AAS 207th Meeting, 8-12 January 2006
Session 26 LSST
Poster, Monday, 9:20am-7:00pm, January 9, 2006, Exhibit Hall

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[26.29] The LSST Image Processing Pipeline

A. Becker (U. Washington), T. Axelrod (LSST Corp), Z. Ivezic (U. Washington), R. Lupton (Princeton), N. Silvestri (U.Washington), A. Rest (CTIO, NOAO)

The impacts of the LSST Science Requirements on the LSST Image Processing Pipeline (IPP) are presented. The IPP will operate on raw images and yield photometrically and astrometrically calibrated science and difference images. The derivation of the astrometric solution, the generation of the Point Spread Function, and the generation of the difference imaging convolution kernel are particularly challenging, and have multiple potential degrees of parallelism (amp, CCD, raft, or focal plane). In particular, we address the trade-off between accuracy, speed, and parallelism in the nightly reduction of images given a real-time alerting requirement. Existing algorithms are currently being tested on available datasets, and we present comparisons and shortcomings with regards to the LSST science and computational requirements. We highlight particularly glaring gaps between existing techniques and what is required.

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