The Proper Motion of the Neutron Star in Cassiopeia A
The Proper Motion of the Neutron Star in Cassiopeia A
复制标题
仙后座 A 中子星的自行运动
DOI：
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发表时间：
2013
期刊：
影响因子：
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通讯作者：
J. Satterfield
中科院分区：
文献类型：
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作者：
T. Delaney;J. Satterfield
钱德拉X射线天文台的高分辨率相机拍摄的图像被用来测量仙后座A中子星星在10年（1999-2009）基线内的自行。选择一个背景源和13个准静止的絮状物来配准两个图像。每个时期的特征之间的像素偏移使用四种不同的统计方法测量：高斯拟合，质心，互相关，和现金统计。在许多情况下，偏移测量在幅度和/或方向上相差多达1角秒，导致很大的不确定性。因此，对中子星星运动的测量结果是东南方向390 +/- 400 km/s的边缘。这种运动是典型的年轻中子星的诞生速度，并且与基于中子星星偏离光学喷出物膨胀中心的推断的自行一致。
Images from the High Resolution Camera on the Chandra X-ray Observatory were used to measure the proper motion of the neutron star in Cassiopeia A over a baseline of 10 years (1999-2009). One background source and 13 quasi-stationary flocculi were chosen to register the two images. Pixel offsets between features at each epoch were measured using four different statistical methods: Gaussian fitting, centroiding, cross correlation, and the Cash statistic. In many cases the offset measurements disagree in magnitude and/or direction by as much as 1 arcsecond, resulting in large uncertainties. As a result, the measurement for the motion of the neutron star is marginal at 390 +/- 400 km/s in the southeast direction. This motion is typical of the birth velocities of young pulsars and is consistent with the inferred proper motion based on the offset of the neutron star from the center of expansion of the optical ejecta.