CIRS-lite, a Fourier Transform Spectrometer for Low-Cost Planetary Missions

Passive spectroscopic remote sensing of planetary atmospheres and surfaces in the thermal infrared is a powerful tool for obtaining information about surface and atmospheric temperatures, composition, and dynamics (via the thermal wind equation). Due to its broad spectral coverage, the Fourier transform spectrometer (FTS) is pmiicularly suited to the exploration and discovery of molecular species. NASA's Goddard Space Flight Center (GSFC) developed the CIRS (Composite Infrared Spectrometer) FTS for the NASNESA Cassini mission to the Saturnian system. CIRS observes Satum, Titan, icy moons such as Enceladus, and the rings in thennal selfemission over the spectral range of 7 to 1000 ell11. CIRS has given us important new insights into stratospheric composition and jets on Jupiter and Saturn, the cryo-geyser and thermal stripes on Enceladus, and the winter polar vortex on Titan. CIRS has a mass of 43 kg, contrasted with the earlier GSFC FTS, pre-Voyager IRIS (14 kg). Future low-cost planetary missions will have very tight constraints on science payload mass, thus we must endeavor to return to IRIS-IeveI mass while maintaining CIRS-Ievel science capabilities ("do more with less"). CIRS-lite achieves this by pursuing: • more sensitive infrared detectors (high Tc superconductor) to enable smaller optics • changed long wavelength limit from 1000 to 300 flm to reduce diffraction by smaller optics • CVD (chemical vapor deposition) diamond beam-splitter for broad spectral coverage • single FTS architecture instead of a dual FTS architecture • novel materials, such as single crystal silicon for the input telescope primary.