helps producing deeper gravitational potential wells in a massive galaxy that retain the metals (re)processed by stars, possibly leading to a higher local metallicity than in a less massive galaxy, even if these galaxies have an identical surface density distribution of stellar mass. [@Barrera-Ballesteros2016a] have found that the stellar mass surface density and metallicity relation is largely independent on the total stellar mass for massive (${\rm log}(M_*/M_\odot) \geq 9.5$) galaxies. In this work, we will investigate whether the global stellar mass, especially for low-mass galaxies, is a potential parameter that participates in controlling local metallicity, and to construct a correlation between global stellar mass, local stellar mass surface density and local metallicity, in order to shed light on understanding the local chemical evolution history in galaxies.

The remainder of this paper is organized as follows. In Section \[sec:data\], we present the sample selection for star-forming galaxies, the methodology for detecting and measuring nebular emission lines, and the determination of dust attenuation properties, gas-phase oxygen abundances and other galaxy parameters. In Section \[sec:results\], we describe the methods for estimating the strength of the correlation between $M_*$ – $Z$ and $\Sigma_*$ – $Z$, as well as that of a new $M_*$ – 