发表机构
University of Szeged; MTA-ELTE Lendület “Momentum” Milky Way Research Group; Caltech/IPAC; Baja Astronomical Observatory of University of Szeged; HUN-REN–SZTE Stellar Astrophysics Research Group; HUN-REN Research Centre for Astronomy and Earth Sciences, Konkoly Observatory; CSFK, MTA Centre of Excellence, Konkoly Thege Miklós út 15-17, 1121 Budapest, Hungary; Department of Astronomy, University of California, Berkeley（塞格德大学; MTA-ELTE 引力“动量”银河系研究组; 加州理工学院/IPAC; 塞格德大学巴贾天文台; 匈牙利研究与教育网络–塞格德大学恒星天体物理学研究组; 匈牙利研究与教育网络天文学与地球科学研究中心，孔科利天文台; CSFK，匈牙利科学院卓越中心; 加州大学伯克利分校天文学系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究分析近邻过渡型IIb/Ib超新星SN 2026dix，通过光变曲线、光谱及前身星建模，揭示其源于相互作用双星系统中的暖超巨星爆炸，为SESN连续分布提供新证据。
AI 中文摘要
理解（极）大质量恒星最终演化阶段及其爆炸产物——剥离包层超新星（SESNe），一直是天体物理学面临的长期挑战。最新研究结果支持传统SESN子类（IIb、Ib、Ic）之间存在连续分布。近邻（$D \approx 17.5$ Mpc）的SN 2026dix似乎是最近发现的过渡型IIb/Ib爆炸群中的又一成员。在多张爆炸前{\it HST}图像的误差范围内，SN位置处探测到一个点源。结合爆炸后的测光和光谱数据，这为详细研究这一罕见超新星类型提供了良好机会。我们对SN 2026dix进行了全面的比较光变曲线（LC）和光谱分析，构建了其热光度光变曲线并进行了半解析建模。此外，我们还构建了假定前身星的谱能量分布，并将其与模型恒星大气和双星演化轨迹进行了比较。我们推断SN 2026dix起源于相互作用双星系统中的爆炸，其性质与一颗温暖的（$T_\textrm{eff} \approx 6750-7750$ K；光谱型F2至A7）、明亮的（$\log(L_{\rm bol}/L_{\odot})\approx 4.9-5.3$）超巨星主星以及一颗光度较低、质量较小的热矮伴星相符。所识别前身星的性质与一些其他已知SNe IIb案例非常相似，并且与我们的半解析光变曲线建模结果以及将SN 2026dix的光变曲线和光谱与$M_\textrm{ini}$ = 18 $M_{\odot}$爆炸恒星的辐射转移模型输出进行比较的结果高度一致。
英文摘要
Understanding the final evolution stages of (very) massive stars and their explosive outcomes, stripped-envelope supernovae (SESNe), represent a long-term challenge for astrophysics. The latest results support a continuous distribution within the traditional SESN subclasses (IIb, Ib, Ic). The nearby ($D \approx 17.5$ Mpc) SN 2026dix seems to be another member of the recently identified group of transitional Type IIb/Ib explosions. A point source is located at the SN position within the uncertainties on multiple pre-explosion {\it HST} images. Together with post-explosion photometry and spectroscopy, it provides a good opportunity to study a rare type of SN in detail. We carried out a thorough comparative light-curve (LC) and spectral analysis of SN 2026dix. We also constructed its bolometric LC and modeled it semi-analytically. In addition, we constructed the spectral energy distribution of the presumed progenitor and compared this to model stellar atmospheres and binary stellar evolution tracks. We infer that SN 2026dix arose from an explosion in an interacting binary system, consistent with the properties of a warm ($T_\textrm{eff} \approx 6750-$7750 K; spectral type F2 to A7), luminous ($\log(L_{\rm bol}/L_{\odot})\approx 4.9-5.3$) supergiant primary and a less luminous, less massive hot dwarf companion. The nature of the identified progenitor closely resembles that of some other known cases of SNe IIb and also well aligns with both the results of our semi-analytical LC modeling and the comparison of the LCs and spectra of SN 2026dix with the output of radiative-transfer models of an exploding star with $M_\textrm{ini}$ = 18 $M_{\odot}$.
Comments20 pages, 16 figures, 7 tables; submitted to A&A
