LCOGT Follow-up Of SuperWASP Extrasolar Planet Candidates

Details LCOGT Follow-up Of SuperWASP Extrasolar Planet Candidates LCOGT Follow-up Of SuperWASP Extrasolar Planet Candidates

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21113411l&link_type=abstract

American Astronomical Society, AAS Meeting #211, #134.11; Bulletin of the American Astronomical Society, Vol. 39, p.970

Astronomy and Astrophysics

Astronomy

Scientific paper

We describe the photometric follow-up of extrasolar planet transit candidates detected by the SuperWASP instruments and followed up with a variety of Las Cumbres Observatory Global Telescope (LCOGT) network telescopes from 0.4 to 2m aperture. LCOGT's variety of available telescopes, flexible nature, longitude coverage and facilities in both hemispheres makes it ideal for following up these type of object.
SuperWASP is an ultra wide field instrument with 8 cameras (each consisting of a 200mm f/1.8 lens + 20482 CCD) on a robotic mount, giving a total field of view of nearly 500 sq. degrees. Two of these instruments have been deployed, SuperWASP-North on La Palma, Canary Islands and SuperWASP-South at SAAO, South Africa.
Three extrasolar planets (Collier Cameron et. al. 2006, Pollacco et al. 2007) have been discovered from the inaugural 2004 season and observations continued in the 2006 & 2007 seasons. Following our experience in the 2004 season, we have implemented several improvements to our extensive candidate filtering procedure, which draws on existing imaging and catalogue information to reduce false positives. Nevertheless, we produced a substantial number of candidates which require additional photometric and spectroscopic follow-up.
These candidates have been followed up with a variety of telescopes accessible by LCOGT, including the 0.35m Muhlenberg College telescope at Siding Spring Observatory, 0.8m Tenagra-II in Arizona and the two 2m Faulkes Telescopes in Hawaii and Australia. We show example transit light curves indicating the precision that can be obtained even with small telescopes. We also discuss some of the advantages of a flexibly scheduled system and the difficulties inherent in operating a heterogeneous telescope network in 4 different time zones.

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