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Tests with a Carlina-type diluted telescope - Primary coherencing

机译：使用Carlina型稀释望远镜进行测试-主要相干性

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Aims. Studies are under way to propose a new generation of post-VLTI interferometers. The Carlina concept studied at the Haute-Provence Observatory is one of the proposed solutions. It consists in an optical interferometer configured like a diluted version of the Arecibo radio telescope: above the diluted primary mirror made of fixed cospherical segments, a helium balloon (or cables suspended between two mountains), carries a gondola containing the focal optics. Since 2003, we have been building a technical demonstrator of this diluted telescope. First fringes were obtained in May 2004 with two closely-spaced primary segments and a CCD on the focal gondola. We have been testing the whole optical train with three primary mirrors. The main aim of this article is to describe the metrology that we have conceived, and tested under the helium balloon to align the primary mirrors separate by 5–10?m on the ground with an accuracy of a few microns. Methods. Getting stellar fringes using delay lines is the main difficulty for astronomical interferometers. Carlina does not use delay lines, but the primary segments have to be positioned on a sphere i.e. coherencing the primary mirrors. As described in this paper, we used a supercontinuum laser source to coherence the primary segments. We characterize the Carlina’s performances by testing its whole optical train: servo loop, metrology, and the focal gondola. Results. The servo loop stabilizes the mirror of metrology under the helium balloon with an accuracy better than 5?mm while it moves horizontally by 30?cm in open loop by 10–20?km/h of wind. We have obtained the white fringes of metrology; i.e., the three mirrors are aligned (cospherized) with an accuracy of ?≈1?μm. We show data proving the stability of fringes over 15?min, therefore providing evidence that the mechanical parts are stabilized within a few microns. This is an important step that demonstrates the feasibility of building a diluted telescope using cables strained between cliffs or under a balloon. Carlina, like the MMT or LBT, could be one of the first members of a new class of telescopes named diluted telescopes.
机译：目的正在进行研究以提出新一代的后VLTI干涉仪。在上普罗旺斯天文台研究的卡利纳概念是提出的解决方案之一。它包含一个光学干涉仪，其配置类似于Arecibo射电望远镜的稀释版：在由固定球面部分制成的稀释主镜上方，一个氦气球（或悬挂在两座山之间的电缆）携带装有聚焦光学器件的吊舱。自2003年以来，我们一直在制造这种稀释望远镜的技术演示器。 2004年5月获得了第一个条纹，在焦点吊船上有两个间隔很近的主要部分和一个CCD。我们已经用三个主镜测试了整个光学系统。本文的主要目的是描述我们构想的，并在氦气球下进行测试的度量衡技术，以在地面上将主反射镜分开5–10？m，精度为几微米。方法。使用延迟线获得星状条纹是天文干涉仪的主要困难。卡利纳（Carlina）不使用延迟线，但主要部分必须放置在球体上，即使主要反射镜相干。如本文所述，我们使用超连续谱激光源使主要部分相干。我们通过测试其整个光学系统来表征卡利纳的性能：伺服回路，计量学和聚焦吊舱。结果。伺服回路使氦气球下的计量镜稳定，其精度优于5？mm，而在开环中以10–20？km / h的风向水平移动30？cm。我们已经获得了度量学的白色边缘;即，三个反射镜以θ≈1μm的精度对准（球形）。我们显示的数据证明了条纹在15分钟内的稳定性，因此提供了机械零件稳定在几微米范围内的证据。这是一个重要的步骤，展示了使用在悬崖之间或气球下面拉紧的电缆建造稀释望远镜的可行性。像MMT或LBT一样，卡利纳（Calina）可能是名为稀释望远镜的新型望远镜的首批成员之一。

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