A Method for Determining Precise Phase Shifts of Eclipses in EB Systems: Detecting Substellar, Non-Transiting Third Bodies in Kepler Mission Eclipsing Binary Light Curves.

Details A Method for Determining Precise Phase Shifts of Eclipses in EB Systems: Detecting Substellar, Non-Transiting Third Bodies in Kepler Mission Eclipsing Binary Light Curves. A Method for Determining Precise Phase Shifts of Eclipses in EB Systems: Detecting Substellar, Non-Transiting Third Bodies in Kepler Mission Eclipsing Binary Light Curves.

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21714012s&link_type=abstract

American Astronomical Society, AAS Meeting #217, #140.12; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

A third body orbiting an eclipsing binary induces a small phase shift in the eclipses due to the light time effect as the binary system orbits about the three-body barycenter. The presence of the small third-body is revealed by a periodicity in the phase shifts consistent with a Keplerian orbit.
We present a cross-correlation method that benefits from the nearly continuously sampled light curves now becoming available from the Kepler mission. For the template, we use a model light curve of the binary system that is stationary in phase (dP/dt=0, dω/dt=0, ...). A window function slides in time along both the observed light curve and template selecting a region for cross-correlation and the phase shift as a function of time is determined from the peak in the resulting correlation function.
We examine the sensitivity limits, through numerical experiments, to the detection of substellar and planet sized masses in multi-year orbits about EBs from Kepler mission light curves.

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