Self-calibration of Coronagraphic OTF

Details Self-calibration of Coronagraphic OTF Self-calibration of Coronagraphic OTF

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007lyot.confe..40l&link_type=abstract

Proceedings of the conference In the Spirit of Bernard Lyot: The Direct Detection of Planets and Circumstellar Disks in the 21s

Computer Science

Scientific paper

Coronagraphic devices are well suited for extrasolar planetary system detection. By extinguishing the light coming from the central star, it allows a photon noise efficient detection. The drawback is a a speckle noise extremely difficult to calibrate, especially because it depends on time-dependant factors like gravitational deformations, temperature gradients, and pointing errors. We propose here an instrumental setup allowing self-calibration of the optical transfer function. The goal is to enable a coronagraphic instrument to detect extrasolar planets at very small angular distance from their parent star, between 0.7 to 5 lambda/d. The concept is based on the fact that, in this zone, the detection is limited by the optical defects instead of the photon noise. To do so, a 4 quadrant coronagraph is complemented by a pupil remapping system as described in Perrin et al. (2006).

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