Deficiency of current photoionisation models and the needs for highly-resolved studies like AMASE-P

Understanding feedback of star formation and chemical evolution of galaxies requires realistic models. However, spatially-resolved observations on kpc scales from SDSS-IV/MaNGA and 100 pc scales from PHANGS-MUSE have revealed many inconsistencies with current photoionization models of star-forming regions. Efforts resolving these puzzles are further complicated by small-scale spatial correlations between dust and ionized gas. These problems would directly lead to systematics in scaling relations such as mass-metallicity relations and its secondary dependences. I will discuss the results of our analyses in these directions, which could only be understood by new spectroscopy observations resolving sub-parsec or few parsec scales. To this end, we are developing the AMASE-P survey, which will be a wide-area integral field spectroscopy survey studying the ionized gas and dust in the Milky Way and nearby galaxies with a spatial resolution of subparsec to 10s of parsecs, and a spectral resolution close to $R\sim 15,000$. It will include both a northern survey and a southern survey, cover hundreds of square degrees of sky, and target Milky Way, LMC, SMC, M31, M33, and other local group galaxies. It is expected to start observing within a year. I will describe the progress of the project and its science prospects.