为达到科学目标而优化测量的适应性调度工具：银河系中心恒星轨道测量的方法和应用
An adaptive scheduling tool to optimize measurements to reach a scientific objective: methodology and application to the measurements of stellar orbits in the Galactic Center
摘要：
在物理学和天文学的各个领域，使用实验设施或望远镜的机会越来越具有竞争性，而且越来越有限。因此，必须优化测量类型及其时间安排，以达到特定的科学目标，并增加科学项目成功的机会。在本通信中，扩展了Ford（2008）和Loredo等人的工作。（2012），我们提出了一种有效的自适应调度工具，旨在优先考虑测量，以达到科学目标。该算法基于Fisher矩阵，可应用于广泛的测量类别。我们详细介绍了这种算法，并讨论了一些实用性，如系统误差或测量损失，由于突发事件（如天气，实验失败，.）。作为一个例子，我们考虑在我们的银河系中心的短周期恒星S 0 -2的测量。我们表明，径向速度曲线的两个转折点处的径向速度测量更强大的检测引力红移比在最大相对论信号的测量。我们还明确提出了用于计划测量的方法，以检测相对论红移考虑系统学和可能的测量损失。对于未来，我们确定天体测量的转折点是高度敏感的相对论性进步的近星点。最后，我们还确定测量特别敏感的距离，我们的银河系中心：径向速度周围的近星点和天体测量的最接近之前，在最大的赤经天体测量的转折点。
英文摘要：
In various fields of physics and astronomy, access to experimental facilities or to telescopes is becoming more and more competitive and limited. It becomes therefore important to optimize the type of measurements and their scheduling to reach a given scientific objective and to increase the chances of success of a scientific project. In this communication, extending the work of Ford (2008) and of Loredo et al. (2012), we present an efficient adaptive scheduling tool aimed at prioritzing measurements in order to reach a scientific goal. The algorithm, based on the Fisher matrix, can be applied to a wide class of measurements. We present this algorithm in detail and discuss some practicalities such as systematic errors or measurements losses due to contigencies (such as weather, experimental failure, ...). As an illustration, we consider measurements of the short-period star S0-2 in our Galactic Center. We show that the radial velocity measurements at the two turning points of the radial velocity curve are more powerful for detecting the gravitational redshift than measurements at the maximal relativistic signal. We also explicitly present the methodology that was used to plan measurements in order to detect the relativistic redshift considering systematics and possible measurements losses. For the future, we identify the astrometric turning points to be highly sensitive to the relativistic advance of the periastron. Finally, we also identify measurements particularly sensitive to the distance to our Galactic Center: the radial velocities around periastron and the astrometric measurements just before closest approach and at the maximal right ascension astrometric turning point.
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