Submillimeter Array Observations of 321 GHz Water Maser Emission in Cepheus A
Submillimeter Array Observations of 321 GHz Water Maser Emission in Cepheus A
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仙王座 A 321 GHz 水脉泽发射的亚毫米阵列观测
DOI：
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发表时间：
2007
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通讯作者：
J. Torrelles
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作者：
N. Patel;S. Curil;Q. Zhang;Sridharan T. K.;P. Ho;J. Torrelles
利用亚毫米波阵（SMA）首次对321.226GHz、1029-936正向水脉泽辐射进行了成像。这也是在仙王座A高质量恒星形成区首次探测到这条线。22.235 GHz，616-523水脉泽也在SMA观测后43天用甚大阵观测到。9个亚毫米脉泽斑中有3个在空间上和运动学上与厘米脉泽有关，而有36个22 GHz脉泽斑没有相应的亚毫米脉泽。在HW 2源中，321和22 GHz脉泽都出现在~ 1 '区，其中包括盘喷系统，但脉泽追踪到的大致线性结构的位置角表明，321 GHz脉泽是沿着喷流，而22 GHz脉泽则垂直于喷流，我们认为仙王座A中的亚毫米波脉泽追踪到的是明显更热的区域（600-2000 K）的厘米脉泽。
Using the Submillimeter Array (SMA) we have imaged for the first time the 321.226 GHz, 1029-936 ortho-H2O maser emission. This is also the first detection of this line in the Cepheus A high-mass star-forming region. The 22.235 GHz, 616-523 water masers were also observed with the Very Large Array 43 days following the SMA observations. Three of the nine detected submillimeter maser spots are associated with the centimeter masers spatially as well as kinematically, while there are 36 22 GHz maser spots without corresponding submillimeter masers. In the HW2 source, both the 321 and 22 GHz masers occur within the region of ~1', which includes the disk-jet system, but the position angles of the roughly linear structures traced by the masers indicate that the 321 GHz masers are along the jet while the 22 GHz masers are perpendicular to it. We interpret the submillimeter masers in Cepheus A to be tracing significantly hotter regions (600-2000 K) than the centimeter masers.