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$\begin{figure}% latex2html id marker 336\par\renewcommand{\thefigure}{\arabic{figure} a} \includegraphics[width=14cm,clip]{4141fig1.eps} \end{figure}$ Figure 1a: The ISO SWS spectrum of IRAS 14331-6435 (Hen3-1013) shows emission due to amorphous (10.8 $\mu$ ) and crystalline silicates and/or H₂O (33.6 $\mu$ , 40.4 $\mu$ , 43.1 $\mu$ ) (see e.g. Waters & Molster 1999). ISO spectrum of IRAS 16206-5956 (SAO 243756) is noisy and only the continuum is seen here.

In the text

$\begin{figure}% latex2html id marker 347\par\renewcommand{\thefigure}{\arabic{figure} b} \includegraphics[width=14cm,clip]{4141fig2.eps} \end{figure}$ Figure 1b: The ISO SWS spectrum of IRAS 17311-4924 (Hen3-1428) shows emission due to the UIR band at 7.7 $\mu$ , SiC (11.5 $\mu$ ) and the "30 $\mu$ feature" (see e.g. Hrivnak et al. 2000; Volk et al. 2002). IRAS 18062+2410 (SAO 85766) shows emission due to amorphous silicates at 10.8 $\mu$ and 17.6 $\mu$ (see e.g. Waters & Molster 1999).

In the text

$\begin{figure}% latex2html id marker 359 \par\renewcommand{\thefigure}{\arabic{figure} c} \includegraphics[width=14cm,clip]{4141fig3.eps} \end{figure}$ Figure 1c: The ISO SWS spectrum of IRAS 22023+5249 (LSIII +5224) shows emission due to amorphous (10.8 $\mu$ ) and crystalline (33.6 $\mu$ ) silicates (see e.g. Waters & Molster 1999). ISO SWS spectrum of IRAS 22495+5134 (LSIII +5142) is noisy and only the continuum is seen here.

In the text

$\begin{figure}% latex2html id marker 383\par\renewcommand{\thefigure}{\arabic{figure} } \includegraphics[width=14.5cm,clip]{4141fig4.eps} \end{figure}$ Figure 2: ISO SWS (2.4 $\mu{-}44.4~\mu$ ) and LWS (43 $\mu{-}171~$ $\mu$ ) spectra of IRAS 17423-1755 (Hen3-1475) are presented in Figs. 2a and 2c respectively. The SWS spectrum shows a broad absorption feature at 3.1 $\mu$ due to C₂H₂ and/or HCN (see e.g. Cernicharo et al. 1999; J $\o$ rgensen et al. 2000). This broad absorption feature is seen clearly in Fig. 2b showing the SWS spectrum of the star from 2.4 $\mu{-}10~\mu$ only. The LWS spectrum of the star (Fig. 2c) appears featureless.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,height=13.5cm,clip]{4141fig5.eps} \end{figure}$ Figure 3: Spectral energy distributions (SEDs) of the hot post-AGB stars. $\it UBVRI$ data (asterisk) are plotted alongwith JHK (triangle), MSX (square) and IRAS data (cross). IRAS 12584-4837 (Hen3-847), IRAS 18062+2410 (SAO 85766) and IRAS 18379-1707 (LSS 5112) are variable in J, H and K bands. The 2MASS, J, H, K data of these three stars is represented by filled diamonds. ISO spectra of the hot post-AGB stars are plotted as solid lines. Dusty model fits are shown by dashed-dotted lines. The model fit corresponding to the 2MASS J, H, K data of IRAS 12584-4837 (Hen3-847) is shown by a solid line. We could not obtain a fit to the "30 $\mu$ emission feature" in IRAS 17311-4924 (Hen3-1428). The IR (8.7, 10, 11.4, 12.6 and 19.5 $\mu$ ) and K, L, M data of IRAS 18062+2410 (SAO 85766) by Lawrence et al. (1990) is indicated by diamonds. Notice the mismatch between the K-band flux of Lawrence et al. (1990; diamond) and García-Lario et al. (1997b; triangle) for the star. The L and M-band fluxes also do not lie on the modelled SED of the star (see Sect. 4.3).
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{4141fig6.eps} \end{figure}$ Figure 3: continued.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{4141fig6.eps} \end{figure}$	Figure 3: continued.
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