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首页> 外文期刊>The Astrophysical journal >PROPER MOTION OF WATER MASERS ASSOCIATED WITH IRAS 21391 + 5802: BIPOLAR OUTFLOW AND AN AU-SCALE DUSTY CIRCUMSTELLAR SHELL
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PROPER MOTION OF WATER MASERS ASSOCIATED WITH IRAS 21391 + 5802: BIPOLAR OUTFLOW AND AN AU-SCALE DUSTY CIRCUMSTELLAR SHELL

机译：与IRAS 21391 + 5802关联的水务器的正确运动：双极性流出和多灰尘的圆形壳

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摘要

We present Very Long Baseline Array (VLBA) observations of water maser emission associated with the star-forming region IRAS 21391 + 5802, which is embedded in a bright-rimmed cometary globule in IC 1396. The angular resolution of the maps is ～0.8 mas, corresponding to a spatial resolution of ～0.6 AU at an estimated distance of 750 pc. Proper motions are derived for 10 maser features identified consistently over three epochs, which were separated by intervals of about 1 month. The masers appear in four groups, which are aligned linearly on the sky, roughly along a northeast-southwest direction, with a total separation of ～520 AU (～0.7″). The three-dimensional velocities of the masers have a maximum value of ～42 km s~(-1) (～9 AU yr~(-1)). The average error on the derived proper motions is ～4 km s~(-1). The overall pattern of proper motions is indicative of a bipolar outflow. Proper motions of the masers in a central cluster, with a projected extent of ～20 AU, show systematic deviations from a radial outflow. However, we find no evidence of Keplerian rotation, as has been claimed elsewhere. A nearly circular loop of masers lies near the middle of the cluster. The radius of this loop is 1 AU, and the line-of-sight velocities of the masers in the loop are within 2 km s~(-1) of the systemic velocity of the region. These masers presumably exist at the radial distance where significant dust condensation occurs in the outflow emanating from the star.
机译：我们提出了非常长基线阵列（VLBA）观测到的与星状形成区域IRAS 21391 + 5802相关的水脉激发射的信息，其嵌入在IC 1396的明亮边缘彗星小球中。这些地图的角分辨率为〜0.8 mas ，对应于估计的750 pc处的〜0.6 AU的空间分辨率。在三个时期内一致确定的10个maser特征获得了正确的运动，每个时期间隔约1个月。微波激射器分为四组，它们在天空中线性排列，大致沿东北-西南方向，总间隔约为520 AU（〜0.7“）。激射器的三维速度的最大值约为〜42 km s〜（-1）（〜9 AU yr〜（-1））。推导的正确运动的平均误差为〜4 km s〜（-1）。适当运动的整体模式指示双极流出。中心星团中脉节的正确运动，预计范围为〜20 AU，显示出与径向流出的系统偏差。但是，我们没有发现开普勒旋转的证据，正如其他地方所声称的。团簇的中央附近有一个近乎圆形的脉石环。该环路的半径为1 AU，环路中的激射器的视线速度在该区域系统速度的2 km s〜（-1）之内。这些脉脉可能存在于径向距离处，在该距离处，从恒星流出的气流中会出现大量的灰尘凝结。

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