LSST Camera Electronics

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Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.8621o&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #86.21; Bulletin of the American Astronomical Society, V

Mathematics

Logic

Scientific paper

The requirements for reading out the focal plane of the Large Synoptic Survey Telescope are driven by the scientific goals of simultaneously achieving exceptionally high throughput and faint limiting magnitude (i.e., 10 square degrees imaged to 24.5 AB magnitude every 15 s). This results in a large pixel count (3.2 Gpix) and very high segmentation (3,200 readout channels) operating at modest pixel rates (250 kHz 500 kHz). Using this massively parallel readout, about six gigabytes of data are generated per exposure. Present plans call for installing front end electronics inside the cryostat adjacent to the sensors at a temperature of -100C. Digitizing and multiplexing electronics will be in a separate thermal zone within the main cryostat, and data will exit the cryostat over a small number of optical fiber links. Strict attention to contamination control will be required to prevent volatile materials from the electronic hardware from condensing on the sensor surfaces. Two critical ASIC developments are underway for the Front End Electronics; an Analog Signal Processing ASIC containing multiple channels of dual slope integrators, and a Clock Driver ASIC to handle conversion of logic levels to CCD clock levels. These developments are crucial to achieve the high density, low power, and low noise levels required.

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