N2O2 diagnostic, O3N2 and N2 almost couldn’t reproduce the super-solar oxygen abundances and will derive lower metallicities [@Blanc2015; @Zhang2017].

In this work, we adopt the N2O2 diagnostic to determine the oxygen abundances. The N2O2 index introduced in [@Dopita2000] and improved by [@Dopita2013], is defined as $$\rm N2O2 \equiv log(\frac{{\hbox{[N\,{\sc ii}]}}\lambda6583}{{\hbox{[O\,{\sc ii}]}}\lambda\lambda3727,3729}),$$ and is converted to metallicity using the relation in [@Kewley2002] as $$\begin{split}
    \rm 12 + log(O/H) = log(1.54020 + 1.26602 \times N2O2 \\
     \rm + 0.167977 \times N2O2^2)+ 8.93,
    \end{split}$$ with a typical error of 0.04 dex when $\rm 12 + log(O/H) \geq 8.6$. In order to obtain the general results that are independent on the metallicity calibrators, we also calculate the metallicities with O3N2 and N2 indices in Appendix.

The global stellar mass $M_*$ is retrieved from the NSA catalog [@Blanton2011]. In order to derive the local stellar mass surface density $\Sigma_*$, we divide the local stellar mass in each spaxel of the output from the <span style="font-variant:small-caps;">STARLIGHT</span> fits by its corresponding physical area, following the method in [@Barrera-Ballesteros2016a] to correct for the inclination by applying the minor-to-major axis ratio ($b/a$) retrieved from the NSA catalog. The uncertainty of the local stellar mass for each spaxel is smaller 