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Abstract:

Supernovae (SNe) are explosive events that occur at the end of the life of massive stars, exhibiting a variety of features in their spectra, primarily depending on their chemical abundances. Some SNe show narrow emission lines in their spectra, which suggests the presence of a dense, slowly-moving circumstellar medium (CSM) around the progenitor. Recent observations indicate that most progenitors of Type II SNe have a confined CSM, making the study of the CSM associated with massive stars crucial for understanding stellar evolution. Although a detailed mechanism that forms the massive CSM is still uncertain, several scenarios have been proposed, including core neutrino emission, burning instability, and pulsational pair-instability. In this talk, I will explain how the CSM affects the observed light curve of interaction-powered SNe and how we can extract the density profile of the CSM, which may vary depending on its formation process. Specifically, I will introduce a newly developed open-source code, Complete History of Interaction-Powered Supernovae (CHIPS), which is suited to model a wide variety of transients that arise from interaction with a CSM. Contrary to existing modelings, which mostly attach the CSM by hand, CHIPS self-consistently simulates both the creation of the CSM from mass eruption of massive stars prior to core-collapse, and the subsequent SN light curve