Surveys, Temporal Variability, and the Las Cumbres Observatory Global Telescope

Details Surveys, Temporal Variability, and the Las Cumbres Observatory Global Telescope Surveys, Temporal Variability, and the Las Cumbres Observatory Global Telescope

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.6601b&link_type=abstract

American Astronomical Society Meeting 210, #66.01; Bulletin of the American Astronomical Society, Vol. 39, p.173

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Upcoming wide-field surveys such as Pan-STARRS, LSST, and Skymapper will detect large numbers of objects that vary photometrically, or that move. These objects will include small bodies in the solar systema, eclipsing binary stars, transiting extrasolar planets, pulsating stars, dwarf novae, novae, supernovae, active galactic nuclei, and quite possibly other transient phenomena for which we have no names as yet. Although they will be a fertile source of such transient detections, wide-field surveys themselves ordinarily will have neither the observing cadence nor the (e.g., spectroscopic) observing capabilities to perform adequate follow-up observations of these variable objects. The Las Cumbres Observatory Global Telescope (LCOGT) will be a global network of moderate-aperture (2m and smaller) telescopes, instrumented and interconnected so as to
facilitate such in-depth variability studies.
The LCOGT now operates the two 2m Faulkes Telescopes: FT North located on the island of Maui, and FT South at the Siding Spring site in Australia. These telescopes will anchor a network of about 7 clusters of 1m-class telescopes, each cluster containing 4 telescopes. First-light instruments will provide visible-light and NIR imaging; spectroscopic capabilities will come later, and will likely include both low- and high-resolution visible-light spectrographs. Scheduling and coordination of observations will be provided from a central site, in pursuit of a single set of scientific goals.

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