Measurement of the Distance and Proper Motions of the H2O Masers in the Young Planetary Nebula K 3-35
Measurement of the Distance and Proper Motions of the H2O Masers in the Young Planetary Nebula K 3-35
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DOI：
10.1093/pasj/63.1.71
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发表时间：
2011-01
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影响因子：
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通讯作者：
D. Tafoya;H. Imai;Y. Gómez;J. Torrelles;N. Patel;G. Anglada;L. F. Miranda;M. Honma;T. Hirota;T. Miyaji
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文献类型：
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作者：
D. Tafoya;H. Imai;Y. Gómez;J. Torrelles;N. Patel;G. Anglada;L. F. Miranda;M. Honma;T. Hirota;T. Miyaji
本文介绍了用射电天体测量的VLBI探测（VERA）阵列和甚长基线阵列（VLBA）对年轻行星状星云K3 -35中的H2O脉泽进行甚长基线干涉（VLBI）观测的结果。利用VERA观测资料，我们测量了K3 -35中一个亮水脉泽斑的年视差和本征运动。结果距离为D = 3.9+0.7 kpc。-0.5这是第一次通过对行星状星云脉泽发射的观测获得其视差。另一方面，K3 -35整体的自行估计为α = -3.34+/-0.10 mas yr-1，δ = -5.93+/-0.07 mas yr-1.根据这些结果，我们确定了K 3-35在银河柱坐标系中的位置和速度：（R，{\theta}，z）=（7.11+0.08-0.06 kpc，27+/-5{\circ}，140+25-18 pc）和（VR，V{\theta}，Vz）=（33+/-16，233 +/-11，11 +/-2）km s-1。此外，从我们的VLBA观测中，我们测量了位于星云中心区域的水脉泽斑点之间的相对自行，这些斑点被认为是追踪环形结构。脉泽的分布和相对自行，与以前报道的观测年代相比，表明这种结构可能在几年内被完全摧毁，由于高速风的作用和星云中电离锋的膨胀。
In this paper we present the results of very long baseline interferometry (VLBI) ob- servations carried out with the VLBI Exploration of Radio Astrometry (VERA) array and the Very Long Baseline Array (VLBA) toward H2O masers in a young planetary nebula K 3-35. From the VERA observations we measured the annual parallax and proper mo- tion of a bright water maser spot in K 3-35. The resulting distance is D = 3.9+0.7 kpc. -0.5 This is the first time that the parallax of a planetary nebula is obtained by observations of its maser emission. On the other hand, the proper motion of K 3-35 as a whole was esti- mated to be {\mu}{\alpha} = -3.34+/-0.10 mas yr-1, {\mu}{\delta} = -5.93+/-0.07 mas yr-1. From these results we determined the position and velocity of K 3-35 in Galactic cylindrical coordinates: (R,{\theta},z) = (7.11+0.08-0.06 kpc, 27+/-5{\circ}, 140+25-18 pc) and (VR, V{\theta}, Vz) = (33+/-16, 233+/-11, 11+/-2) km s-1, respectively. Additionally, from our VLBA observations we measured the relative proper motions among the water maser spots located in the central region of the nebula, which have been proposed to be tracing a toroidal structure. The distribution and relative proper motions of the masers, compared with previous reported observed epochs, suggest that such structure could be totally destroyed within a few years, due to the action of high velocity winds and the expansion of the ionization front in the nebula.