SN 2025qe：低光度热核爆炸多样性案例研究
SN 2025qe: A case study of diversity in low-luminosity thermonuclear explosions
- Indian Institute of Astrophysics（印度天体物理研究所）
- Pondicherry University（本地治里大学）
- National Central University（中央大学）
- Sardar Vallabhbhai National Institute of Technology（萨达尔·瓦拉巴伊国立理工学院）
- Indian Institute of Technology Bombay（孟买印度理工学院）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
本研究通过观测和建模Iax型超新星SN 2025qe，揭示其位于光度间隙，具有双组分抛射物结构，强调了低光度热核爆炸中抛射物多样性的重要性。
AI中文摘要：
我们展示了SN 2025qe的光学测光和光谱观测，这是一颗位于IC 0529星系中的Iax型超新星，使用GROWTH-India和喜马拉雅钱德拉望远镜，从相对于g'波段最大亮度的-10天到+150天（静止系）进行了监测。SN 2025qe达到峰值g'波段绝对星等M_g' ≈ -16.16 ± 0.15等，使其位于Iax型超新星中最亮和最暗成员之间稀疏采样的光度间隙中。多波段光变曲线在晚期表现出明显的波长依赖性展宽，其中红波段比其他Iax型超新星保持更亮。对伪热光变曲线进行半解析（Arnett）建模，得出合成的^56Ni质量为0.02 M_sun，抛射物质量为0.45 M_sun，动能为7.0×10^49 erg。钱德拉塞卡质量碳氧白矮星的三维纯爆燃模型能够重现峰值光度和^56Ni产量，但低估了缓慢的红色最大亮度后下降；包含束缚残骸能量输入的模型更好地匹配晚期演化，尤其是在红波段。我们使用TARDIS结合改进的爆燃模型对早期光谱进行建模，并使用syn++识别晚期光谱特征。我们定性尝试用双组分抛射物结构解释持续的红波段通量，该结构包括一个致密的内区（可能包含束缚残骸）和一个密度增强的外壳，以维持更红的辐射。总之，SN 2025qe的测光和光谱特性突显了具有相似峰值光度的Iax型超新星中抛射物结构和演化的多样性，强调了对它们的抛射物进行详细观测和建模的必要性。
英文摘要：
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 $M_{g'} \approx -16.16 \pm 0.15$ 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 $^{56}$Ni mass of $0.02\,M_\odot$, an ejecta mass of $0.45\,M_\odot$, and a kinetic energy of $7.0\times 10^{49}$ erg. Three-dimensional pure-deflagration models of Chandrasekhar-mass carbon-oxygen white dwarfs reproduce the peak luminosity and $^{56}$Ni 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.
