Virtual Interferometry for the Direct Search of Young Giant Exoplanets

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By placing an aperture mask onto the telescope pupil its angular resolution as well as its robustness with respect to phase noise can be significantly improved enabling the detection of forming giant exoplanets on solar system scales. However, the aperture mask blocks most of the light and therefore reduces the sensitivity which is a major caveat for the detection of faint companions.
Treating the full telescope pupil as a continuous array of interferometers and measuring a quantity called kernel-phase allows us take advantage of the improved resolution and robustness of an aperture mask without losing throughput. We are sensitive to young giant exoplanets on angular scales < 150 mas, which are scales inaccessible by coronagraphic observations.
In this talk, we briefly introduce the mathematical framework behind kernel-phase and present preliminary results of a re-analysis of NACO cube mode data.

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