Roman Space Telescope CGI: prism and polarizer characterization modes

Tyler D. Groff; Neil T. Zimmerman; Hari B. Subedi; Maxime J. Rizzo; John Titus; Jim Lyons; Dylan Bell; Samuel Gaylin; Guangjun Gao; Bert Pasquale; Nicholas Nicolaeff; Motohide Tamura; Fang Shi

doi:10.1117/12.2562925

7 January 2021 Roman Space Telescope CGI: prism and polarizer characterization modes

Tyler D. Groff, Neil T. Zimmerman, Hari B. Subedi, Maxime J. Rizzo, John Titus, Jim Lyons, Dylan Bell, Samuel Gaylin, Guangjun Gao, Bert Pasquale, Nicholas Nicolaeff, Motohide Tamura, Fang Shi

Author Affiliations +

Proceedings Volume 11443, Space Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave; 114433D (2021) https://doi.org/10.1117/12.2562925
Event: SPIE Astronomical Telescopes + Instrumentation, 2020, Online Only

Conference Poster

Abstract

As part of its technology demonstration, the Nancy Grace Roman Space Telescope (RST) Coronagraph Instrument (CGI) will demonstrate point source spectroscopy and polarization measurements of disks. The specific implementation of spectroscopy is a zero-deviation Amici prism and a slit to be placed on the planet after high contrast has been achieved by CGI. The polarization optics are a set of Wollaston prisms so that orthogonal polarization states can be measured simultaneously. The CGI spectral characterization mode, being designed and built and Goddard Space Flight Center (GSFC), has a spectral resolution of R50 at its central wavelength and is designed to accommodate a 15% bandpass spanning 610􀀀785nm. In order to recover Stokes information, there are two sets of Wollaston prisms clocked 45 degrees with respect to one another with each measurement taken in series. The Wollaston design and optical elements are a contribution by the Japanese Aerospace Exploration Agency (JAXA), with final alignment and testing being done at GSFC. The spectroscopy mode is designed to target Methane absorption features around 730nm, keeping the spectral resolution as low as possible to improve the signal-to-noise ratio and hence reduce detection time. We highlight the requirements for these modes and address the challenge of on-orbit spectral calibration for a deployable slit in the presence of pointing drifts. Of unique interest is how the observatory error budget couples into good stellar spectrum calibration and subsequent speckle subtraction. We also provide further detail on the optomechanical design, its modeled performance, and operations concept. These performance metrics are simulated to demonstrate how a slit located at an arbitrary field point is homed onto the planet and converted to a calibrated spectrum.

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Tyler D. Groff, Neil T. Zimmerman, Hari B. Subedi, Maxime J. Rizzo, John Titus, Jim Lyons, Dylan Bell, Samuel Gaylin, Guangjun Gao, Bert Pasquale, Nicholas Nicolaeff, Motohide Tamura, and Fang Shi "Roman Space Telescope CGI: prism and polarizer characterization modes", Proc. SPIE 11443, Space Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave, 114433D (7 January 2021); https://doi.org/10.1117/12.2562925

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