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The distribution of galaxies in the Universe is inhomogeneous and represents large-scale structures (LSS) that consist of galaxy clusters, groups, and filaments connecting them. Understanding how galaxy characteristics are influenced by their environments and how they evolve over cosmic time within LSS is crucial. The challenge lies in obtaining accurate redshift measurements to precisely identify galaxy environments. Using the Hyper Supreme-Cam on the Subaru Telescope, we demonstrate a method to estimate precise redshifts of star-forming galaxies via flux ratio measurements of the same emission line from slightly overlapping narrow-band filters. We obtain redshifts for H𝛼 and [Oii] emitters at 𝑧 ∼ 0.4 and 1.5 respectively. To accurately trace the galaxy distribution in the LSS, we use these redshifts to provide a more detailed representation of the spatial distribution of galaxies instead of relying on the projected celestial distribution. We then investigate the environmental dependence of galaxy properties with the projection corrected density and some well-defined populations of galaxies. At low redshift, clusters identified with red sequence galaxies are likely more developed, and cluster-specific quenching processes reduce their star-forming activity. However, at high redshift, clusters are younger and have not evolved well yet. We also find that “close companion galaxies” are inducing star formation activity. Moreover, there is a positive correlation between star formation rates and over-densities at 𝑧 ∼ 0.4 and 1.5 particularly in high-density regions, which is dominated by the effect of increasing stellar masses towards high density environments. Such trends are weak or absent locally in star-forming galaxies.