  Edge-on galaxies act as the best laboratories to understand the origin of
thin and thick discs in galaxies. Measurement of spatially resolved stellar
population properties in such galaxies, particularly age, metallicity and
[$\alpha$/Fe], are crucial to understanding the formation and evolution of disc
galaxies. Such measurements are made possible from stellar population model
fits to deep integral field spectroscopic (IFU) observations of resolved
galaxies. We utilise archival MUSE IFU observations of the edge-on galaxy ESO
544-27 to uncover the formation history of its thin and thick discs through its
stellar populations. We find the thin disc of the galaxy is dominated by an old
($>9$ Gyr) low [$\alpha$/Fe] metal-rich stellar population. Its outer thick
disc is dominated by an old ($>9$ Gyr) high [$\alpha$/Fe] metal-rich component
that should have formed with higher star-formation efficiency than the Milky
Way thick disc. We thus find [$\alpha$/Fe] dichotomy in ESO 544-27 with its
thin and thick discs dominated by low and high [$\alpha$/Fe] stellar
populations respectively. However, we also find a metal-rich younger ($<2$ Gyr
old) stellar population in ESO 544-27. The galaxy was nearly quenched until its
star-formation was reignited recently first in the outer and inner thick disc
($\sim$1 Gyr ago) and then in the thin disc ($\sim$600 Myr ago). We thus find
that both the low [$\alpha$/Fe] thin and high [$\alpha$/Fe] thick discs of ESO
544-27 are inhabited primarily by similarly old metal-rich stellar populations,
a contrast to that of other galaxies with known thin and thick disc stellar
population properties.
