In this talk, I will present the multi-wavelength observations concerning photometry, spectroscopy, and polarimetry of the nearest SN of the decade, SN 2023ixf. I will primarily explore the significance of polarimetry and hydrodynamical modeling in understanding the complex nature of core-collapse supernovae. Polarization provides crucial insights into the geometry of the supernova ejecta and the circumstellar matter (CSM), revealing the dynamics at play during and after the explosion. Hydrodynamical modeling, on the other hand, enables us to simulate the physical conditions of the progenitor star and its environment, helping to reconstruct the mass-loss history and the explosion parameters.Building on this framework, the polarimetric observations revealed three distinct peaks post-explosion. These peaks indicate a highly asymmetric dense CSM, an aspherical shock front, and/or clumpiness within the extended CSM, as well as asymmetry in the inner ejecta and He-core. The evolution of polarization in time exhibits two axes of asymmetry: one linked to the CSM and outer ejecta and the other to the inner ejecta/He-core, suggesting independent origins of asymmetry in the early and late evolution of SN2023ixf. Complementing these observations, hydrodynamical modeling suggested a two-zone CSM structure consisting of a dense inner region with a significant mass-loss rate and a more extended outer region with a lower mass-loss rate. Spectroscopic data further supported the presence of an aspherical shock front, evidenced by high-velocity broad absorption features in the Balmer lines. Together, these findings point to a red supergiant progenitor star with a mass of around 10 solar mass, having enhanced stages of mass loss closer to the explosion, offering new insights into the intricate dynamics and complex environments of hydrogen-rich supernovae.