Statistical Validation Of (Super-)Earth-size Planets Detections By Combining Kepler Follow-up Tools.

Details Statistical Validation Of (Super-)Earth-size Planets Detections By Combining Kepler Follow-up Tools. Statistical Validation Of (Super-)Earth-size Planets Detections By Combining Kepler Follow-up Tools.

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21821107f&link_type=abstract

American Astronomical Society, AAS Meeting #218, #211.07; Bulletin of the American Astronomical Society, Vol. 43, 2011

Physics

Optics

Scientific paper

We first model Kepler transit light curves assuming it is 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 from WIYN at Kitt Peak, Adaptive optics image using the PHARO instrument at Palomar, 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 observation excludes that it could be due to a blend of a significantly different spectral type.
Combining Blender results with these observational constraints, we determine a false alarm rate that an observed signal could be a blend. Provided this number is low enough, we can validate that the observed signal corresponds to a small planet detection. We illustrate this technique with the discoveries of Super-Earths Kepler-9d, Kepler-10b and -c.

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