8 August 2016 LSST active optics system software architecture
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Abstract
The Large Synoptic Survey Telescope (LSST) is an 8-meter class wide-field telescope now under construction on Cerro Pachon, near La Serena, Chile. This ground-based telescope is designed to conduct a decade-long time domain survey of the optical sky. In order to achieve the LSST scientific goals, the telescope requires delivering seeing limited image quality over the 3.5 degree field-of-view. Like many telescopes, LSST will use an Active Optics System (AOS) to correct in near real-time the system aberrations primarily introduced by gravity and temperature gradients. The LSST AOS uses a combination of 4 curvature wavefront sensors (CWS) located on the outside of the LSST field-of-view. The information coming from the 4 CWS is combined to calculate the appropriate corrections to be sent to the 3 different mirrors composing LSST. The AOS software incorporates a wavefront sensor estimation pipeline (WEP) and an active optics control system (AOCS). The WEP estimates the wavefront residual error from the CWS images. The AOCS determines the correction to be sent to the different degrees of freedom every 30 seconds. In this paper, we describe the design and implementation of the AOS. More particularly, we will focus on the software architecture as well as the AOS interactions with the various subsystems within LSST.
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Sandrine J. Thomas, Srinivasan Chandrasekharan, Paul Lotz, Bo Xin, Charles Claver, George Angeli, Jacques Sebag, Gregory P. Dubois-Felsmann, "LSST active optics system software architecture", Proc. SPIE 9906, Ground-based and Airborne Telescopes VI, 99063B (8 August 2016); doi: 10.1117/12.2231798; https://doi.org/10.1117/12.2231798
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