Microarcsecond Radio Astrometry
Microarcsecond Radio Astrometry
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DOI：
10.1146/annurev-astro-081913-040006
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发表时间：
2013-12
影响因子：
33.3
通讯作者：
M. Reid;M. Honma
中科院分区：
文献类型：
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作者：
M. Reid;M. Honma
天体测量学为天体物理学提供了基础。在不同时间或波长探测到的源的关联需要精确的位置，距离对于估计大多数物体的大小，光度，质量和年龄至关重要。射电波长的甚长基线干涉测量法，以亚毫弧秒分辨率进行衍射极限成像，长期以来一直是微弧秒天体测量的希望所在。然而，只是在过去十年中，这一点才经常实现。目前，测量银河系各源的弛豫时间的精度为10 μas，而确定星系自行的精度为11 μas-1年。这些测量的天体物理学应用涵盖了许多领域，包括星星的形成、演化的恒星、恒星和超大质量黑洞、银河系结构、本星系群的历史和命运、哈勃常数和广义相对论的检验。本文综述了该方法的应用及其在天体物理中的应用。
Astrometry provides the foundation for astrophysics. Accurate positions are required for the association of sources detected at different times or wavelengths, and distances are essential to estimate the size, luminosity, mass, and ages of most objects. Very long baseline interferometry at radio wavelengths, with diffraction-limited imaging at submilliarcsecond resolution, has long held the promise of microarcsecond astrometry. However, only in the past decade has this been routinely achieved. Currently, parallaxes for sources across the Milky Way are being measured with ∼10 μas accuracy, and proper motions of galaxies are being determined with accuracies of ∼1 μas year−1. The astrophysical applications of these measurements cover many fields, including star formation, evolved stars, stellar and supermassive black holes, Galactic structure, the history and fate of the Local Group, the Hubble constant, and tests of general relativity. This review summarizes the methods used and the astrophysical applicatio...