TY - JOUR
T1 - Bridging between type IIb and Ib supernovae
T2 - SN IIb 2022crv with a very thin hydrogen envelope
AU - Gangopadhyay, Anjasha
AU - Maeda, Keiichi
AU - Singh, Avinash
AU - Nayana, A. J.
AU - Nakaoka, Tatsuya
AU - Kawabata, Koji S.
AU - Taguchi, Kenta
AU - Singh, Mridweeka
AU - Chandra, Poonam
AU - Ryder, Stuart D.
AU - Dastidar, Raya
AU - Yamanaka, Masayuki
AU - Kawabata, Miho
AU - Alsaberi, Rami Z. E.
AU - Dukiya, Naveen
AU - Teja, Rishabh Singh
AU - Ailawadhi, Bhavya
AU - Dutta, Anirban
AU - Sahu, D. K.
AU - Moriya, Takashi J.
AU - Misra, Kuntal
AU - Tanaka, Masaomi
AU - Chevalier, Roger
AU - Tominaga, Nozomu
AU - Uno, Kohki
AU - Imazawa, Ryo
AU - Hamada, Taisei
AU - Hori, Tomoya
AU - Isogai, Keisuke
N1 - Copyright © 2023. The Author(s). Published by the American Astronomical Society. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.
PY - 2023/11/1
Y1 - 2023/11/1
N2 - We present optical, near-infrared, and radio observations of supernova (SN) SN IIb 2022crv. We show that it retained a very thin H envelope and transitioned from an SN IIb to an SN Ib; prominent Hα seen in the pre-maximum phase diminishes toward the post-maximum phase, while He i lines show increasing strength. SYNAPPS modeling of the early spectra of SN 2022crv suggests that the absorption feature at 6200 Å is explained by a substantial contribution of Hα together with Si ii, as is also supported by the velocity evolution of Hα. The light-curve evolution is consistent with the canonical stripped-envelope SN subclass but among the slowest. The light curve lacks the initial cooling phase and shows a bright main peak (peak MV = −17.82 ± 0.17 mag), mostly driven by radioactive decay of 56Ni. The light-curve analysis suggests a thin outer H envelope (Menv ∼ 0.05 M⊙) and a compact progenitor (Renv ∼ 3 R⊙). An interaction-powered synchrotron self-absorption model can reproduce the radio light curves with a mean shock velocity of 0.1c. The mass-loss rate is estimated to be in the range of (1.9−2.8) × 10−5 M⊙ yr−1 for an assumed wind velocity of 1000 km s−1, which is on the high end in comparison with other compact SNe IIb/Ib. SN 2022crv fills a previously unoccupied parameter space of a very compact progenitor, representing a beautiful continuity between the compact and extended progenitor scenario of SNe IIb/Ib.
AB - We present optical, near-infrared, and radio observations of supernova (SN) SN IIb 2022crv. We show that it retained a very thin H envelope and transitioned from an SN IIb to an SN Ib; prominent Hα seen in the pre-maximum phase diminishes toward the post-maximum phase, while He i lines show increasing strength. SYNAPPS modeling of the early spectra of SN 2022crv suggests that the absorption feature at 6200 Å is explained by a substantial contribution of Hα together with Si ii, as is also supported by the velocity evolution of Hα. The light-curve evolution is consistent with the canonical stripped-envelope SN subclass but among the slowest. The light curve lacks the initial cooling phase and shows a bright main peak (peak MV = −17.82 ± 0.17 mag), mostly driven by radioactive decay of 56Ni. The light-curve analysis suggests a thin outer H envelope (Menv ∼ 0.05 M⊙) and a compact progenitor (Renv ∼ 3 R⊙). An interaction-powered synchrotron self-absorption model can reproduce the radio light curves with a mean shock velocity of 0.1c. The mass-loss rate is estimated to be in the range of (1.9−2.8) × 10−5 M⊙ yr−1 for an assumed wind velocity of 1000 km s−1, which is on the high end in comparison with other compact SNe IIb/Ib. SN 2022crv fills a previously unoccupied parameter space of a very compact progenitor, representing a beautiful continuity between the compact and extended progenitor scenario of SNe IIb/Ib.
UR - http://www.scopus.com/inward/record.url?scp=85176949883&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/acfa94
DO - 10.3847/1538-4357/acfa94
M3 - Article
AN - SCOPUS:85176949883
SN - 0004-637X
VL - 957
SP - 1
EP - 21
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 100
ER -