An Updated 2017 Astrometric Solution for Betelgeuse
An Updated 2017 Astrometric Solution for Betelgeuse
复制标题
2017 年更新的参宿四天体测量解决方案
DOI：
10.3847/1538-3881/aa6ff9
复制
发表时间：
2017
期刊：
影响因子：
--
通讯作者：
L. Decin
中科院分区：
文献类型：
--
作者：
G. Harper;Alexander Brown;E. Guinan;E. O’Gorman;A. Richards;P. Kervella;P. Kervella;L. Decin
我们提供了一个更新的天体测量解决方案的II型超新星的祖先参宿四使用修订的依巴谷中间天体测量数据（HIAD）的货车Leeuwen，结合现有的VLA和新的e-MERLIN和阿尔马的立场。2007年依巴谷的精细横坐标测量需要添加所谓的2.4质量的宇宙噪声，以找到一个可接受的5参数随机解。我们发现，无线电宇宙噪声的措施也应该包括无线电的位置，因为表面的不均匀性存在的水平显着足以引入额外的强度质心的不确定性。将2007年的HIAD与仅基于射电位置的自行相结合，得到的视差为mas（pc），小于依巴谷2007年的6.56 ± 0.83 mas（pc）。此外，将VLA和新的e-MERLIN和阿尔马射电位置与2007年HIAD结合，并包括2.4 mas的射电宇宙噪声，导致4.51 ± 0.80 mas（pc）的标称视差解，尽管与哈珀等人的2008年解仅不同，与货车Leeuwen的解相差2.6σ。参宿四的精确视差总是很难获得，因为它与恒星的角直径（mas）相比很小。我们概述了一个观察策略，利用未来的毫米和亚毫米高空间分辨率干涉，必须使用，如果要实现视差和距离的精度和准确性的大幅改善。
We provide an update for the astrometric solution for the Type II supernova progenitor Betelgeuse using the revised Hipparcos Intermediate Astrometric Data (HIAD) of van Leeuwen, combined with existing VLA and new e-MERLIN and ALMA positions. The 2007 Hipparcos refined abscissa measurements required the addition of so-called Cosmic Noise of 2.4 mas to find an acceptable 5-parameter stochastic solution. We find that a measure of radio Cosmic Noise should also be included for the radio positions because surface inhomogeneities exist at a level significant enough to introduce additional intensity centroid uncertainty. Combining the 2007 HIAD with the proper motions based solely on the radio positions leads to a parallax of mas ( pc), smaller than the Hipparcos 2007 value of 6.56 ± 0.83 mas ( pc). Furthermore, combining the VLA and new e-MERLIN and ALMA radio positions with the 2007 HIAD, and including radio Cosmic Noise of 2.4 mas, leads to a nominal parallax solution of 4.51 ± 0.80 mas ( pc), which, while only different from the 2008 solution of Harper et al., is 2.6σ different from the solution of van Leeuwen. An accurate and precise parallax for Betelgeuse is always going to be difficult to obtain because it is small compared to the stellar angular diameter ( mas). We outline an observing strategy utilizing future mm and sub-mm high-spatial resolution interferometry that must be used if substantial improvements in the precision and accuracy of the parallax and distance are to be achieved.