LSST Survey Strategy

Details LSST Survey Strategy LSST Survey Strategy

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.8602i&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #86.02; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The LSST is envisioned to be a large, wide-field ground based telescope designed to obtain sequential images covering the entire visible sky every few nights. The current baseline design with an 8.4m primary mirror and a 10 sq.deg. field of view will allow to do so in two photometric bands every three nights. The system is designed and engineered to yield exquisite astrometric and photometric accuracy, and image quality. The survey area will include 30,000 sq.deg. of sky 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 spent in a deep-wide-fast survey mode which will observe a 20,000 sq.deg. large region about 1000 times during the 10-year long 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 will illustrate how LSST science drivers led to these choices of system design parameters.

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