High-Order Adaptive Optics Sample Clauses

High-Order Adaptive Optics. High-resolution observations of the Sun are essential in solving many of the outstanding problems of solar astronomy. The current high-resolution solar telescopes are in the one-meter class. Without AO the resolution of these telescopes is limited to about 1 arcsec (long exposure) because the Fried parameter (roughly speaking, the largest aperture telescope that would have diffraction-limited seeing) of a good daytime site is about 10 cm. AO is necessary to obtain full benefit from existing telescopes. Since August 2000, the NSO, in primary partnership with the New Jersey Institute of Technology, has been developing high-order solar adaptive optics for use at the 65-cm telescope at Big Bear Solar Observatory (BBSO) and the 76-xx Xxxx Solar Telescope at Sacramento Peak. The NSF has sponsored this project within the Major Research Instrumentation (MRI) program with substantial matching funds from the participating partner organizations, which include the NSO, the NJIT, the Kiepenheuer Institute in Germany, and the Air Force Research Laboratory. The high-order AO systems will upgrade each of these high-resolution solar telescopes and greatly improve their scientific output. The resulting systems also serve as proofs-of-concept for a scalable AO design for the much larger 4-meter ATST. Compared to the low-order AO system that has been operating at the DST since 1998, the high-order AO system provides a threefold increase in the number of deformable mirror actuators that are actively controlled. During FY 2003, the AO project made excellent progress and is well on track towards a timely completion of the project. In April 2003, the high-order AO system was operated for the first time with the new high-speed wavefront sensor camera. This camera is based on a CMOS device and operates at a rate of 2500 frames per second, which more than doubles the closed-loop servo bandwidth of the system compared to the DALSA camera. The camera was custom developed for the AO project by BAJA Technologies and lead AO project engineer, Xxx Xxxxxxxx of NSO. Xxxxxxxx also implemented improved control software for the April engineering run. Several “shared-risk” science runs were performed with the high-order AO at the DST by local staff and in collaboration with, for example, members from NJIT and the University of Hawaii Institute for Astronomy (IFA). All of these runs have produced excellent results (e.g., Xxxxxxx, 2004, ApJ, 604, 906-923 and December 2003 NOAO/NSO Newsletter 76)....
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