LSST Survey Strategy

Details LSST Survey Strategy LSST Survey Strategy

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21113702i&link_type=abstract

American Astronomical Society, AAS Meeting #211, #137.02; Bulletin of the American Astronomical Society, Vol. 39, p.978

Astronomy and Astrophysics

Astronomy

Scientific paper

The LSST will be a large, wide-field ground based telescope designed to obtain sequential images covering the entire visible sky from Cerro Pachon in Northern Chile. The current baseline design, with an 8.4m (6.5m effective) primary mirror and a 9.6 sq.deg. field of view, will allow about 15,000 square degrees of sky to be covered in two photometric bands every four nights (assuming two 15-second exposures per field). The system is designed to yield high image quality as well as superb astrometric and photometric accuracy. The survey area will include 30,000 sq.deg. with Dec<+34.5, and will be imaged multiple times in six bands covering the wavelength range 320--1050 nm. The vast majority (about 90%) of the observing time will be devoted to a deep-wide-fast survey mode which will observe a 20,000 sq.deg. region in the ugrizy bands about 1000 times (including all bands) during the 10-year survey. The deep-wide-fast survey data will serve the majority of science programs. The remaining 10% of observing time will be allocated to special programs such as Very Deep and Very Fast time domain surveys. We illustrate how LSST science drivers led to these choices of system design parameters.

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