  The Stellar Initial Mass Function (IMF) characterizes the mass distribution
of newly formed stars in various cosmic environments, serving as a fundamental
assumption in astrophysical research. Recent findings challenge the prevalent
notion of a universal and static IMF, proposing instead that the IMF's shape is
contingent upon the star formation environment. In this study, we analyze the
galaxy-wide variation of the IMF for low-mass stars in both dwarf and massive
galaxies with diverse observational methods. Despite systematic discrepancies
between different approaches, an IMF model with a metallicity-dependent slope
for the low-mass stars aligns with the majority of observations, indicating a
high degree of uniformity in the star formation processes across the universe.
We also emphasize the need for a more comprehensive understanding of the
variation of the low-mass IMF, considering measurement biases and factors
beyond metallicity.
