Status Report

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

By SpaceRef Editor
December 17, 2019
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Robert A. Woodruff, William C. Danchi, Sara R. Heap, Tony Hull, Stephen E. Kendrick, Lloyd R. Purvesb, Michael S. Rhee, Eric Mentzell, Brian Fleming, Marty Valente, James Burge, Ben Lewis, Kelly Dodson, Greg Mehle, Matt Tomic

(Submitted on 14 Dec 2019)

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

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM)

Journal reference: Journal of Astronomical Telescopes, Instruments, and Systems 024006 1 Apr Jun 2019 Vol. 5(2)

Cite as: arXiv:1912.06763 [astro-ph.IM] (or arXiv:1912.06763v1 [astro-ph.IM] for this version)

Submission history

From: Robert Woodruff 

[v1] Sat, 14 Dec 2019 01:16:10 UTC (946 KB)

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