银河系中心PRIMA科学能力研究
Study of the Science Capabilities of PRIMA in the Galactic Center
摘要：
相位参考成像和微弧秒天体测量设施计划于2008年下半年安装在智利帕拉纳尔的甚大望远镜干涉仪观测台。其目标是提供微弧秒范围内的天体测量精度。高精度天体测量可以用来研究致密星团的动力学。特别是超大质量黑洞附近恒星形成的模型，或者短寿命大质量恒星快速转移到我们银河系最里面的秒差距的模型，都可以进行测试。通过测量靠近大质量黑洞的恒星的轨道，人们可以探测开普勒运动的偏差。这样的偏差可能是由于一群黑暗的恒星质量的物体扰乱了质点解。同时，轨道受到相对论修正的影响，因此可以进行测试。最终目的是检验广义相对论在强引力场中的作用。后者可以用SgrA* 的近红外耀斑探测，这很可能是由于黑洞上的吸积现象造成的。我们研究的预期性能的PRIMA天文测量在银河系中心的实验室测量的基础上，讨论可能的观测策略。
英文摘要：
The Phase-Referenced Imaging and Micro-arcsecond Astrometry (PRIMA) facility is scheduled for installation in the Very Large Telescope Interferometer observatory in Paranal, Chile, in the second half of 2008. Its goal is to provide astrometric accuracy in the micro-arcsecond range. High precision astrometry can be applied to explore the dynamics of the dense stellar cluster. Especially models for the formation of stars near super massive black holes or the fast transfer of short-lived massive stars into the innermost parsec of our galaxy can be tested. By measuring the orbits of stars close to the massive black hole one can probe deviations from a Keplerian motion. Such deviations could be due to a swarm of dark, stellar mass objects that perturb the point mass solution. At the same time the orbits are affected by relativistic corrections which thus can be tested. The ultimate goal is to test the effects of general relativity in the strong gravitational field. The latter can be probed with the near infrared flares of SgrA* which are most likely due to accretion phenomena onto the black hole. We study the expected performance of PRIMA for astrometric measurements in the Galactic Center based on laboratory measurements and discuss possible observing strategies.
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