Distributed computing architecture for image-based wavefront sensing and 2D FFTs

Details Distributed computing architecture for image-based wavefront sensing and 2D FFTs Distributed computing architecture for image-based wavefront sensing and 2D FFTs

Jul 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spie.6274e..64s&link_type=abstract

Advanced Software and Control for Astronomy. Edited by Lewis, Hilton; Bridger, Alan. Proceedings of the SPIE, Volume 6274, pp.

Astronomy and Astrophysics

Astronomy

Scientific paper

Image-based wavefront sensing provides significant advantages over interferometric-based wavefront sensors such as optical design simplicity and stability. However, the image-based approach is computationally intensive, and therefore, applications utilizing the image-based approach gain substantial benefits using specialized high-performance computing architectures. The development and testing of these computing architectures are essential to missions such as James Webb Space Telescope (JWST), Terrestrial Planet Finder-Coronagraph (TPF-C and CorSpec), and the Spherical Primary Optical Telescope (SPOT). The algorithms implemented on these specialized computing architectures make use of numerous two-dimensional Fast Fourier Transforms (FFTs) which necessitate an all-to-all communication when applied on a distributed computational architecture. Several solutions for distributed computing are presented with an emphasis on a 64 Node cluster of digital signal processors (DSPs) and multiple DSP field programmable gate arrays (FPGAs), offering a novel application of low-diameter graph theory. Timing results and performance analysis are presented. The solutions offered could be applied to other computationally complex all-to-all communication problems.

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