揭示年轻 Iax 型超新星残留物 Pa 30 的膨胀特性

Tim Cunningham, Ilaria Caiazzo, Nikolaus Z. Prusinski, James Fuller, John C. Raymond, S. R. Kulkarni, James D. Neill, Paul Duffell, Chris Martin, Odette Toloza, David Charbonneau, Scott J. Kenyon, Zeren Lin, Mateusz Matuszewski, Rosalie McGurk, Abigail Polin and Philippe Z. Yao
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摘要

最近发现的 Pa 30 星云是与公元 1181 年历史超新星相关的推定 Iax 型超新星残余物,它显示出令人费解的特征,使其在已知超新星残余物中独一无二。特别是,Pa 30呈现出一种复杂的形态,具有独特的径向和丝状结构,其中心有一颗炙热的恒星残余,显示出以氧为主的超快风。由于残余恒星的存在以及其丝状结构中氢和氦的缺乏,有人认为Pa 30是近白矮星或超白矮星热核爆炸失败的产物,它产生了一个亚光速瞬变体,是Ia类超新星中一种罕见的亚型,被称为Iax型。我们在此详细研究了该残余物全径向截面的三维结构和速度。利用凯克宇宙网成像仪光谱仪的新红色通道获得的积分场单元观测结果显示,喷出物与弹道一致,速度接近自由膨胀速度。此外,我们还探测到超新星残余物内部有一个巨大的空腔,丝状结构的内侧有一个尖锐的边缘,这与红外图像中探测到的亮环的外侧边缘相吻合。最后,我们探测到沿视线方向的喷出物数量存在强烈的不对称性,这可能暗示了一次不对称爆炸。我们的分析有力地证实了爆炸源自 SN 1181。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Expansion Properties of the Young Supernova Type Iax Remnant Pa 30 Revealed
The recently discovered Pa 30 nebula, the putative type Iax supernova remnant associated with the historical supernova of 1181 AD, shows puzzling characteristics that make it unique among known supernova remnants. In particular, Pa 30 exhibits a complex morphology, with a unique radial and filamentary structure, and it hosts a hot stellar remnant at its center, which displays oxygen-dominated, ultrafast winds. Because of the surviving stellar remnant and the lack of hydrogen and helium in its filaments, it has been suggested that Pa 30 is the product of a failed thermonuclear explosion in a near- or super-Chandrasekhar white dwarf, which created a subluminous transient, a rare subtype of the Ia class of supernovae called type Iax. We present here a detailed study of the 3D structure and velocities of a full radial section of the remnant. The Integral Field Unit observations, obtained with the new red channel of the Keck Cosmic Web Imager spectrograph, reveal that the ejecta are consistent with being ballistic, with velocities close to the free-expansion velocity. Additionally, we detect a large cavity inside the supernova remnant and a sharp inner edge to the filamentary structure, which coincides with the outer edge of a bright ring detected in infrared images. Finally, we detect a strong asymmetry in the amount of ejecta along the line of sight, which might hint at an asymmetric explosion. Our analysis provides strong confirmation that the explosion originated from SN 1181.
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