ASASSN-14ms: The Most Energetic Known Explosion of a Type Ibn Supernova and Its Physical Origin

• Published in: The Astrophysical journal 2021-08, Vol.917 (2), p.97
• Main Authors: Wang, Xiaofeng, Lin, Weili, Zhang, Jujia, Zhang, Tianmeng, Cai, Yongzhi, Zhang, Kaicheng, Filippenko, Alexei V., Graham, Melissa, Maeda, Keiichi, Mo, Jun, Xiang, Danfeng, Xi, Gaobo, Yan, Shengyu, Wang, Lifan, Wang, Lingjun, Kawabata, Koji, Zhai, Qian
• Format: Article
• Language: English
• Subjects: Astrophysics; Circumstellar dust; Ejecta; Helium; Light curve; Luminosity; Stellar mass loss; Supernova
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ac0c17

ASASSN-14ms may represent the most luminous Type Ibn supernova (SN Ibn) ever detected, with an absolute U -band magnitude brighter than −22.0 mag and a total bolometric luminosity >1.0 × 10 44 erg s −1 near maximum light. The early-time spectra of this SN are characterized by a blue continuum on which are superimposed narrow P Cygni profile lines of He i , suggesting the presence of slowly moving (∼1000 km s −1 ), He-rich circumstellar material (CSM). At 1–2 months after maximum brightness, the He i line profiles become only slightly broader, with blueshifted velocities of 2000–3000 km s −1 , consistent with the CSM shell being continuously accelerated by the SN light and ejecta. Like most SNe Ibn, the light curves of ASASSN-14ms show rapid post-peak evolution, dropping by ∼7 mag in the V band over three months. Such a rapid post-peak decline and high luminosity can be explained by interaction between SN ejecta and helium-rich CSM of 0.9 M ⊙ at a distance of ∼10 15 cm. The CSM around ASASSN-14ms is estimated to originate from a pre-explosion event with a mass-loss rate of 6.7 M ⊙ yr −1 (assuming a velocity of ∼1000 km s −1 ), which is consistent with abundant He-rich material violently ejected during the late Wolf–Rayet (WN9-11 or Opfe) stage. After examining the light curves for a sample of SNe Ibn, we find that the more luminous ones tend to have slower post-peak decline rates, reflecting that the observed differences may arise primarily from discrepancies in the CSM distribution around the massive progenitors.