通过HI吸收和自吸收，到SNR CTB 109/ AXP 1 E 2259+586的距离
Distance to the SNR CTB 109/AXP 1E 2259+586 by HI absorption and self-absorption
摘要：
通过分析超新星遗迹G109.1-1.0（CTB 109）、HII区Sh 152和邻近分子云复合体的21 cm HI线和12 CO线光谱，提出了一个与其相关的异常X射线脉冲星1 E 2259+586的修正距离。CTB 109已经被确定与一个大分子云相互作用（后退速度v=-55 km s^-1）。朝向CTB 109的吸收特征的最高径向速度（-56 km s^-1）和Sh 152（-65 km s^-1）大于复合线速度（-50 km s^-1），表明英仙座臂内的速度反转。分子云具有足够大的冷HI柱密度，可以产生HI自吸收（HISA）和HI窄自吸收（HINSA），如果它是在速度反转的近侧。HISA和HINSA的缺失表明云位于英仙座臂内速度反转的远侧，因此我们获得CTB 109的距离为4+/-0.8 kpc。新的距离仍然导致CTB 109/AXP 1 E 2259+586的正常爆炸能量。
英文摘要：
We suggest a revised distance to the supernova remnant (SNR) G109.1-1.0 (CTB 109) and its associated anomalous X-ray pulsar (AXP) 1E 2259+586 by analyzing 21cm HI-line and 12CO-line spectra of CTB 109, HII region Sh 152, and the adjacent molecular cloud complex. CTB 109 has been established to be interacting with a large molecular cloud (recession velocity at v=-55 km s^-1). The highest radial velocities of absorption features towards CTB 109 (-56 km s^-1) and Sh 152 (-65 km s^-1) are larger than the recombination line velocity (-50 km s^-1) of Sh 152 demonstrating the velocity reversal within the Perseus arm. The molecular cloud has cold HI column density large enough to produce HI self-absorption (HISA) and HI narrow self-absorption (HINSA) if it was at the near side of the velocity reversal. Absence of both HISA and HINSA indicates that the cloud is at the far side of the velocity reversal within the Perseus Arm, so we obtain a distance for CTB 109 of 4+/-0.8 kpc. The new distance still leads to a normal explosion energy for CTB 109/AXP 1E 2259+586.
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