WFIRST-CGI Off-axis PSFs in HLC narrow FOV imaging mode ---------------------------------------------------------------------- Hanying Zhou Jet Propulsion Laboratory, California Institute of Technology January 7, 2019 Cleared for public distribution. Realistic off-axis PSF images in HLC narrow FOV imaging mode (filter Band 1) are provided for science modeling purposes. The simulation is based on a recent HLC design for the (pre-) phase B pupil, and uses near-latest (phase A) OTA misalignment + OTA+CGI surface aberrations + (phase B) polarization effects. ---------------------------------------------------------------------- This file package contains five *.fits files, one png file, and one .txt file: 20180718_hlc_nfov_PSFs_1Dcube.fits 20180718_hlc_nfov_PSFs_1Dcube_info.fits 20180718_hlc_nfov_PSFs_2Dcube.fits 20180718_hlc_nfov_PSFs_2Dcube_info.fits DH_mask0.fits offaxis_psfs_2D_grid.png readme.txt ---------------------------------------------------------------------- Description of PSF generation: The model consists of a full Fresnel diffraction model for high-accuracy contrast truth and an economical compact model for realistic wavefront control (dark hole digging), mimicking flight-constrained EFC performance. PSFs are taken post dark hole digging of a system* with CBE (Phase A) OTA misalignments + OTA/CGI surface aberrations + (Phase B) polarization effects. The dark hole is static, and no jitter was added. No detector noise was added. Post EFC control, off-axis sources are introduced as wavefront tilts, one at a time, and each resulting PSF image is obtained. A coarse 2D off-axis grid and a finer 1D off-axis scan of PSFs are simulated. HLC design: Dwight Moody 20180925-251 (narrow fov imager 1, 575nm @ 10% bw), for 20180718 (pre-) Phase B pupil. It includes an occulter mask and a Lyot stop. No field stop is used in this simulation, to provide full field information for users. The dark hole region is from 2.5~9 lambda/D, for D = 2.3631 m. Detector plane sampling: 0.2 lam/D per pixel * Most details about the model, the system condition, and the modeling tool, are described in: 1) Hanying Zhou, et al., "High Accuracy Coronagraph Flight Model for WFIRST-CGI Raw Contrast Sensitivity Analysis", Proc. SPIE, 10698-92 (2018) 2) John Krist, et al.,�WFIRST coronagraph optical modeling,� Proc. SPIE,10400-4 (2017) 3) John Krist, "PROPER: an optical modeling program for IDL," Proc. SPIE,66750P (2007) Also: http://proper-library.sourceforge.net ---------------------------------------------------------------------- Details on the HLC coarse 2D and fine 1D PSF cubes and their off-axis info. Column variables in xx_info.fits files: 1. ith PSF (as in xx_cube.fits file) 2. source x-offset in lam/D 3. source y-offset in lam/D 4. core throughput, in % Fraction of the power inside the PSF core (those >=0.5*PSF peak) relative to the power incident on the telescope primary 5. core area, in arcsec^2 Pixels whose value exceed half max of PSF peak Data in xx_2Dcube.fits file: 2D PSF of 128x128 size, total 429 each offset is sequentially defined in the companion xx_info.fits resolutions: 0.5 lam/D for 2.5- 5lam/D 1 lam/D for the rest of 0-9 lam/D see also the grid.png file Data in xx_1Dcube.fits file: 2D PSF of 128x128 size, total 85 each offset is sequentially defined in the companion xx_info.fits resolutions: 3mas (or 0.06 lam/D) for <4 lam/D 0.5 lam/D for 4-9 lam/D 0.25lam/D for 9-11 lam/D DH_mask0.fits This file can be used as visualization aid (use 'contour' in Matlab) to superimpose the mask on to a PSF image to see the boundary of dark hole area or to mask out (multiply directly with a PSF image) light outside the dark hole region ---------------------------------------------------------------------- contact hanying.zhou@jpl.caltech.edu for any questions or suggestions (c) 2019 California Institute of Technology. Government sponsorship acknowledged.