The Wide-Field instrument (WFI) for the Roman Space Telescope (RST) features an imaging camera that comprises the Wide-Field Channel (WFC) with several bandpass filters, a spectroscopic dispersion unit called the Grism, and a Prism Assembly (PA), which took the place of the descoped Integral-Field Channel (IFC) assembly. The PA system consists of two prism elements made from S-TIH1 glass (P1) and CaF2 substrate (P2) that together will provide slitless low resolution spectroscopy with a spectral resolution R < 70 at all wavelengths, and R < 170 for wavelengths λ < 0.8 μm, across the full field. One key feature of the P1 element is the application of a bandpass coating that operates in the 0.75-1.8 μm spectral region. The extension of the bandpass towards short wavelengths greatly enhances the capabilities of RST for studies of stellar populations that provides additional means of testing in supernova studies. We have used spectroscopic techniques such as a double-beam monochromator and Fourier Transform InfraRed (FTIR) spectroscopy to characterize the spectral performance of the bandpass coatings of the P1 element. The coating technology used to produce these bandpass optical coatings has been demonstrated in the successful mission of the Mars Perseverance Rover in February of 2021.
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