SN 2025qe: A case study of diversity in low-luminosity thermonuclear explosions
Abstract
We present optical photometric and spectroscopic observations of SN 2025qe, a Type Iax supernova in IC 0529, monitored from −10 to +150 rest-frame days relative to g'-band maximum using the GROWTH-India and the Himalayan Chandra Telescopes. SN 2025qe reaches a peak g'-band absolute magnitude of Mg' ≈ −16.16 ± 0.15 mag, placing it in the sparsely sampled luminosity gap between the brightest and faintest members of the SNe Iax class. The multiband light curves show pronounced wavelength-dependent broadening at late times, with the redder bands remaining brighter than in other SNe Iax. Semi-analytical (Arnett) modeling of the pseudobolometric light curve yields a synthesized 56Ni mass of 0.02 M⊙, an ejecta mass of 0.45 M⊙, and a kinetic energy of 7.0× 1049 erg. Three-dimensional pure-deflagration models of Chandrasekhar-mass carbon-oxygen white dwarfs reproduce the peak luminosity and 56Ni yield but underpredict the slow, red post-maximum decline; models including energy input from a bound remnant better match the late-time evolution, especially in the red bands. We model early-time spectra using TARDIS with a modified deflagration model and identify late-time spectral features using syn++. We qualitatively try to explain the persistent red-band flux with a two-component ejecta structure comprising a dense inner region, possibly including a bound remnant, and a density-enhanced outer shell that sustains redder emission. Together, the photometric and spectroscopic properties of SN 2025qe highlight the diversity of ejecta structure and evolution among SNe Iax with similar peak luminosities, emphasizing the need for detailed observations and modeling of their ejecta.
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BibTeX
@misc{das20262025qe,
title = {{SN 2025qe: A case study of diversity in low-luminosity thermonuclear explosions}},
author = {Hrishav Das and Anirban Dutta and Devendra K. Sahu and G. C. Anupama and Prathamesh S. Kadam and Vishwajeet Swain},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.35720},
eprint = {2609.35720},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.35720},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - SN 2025qe: A case study of diversity in low-luminosity thermonuclear explosions
AU - Hrishav Das
AU - Anirban Dutta
AU - Devendra K. Sahu
AU - G. C. Anupama
AU - Prathamesh S. Kadam
AU - Vishwajeet Swain
PY - 2026
DA - 2026/09/28
PB - arXiv
DO - 10.48550/arxiv.2609.35720
UR - https://arxiv.org/abs/2609.35720
AB - We present optical photometric and spectroscopic observations of SN 2025qe, a Type Iax supernova in IC 0529, monitored from −10 to +150 rest-frame days relative to g'-band maximum using the GROWTH-India and the Himalayan Chandra Telescopes. SN 2025qe reaches a peak g'-band absolute magnitude of M_g' ≈ −16.16 ± 0.15 mag, placing it in the sparsely sampled luminosity gap between the brightest and faintest members of the SNe Iax class. The multiband light curves show pronounced wavelength-dependent broadening at late times, with the redder bands remaining brighter than in other SNe Iax. Semi-analytical (Arnett) modeling of the pseudobolometric light curve yields a synthesized ^56Ni mass of 0.02 M_⊙, an ejecta mass of 0.45 M_⊙, and a kinetic energy of 7.0× 10^49 erg. Three-dimensional pure-deflagration models of Chandrasekhar-mass carbon-oxygen white dwarfs reproduce the peak luminosity and ^56Ni yield but underpredict the slow, red post-maximum decline; models including energy input from a bound remnant better match the late-time evolution, especially in the red bands. We model early-time spectra using TARDIS with a modified deflagration model and identify late-time spectral features using syn++. We qualitatively try to explain the persistent red-band flux with a two-component ejecta structure comprising a dense inner region, possibly including a bound remnant, and a density-enhanced outer shell that sustains redder emission. Together, the photometric and spectroscopic properties of SN 2025qe highlight the diversity of ejecta structure and evolution among SNe Iax with similar peak luminosities, emphasizing the need for detailed observations and modeling of their ejecta.
ER -