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Direct imaging of extra-solar planets has now become a reality, especiallywith the deployment and commissioning of the first generation of specializedground-based instruments such as the GPI, SPHERE, P1640 and SCExAO. Thesesystems will allow detection of planets 1e7 times fainter than their host star.  For space-based missions, such as EXCEDE, EXO-C, EXO-S, WFIRST-AFTA,different teams have shown in laboratories contrasts reaching 1e-10 within afew diffraction limits from the star using a combination of a coronagraph tosuppress light coming from the host star and a wavefront control system. Thesedemonstrations use a deformable mirror (DM) to remove residual starlight(speckles) created by the imperfections of telescope. However, all thesecurrent and future systems focus on detecting faint planets around a singlehost star or unresolved binaries/multiples, while several targets or planetcandidates are located around nearby binary stars such as our neighbor starAlpha Centauri.  Until now, it has been thought that removing the light of a companion star isimpossible with the current technology, excluding binary star systems fromtarget lists of direct imaging missions. Direct imaging around binaries ormultiples systems at a level of contrast allowing Earth-like planets detectionis challenging because the region of interest, where a dark zone is essential,is contaminated by the light coming from the host star's companion. We proposea method to simultaneously correct aberration sand diffraction of light comingfrom the target star. This method works even if the companion star is outsidethe control region of the DM (beyond its half-Nyquist frequency), by takingadvantage of aliasing effects.

Simulation of a method to directly image exoplanets around multiple stars systems