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The gas-phase metallicity reflects the complex interactions between gas inflows, gas outflows, and star formation processes, making it a crucial factor in understanding galaxy formation and evolution. Most metallicity diagnostics are designed based on H II regions and are not suitable for calibrating metallicity when there is contamination from Active Galactic Nuclei (AGN). In this talk, I will introduce a Bayesian method that separates the emission line fluxes from H II regions and AGN-ionized narrow-line regions (NLR) in a consistent manner, allowing us to measure the metallicity in galaxies where AGN and star formation (SF) activities are significantly mixed. Our findings show that in the local universe, AGN indirectly affect both total metallicity and fluctuations in the metallicity field by reducing or correlating with suppressed SF activity. We are also preparing for the next generation of integral field spectroscopy (IFS) instruments with adaptive optics (AO), which hold promise for studying metallicity fields in early-universe galaxies. |
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