An Overview of the LSST Telescope and Site

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The LSST uses a modified Paul-Baker 3-mirror optical design with 8.4-m primary, 3.4-m secondary and 5-m tertiary mirrors. The 3mirror telescope feeds a 3 element refractive corrector to produce a 3.5-degree diameter field of view over a 64-cm flat focal surface. This design provides excellent image quality with 80% encircled energy diameters of <0.3” in u and g; <0.25” in Y; and <0.2” in r and i spectral bands over the full field of view. The etendue (collecting area times field of view), a measure of survey capability, for the LSST is 319m2deg2, many times that of any other existing or proposed facility.
The primary and tertiary mirrors are arranged so that their surfaces form a cusp at their intersection, allowing them to be fabricated from a single substrate. This is a unique feature of the LSST and is called the M1M3 monolith. The M1M3 monolith will be fabricated the Steward Observatory Mirror Lab using their structured borosilicate spin casting technology. Fabrication is scheduled to start in mid 2007.
The optical design has been analyzed for correctability and is shown to be remarkably tolerant to anticipated fabrication errors with a limited number of compensators. The active optical compensation and figure control of the three mirrors and camera is done by tomographic analysis of four wavefront sensors at the edge of the field of view. Stray and scattered light analysis shows the LSST will achieve its signal to noise requirements.
The summit facility on Cerro Peñón in Northern Chile consists of a 30-m cylindrical dome and support building. The cylindrical dome design utilizes extensive natural ventilation to maintain thermal equilibrium. Numerical fluid models of this desig indicate more than 50 dome air changes per hour in median wind conditions.

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