[论文解读] The fate of the failed supernova candidate M31-2014-DS1

Emma R. Beasor, Nathan K. Smith+5 more|arXiv (Cornell University)|Jan 8, 2026

Gamma-ray bursts and supernovae被引用 0

一句话总结

该论文报告了对M31-2014-DS1的JWST、SMA和Chandra观测，显示一个持续存在的中红外源，存在大量尘埃遮挡，反对简单的失败超新星解释，并考虑恒星并合情景作为备选。

ABSTRACT

The fate of massive stars above 20M$_{\odot}$ remains uncertain. Debate persists about whether they die as supernovae (SNe), or if they collapse directly into black holes (BHs) with little or no optical outburst -- so-called ``failed supernovae''. The source M31-2014-DS1 experienced an optical outburst in 2014 and has remained faint at visual wavelengths since then. Due to its persistent faintness, it has been proposed as a failed SN candidate. We present new observations of this candidate obtained using the James Webb Space Telescope (JWST), the Submillimeter Array (SMA), and Chandra. The JWST observations demonstrate that a luminous mid-infrared source persists at the same location a decade after the star faded at visual wavelengths. We model its current spectral energy distribution (SED) as a dust-enshrouded star. No X-ray emission is detected, disfavoring the hypothesis that the late-time luminosity is powered by accretion onto a BH. We find that the remaining source is highly obscured by an asymmetric distribution of circumstellar dust, making it difficult to quantify its physical properties using spherically symmetric radiative transfer codes. The dust geometry requires that the inferred bolometric luminosity is only a lower limit, as a significant fraction of the central source's radiation may escape without being reprocessed by dust. We discuss the implications of these findings in the context of failed SN models and consider the potential overlap with signatures expected from a stellar merger, which also seems to provide a plausible explanation of this source.

研究动机与目标

• 调查在2014年爆发后，M31-2014-DS1 是否为真正的失败超新星。
• 结合JWST、SMA和Chandra数据表征当前的光谱能量分布（SED）。
• 评估尘几何结构及其对总辐射光度估计的影响。
• 将观测结果与理论的失败超新星模型和恒星并合情景进行比较。
• 判定是否存在X射线辐射以支持或反驳对黑洞的回落吸积。

提出的方法

• 通过JWST的NIRSpec和MIRI光谱与拍摄在1–14 μm范围内构建当前的SED。
• 在209.5–241.5 GHz进行SMA观测，以在源位置搜索射电发射。
• 利用Chandra ACIS-S X射线观测约束高能发射。
• 使用DUSTY辐射传输建模，假设球对称以拟合较冷的尘埃成分。
• 采用两组分SED建模以模拟非对称尘埃分布和消光效应。
• 将观测到的SED与未检测到的情况与失败超新星和并合情景的预测进行比较。

实验结果

研究问题

• RQ1 M31-2014-DS1 是否呈现光学瞬变或持续的X射线信号，与失败超新星图景相一致？
• RQ2 剩余源是否为尘埃包裹的恒星，其总辐射光度因非对称几何而为下限？
• RQ3 单源球对称辐射传输模型是否能再现完整的JWST SED，还是需要多分量建模？
• RQ4 观测结果更支持失败超新星情景、恒星并合，还是该对象的其他瞬变通道？
• RQ5 尘埃几何对在失败超新星候选对象中解读晚期光度有何影响？

主要发现

• 在光学衰退十年后，同一位置仍存在一个明亮的中红外源。
• 未检测到X射线发射，使得以吸积驱动的黑洞晚期光度成为唯一来源的可能性降低。
• 尘埃几何极可能高度非对称，使球对称模型拟合不佳，暗示总辐射光度为下限。
• SED 至少需要两组分以同时解释热的近红外和较冷的中红外发射。
• 在约10 μm处的硅酸盐吸收指示沿视线存在大量冷的恒星周尘埃。
• 长波长（>10 μm）通量长期保持近似不变，与简单的全局光度下降不一致。