The WFIRST CGI instrument team at JPL has provided the following sets of simulated images in order to facilitate investigations of optimum image processing algorithms and expected scientific performance.
As the instrument, optics simulations and observing scenarios mature, we will keep this page updated with the latest sets of simulated images.
These simulated CGI image time sequences (John Krist, JPL) are for direct imaging with the Hybrid Lyot Coronagraph (HLC) and the Shaped Pupil Coronagraph (SPC).
For HLC, speckle fields are produced in a 10% bandpass filter centered at 575 nm, with and without optical model uncertainty factors (MUFs).
For SPC, multiwavelength speckle fields are produced in a 18% bandpass centered at 770 nm, with and without optical MUFs.
The observing scenario is a combination of Reference Differential Imaging (RDI) and Angular Differential Imaging (ADI):
Fixed offsets in some SPC source-offset images, see README for details.
These files are used to model the performance of the WFIRST CGI. The optical WFE maps (John Krist, JPL) are a combination of mid-spatial-frequency and low-order errors representative of the WFIRST telescope and coronagraph optics as might be expected from manufacturing (polishing). The polarization aberration maps (John Krist, JPL) are wavelength-dependent combinations of low-order Zernike modes representative of what might be generated from the WFIRST telescope optics. The coronagraph mask files (A.J. Riggs and Dwight Moody, JPL) are for the two shaped pupil modes and one baselined hybrid Lyot coronagraph mode in the CGI. These files are meant to be used in the Phase B PROPER optical model maintained on Github at https://github.com/ajeldorado/proper-models/ in the wfirst_cgi subfolder. Refer to the "FALCO+PROPER" section at https://wfirst.ipac.caltech.edu/sims/Code.html for how to run closed-loop wavefront correction simulations of the WFIRST CGI.
The data can be found as a single zip file here.
These simulated CGI images (John Krist, JPL) are provided to evaluate the performance of the coronagraph. They represent optimal static dark hole fields (PSF and contrast) for the Shaped Pupil Coronagraph (SPC, over a 18% spectral bandpass centered at 800nm) and the Hybrid Lyot Coronagraph (HLC, over a 10% spectral bandpass centered at 550nm). These images correspond to the performance statistics and simulation results from Krist et al. and Traub et al. described at the WFIRST Coronagraph special section of JATIS 2016.
These simulated CGI image time sequences (John Krist, JPL) are for direct imaging with the Hybrid Lyot Coronagraph (HLC), over a 15% spectral bandpass centered at 550 nm, and for the following observing scenario (please see additional details in the README files):
Please see this (PDF) file for a more detailed description of the simulated data generation for the OS5 scenario.
SPOILER ALERT: this (PDF) file contains information about the planets injected into the simulated images. Do not look at this if your intent is to perform a blind retrieval exercise!