Techniques and Instrumentation for Detection of Exoplanets VIII 2017
DOI: 10.1117/12.2274887
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Dynamic testbed demonstration of WFIRST coronagraph low order wavefront sensing and control (LOWFS/C)

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Cited by 36 publications
(22 citation statements)
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“…When, stacking the real and imaginary parts of allÊ OL ij (k − 1) into a column vectorÊ OL (k − 1), the control deviation is given by Eqs. (29) and (30),…”
Section: A Dark Hole Maintenance Algorithmmentioning
confidence: 96%
“…When, stacking the real and imaginary parts of allÊ OL ij (k − 1) into a column vectorÊ OL (k − 1), the control deviation is given by Eqs. (29) and (30),…”
Section: A Dark Hole Maintenance Algorithmmentioning
confidence: 96%
“…The Roman Space Telescope CGI will make use of a spatially filtered version of the ZWFS to sense and correct low-order wavefront errors using light reflected off the coronagraph focal plane mask (FPM). [29][30][31][32] When used without spatial filtering in the image plane, the spatial resolution of a ZWFS is limited by the number of detector pixels across the beam. For context, the ZWFS is also similar in principle to a point-diffraction interferometer.…”
Section: Introductionmentioning
confidence: 99%
“…However, because of the finite stellar diameter (~1 mas for a G type star at 10 pc) even with the charge 4 VVC, pointing jitter as low as 0.4 mas is required 5 . In summary, both sensing and correcting rigid body motion of the front end optics will be required to maintain a high contrast dark hole.…”
Section: Laser Gaugesmentioning
confidence: 99%
“…The signals can be fed back to a focus mirror (or a deformable mirror) and a pointing control mirror and subsequently off-loaded to the spacecraft attitude control system. However, this technique has not been demonstrated in the lab for jitter and wavefront control at the 10 -11 contrast level even for bright host stars [5] . The problem will become increasingly difficult as the magnitude of the host star diminishes.…”
Section: Introductionmentioning
confidence: 99%