All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{7415fig1.eps}\end{figure}$ Figure 1: J = 9-8, 11-10, 12-11, 14-13 and 15-14 lines of C₄H^- toward IRC+10216. The spectral resolution is 1 MHz and the frequency scale (rest frequency) is relative to a systemic velocity of -26.5 km s^-1. The positions of the C₄H^- lines are indicated by downward arrows. The lines of HCCC¹³CCN correspond to its J = 42-41, and 49-48 transitions. The corresponding transitions of HCC¹³CCCN could be present in the same panels. However, within the S/N of the data these lines are not detected. Spectral intensities are in the antenna temperature scale, $T_{\rm A}^*$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{7415fig2.eps}\end{figure}$ Figure 2: Averaged spectrum of the J = 9-8, 11-10, 12-11, 14-13 and 15-14 lines of C₄H^- (histogram) and C₄H (thick continuous line). All lines blended with those of C₄H^-have been fitted and removed. The C₄H averaged spectrum has been scaled by a factor 100.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7415fig3.eps}\end{figure}$ Figure 3: Rotational diagrams for C₄H^-, C₆H^- and C₆H $^2\Pi _{3/2}$ . Main beam integrated intensities (data in Table 1 multiplied by 1.33) have been corrected for beam dilution assuming an uniform source of radius 19''.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{7415fig4.eps}\end{figure}$ Figure 4: Abundance profiles of C_nH and C_nH^- given by chemical modelling. Angular distance is given on the top axis for an assumed distance to the star of 150 pc.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7415fig5.eps}\end{figure}$ Figure 5: Spectrum of IRC+10216 covering the J = 71-70 rotational transition of C₈H^-. The upward arrows indicate the position of the edges of the C₈H^- line.
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{7415fig2.eps}\end{figure}$	Figure 2: Averaged spectrum of the J = 9-8, 11-10, 12-11, 14-13 and 15-14 lines of C₄H^- (histogram) and C₄H (thick continuous line). All lines blended with those of C₄H^-have been fitted and removed. The C₄H averaged spectrum has been scaled by a factor 100.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7415fig3.eps}\end{figure}$	Figure 3: Rotational diagrams for C₄H^-, C₆H^- and C₆H $^2\Pi _{3/2}$ . Main beam integrated intensities (data in Table 1 multiplied by 1.33) have been corrected for beam dilution assuming an uniform source of radius 19''.
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$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{7415fig4.eps}\end{figure}$	Figure 4: Abundance profiles of C_nH and C_nH^- given by chemical modelling. Angular distance is given on the top axis for an assumed distance to the star of 150 pc.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7415fig5.eps}\end{figure}$	Figure 5: Spectrum of IRC+10216 covering the J = 71-70 rotational transition of C₈H^-. The upward arrows indicate the position of the edges of the C₈H^- line.
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