A prolonged plateau-to-tail transition in the Type II supernova SN2025abyc

@misc{li2026prolonged,
  title = {{A prolonged plateau-to-tail transition in the Type II supernova SN2025abyc}},
  author = {Luhan Li and Bo Wang and Jujia Zhang and Zhengyang Zhang and Xinjie Luo and Shiyang Dong and Saien Xu and Zhengwei Liu and Zhanwen Han},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.11031},
  eprint = {2609.11031},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.11031},
}

TY  - UNPB
TI  - A prolonged plateau-to-tail transition in the Type II supernova SN2025abyc
AU  - Luhan Li
AU  - Bo Wang
AU  - Jujia Zhang
AU  - Zhengyang Zhang
AU  - Xinjie Luo
AU  - Shiyang Dong
AU  - Saien Xu
AU  - Zhengwei Liu
AU  - Zhanwen Han
PY  - 2026
DA  - 2026/09/10
PB  - arXiv
DO  - 10.48550/arxiv.2609.11031
UR  - https://arxiv.org/abs/2609.11031
AB  - We present optical photometric and spectroscopic observations of the Type II supernova SN2025abyc. During the optically thick phase between approximately 10 and 70 d after explosion, its light curves show strongly wavelength-dependent decline rates of approximately 2.7, 2.1, 0.9, and 0.8 mag/100d in the g, c, r, and o bands, respectively. At approximately 70 d, the light curves begin to depart from their nearly linear plateau evolution and gradually transition toward the radioactive tail. A Fermi-Dirac fit to the well-sampled ATLAS o-band light curve yields a transition midpoint of t_PT ~ 100.5d. The interval between the end of the linear plateau and this transition midpoint is approximately 30 d, indicating a prolonged plateau-to-tail transition. This timescale is comparable to those measured for SN2013by, SN2013ej, and SN2014G. Spectroscopically, at +13 d post-explosion, the Halpha profile appears weak and broad, whereas Hbeta and Hgamma display clear P-Cygni profiles. This morphology can be explained by the normal early spectroscopic evolution of SNe II, although partial filling of the Halpha absorption trough by emission associated with circumstellar interaction cannot be excluded. SN2025abyc otherwise follows the general photospheric velocity evolution of SNe II, while remaining toward the high-velocity side of the comparison distribution in Halpha, Hbeta, and FeII. Exploratory light-curve modelling suggests a synthesized Ni mass of approximately 0.03-0.04 solar mass. We suggest that the extended circumstellar environment, Ni distribution, and hydrogen-envelope structure could all play a role in shaping the observed light-curve evolution, particularly the prolonged plateau-to-tail transition.
ER  -