The validation of Kepler planet detections

Physics – Optics

Scientific paper

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Scientific paper

Many of the most interesting candidate transiting planets identified by the Kepler Mission can not be confirmed by spectroscopic means, with the detection of the reflex motion of the star. These include rocky planets in the habitable zone of their parent stars. The Kepler team has developed ways of "validating" candidates by modeling the photometry to place constraints on the wide range of false positives ("blends") that can mimic the transit light curves. We model Kepler transit light curves assuming they are the result of the brightness variations of an eclipsing binary being attenuated by the brighter candidate star. This so-called 'Blender' study allows identifying the range of spectral type and magnitude difference compared to the target for possible blends.
We combine the frame of the Blender results with constraints from the different follow-up observations. Speckle interferometry, Adaptive optics imaging, and the detection of a centroid shift during the transit in the Kepler photometric aperture, all combine to constrain the possible separation of an unseen background star. We also observe the most interesting targets with WarmSpitzer to check the achromaticity of the transit signal. This presentation will describe the Blender modeling, and how it is combined with complementary constraints from follow-up observations to estimate the frequency of blends, and ultimately the probability that a candidate is a bona-fide planet. We illustrate this technique with the discoveries of several Super-Earths.

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