epsfig{figure=0226f04.eps,width=7.9cm,height=6.2cm} \end{figure}$ Figure 4: PRONAOS/SPM dual beam section measured on Saturn.
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In the text

$\begin{figure} \par\epsfig{figure=0226f05.eps,width=8.8cm,height=6.5cm} \end{figure}$ Figure 5: Optics design of the SPM instrument and the ICS as seen from the back of the telescope primary mirror (M 1).
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In the text

$\begin{figure} \par\epsfig{figure=0226f06.eps,width=8.3cm,height=5.8cm} \end{figure}$ Figure 6: PRONAOS/SPM response variation on ICS during the 1996 flight. Response is expressed as SPM internal units vs. brightness temperature for extended sources in mK.
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In the text

$\begin{figure} \par\epsfig{figure=0226f07.eps,width=8cm,height=6.2cm} \end{figure}$ Figure 7: PRONAOS/SPM response variation with background temperature. Lines are polynomial fits to data points sets.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{0226f08.ps} \end{figure}$ Figure 8: Spectrum of M 82 measured by PRONAOS and DIRBE . The data in Table 10 have been iteratively color corrected in order to take into account of the actual spectral shape: $\epsilon_{250 ~{\rm \mu m}}=5.7^{+1.2}_{-1.9}~10^{-4}$ , $\beta =1.94^{+0.2}_{-0.3}$ , $T=35.1_{-2.5}^{+6.9}~\rm K$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,angle=0]{0226f09.eps} % \end{figure}$ Figure 9: This figure illustrates the method used when comparing the PRONAOS and DIRBE brightnesses for extended sources on the M 42 data. The grey scale shows the DIRBE $240~{\rm\mu m}$ map and the contours represent the PRONAOS 200 $\mu$ m data. The central square marks the central DIRBE pixel chosen for the comparison (see text). The triangles mark the DIRBE pixels chosen for computing the linear background. The circle represents the DIRBE beam size at $240~{\rm\mu m}$ (55').
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{0226f10.eps} \end{figure}$ Figure 10: PRONAOS DIRBE intercalibration results on extended sources. Spectra of M 42, M 17, $\rho$ -Ophiuchi and CygnusB.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,angle=0]{0226f13.eps}\includegraphics[width=8cm,angle=0]{0226f14.eps} \end{figure}$ Figure 11: ISOPHOT (grey scale) and PRONAOS $200~{\rm\mu m}$ maps (contours) of $\rho$ -Ophiuchi ( left) and M 42 ( right) used for the comparison of their calibration. The PRONAOS scans positions are shown as the dashed lines.
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In the text

$\begin{figure} \par\includegraphics[width=18cm]{0226f15.eps} \end{figure}$ Figure 12: Correlation diagrams between the ISOPHOT and PRONAOS modulated data at $200~{\rm\mu m}$ for $\rho$ -Ophiuchi ( left), M 42-1 ( center) and M 42-2 ( right).
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In the text

$\begin{figure} \par\epsfig{figure=0226f11.eps,width=8.3cm,height=5.7cm} \end{figure}$ Figure A.1: Spectrum of Saturn's disk (continuous line) as quoted in Bézard et al. (1986), and the transmission shape of the four PRONAOS/SPM spectral channels (dashed lines).

In the text

$\begin{figure} \par\psfig{figure=0226f12.eps,width=8.4cm,height=7.4cm,angle=0} \end{figure}$ Figure A.2: Brightness temperature spectrum of the Saturn rings. The black diamonds are the data collected by Esposito et al. (1984), the grey squares are the Roellig et al. (1988), Grossman et al. (1990), Dowling et al. (1987) and de Pater & Dickel (1991) data and their 1 $\sigma$ error bars. The continuous lines show the analytic laws: $T_{1}=0.2 \times \left(\frac{\lambda}{20~\rm cm}\right)^{-1} + 5~\rm K$ for $\lambda>480~\mu\rm m$ (de Pater & Dickel 1991) and $T_{1}=55 + \left(\frac{\lambda}{480~\mu{\rm m}}\right)^{3} \times (T_{1}(480~\mu \rm m)-55)~K$ . The dashed lines are the 1 $\sigma$ error bars of the models.

In the text

$\begin{figure} {\epsfig{figure=0226f01,height=10cm} } \end{figure}$	Figure 1: Artist view of the PRONAOS/SPM gondola in flight. The front side of the telescope is not represented in order to show the primary mirror structure and the focal plane instrument.
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$\begin{figure} \par\epsfig{figure=0226f02.eps,width=8.8cm,height=6.5cm} \end{figure}$	Figure 2: Design of the warm optics of the SPM instrument located behind the primary mirror M 1.
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$\begin{figure} \par\epsfig{figure=0226f03.ps,width=8.4cm,height=5.7cm} \end{figure}$	Figure 3: Measurements of the PRONAOS/SPM spectral response. The vertical lines correspond to the effective wavelength positions for each band (Sect. 3.1.2).
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$\begin{figure} \par\epsfig{figure=0226f04.eps,width=7.9cm,height=6.2cm} \end{figure}$	Figure 4: PRONAOS/SPM dual beam section measured on Saturn.
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$\begin{figure} \par\epsfig{figure=0226f05.eps,width=8.8cm,height=6.5cm} \end{figure}$	Figure 5: Optics design of the SPM instrument and the ICS as seen from the back of the telescope primary mirror (M 1).
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$\begin{figure} \par\epsfig{figure=0226f06.eps,width=8.3cm,height=5.8cm} \end{figure}$	Figure 6: PRONAOS/SPM response variation on ICS during the 1996 flight. Response is expressed as SPM internal units vs. brightness temperature for extended sources in mK.
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$\begin{figure} \par\epsfig{figure=0226f07.eps,width=8cm,height=6.2cm} \end{figure}$	Figure 7: PRONAOS/SPM response variation with background temperature. Lines are polynomial fits to data points sets.
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$\begin{figure} \par\includegraphics[width=8.5cm]{0226f08.ps} \end{figure}$	Figure 8: Spectrum of M 82 measured by PRONAOS and DIRBE . The data in Table 10 have been iteratively color corrected in order to take into account of the actual spectral shape: $\epsilon_{250 ~{\rm \mu m}}=5.7^{+1.2}_{-1.9}~10^{-4}$ , $\beta =1.94^{+0.2}_{-0.3}$ , $T=35.1_{-2.5}^{+6.9}~\rm K$ .
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$\begin{figure} \par\includegraphics[width=8.5cm]{0226f10.eps} \end{figure}$	Figure 10: PRONAOS DIRBE intercalibration results on extended sources. Spectra of M 42, M 17, $\rho$ -Ophiuchi and CygnusB.
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$\begin{figure} \par\includegraphics[width=8cm,angle=0]{0226f13.eps}\includegraphics[width=8cm,angle=0]{0226f14.eps} \end{figure}$	Figure 11: ISOPHOT (grey scale) and PRONAOS $200~{\rm\mu m}$ maps (contours) of $\rho$ -Ophiuchi ( left) and M 42 ( right) used for the comparison of their calibration. The PRONAOS scans positions are shown as the dashed lines.
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$\begin{figure} \par\includegraphics[width=18cm]{0226f15.eps} \end{figure}$	Figure 12: Correlation diagrams between the ISOPHOT and PRONAOS modulated data at $200~{\rm\mu m}$ for $\rho$ -Ophiuchi ( left), M 42-1 ( center) and M 42-2 ( right).
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