All Figures

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{c4222f1.ps} \end{figure}$ Figure 1: Example of the ISO-SWS band 4 spectrum of $\alpha$ Boo, the brightest star of our sample.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.6cm,clip]{c4222f2.ps} \end{figure}$ Figure 2: Comparison for $\alpha$ Cet between the rather standard OLP10.1 reduction method (upper black) and our detailed reduction which includes a thorough check of all detectors and both scans (lower black). It should be noted that the more detailed reduced spectrum has lower uncertainties on the individual points and that it agrees "better'' with the synthetic spectrum (grey). A glitch, marked by the arrow, is efficiently removed through our reduction, while it remains present in the data after the automatic mode reduction. The noticed discrepancies between the synthetic and observed spectrum will be extensively discussed later in this paper.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{c4222f3.ps} \end{figure}$ Figure 3: Overview of the band 3A spectra of $\beta$ Peg, reduced by using resp_inter and/or fringes, i.e. two different fringe removal tools which are at the disposal of the SWS user, together with the pipeline attempt to remove fringes (respcal).
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{c4222f4.ps} \end{figure}$ Figure 4: Comparison between the synthetic spectra at SWS resolution, the (colour corrected) IRAS-PSC fluxes at 12 and $25~\mu$ m and the IRAS-LRS spectra. We also plotted the (unshifted) ISO-SWS bands 2C and 3(A till D) spectra for our 10 program stars.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.6cm,clip]{c4222f5.ps} \end{figure}$ Figure 5: Relative comparison between the OH synthetic spectra generated by using the line lists at our disposal for $\alpha$ Tau. The used stellar parameters can be found in Table 2.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{c4222f6.ps} \end{figure}$ Figure 6: Comparison between H₂O $12{-}16.5~ \mu$ m synthetic spectra, using the different line data at our disposal, for a model star with $T_{{\rm eff}}~=3000~$ K, $\log~g~=1.00$ , $\xi_{\rm t}=2.0~$ km s^-1, ${{\rm [Fe/H]}}=0.00$ , $\varepsilon$ (C) = 8.35, $\varepsilon$ (N) = 8.35, $\varepsilon$ (O) = 8.83, ${\rm ^{12}C/^{13}C}$ =10, and $M=2.0~M_{\odot}$ in a plane-parallel geometry. The spectra are offset with the values mentioned in the legend. The synthetic spectra have the ISO resolution of band 3A (1150). The references of the line lists can be found in the text.
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In the text

$\begin{figure} \par\includegraphics[width=16.6cm,clip]{c4222f7.ps} \end{figure}$ Figure 7: Relative contribution of the atoms and molecules for $\alpha$ Boo in the wavelength range $12{-}27.5~\mu$ m. The adopted parameters can be found in Table 2. All synthetic spectra are based on the same model atmosphere. The total spectrum coincides with the synthetic spectrum discussed elsewhere in this paper and thus includes all atomic and molecular opacities in its calculation by TurboSpectrum.
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In the text

$\begin{figure} \par\includegraphics[width=16.6cm]{c4222f8.ps} \end{figure}$ Figure 8: Relative contribution of the atoms and molecules for $\alpha$ Tau in the wavelength range $12{-}27.5~\mu$ m. The adopted parameters can be found in Table 2. See Fig. 7 for the meaning of the different synthetic spectra.
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In the text

$\begin{figure} \par\includegraphics[width=16.2cm]{c4222f9.ps} \end{figure}$ Figure 9: Relative contribution of the atoms and molecules for $\beta$ Peg in the wavelength range $12{-}27.5~\mu$ m. The adopted parameters can be found in Table 2. See Fig. 7 for the meaning of the different synthetic spectra.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=15.6cm]{c4222f10.ps} \end{figure}$ Figure 10: Global overview of the final modelling (grey) of the SWS bands 3A, 3C and 3D spectra (black) of the 5 hottest stars of our sample.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16cm]{c4222f11.ps} \end{figure}$ Figure 11: Global overview of the final modelling (grey) of the SWS bands 3A, 3C and 3D spectra (black) of the 5 coolest stars of our sample.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=17.7cm]{c4222f12.ps} \end{figure}$ Figure 12: Suspected atomic (top panel) and molecular (bottom panel) lines in the SWS spectra (black), but absent in the synthetic spectra (grey). The SWS spectra are cleaned up a bit, by dividing out some remaining instrumental response artifacts, see Fig. 14, in order to enable a more detailed comparison with the synthetic spectra. Spectra are offset. The broad feature at 12.3 $\mu$ m is a residue of an artifact in the RSRF.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=15.2cm]{c4222f13.ps} \end{figure}$ Figure 13: Two examples of residual fringes in band 3A. The (scaled and shifted) RSRF are displayed in black, the final reduced - defringed - spectra in mid-grey, synthetic spectra in dark grey (uppermost spectra). Spectra are offset and normalised.
Top panel: For $\beta$ Peg, we also included the spectrum reduced without defringing in light grey (lowest). In this spectrum, the fringe pattern of the RSRF can easily be recognised. Some of these fringes still survive (see the vertical dotted lines) after fringe removal.
Bottom panel: In the spectrum of $\alpha$ Cen A, the fringe pattern of the RSRF is detected. Additionally, the spectrum contains fringes at wavelengths which can not be identified with the fringes of the RSRF. The light grey spectrum is the ATMOS (Atmospheric Trace Molecule Spectroscopy, Farmer et al. 1989; Geller 1992) spectrum of the Sun, $\alpha$ Cen A's twin.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=15.2cm]{c4222f14.ps} \end{figure}$ Figure 14: Division between the SWS spectra and their synthetic spectra at a resolving power of 50, ordered by spectral type. The mean of all these calculated "RSRFs'' is shown at the bottom of the figures.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=17.3cm]{c4222f15.ps} \end{figure}$ Figure 15: Division of SWS spectra of different speeds and the synthetic spectra at resolution 50 for $\beta$ And and $\beta$ Peg.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.6cm]{c4222f16.ps} \end{figure}$ Figure 16: Example of how the reduction strategy, i.e. with or without glitch and bad detector points removal, affects the phase and amplitude of the baseline ripples present in the SWS band 3 spectra.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{c4222f1.ps} \end{figure}$	Figure 1: Example of the ISO-SWS band 4 spectrum of $\alpha$ Boo, the brightest star of our sample.
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$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{c4222f3.ps} \end{figure}$	Figure 3: Overview of the band 3A spectra of $\beta$ Peg, reduced by using `resp_inter` and/or `fringes`, i.e. two different fringe removal tools which are at the disposal of the SWS user, together with the pipeline attempt to remove fringes (`respcal`).
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$\begin{figure} \par\includegraphics[width=18cm,clip]{c4222f4.ps} \end{figure}$	Figure 4: Comparison between the synthetic spectra at SWS resolution, the (colour corrected) IRAS-PSC fluxes at 12 and $25~\mu$ m and the IRAS-LRS spectra. We also plotted the (unshifted) ISO-SWS bands 2C and 3(A till D) spectra for our 10 program stars.
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$\begin{figure} \par\includegraphics[angle=90,width=8.6cm,clip]{c4222f5.ps} \end{figure}$	Figure 5: Relative comparison between the OH synthetic spectra generated by using the line lists at our disposal for $\alpha$ Tau. The used stellar parameters can be found in Table 2.
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$\begin{figure} \par\includegraphics[width=16.6cm]{c4222f8.ps} \end{figure}$	Figure 8: Relative contribution of the atoms and molecules for $\alpha$ Tau in the wavelength range $12{-}27.5~\mu$ m. The adopted parameters can be found in Table 2. See Fig. 7 for the meaning of the different synthetic spectra.
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$\begin{figure} \par\includegraphics[width=16.2cm]{c4222f9.ps} \end{figure}$	Figure 9: Relative contribution of the atoms and molecules for $\beta$ Peg in the wavelength range $12{-}27.5~\mu$ m. The adopted parameters can be found in Table 2. See Fig. 7 for the meaning of the different synthetic spectra.
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$\begin{figure} \par\includegraphics[angle=90,width=15.6cm]{c4222f10.ps} \end{figure}$	Figure 10: Global overview of the final modelling (grey) of the SWS bands 3A, 3C and 3D spectra (black) of the 5 hottest stars of our sample.
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$\begin{figure} \par\includegraphics[angle=90,width=16cm]{c4222f11.ps} \end{figure}$	Figure 11: Global overview of the final modelling (grey) of the SWS bands 3A, 3C and 3D spectra (black) of the 5 coolest stars of our sample.
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$\begin{figure} \par\includegraphics[angle=90,width=15.2cm]{c4222f14.ps} \end{figure}$	Figure 14: Division between the SWS spectra and their synthetic spectra at a resolving power of 50, ordered by spectral type. The mean of all these calculated "RSRFs'' is shown at the bottom of the figures.
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$\begin{figure} \par\includegraphics[angle=90,width=17.3cm]{c4222f15.ps} \end{figure}$	Figure 15: Division of SWS spectra of different speeds and the synthetic spectra at resolution 50 for $\beta$ And and $\beta$ Peg.
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$\begin{figure} \par\includegraphics[angle=90,width=8.6cm]{c4222f16.ps} \end{figure}$	Figure 16: Example of how the reduction strategy, i.e. with or without glitch and bad detector points removal, affects the phase and amplitude of the baseline ripples present in the SWS band 3 spectra.
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