Barred galaxies are a common type of galaxies in the local universe, observed in over 60% of disk galaxies. The bar structure plays a significant role in determining galaxy substructures such as spiral arms, rings and central dust structures. It is also a crucial driver of the secular evolution of galaxies, redistributing the mass of gas, stars, and even dark matter: it drives gas into the central regions of galaxies, builds a pseudo- or boxy/peanut bulge, and can even elongate the dark matter halo. According to theoretical studies, in an isolated system, a bar structure rapidly forms when a stellar disk is unstable and grows by interacting with the dark matter halo. However, observations do not find evidence for the growth of bar structures in terms of their length, strength, and pattern speed, which induces tension between the distribution of dark matter in simulations and observations. Furthermore, galaxy interactions that induce barred galaxies add complexity to our understanding of barred galaxies. In this talk, I will introduce our recent and ongoing work on barred galaxies using photometry from SDSS, PS1, HST, DESI, and CFHT and spectroscopy from Gemini, CALIFA, MUSE, and JWST. Our work spans the methods to detect barred galaxies to their evolution in the context of their main properties: length, strength, and pattern speed. Lastly, I will introduce the important role of the KASI’s next projects, including K-DRIFT, LSST, and the DARWIN project, in the study of barred galaxies.