论文标题
光学发射，高速，富氧弹出的三维运动学重建
Three-Dimensional Kinematic Reconstruction of the Optically-Emitting, High-Velocity, Oxygen-Rich Ejecta of Supernova Remnant N132D
论文作者
论文摘要
我们提出了大型麦哲伦云中超新星残留N132D的光发射，富氧弹出的三维运动学重建。 Data were obtained with the 6.5 m Magellan telescope in combination with the IMACS+GISMO instrument and survey [O III] $λλ$4959,5007 line emission in a ${\sim}$3$^{\prime}~\times$ 3$^{\prime}$ region centered on N132D.我们数据的空间和光谱分辨率可以详细检查光弹出结构。 N132D的大部分光亮氧气弹出量都以圆环的几何形状排列，相对于天空平面，大约28 $^{\ circ} $倾斜了大约28 $^{\ circ} $。圆环的半径为4.4 pc（$ d _ {\ rm lmc} $/50 kpc），表现出蓝移的径向速度不对称的$ -3000 $ -3000 $至$+2300 $+2300 $ km s $^{ - 1} $，并且在周围中有明显的休息。假设O富含丝的几何中心从几何中心进行了同源扩展，则自爆炸2450 $ \ pm $ 195年以来，平均膨胀速度为1745 km s $^{ - 1} $。一个微弱的，空间分离的“失控结”（RK），总空间速度为3650 km s $^{ - 1} $几乎垂直于圆环飞机，并且与X射线发射相吻合，而SI相对于LMC和N132D的Bulk siement而言，SI在SI中大大增强。这些运动学和化学特征表明RK可能起源于祖细胞之恒。总体而言，N132D的主要壳形态和高速度，富含Si富集的成分与Cassiopeia A的相似性是显着的，这是IIB型超新星爆炸型的结果。我们的结果强调了需要进行进一步观察和模拟的必要性，这些观察和模拟可以稳健地协调观察到的形态是由爆炸动力学主导还是通过与环境的相互作用来塑造。
We present a three-dimensional kinematic reconstruction of the optically-emitting, oxygen-rich ejecta of supernova remnant N132D in the Large Magellanic Cloud. Data were obtained with the 6.5 m Magellan telescope in combination with the IMACS+GISMO instrument and survey [O III] $λλ$4959,5007 line emission in a ${\sim}$3$^{\prime}~\times$ 3$^{\prime}$ region centered on N132D. The spatial and spectral resolution of our data enable detailed examination of the optical ejecta structure. The majority of N132D's optically bright oxygen ejecta are arranged in a torus-like geometry tilted approximately 28$^{\circ}$ with respect to the plane of the sky. The torus has a radius of 4.4 pc ($D_{\rm LMC}$/50 kpc), exhibits a blue-shifted radial velocity asymmetry of $-3000$ to $+2300$ km s$^{-1}$, and has a conspicuous break in its circumference. Assuming homologous expansion from the geometric center of O-rich filaments, the average expansion velocity of 1745 km s$^{-1}$ translates to an age since explosion of 2450 $\pm$ 195 yr. A faint, spatially-separated "runaway knot" (RK) with total space velocity of 3650 km s$^{-1}$ is nearly perpendicular to the torus plane and coincident with X-ray emission that is substantially enhanced in Si relative to the LMC and N132D's bulk ejecta. These kinematic and chemical signatures suggest that the RK may have had its origin deep within the progenitor star. Overall, the main shell morphology and high-velocity, Si-enriched components of N132D have remarkable similarity with that of Cassiopeia A, which was the result of a Type IIb supernova explosion. Our results underscore the need for further observations and simulations that can robustly reconcile whether the observed morphology is dominated by explosion dynamics or shaped by interaction with the environment.
