All Figures

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{7183fig1up.eps}\vspace*{5mm} \includegraphics[width=6.6cm,clip]{7183fig1low.eps}\end{figure}$ Figure 1: Upper panel: $12~+~{\rm log~(O/H)}$ vs. log (Ne3O2) for our data sample. Dots are galaxies from SDSS DR4. Crosses are from the literature. Lower panel: the solid line represents Eq. (2). Stars denote the mean for each bin of the oxygen abundance. The dot-dashed lines denote the best-fit function for each metallicity bin. The dashed curves are the calibration of Nagao et al. (2006).
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{7183fig2.eps}\end{figure}$ Figure 2: The relationship between Ne3O2 index and the P parameter for H II galaxies in SDSS DR4. P = ([O III] $\lambda 4959$ +[O III] $\lambda 5007$ )/ ([O II] $\lambda 3727$ +[O III] $\lambda 4959$ +[O III] $\lambda 5007$ ).
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{7183fig3.eps}\end{figure}$ Figure 3: The relationship between Ne3O2 index and the electron temperature for H II galaxies in SDSS DR4. The electron temperature is in units of 10⁴ K.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{7183fig4up.eps}\vspace*{5mm} \includegraphics[width=6.7cm,clip]{7183fig4low.eps}\end{figure}$ Figure 4: Upper panel: correlation between $\log~({\rm O/H})_{T_{\rm e}}$ - $\log~({\rm O/H})_{\rm Ne3O2}$ and the $\log~({\rm Ne/O})$ abundance ratios of Sample I (crosses) and the sample of Izotov et al. (2006) (diamonds). $\log~({\rm O/H})_{T_{\rm e}}$ - $\log~({\rm O/H})_{\rm Ne3O2}$ is the difference between $T_{\rm e}$ metallicity determined from the expressions in Izotov et al. (2006) and Ne3O2 metallicity determined from Eq. (2). Lower panel: correlation between $\log~({\rm O/H})_{T_{\rm e}}$ - $\log~({\rm O/H})_{\rm Ne3O2}$ and the $\log~({\rm Ne/O})$ abundance ratios of Sample II (dots).
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{7183fig5.eps}\end{figure}$ Figure 5: Comparison of the $T_{\rm e}$ metallicities and Bayesian metallicities. Crosses are Sample I. Small dots are Sample II.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{7183fig6.eps}\end{figure}$ Figure 6: Comparison of the Ne3O2 and Ar3O3 methods. Ar3O3 metallicity is calculated using the calibration of Stasinska (2006). Ne3O2 metallicity is calculated using Eq. (2). Sample I is indicated by stars, and Sample II is indicated by crosses.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{7183fig2.eps}\end{figure}$	Figure 2: The relationship between Ne3O2 index and the P parameter for H II galaxies in SDSS DR4. P = ([O III] $\lambda 4959$ +[O III] $\lambda 5007$ )/ ([O II] $\lambda 3727$ +[O III] $\lambda 4959$ +[O III] $\lambda 5007$ ).
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$\begin{figure} \par\includegraphics[width=6.6cm,clip]{7183fig3.eps}\end{figure}$	Figure 3: The relationship between Ne3O2 index and the electron temperature for H II galaxies in SDSS DR4. The electron temperature is in units of 10⁴ K.
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{7183fig5.eps}\end{figure}$	Figure 5: Comparison of the $T_{\rm e}$ metallicities and Bayesian metallicities. Crosses are Sample I. Small dots are Sample II.
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{7183fig6.eps}\end{figure}$	Figure 6: Comparison of the Ne3O2 and Ar3O3 methods. Ar3O3 metallicity is calculated using the calibration of Stasinska (2006). Ne3O2 metallicity is calculated using Eq. (2). Sample I is indicated by stars, and Sample II is indicated by crosses.
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