2024MNRAS.534.1175W

Ongoing deep integral-field spectroscopy (IFS) observations of disc galaxies provide opportunities for comparison with the Milky Way (MW) to understand galaxy evolution. However, such comparisons are marred by many challenges such as selection effects, differences in observations and methodology, and proper validation of full-spectrum fitting methods. In this study, we present a novel code GALCRAFT to address these challenges by generating mock IFS data cubes of the MW using simple stellar population models and a mock MW stellar catalogue derived from E-GALAXIA. We use the widely adopted full-spectrum fitting code PPXF to investigate the ability to recover kinematics and stellar populations for an edge-on mock MW IFS observation. We confirm that differences in kinematics, mean age, $[\mathrm{M/H}]$, and $[\mathrm{\alpha /Fe}]$ between thin and thick discs can be distinguished. However, the age distribution is overestimated in the ranges between $2{-}4$ and $12{-}14$ Gyr compared to the expected values. This is likely due to the age spacing and degeneracy of SSP templates. We find systematic offsets in the recovered kinematics due to insufficient spectral resolution and the variation of line-of-sight velocity distribution with age and $[\mathrm{M/H}]$. With future higher resolution and multi-$[\mathrm{\alpha /Fe}]$ simple stellar population templates, GALCRAFT will be useful to validate key signatures such as $[\mathrm{\alpha /Fe}]$-$[\mathrm{M/H}]$ distribution at different R and $|z|$ and potentially infer radial migration and kinematic heating efficiency to study detailed chemodynamical evolution of MW-like galaxies.