Microshutter arrays are powerful tools enabling simultaneous spectroscopy of multiple objects within a single, crowded field-of-view. This technology is currently employed on the James Webb Space Telescope, and next-generation arrays are being proposed for future flagship missions such as LUVOIR and HabEx. For these future large missions, it is important to fully characterize the performance of the next-generation microshutter arrays in the lab, particularly in the ultraviolet range not probed with JWST. To this end, we have developed a laboratory testbed to measure the contrast between opened and closed shutters achievable with these devices.
We describe our efforts to build a Wide-Field Lyman alpha Geocoronal simulator (WFLaGs) for characterizing the end-to-end sensitivity of FORTIS (Far-UV Off Rowland-circle Telescope for Imaging and Spectroscopy) to scattered Lyman α emission from outside of the nominal (1/2 degree)2 field-of-view. WFLaGs is a 50 mm diameter F/1 aluminum parabolic collimator fed by a hollow cathode discharge lamp with a 80 mm clear MgF2 window housed in a vacuum skin. It creates emission over a 10 degree FOV. WFLaGS will allow us to validate and refine a recently developed scattered light model and verify our scatter light mitigation strategies, which will incorporate low scatter baffle materials, and possibly 3-d printed light traps, covering exposed scatter centers. We present measurements of scattering intensity of Lyman alpha as a function of angle with respect to the specular reflectance direction for several candidate baffle materials. Initial testing of WFLaGs will be described.
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