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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{10193fig1.eps}\end{figure}$ Figure 1: Spectra of IRC +10216 observed with the IRAM 30-m telescope showing on top the $J_{\rm K}$ = 1₀-0₀ line of PH₃ blended with a narrower line assigned to the J = 15-14 line of SiS v = 4. Shown below are the immediate lower rotational transitions of SiS v = 4. Fits to the line profiles using the CLASS shell method are shown as thick grey lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{10193fig2.eps}\end{figure}$ Figure 2: The lower panel shows the PH₃ $J_{\rm K}$ = 1₀-0₀ line at 267 GHz as observed with the IRAM 30-m telescope, in which the fit to the SiS v = 4 J = 15-14 line has been subtracted. The upper panel shows the observation at 800 GHz with the CSO smoothed to a spectral resolution of 2 MHz. The thick grey lines in both panels correspond to the line profiles given by the LVG model.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{10193fig1.eps}\end{figure}$	Figure 1: Spectra of IRC +10216 observed with the IRAM 30-m telescope showing on top the $J_{\rm K}$ = 1₀-0₀ line of PH₃ blended with a narrower line assigned to the J = 15-14 line of SiS v = 4. Shown below are the immediate lower rotational transitions of SiS v = 4. Fits to the line profiles using the CLASS shell method are shown as thick grey lines.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{10193fig2.eps}\end{figure}$	Figure 2: The lower panel shows the PH₃ $J_{\rm K}$ = 1₀-0₀ line at 267 GHz as observed with the IRAM 30-m telescope, in which the fit to the SiS v = 4 J = 15-14 line has been subtracted. The upper panel shows the observation at 800 GHz with the CSO smoothed to a spectral resolution of 2 MHz. The thick grey lines in both panels correspond to the line profiles given by the LVG model.
Open with DEXTER