TRIGONOMETRIC PARALLAXES OF MASSIVE STAR-FORMING REGIONS. I. S 252 & G232.6+1.0
TRIGONOMETRIC PARALLAXES OF MASSIVE STAR-FORMING REGIONS. I. S 252 & G232.6+1.0
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DOI：
10.1088/0004-637x/693/1/397
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发表时间：
2008-11
期刊：
影响因子：
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通讯作者：
M. Reid;K. Menten;A. Brunthaler;X. Zheng;L. Moscadelli;Ye Xu;Ye Xu
中科院分区：
文献类型：
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作者：
M. Reid;K. Menten;A. Brunthaler;X. Zheng;L. Moscadelli;Ye Xu;Ye Xu
我们正在进行一个大型计划与NRAO甚长基线阵列（VLBA）测量三角形的恒星形成区域在整个银河系。本文报道了S252和G232.6+1.0甲醇脉泽的视差和自行测量结果。S252的视差为0.476 ± 0.006mas（2.10+0.027−0.026 kpc），位于英仙座旋臂。G232.6+1.0的视差为0.596 ± 0.035 mas（1.68+0.11−0.09 kpc），位于船底座-人马座臂和英仙座臂之间，可能位于船底座-人马座臂的本地（猎户座）支线。运动学距离明显大于它们的视差距离。我们的松弛和自行产生精确到1.01 km s-1的全空间运动。这两个辐射源绕银河系公转的速度都比圆自转慢约13 km s−1。
We are conducting a large program with the NRAO Very Long Baseline Array (VLBA) to measure trigonometric parallaxes of massive star-forming regions across the Milky Way. Here we report measurement of the parallax and proper motion of methanol masers in S 252 and G232.6+1.0. The parallax of S 252 is 0.476 ± 0.006 mas (2.10+0.027−0.026 kpc), placing it in the Perseus spiral arm. The parallax of G232.6+1.0 is 0.596 ± 0.035 mas (1.68+0.11−0.09 kpc), placing it between the Carina–Sagittarius and Perseus arms, possibly in a Local (Orion) spur of the Carina–Sagittarius arm. For both sources, kinematic distances are significantly greater than their parallax distances. Our parallaxes and proper motions yield full space motions accurate to ≈1 km s−1. Both sources orbit the Galaxy ∼13 km s−1 slower than circular rotation.