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Halo Measurement Using Phase-Sorting Interferometry

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Imperfections, misalignments, aberrations, and even dust can significantly limit sensitivity in high-contrast imaging systems such as coronagraphs. An upstream deformable mirror (DM) can be used to correct or compensate for these flaws. To include non-common-path errors introduced after the an AO system closed loop, correcting measurements must be made with the science camera. Measurement of the phase and amplitude of a star's halo is sufficient to compute a compensating pupil DM shape that suppresses the scattered halo. Phase-Sorting Interferometry (PSI) is a technique that uses AO residual starlight speckles and wavefront sensor measurements to estimate the complex halo. We have demonstrated PSI on-sky at the 6.5m MMTO telescope using mid-IR L and M-band images.

© 2011 Optical Society of America

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