All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{0451fig1.eps} \end{figure}$ Figure 1: The whole spectral range measured near the C³⁶S J=2-1 ( lower panel) and 3-2 ( upper panel) transitions toward IRC+10216. The channel spacing corresponds to $3.1~\rm km~s^{-1}$ for the 3 mm spectrum and $4.2~\rm km~s^{-1}$ for the 2 mm spectrum. The intensity is in mK ( $T_{\rm A}^*$ ).For identifications, see the Appendix A.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{0451fig2.eps} \end{figure}$ Figure 2: C³⁴S and C³⁶S J=2-1 and 3-2 spectra toward IRC+10216. The channel spacing corresponds to $3~\rm km~s^{-1}$ for the 2-1 lines of C³⁴S and C³⁶S, $2~\rm km~s^{-1}$ for the 3-2 line of C³⁴S and $4~\rm km~s^{-1}$ for the 3-2 transition of C³⁶S. Intensities are in mK ( $T_{\rm A}^*$ ). Also shown are fits (convolved with the channel widths) of a shell type emission profile to the lines. The lineshapes of the C³⁶S transitions were determined from the fits to the corresponding C³⁴S lines. In the frame for C³⁶S (2-1), the emission feature at the extreme left corresponds to the 2-1 line of the main isotope of CS observed in the image band. A fit to the C³²S line and to two l-C₃H lines from the image band fixing the intensity ratios to the values obtained from a well calibrated spectrum (Mauersberger et al. 1996) is overlayed on the spectrum. In the third frame the residuals obtained from subtracting the fit to the lines from the image sideband are shown.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{0451fig3.eps} \end{figure}$ Figure 3: Si³⁴S and Si³⁶S J=5-4 and 6-5 spectra toward IRC+10216. The channel spacing corresponds to $\sim$ 3.5-4 km s^-1. Intensities are in mK ( $T_{\rm A}^*$ ). Also shown are fits (convolved with the channel widths) of a shell type emission profile to the lines. In case of the Si³⁶S J=6-5 transition, a simultaneous fit (assuming identical line width) with a blended unidentified line is shown.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0451fig4.eps} \end{figure}$ Figure 4: Isotopic ratios of ³⁶S/³⁴S obtained from four transitions. The straight line indicates the weighted mean value; a dashed line indicates the error of the mean value. Also shown is the solar system ratio ( $3.47\times 10^{-3}$ ).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0451fig5.eps} \end{figure}$ Figure 5: Sulfur isotopic ratios in IRC+10216, normalized to ³⁴S and solar ratios. Data from Kahane et al. (2000) and this work. Also shown are the S isotope ratios predicted for the envelope of a 1.5 $M_\odot$ solar-metallicity, TP-AGB star at the time the Cl isotope ratio is matched (see text; with updated solar abundances), and the ratios measured for the ISM by Mauersberger et al. (1996).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0451fig1.eps} \end{figure}$	Figure 1: The whole spectral range measured near the C³⁶S J=2-1 ( lower panel) and 3-2 ( upper panel) transitions toward IRC+10216. The channel spacing corresponds to $3.1~\rm km~s^{-1}$ for the 3 mm spectrum and $4.2~\rm km~s^{-1}$ for the 2 mm spectrum. The intensity is in mK ( $T_{\rm A}^*$ ).For identifications, see the Appendix A.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0451fig4.eps} \end{figure}$	Figure 4: Isotopic ratios of ³⁶S/³⁴S obtained from four transitions. The straight line indicates the weighted mean value; a dashed line indicates the error of the mean value. Also shown is the solar system ratio ( $3.47\times 10^{-3}$ ).
Open with DEXTER