The evolution and dependence of the local mass-metallicity relation

We present a sample of 86,111 star-forming galaxies (SFGs) selected from the catalogue of the MPA-JHU emission-line measurements for SDSS DR7 to investigate the evolution of mass-metallicity (MZ) relation. We find that: under the $\rm log(L_{H \alpha})>41.0$threshold,the$0.04<z\leqslant0.06$SFGswith$9.2<$log($M_{\star}/M_{\sun})<9.5$havealwayshighermetallicities($\sim 0.1$ dex) than the $0.10<z<0.12$ SFGs by using the closely-matched control sample method; under the $\mathrm{l}\mathrm{o}\mathrm{g}({\mathrm{L}}_{\text{OIII}})>39.7$ threshold, the $0.04<z⩽0.06$ SFGs with $9.2<$ log($M_{\star }\mathrm{/}{M}_{\text{sun}})<9.5$ do not exhibit the evolution of the MZ relation, in contrast to the $0.10<z<0.12$ SFGs. We find that the metallicity tends to be lower in galaxies with a higher concentration, higher S'{e}rsic index, or higher SFR. In addition, we can see that the stellar mass and metallicity usually present higher in galaxies with a higher $D_{n}4000$ or higher log(N/O) ratio. Moreover, we present the two galaxy populations with log($M_{\star }\mathrm{/}{M}_{\text{sun}}$) below $10.0$ or greater than $10.5$ in the MZ relation, showing clearly an anticorrelation and a positive correlation between specific star formation rate and 12+log(O/H).