Focal plane wavefront sensor sensitivity for ELT planet finder

Details Focal plane wavefront sensor sensitivity for ELT planet finder Focal plane wavefront sensor sensitivity for ELT planet finder

Jul 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010spie.7736e.193b&link_type=abstract

Adaptive Optics Systems II. Edited by Ellerbroek, Brent L.; Hart, Michael; Hubin, Norbert; Wizinowich, Peter L. Proceedings o

Physics

Optics

1

Scientific paper

In the framework of Extremely Large Telescope (ELT), several instruments are considered for the characterization of extrasolar planets. Since the performance of such an instrument is limited by wavefront errors, the use of extreme Adaptive Optic (AO) systems is mandatory. Studies for future planet finder instruments such as SPHERE/VLT or GPI/GEMINI show that one limitation of the performance for a planet finder is the differential aberrations that are not measured by the wavefront sensor, which is physically separated from the common optics by a beam splitter. These defects create a field of residual speckles in the focal plane that need to be calibrated to separate the planet signal from the speckle noise [1]. We propose here to simultaneously estimate these aberrations and also detect the planet directly from the final science image. To do so, we propose to couple the foreseen extreme high speed AO of an ELT planet Finder with a low speed Self-Coherent Camera (SCC [2-5]). The SCC which is based on the principle of light coherence can both estimate the wavefront errors and reduce speckle noise by calibration. After recalling the principle of the SCC, we present simulation results of the SCC performance in the context of EPICS.

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