标题： 脉冲星在超新星遗迹 G18.9-1.1 中的自行运动 显示英文标题

标题： Proper Motion of the Neutron Star in the Supernova Remnant G18.9-1.1

摘要： 在本文中，我们使用15年的钱德拉观测基线，首次直接测量了超新星遗迹G18.9-1.1中的中子星（NS）的自行。在使用参考盖亚恒星的位置校正观测的天体测量解后，我们测得总自行速度为24.7 $\pm$ 6.8 毫角秒年$^{-1}$，方向为$336^\circ \pm$ 16$^\circ$ 北偏东。 使用文献中的距离估计值2.1 kpc和3.8 kpc，这个自行对应于银河系旋转校正后的横向速度分别为264d$_{2.1}$ $\pm$ 79 km s$^{-1}$和474d$_{3.8}$$\pm$129 km s$^{-1}$。 我们对SNR抛射物的功率比方法分析略微支持较高的速度，因为使用更远的距离反向演化中心计算出的多极矩与其他CCSNRs的值更加一致。 中子星的运动方向与G18.9$-$1.1中整体抛射物的运动方向直接相反，这进一步证明了中子星的踢动是通过中子星和抛射物之间的动量守恒类似过程产生的，这在其他超新星遗迹中已有观察结果。 显示英文摘要

摘要： In this paper, we present the first direct measurement of the proper motion of the neutron star (NS) in the supernova remnant (SNR) G18.9-1.1 using a 15-year Chandra baseline. After correcting the observations' astrometric solutions using reference Gaia stars' positions, we measure a total proper motion of 24.7 $\pm$ 6.8 mas yr$^{-1}$ at an angle of $336^\circ \pm$ 16$^\circ$ east of north. Using the distance estimates from literature of 2.1 kpc and 3.8 kpc, this proper motion corresponds to Galactic rotation-corrected transverse velocities of 264d$_{2.1}$ $\pm$ 79 km s$^{-1}$ and 474d$_{3.8}$ $\pm$ 129 km s$^{-1}$, respectively. Our power ratio method analysis of SNR ejecta slightly favors the higher velocity, as multipole moments calculated from the back-evolved center using the farther distance are more consistent with values from other CCSNRs. The NS's motion is directly opposite the motion of bulk ejecta in G18.9$-$1.1, providing yet more evidence that NS kicks are generated via a conservation of momentum-like process between the NS and the ejecta, as has been observed in other SNRs.