SN 2025aedz: A typical short-plateau type IIP supernova with rapid post-peak decline
Abstract
Type IIP supernovae (SNe IIP) are the most common subclass of core-collapse SNe in observations. However, SNe IIP with short plateaus of the order of tens of days are rarely observed. The progenitors for this kind of SN can help to address the red supergiant issue in stellar evolution. In this article, we report optical photometry and spectroscopy of SN\,2025aedz, a rapidly post-peak declining SN IIP with a typical short plateau. It exhibits a peak absolute magnitude of Mr=−17.16±0.03\,mag. The r-band light curve shows a steep early post-peak decline of ∼5 mag (100 d)−1 followed by a relatively short plateau, with a plateau duration of ∼50±3\,d. The overall spectral evolution is consistent with that of normal SNe~IIP, showing a blue continuum with prominent Balmer P-Cygni profiles during the photospheric phase, followed by the gradual strengthening of hydrogen and metal lines as the ejecta cools down, although the metal lines remain weak and the expansion velocities decline rapidly. SN\,2025aedz is similar to the short-plateau SN\,2018gj in its overall evolution, whereas its pronounced early decline resembles that of SN\,2023ufx, which has the shortest plateau duration known so far. The radioactive tail of the bolometric light curve implies a synthesized 56Ni mass of ∼0.03±0.01 M⊙. Motivated by the steep early decline, we performed radiation hydrodynamic simulations by exploring different circumstellar material configurations to reproduce its early bolometric light curve. These simulations indicate that SN\,2025aedz originated from a progenitor with a relatively low-mass hydrogen envelope, possibly produced through enhanced mass loss or binary interaction, while the steep early decline is likely explained by additional luminosity from circumstellar interaction.
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BibTeX
@misc{wang20262025aedz,
title = {{SN 2025aedz: A typical short-plateau type IIP supernova with rapid post-peak decline}},
author = {Bo Wang and Luhan Li and Chengyuan Wu and Jujia Zhang and Yongzhi Cai and Yize Dong and Xuefei Chen and Zhanwen Han},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.29139},
eprint = {2609.29139},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.29139},
}
RIS
TY - UNPB
TI - SN 2025aedz: A typical short-plateau type IIP supernova with rapid post-peak decline
AU - Bo Wang
AU - Luhan Li
AU - Chengyuan Wu
AU - Jujia Zhang
AU - Yongzhi Cai
AU - Yize Dong
AU - Xuefei Chen
AU - Zhanwen Han
PY - 2026
DA - 2026/09/24
PB - arXiv
DO - 10.48550/arxiv.2609.29139
UR - https://arxiv.org/abs/2609.29139
AB - Type IIP supernovae (SNe IIP) are the most common subclass of core-collapse SNe in observations. However, SNe IIP with short plateaus of the order of tens of days are rarely observed. The progenitors for this kind of SN can help to address the red supergiant issue in stellar evolution. In this article, we report optical photometry and spectroscopy of SN\,2025aedz, a rapidly post-peak declining SN IIP with a typical short plateau. It exhibits a peak absolute magnitude of M_r=−17.16±0.03\,mag. The r-band light curve shows a steep early post-peak decline of ∼5 mag (100 d)^−1 followed by a relatively short plateau, with a plateau duration of ∼50±3\,d. The overall spectral evolution is consistent with that of normal SNe~IIP, showing a blue continuum with prominent Balmer P-Cygni profiles during the photospheric phase, followed by the gradual strengthening of hydrogen and metal lines as the ejecta cools down, although the metal lines remain weak and the expansion velocities decline rapidly. SN\,2025aedz is similar to the short-plateau SN\,2018gj in its overall evolution, whereas its pronounced early decline resembles that of SN\,2023ufx, which has the shortest plateau duration known so far. The radioactive tail of the bolometric light curve implies a synthesized ^56Ni mass of ∼0.03±0.01 M_⊙. Motivated by the steep early decline, we performed radiation hydrodynamic simulations by exploring different circumstellar material configurations to reproduce its early bolometric light curve. These simulations indicate that SN\,2025aedz originated from a progenitor with a relatively low-mass hydrogen envelope, possibly produced through enhanced mass loss or binary interaction, while the steep early decline is likely explained by additional luminosity from circumstellar interaction.
ER -