Hunting for Near-Earth Asteroids Using LSST: Detection Methods and Observational Strategies

Details Hunting for Near-Earth Asteroids Using LSST: Detection Methods and Observational Strategies Hunting for Near-Earth Asteroids Using LSST: Detection Methods and Observational Strategies

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...20113404b&link_type=abstract

American Astronomical Society, 201st AAS Meeting, #134.04; Bulletin of the American Astronomical Society, Vol. 34, p.1318

Computer Science

Performance

Scientific paper

We will discuss the modeled performance of LSST in detecting near-Earth asteroids (NEAs), and pinpoint a number of considerations that dictate the telescope's optimum use as an NEA search instrument. For example, current surveys detect moving objects either as starlike or streaked images on three to five frames of a given region, or by image subtraction of two or more images. How does the choice of detection algorithm affect the observing strategy? Modeling has shown that, in the trade-off between areal coverage and magnitude limit, it is generally better to observe as large an area of sky as possible on a monthly basis. Is this the most effective use of LSST? LSST will image moving objects as faint as V = 24 mag, implying a detection rate of 105 or 106 asteroids per night, several hundred of which might be Earth approachers. How can asteroids detected on one night be unambiguously linked to detections on another night? The faintness and abundance of the asteroid detections will require that LSST operate in such a way that orbits be derived for as many of the asteroids as possible (LSST must undertake its own follow-up). What are the orbital requirements, and how do they dictate the cadence of LSST pointings? If observations are made in several passbands, so as to provide compositionally diagnostic information on asteroids (or for other programatic reasons), how will LSST's survey efficiency be affected?

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