학술논문
The Prevalence and Influence of Circumstellar Material around Hydrogen-rich Supernova Progenitors
Document Type
article
Author
Rachel J. Bruch; Avishay Gal-Yam; Ofer Yaron; Ping Chen; Nora L. Strotjohann; Ido Irani; Erez Zimmerman; Steve Schulze; Yi Yang; Young-Lo Kim; Mattia Bulla; Jesper Sollerman; Mickael Rigault; Eran Ofek; Maayane Soumagnac; Frank J. Masci; Christoffer Fremling; Daniel Perley; Jakob Nordin; S. Bradley Cenko; Anna Y. Q. Ho; S. Adams; Igor Adreoni; Eric C. Bellm; Nadia Blagorodnova; Kevin Burdge; Kishalay De; Richard G. Dekany; Suhail Dhawan; Andrew J. Drake; Dmitry A. Duev; Matthew Graham; Melissa L. Graham; Jacob Jencson; Emir Karamehmetoglu; Mansi M. Kasliwal; Shrinivas Kulkarni; A. A. Miller; James D. Neill; Thomas A. Prince; Reed Riddle; Benjamin Rusholme; Y. Sharma; Roger Smith; Niharika Sravan; Kirsty Taggart; Richard Walters; Lin Yan
Source
The Astrophysical Journal, Vol 952, Iss 2, p 119 (2023)
Subject
Language
English
ISSN
1538-4357
Abstract
Narrow transient emission lines (flash-ionization features) in early supernova (SN) spectra trace the presence of circumstellar material (CSM) around the massive progenitor stars of core-collapse SNe. The lines disappear within days after the SN explosion, suggesting that this material is spatially confined, and originates from enhanced mass loss shortly (months to a few years) prior to the explosion. We performed a systematic survey of H-rich (Type II) SNe discovered within less than 2 days from the explosion during the first phase of the Zwicky Transient Facility survey (2018–2020), finding 30 events for which a first spectrum was obtained within 36% at the 95% confidence level) confirms that elevated mass loss in massive stars prior to SN explosion is common. We find that SNe II showing flash-ionization features are not significantly brighter, nor bluer, nor more slowly rising than those without. This implies that CSM interaction does not contribute significantly to their early continuum emission, and that the CSM is likely optically thin. We measured the persistence duration of flash-ionization emission and find that most SNe show flash features for ≈5 days. Rarer events, with persistence timescales >10 days, are brighter and rise longer, suggesting these may be intermediate between regular SNe II and strongly interacting SNe IIn.