The Early Light Curve of a Type Ia Supernova 2021hpr in NGC 3147: Progenitor Constraints with the Companion Interaction Model

• Published in: arXiv.org
• Main Authors: Lim, Gu, Im, Myungshin, Paek, Gregory S H, Sung-Chul Yoon, Choi, Changsu, Kim, Sophia, Wheeler, J Craig, Thomas, Benjamin P, Vinkó, Jozsef, Kim, Dohyeong, Seo, Jinguk, Kang, Wonseok, Kim, Taewoo, Hyun-Il Sung, Kim, Yonggi, Joh-Na Yoon, Kim, Haeun, Kim, Jeongmook, Bae, Hana, Ehgamberdiev, Shuhrat, Burhonov, Otabek, Mirzaqulov, Davron
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 09.03.2023
• Subjects: Color; Companion stars; Constraint modelling; Ejecta; Interaction models; Light; Light curve; Physics - Astrophysics of Galaxies; Physics - High Energy Astrophysical Phenomena; Physics - Solar and Stellar Astrophysics; Power law; Shock cooling; Spiral galaxies; Supernovae; White dwarf stars
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2303.05051

The progenitor system of Type Ia supernovae (SNe Ia) is expected to be a close binary system of a carbon/oxygen white dwarf (WD) and a non-degenerate star or another WD. Here, we present results from a high-cadence monitoring observation of SN 2021hpr in a spiral galaxy, NGC 3147, and constraints on the progenitor system based on its early multi-color light curve data. First, we classify SN 2021hpr as a normal SN Ia from its long-term photometric and spectroscopic data. More interestingly, we found a significant "early excess" in the light curve over a simple power-law \(\sim t^{2}\) evolution. The early light curve evolves from blue to red and blue during the first week. To explain this, we fitted the early part of \(BVRI\)-band light curves with a two-component model of the ejecta-companion interaction and a simple power-law model. The early excess and its color can be explained by shock cooling emission due to a companion star having a radius of $8.84\pm0.58$$R_{\odot}\(. We also examined HST pre-explosion images with no detection of a progenitor candidate, consistent with the above result. However, we could not detect signs of a significant amount of the stripped mass from a non-degenerate companion star (\)\lesssim0.003\,M_{\odot}\( for H\)\alpha$ emission). The early excess light in the multi-band light curve supports a non-degenerate companion in the progenitor system of SN 2021hpr. At the same time, the non-detection of emission lines opens a door for other methods to explain this event.