Transits of Extrasolar Planets and Analysis Methods

Details Transits of Extrasolar Planets and Analysis Methods Transits of Extrasolar Planets and Analysis Methods

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aps..osf.p1008f&link_type=abstract

American Physical Society, Fall 2007 Meeting of the Ohio-Region Section of APS, October 19-20, 2007, abstract #P1.008

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Using Wittenberg's 10-inch refracting telescope housed in Elgar Weaver Observatory, and an ST-8XE CCD camera, the egress of the transit of planet HD209458 `b' was observed on the night of December 18^th, 2006. This transit occurs when the planet passes directly between its host star and the telescope on Earth, and the brightness of the star decreases by about 1.5%. The brightness of the stars is measured by the number of counts in pixels in images taken as 30 second exposures over a period of 64 minutes. Data analysis techniques using Diffraction Limited's MaxImDL^TM yield a standard deviation of less than .004 magnitudes using a sliding box averaging method. This means that a change in brightness can be measured of about .4% and much dimmer transits of other planets may be recorded from this telescope. Analysis methods using MathWork's MATLAB^ are being developed to gain more control over how pixels are combined to determine the brightness of stars and more effective modes of combining images.

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