All Figures

$\begin{figure} \par\psfig{figure=3763f1.ps,angle=-90,height=7.5cm,clip=} \end{figure}$ Figure 1: Diagnostic diagram [O III] $\lambda$ 5007/H $\beta$ vs. [N II] $\lambda$ 6583/H $\alpha$ for our SDSS sample. The dashed line separates galaxies with H II regions-like spectra from galaxies containing an active nucleus (labeled "AGN'') (Kauffmann et al. 2003). As in all the figures with observational data, the number of points is indicated in the left lower corner.
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In the text

$\begin{figure} \psfig{figure=3763f2.ps,angle=-90,height=7.4cm,clip=} \end{figure}$ Figure 2: Difference between ionic abundances calculated with the new and old emissivities in the case of the low-density limit as a function of the electron temperature. Curves are labeled by the emission lines used for the abundance determination.
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In the text

$\begin{figure} \mbox{\psfig{figure=3763f3a.ps,angle=270,width=7.2cm}\hspace*{0.4cm}\psfig{figure=3763f3b.ps,angle=270,width=7.2cm,clip=} } \end{figure}$ Figure 3: Relations between the electron temperatures a) $t_{\rm e}$ (O II) and $t_{\rm e}$ (O III) ( $t_{\rm e}$ = 10^-4 $T_{\rm e}$ ) and b) $t_{\rm e}$ (S III) and $t_{\rm e}$ (O III) obtained from the sequences of photoionization models for H II galaxies (Stasinska & Izotov 2003) using stellar atmosphere models from Smith et al. (2002). Filled circles are for the models with Z = 0.02 $Z_\odot$ , open circles are for the models with Z = 0.05 $Z_\odot$ , and stars are for the models with Z = 0.2 $Z_\odot$ . The dotted lines are the approximation of the models of Stasinska (1990) in a) and the approximation of the models of Garnett (1992) in b).
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In the text

$\begin{figure} \mbox{\psfig{figure=3763f4a.ps,angle=270,height=6.5cm,clip=}\hspace*{0.4cm}\psfig{figure=3763f4b.ps,angle=270,height=6.5cm,clip=} } \end{figure}$ Figure 4: a) Relation between the electron temperatures $t_{\rm e}$ (O II) and $t_{\rm e}$ (O III) for the SDSS sample (small circles) and HeBCD galaxies (large circles). b) Relation between the electron temperatures $t_{\rm e}$ (S III) and $t_{\rm e}$ (O III) for the SDSS sample. The solid and dashed lines in a) and b) are respectively the predictions for H II region models (Eqs. (14)-(15)) with low- and intermediate metallicities.
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In the text

$\begin{figure} \hspace*{-0.0cm}\psfig{figure=3763f5.ps,angle=270,height=6.5cm,clip=}\end{figure}$ Figure 5: Ionization correction factor ICF(S⁺+S²⁺) vs. the fraction O⁺/(O⁺+O²⁺) for the "low Z'' models with different rates of dielectronic recombination for sulfur ions. Nominal dielectronic recombination for sulfur ions is the same as that for oxygen ions.
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In the text

$\begin{figure} \mbox{\psfig{figure=3763f6a.ps,angle=0,height=12.5cm}\hspace*{0.4... ...pace*{0.4cm}\psfig{figure=3763f6c.ps,angle=0,height=12.5cm,clip=} } \end{figure}$ Figure 6: Left: sulfur-to-oxygen abundance ratio vs. the fraction O⁺/(O⁺+O²⁺) in the H II regions with 12 + log O/H $\leq$ 7.6 for different rates of dielectronic recombination for sulfur. The nominal dielectronic recombination for S ions is the same as that for O ions. Large filled circles are data for the HeBCD sample, dots are for the SDSS sample. Solid horizontal line shows the mean S/O abundance ratio from the data with the nominal rate of dielectronic recombination for sulfur ions. Middle: the same as in the left panel but for H II regions with 7.6 < 12 + log O/H $\leq$ 8.2. Right: the same as in the left panel but for H II regions with 12 + log O/H > 8.2. The total number of galaxies in each panel is shown in the lower left corner.
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In the text

$\begin{figure} \mbox{\psfig{figure=3763f7a.ps,angle=0,height=12.5cm}\hspace*{0.4... ...pace*{0.4cm}\psfig{figure=3763f7c.ps,angle=0,height=12.5cm,clip=} } \end{figure}$ Figure 7: The same as in Fig. 6 but for argon. Nominal dielectronic recombination for Ar ions is the same as that for Ne ions.
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In the text

$\begin{figure} \mbox{\psfig{figure=3763f8a.ps,angle=0,height=12.5cm}\hspace*{0.4... ...pace*{0.4cm}\psfig{figure=3763f8c.ps,angle=0,height=12.5cm,clip=} } \end{figure}$ Figure 8: The same as in Fig. 6 but for chlorine. Nominal dielectronic recombination for Cl ions is the same as that for O ions.
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In the text

$\begin{figure} \psfig{figure=3763f9.ps,angle=270,width=14.0cm,clip=}\end{figure}$ Figure 9: Ionization correction factors for heavy elements. Filled circles are for the models with Z = 0.02 $Z_\odot$ , open circles are for the models with Z = 0.05 $Z_\odot$ , and stars are for the models with Z = 0.2 $Z_\odot$ . The dotted line is the approximation of the models of Stasinska (1990).
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In the text

$\begin{figure} \par {\includegraphics[angle=0,width=8.5cm]{3763f10a.ps}\hspace*{... ...\includegraphics[angle=0,width=8.5cm]{3763f10c.ps}\hspace*{4.5cm}}\end{figure}$ Figure 10: SDSS spectra of the H II regions listed in Table 3. The names of the spectra in the SDSS database are shown in parentheses.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=0,height=10.5cm]{3763f11a.ps}\includegraphics[angle=0,height=10.5cm]{3763f11b.ps} } \end{figure}$ Figure 11: log N/O a), g), log Ne/O b), h), log S/O c), i), log Cl/O d), j), log Ar/O e), k) and log Fe/O f), l) vs. oxygen abundance 12 + log O/H for the emission-line galaxies. Large filled circles are galaxies from the HeBCD sample, dots are galaxies from the SDSS sample. Abundances in the left panel are calculated with the expressions used by Izotov et al. (1997,1994) and Thuan et al. (1995) and those in the right panel are obtained with expressions from this paper. The solar values as compiled by Lodders (2003) are indicated by the large open circles and the associated error bars are shown. Straight lines are linear regressions obtained for the HeBCD sample.
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In the text

$\begin{figure} \mbox{\psfig{figure=3763f12a.ps,angle=0,height=9.0cm}\hspace*{0.1... ...cm}\hspace*{0.1cm}\psfig{figure=3763f12e.ps,angle=0,height=9.0cm} } \end{figure}$ Figure 12: a)-c) Nitrogen-to-oxygen abundance ratio, log N/O, vs. equivalent width of H $\beta$ emission line, EW(H $\beta$ ), for the galaxies in three metallicity bins. d)-f) The same as in a)-c), but for neon-to-oxygen abundance ratio. g)-i) The same as in a)-c), but for sulfur-to-oxygen abundance ratio. j)-l) The same as in a)-c), but for argon-to-oxygen abundance ratio. m)-o) The same as in a)-c), but for iron-to-oxygen abundance ratio. Straight lines are linear regressions obtained for intermediate Z and high Z samples.
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In the text

$\begin{figure} \par\psfig{figure=3763f1.ps,angle=-90,height=7.5cm,clip=} \end{figure}$	Figure 1: Diagnostic diagram [O III] $\lambda$ 5007/H $\beta$ vs. [N II] $\lambda$ 6583/H $\alpha$ for our SDSS sample. The dashed line separates galaxies with H II regions-like spectra from galaxies containing an active nucleus (labeled "AGN'') (Kauffmann et al. 2003). As in all the figures with observational data, the number of points is indicated in the left lower corner.
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$\begin{figure} \psfig{figure=3763f2.ps,angle=-90,height=7.4cm,clip=} \end{figure}$	Figure 2: Difference between ionic abundances calculated with the new and old emissivities in the case of the low-density limit as a function of the electron temperature. Curves are labeled by the emission lines used for the abundance determination.
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$\begin{figure} \hspace*{-0.0cm}\psfig{figure=3763f5.ps,angle=270,height=6.5cm,clip=}\end{figure}$	Figure 5: Ionization correction factor ICF(S⁺+S²⁺) vs. the fraction O⁺/(O⁺+O²⁺) for the "low Z'' models with different rates of dielectronic recombination for sulfur ions. Nominal dielectronic recombination for sulfur ions is the same as that for oxygen ions.
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$\begin{figure} \mbox{\psfig{figure=3763f7a.ps,angle=0,height=12.5cm}\hspace{0.4... ...pace{0.4cm}\psfig{figure=3763f7c.ps,angle=0,height=12.5cm,clip=} } \end{figure}$	Figure 7: The same as in Fig. 6 but for argon. Nominal dielectronic recombination for Ar ions is the same as that for Ne ions.
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$\begin{figure} \mbox{\psfig{figure=3763f8a.ps,angle=0,height=12.5cm}\hspace{0.4... ...pace{0.4cm}\psfig{figure=3763f8c.ps,angle=0,height=12.5cm,clip=} } \end{figure}$	Figure 8: The same as in Fig. 6 but for chlorine. Nominal dielectronic recombination for Cl ions is the same as that for O ions.
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$\begin{figure} \psfig{figure=3763f9.ps,angle=270,width=14.0cm,clip=}\end{figure}$	Figure 9: Ionization correction factors for heavy elements. Filled circles are for the models with Z = 0.02 $Z_\odot$ , open circles are for the models with Z = 0.05 $Z_\odot$ , and stars are for the models with Z = 0.2 $Z_\odot$ . The dotted line is the approximation of the models of Stasinska (1990).
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$\begin{figure} \par {\includegraphics[angle=0,width=8.5cm]{3763f10a.ps}\hspace{... ...\includegraphics[angle=0,width=8.5cm]{3763f10c.ps}\hspace{4.5cm}}\end{figure}$	Figure 10: SDSS spectra of the H II regions listed in Table 3. The names of the spectra in the SDSS database are shown in parentheses.
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