All of the optical reference information below pertains to the "Cycle 6" point design for the WFIRST Observatory, which is the design that was presented at the Mission Concept Review, held on December 8-9, 2015. This is the baseline for studies in early Phase A.
This file contains a compendium of basic information on the WFIRST observatory:
This file gives the projection of instrument fields of view onto the sky (neglecting distortions). The numbering of the WFI detectors in this drawing corresponds to the Zemax 'Configurations' in the Zernike spreadsheet below.
This file contains a compendium of basic information on the WFIRST Wide-Field Instrument:
Point-spread functions for the WFIRST Wide-Field Instrument (aka 'Wide Field Camera') can be computed at any wavelength and at any position in the field of view, given knowledge of the pupil function. The following files give Zernike decompositions of the wavefront error and pupil masks needed to perform this calculation. The first file contains the Zernike coefficients for the WFI, and also provides a fit to distortions in WFI imaging mode (WIM), a mapping of WIM detector positions onto the sky, WFI SCA positions in the focal plane, etc. Zernike coefficients are also provided for the grism Wide-Field Spectroscopy Mode (WSM) in first order, and for a single field position in 0th and 2nd order.
The following file provides additional information on the contents of the Zernike spreadsheet.