All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4488fig1.ps} \end{figure}$ Figure 1: Representative red spectra of galaxies of the sample.
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{4488fig2.ps} \end{figure}$ Figure 2: The ratio between observed and theoretical Paschen to H $\alpha$ flux, $P_{\lambda }$ /H $\alpha$ , versus the reddening function, f(H $\alpha$ ) - f(P $_{\lambda }$ ), for IIZw40. The line shows the least-square fit to the data.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{4488fig3.ps}\end{figure}$ Figure 3: The left panel presents the relation between S₂₃ and R₂₃; the middle and right panels show the relations between log (1.3 x[NII]6584/H $\alpha$ ) and the empirical indicators of abundances, R₂₃ and S₂₃ respectively, for all galaxies of our sample.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{4488fig4.ps}\end{figure}$ Figure 4: The left panel shows the relation of log ([SII]6717,31/H $\alpha$ ) vs. log (1.3 x[NII]6584/H $\alpha$ ); the right panel presents the relation between log ([SIII]/[SII]) and log S₂₃ for all galaxies of our sample.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{4488fig5.ps}\end{figure}$ Figure 5: The left panel shows the relation log $\eta '$ vs. log S₂₃ for all galaxies in our sample. Full and empty symbols represent the objects with and without $T_{\rm e}$ [OIII], respectively. The right panel presents the relation between log (S⁺/S⁺⁺) and log (O⁺/O⁺⁺) for the galaxies with electron temperature; solid, short-dashed, and long-dashed lines show the loci for three series of photoionization models for $T_{\rm eff}$ = 50 kK, 40 kK, and 30 kK, respectively. See the text for details.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{4488fig6.ps}\end{figure}$ Figure 6: A comparison between the measured line temperatures of [OIII] and [SIII]. The electron temperatures, $t_{\rm e}$ [OIII] and $t_{\rm e}$ [SIII], are shown in units of 10⁴ K. The dashed and solid lines are the photoionization models' relation between these temperatures from PMD05 and I05, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=6.25cm,clip]{4488fig7.ps}\end{figure}$ Figure 7: The distribution of total sulfur abundance for our sample of galaxies. The dashed and empty histograms show the number of galaxies with S/H derived from $T_{\rm e}$ [SIII] (see Table 2) and obtained from the S₂₃ calibration, respectively (see the text for details).
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{4488fig8.ps}\end{figure}$ Figure 8: The observed sulfur-to-oxygen abundance ratio for the subset of galaxies of the sample with $T_{\rm e}$ [OIII] plotted as a function of the oxygen abundance. The solar value is shown. The dashed lines are +/- (1 $\sigma$ ) of the mean as shown by the continuous line.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4488fig1.ps} \end{figure}$	Figure 1: Representative red spectra of galaxies of the sample.
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$\begin{figure} \par\includegraphics[width=8.15cm,clip]{4488fig2.ps} \end{figure}$	Figure 2: The ratio between observed and theoretical Paschen to H $\alpha$ flux, $P_{\lambda }$ /H $\alpha$ , versus the reddening function, f(H $\alpha$ ) - f(P $_{\lambda }$ ), for IIZw40. The line shows the least-square fit to the data.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{4488fig3.ps}\end{figure}$	Figure 3: The left panel presents the relation between S₂₃ and R₂₃; the middle and right panels show the relations between log (1.3 x[NII]6584/H $\alpha$ ) and the empirical indicators of abundances, R₂₃ and S₂₃ respectively, for all galaxies of our sample.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{4488fig4.ps}\end{figure}$	Figure 4: The left panel shows the relation of log ([SII]6717,31/H $\alpha$ ) vs. log (1.3 x[NII]6584/H $\alpha$ ); the right panel presents the relation between log ([SIII]/[SII]) and log S₂₃ for all galaxies of our sample.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{4488fig6.ps}\end{figure}$	Figure 6: A comparison between the measured line temperatures of [OIII] and [SIII]. The electron temperatures, $t_{\rm e}$ [OIII] and $t_{\rm e}$ [SIII], are shown in units of 10⁴ K. The dashed and solid lines are the photoionization models' relation between these temperatures from PMD05 and I05, respectively.
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$\begin{figure} \par\includegraphics[width=6.25cm,clip]{4488fig7.ps}\end{figure}$	Figure 7: The distribution of total sulfur abundance for our sample of galaxies. The dashed and empty histograms show the number of galaxies with S/H derived from $T_{\rm e}$ [SIII] (see Table 2) and obtained from the S₂₃ calibration, respectively (see the text for details).
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$\begin{figure} \par\includegraphics[width=8.15cm,clip]{4488fig8.ps}\end{figure}$	Figure 8: The observed sulfur-to-oxygen abundance ratio for the subset of galaxies of the sample with $T_{\rm e}$ [OIII] plotted as a function of the oxygen abundance. The solar value is shown. The dashed lines are +/- (1 $\sigma$ ) of the mean as shown by the continuous line.
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