The Mark III stellar interferometer
The Mark III stellar interferometer
复制标题
Mark III 恒星干涉仪
DOI：
--
复制
发表时间：
1988
影响因子：
6.5
通讯作者：
G. Kaplan
中科院分区：
文献类型：
--
作者：
M. Shao;M. Colavita;B. Hines;D. Staelin;D. Hutter;K. Johnston;D. Mozurkewich;R. Simon;J. Hershey;J. Hughes;G. Kaplan
翻译后摘要：马克III干涉仪是一个业务的长基线恒星干涉仪山。威尔逊与四种可能的基线配置从9米NE-SW到20米N-S。干涉仪被设计成一种高度自动化的天文仪器，用于测量恒星的位置和直径，最大星等限制为7等。最初的条纹观测是在1986年9月用12米的南北基线进行的。在接下来的几个月里，还进行了半自动天体测量和恒星直径测量。本文介绍了该仪器的硬件和软件组成及其工作特点。干涉仪有几个新的特点。一种是在控制回路中使用最佳估计和控制算法（例如卡尔曼滤波器）。另一个是既能作为闭环相控干涉仪工作，又能最终作为开环或绝对相干干涉仪工作的能力。高的热稳定性和机械精度应使该仪器能够盲指向天文物体，并将光程相等保持在大气层设定的限度内。在这种绝对干涉测量工作模式下，应该可以观测到太暗而无法进行相位跟踪的微弱天体。理论上，幅度、群延迟和闭合相位的测量将可能达到14兆磁。
Abstract : The Mark III interferometer is an operational long baseline stellar interferometer on Mt. Wilson with four-possible baseline configurations from 9m NE-SW to 20m N-S. The interferometer was designed to be a highly automated astronomical instrument to measure stellar positions and diameters to a magnitude limit of seven. Initial fringe observations were made in September 1986 with a 12-m N-S baseline. In the following months, semi-automated astrometric and stellar diameter measurements were also made. This paper describes the hardware and software components of the instrument and its operational characteristics. The interferometer has several novel features. One is the use of optimal estimation and control algorithms (e.g. Kalman filters) in the control loops. Another is the ability to operate both as a closed-loop phased interferometer and eventually as an open-loop or absolute coherent interferometer. High thermal stability and mechanical accuracy should permit the instrument to point blind at an astronomical object and maintain optical path equality to within the limits set by the atmosphere. In this absolute interferometric mode of operation, it should be possible to observe faint astronomical objects that are too dim for phase tracking. In theory, measurements of amplitude, group delay, and closure phase will be possible to 14 mag.