Addressing the Challenge of Partially Resolved Stellar Population with PHOENIX and FASTWIND

Unveiling stellar populations in the nearby spiral galaxy NGC 300, using the Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope (VLT), provides profound insights into galaxy formation and evolution. This talk will cover the spatial distribution, effective temperature, and line of sight kinematic properties of these stellar populations. We will address the technical challenges encountered during the data acquisition and analysis process. One significant difficulty is the partial resolution of data, where individual stars are not fully resolved, complicating the extraction of precise stellar properties, especially in NGC 300 given its distance of 1.9 Mpc. This challenge makes it difficult to isolate and analyze individual stars without contamination from nearby sources. The talk will explore the strategies employed to mitigate these issues, such as the application of advanced deblending algorithm PampelMUSE, and the use of complementary high-resolution photometric data like HST. Furthermore, analyzing the spectral parameters and kinematics of these crowded fields requires fitting tools such as SPEXXY, which is used to cover the full range of the Hertzsprung-Russell diagram by utilizing two different sets of models, PHOENIX and FASTWIND. By sharing these technical insights, this talk aims to provide a semi-automatic method for future studies using integral field spectroscopy in crowded stellar environments.