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.
Similar wavefront error information for the Integral Field Channel (IFC) is provided in the next file, for two locations in the optical path: the image slicer and the detector surface. WFE information at the slit mirrors is not yet available. The IFC resolving power vs. wavelength tables are included in one of the tabs in this spreadsheet.
Sample PSF calculations for the IFC are provided in the next file:
The ordering of the tabulated PSF data in this file is the same as for a displayed image: the first row in the table corresponds to the top of the image, and the first column corresponds to the left edge of the image, etc.
Information on the pupils is provided in the next set of files. The first file describes the orientation of the pupils, and includes other relevant information:
This spreadsheet gives the effective area for the wide-field imager through each filter and through the grism, and for both IFC channels. This version provides two updates for the IFC: the throughput has been improved and the bandpass has been extended to 0.42 microns.
The next file is the same, but has a new IFC prism design with higher throughput:
This spreadsheet provides a calculator for each SCA giving the mapping in both directions between sky angle and wavelength to detector position.