Electronics imaging system overview and performance for the Keck long-wavelength spectrometer

Details Electronics imaging system overview and performance for the Keck long-wavelength spectrometer Electronics imaging system overview and performance for the Keck long-wavelength spectrometer

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995spie.2475..162m&link_type=abstract

Proc. SPIE Vol. 2475, p. 162-170, Infrared Detectors and Instrumentation for Astronomy, Albert M. Fowler; Ed.

Astronomy and Astrophysics

Astronomy

1

Scientific paper

This paper presents an overview of the electronic imaging system design and performance for the long wavelength spectrometer that is to be deployed on the Keck Telescope. Because the LWS employs 96 parallel read-out channels and 24 parallel processing channels, the LWS serves as a forerunner of next generation infrared astronomical instruments that are to use highly parallel output focal plane arrays like the Santa Barbara Research Center ALADDIN Near-IR 32 output FPA or any of the Rockwell Mid-IR 16 output arrays. Several principles regarding noise and grounding issues are discussed with the hope that they may help the developers of the next generation of infrared astronomical instruments. It is concluded that low noise performance is not something that can be added after-the-fact in the lab unless the necessary efforts have been made in the early phases of an instrument's conceptual design. Low noise requirements will drive the highest level architectural issues of the electronics, and hence cannot be an afterthought.

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