银河系中心以南2.2角秒高速致密星云细丝的识别
Identification of a high-velocity compact nebular filament 2.2 arcsec south of the Galactic Centre
摘要：
银河系的中央秒差距是我们银河系中一个非常特殊的区域;它包含与Sgr A* 有关的超大质量黑洞以及大量的早期型恒星和中性和电离气体流的复杂结构，距离中心不到两个秒差距，代表一个独特的实验室。我们报告的识别高速致密星云灯丝2.2角秒以南的Sgr A*。该构造延伸超过约1角秒，并呈现出约200 km s^{-1}角秒^{-1}的强烈速度梯度。在[Fe III]和He I谱线中看到的最大发射峰位于相对于Sgr A* 的dα = +0.20 +/- 0.06 arcsec和dδ = -2.20 +/- 0.06 arcsec处。这个位置靠近恒星IRS 33 N。发射峰值处的速度为Vr = -267 km s^{-1}。灯丝的位置角为PA = 115{ \degr } +/- 10{ \degr }，与沙洲和东旋臂在该位置的位置角相似。峰值位置位于X射线和射电瞬变双星CXOGX J174540.0-290031以北0.7角秒处，CXOGX J174540.0-290031是一个低质量X射线双星，轨道周期为7.9小时，在暗条及其附近有很强的[Fe III]线发射。这些谱线可能是由激波加热产生的，但我们不能排除低质量X射线双星中的一些X射线光电离。虽然我们不能排除一个紧凑的星云喷流的想法，我们解释这个灯丝作为一个可能的冲击之间的北和东臂或北臂和小型螺旋“酒吧”。
英文摘要：
The central parsec of the Milky Way is a very special region of our Galaxy; it contains the supermassive black hole associated with Sgr A* as well as a significant number of early-type stars and a complex structure of streamers of neutral and ionized gas, within two parsecs from the centre, representing a unique laboratory. We report the identification of a high velocity compact nebular filament 2.2 arcsec south of Sgr A*. The structure extends over ~1 arcsec and presents a strong velocity gradient of ~200 km s^{-1} arcsec^{-1}. The peak of maximum emission, seen in [Fe III] and He I lines, is located at dα = +0.20 +/- 0.06 arcsec and dδ = -2.20 +/- 0.06 arcsec with respect to Sgr A*. This position is near the star IRS 33N. The velocity at the emission peak is Vr = -267 km s^{-1}. The filament has a position angle of PA = 115{\degr} +/- 10{\degr}, similar to that of the Bar and of the Eastern Arm at that position. The peak position is located 0.7 arcsec north of the binary X-ray and radio transient CXOGX J174540.0-290031, a low-mass X-ray binary with an orbital period of 7.9 hr. The [Fe III] line emission is strong in the filament and its vicinity. These lines are probably produced by shock heating but we cannot exclude some X-ray photoionization from the low-mass X-ray binary. Although we cannot rule out the idea of a compact nebular jet, we interpret this filament as a possible shock between the Northern and the Eastern Arm or between the Northern Arm and the mini-spiral "Bar".
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