Baldwin John E, Haniff Christopher A
Department of Physics, University of Cambridge, Madingley Road, Cambridge CB3 0HE, UK.
Philos Trans A Math Phys Eng Sci. 2002 May 15;360(1794):969-86. doi: 10.1098/rsta.2001.0977.
In the first part of this review we survey the role optical/infrared interferometry now plays in ground-based astronomy. We discuss in turn the origins of astronomical interferometry, the motivation for its development, the techniques of its implementation, examples of its astronomical significance, and the limitations of the current generation of interferometric arrays. The second part focuses on the prospects for ground-based astronomical imaging interferometry over the near to mid-term (i.e. 10 years) at optical and near-infrared wavelengths. An assessment is made of the astronomical and technical factors which determine the optimal designs for imaging arrays. An analysis based on scientific capability, technical feasibility and cost argues for an array of large numbers of moderate-sized (2 m class) telescopes rather than one comprising a small number of much larger collectors.
在本综述的第一部分，我们考察了光学/红外干涉测量目前在地面天文学中所起的作用。我们依次讨论了天文干涉测量的起源、其发展的动机、实施技术、其天文学意义的实例以及当前一代干涉阵列的局限性。第二部分聚焦于近中期（即10年）在光学和近红外波段进行地面天文成像干涉测量的前景。对决定成像阵列最佳设计的天文学和技术因素进行了评估。基于科学能力、技术可行性和成本的分析表明，应采用大量中等尺寸（2米级）望远镜组成的阵列，而不是由少数大得多的收集器组成的阵列。
