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As part of a study funded by NASA Headquarters, we are developing aProbe-class mission concept called the Cosmic Evolution Through UV Spectroscopy(CETUS). CETUS includes a 1.5-m aperture diameter telescope with a largefield-of-view (FOV). CETUS includes three scientific instruments: a FarUltraviolet (FUV) and Near Ultraviolet (NUV) imaging camera (CAM); a NUVMulti-Object Spectrograph (MOS); and a dual-channel Point Source Spectrograph(PSS) in the Lyman Ultraviolet (LUV), FUV, and NUV spectral regions. The largeFOV Three Mirror Anastigmatic (TMA) Optical Telescope Assembly (OTA)simultaneously feeds the three separate scientific instruments. That is, theinstruments view separate portions of the TMA image plane, enabling paralleloperation of the three instruments. The field viewed by the MOS, whose designis based on an Offner-type spectrographic configuration to provide wide FOVcorrection, is actively configured to select and isolate numerous field sourcesusing a next-generation Micro-Shutter Array (MSA). The two-channel cameradesign is also based on an Offner-like configuration. The Point SourceSpectrograph (PSS) performs high spectral resolution spectroscopy on unresolvedobjects over the NUV region with spectral resolving power, R~ 40,000, in anechelle mode. The PSS also performs long-slit imaging spectroscopy at R~ 20,000in the LUV and FUV spectral regions with two aberration-corrected, blazed,holographic gratings used in a Rowland-like configuration. The optical systemalso includes two Fine Guidance Sensors (FGS), and Wavefront Sensors (WFS) thatsample numerous locations over the full OTA FOV. In-flight wavelengthcalibration is performed by a Wavelength Calibration System (WCS), andflat-fielding is also performed, both using in-flight calibration sources. Thispaper will describe the current optical design and the major trade studiesleading to the design.

Optical design for CETUS: a wide-field 1.5m aperture UV payload being studied for a NASA probe class mission study