All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4463F1.eps}\end{figure}$ Figure 1: Two average interstellar radiation fields of Mathis et al. (1983), 5 kpc and 13 kpc away from the galactic centre are compared to the radiation fields of the stars illuminating the specific reflection and planetary nebulae considered in this work; both of them were obtained from stellar atmospheric models of Kurucz (1992) scaled by the blackbody dilution factor corresponding to the geometry of the source (cf. mal03c).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{H4463F2.eps}\end{figure}$ Figure 2: Ground state geometry of C₃₂H₁₄ showing the 9 inequivalent C atoms (labelled by 1, 3, 7, 11, 15, 19, 23, 27 and 29) and the 4 inequivalent H atoms (labelled by 33, 35, 39 and 43); the molecule lies in the xy-plane, the y-axis being the longer one.
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In the text

$\begin{figure} \par\includegraphics[width=17.8cm,clip]{H4463F3.eps}\end{figure}$ Figure 3: IR emission spectrum of C₃₂H₁₄ in all the radiation fields considered, expressed in terms of flux per unit column density of the emitting species in units of W sr $^{-1}~\mu$ m^-1. We arbitrarily assumed a fixed band width of $0.1~\mu$ m in order to make sure that peak heights be proportional to band fluxes.
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In the text

$\begin{figure} \par\includegraphics[width=17.8cm,clip]{H4463F4.eps}\end{figure}$ Figure 4: IR emission spectrum of C₃₂H₁₄⁺ in all the radiation fields considered, expressed in terms of flux per unit column density of the emitting species in units of W sr $^{-1}~\mu$ m^-1. We arbitrarily assumed a fixed band width of $0.1~\mu$ m in order to make sure that peak heights be proportional to band fluxes.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4463F5.eps}\end{figure}$ Figure 5: Expected emission spectrum of C₃₂H₁₄⁺ in the radiation field of the Red Rectangle in the wavelength range between $\sim$ 5 and $\sim$ 9 $\mu$ m, assuming educated guesses for the bandwidth following Pech et al. (2002). The top box shows individual spectra for each isotopic substitution, the bottom box compares the spectrum for the unsubstituted molecule with the weighted average assuming standard interstellar isotopic abundances and no fractionation.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4463F6.eps}\end{figure}$ Figure 6: Expected emission spectrum of C₃₂H₁₄⁺ in the radiation field of the Red Rectangle in the wavelength range around its strongest far infrared skeletal band, near $\sim$ 80 $\mu$ m, assuming a bandwidth of $\sim$ 1 $\mu$ m. The top box shows individual spectra for each isotopic substitution, the bottom box compares the spectrum for the unsubstituted molecule with the weighted average assuming standard interstellar isotopic abundances and no fractionation.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4463F7.eps}\end{figure}$ Figure 7: Expected emission spectrum of C₃₂H₁₄⁺ in the radiation field of the Red Rectangle in the wavelength range around its strongest far infrared skeletal band, near $\sim$ 80 $\mu$ m, assuming a bandwidth of $\sim$ 0.1 $\mu$ m. The top box shows individual spectra for each isotopic substitution, the bottom box compares the spectrum for the unsubstituted molecule with the weighted average assuming standard interstellar isotopic abundances and no fractionation.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{H4463F2.eps}\end{figure}$	Figure 2: Ground state geometry of C₃₂H₁₄ showing the 9 inequivalent C atoms (labelled by 1, 3, 7, 11, 15, 19, 23, 27 and 29) and the 4 inequivalent H atoms (labelled by 33, 35, 39 and 43); the molecule lies in the xy-plane, the y-axis being the longer one.
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$\begin{figure} \par\includegraphics[width=17.8cm,clip]{H4463F3.eps}\end{figure}$	Figure 3: IR emission spectrum of C₃₂H₁₄ in all the radiation fields considered, expressed in terms of flux per unit column density of the emitting species in units of W sr $^{-1}~\mu$ m^-1. We arbitrarily assumed a fixed band width of $0.1~\mu$ m in order to make sure that peak heights be proportional to band fluxes.
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$\begin{figure} \par\includegraphics[width=17.8cm,clip]{H4463F4.eps}\end{figure}$	Figure 4: IR emission spectrum of C₃₂H₁₄⁺ in all the radiation fields considered, expressed in terms of flux per unit column density of the emitting species in units of W sr $^{-1}~\mu$ m^-1. We arbitrarily assumed a fixed band width of $0.1~\mu$ m in order to make sure that peak heights be proportional to band fluxes.
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