A Selective High-Resolution Metamaterial Filter for Infrared Spectroscopy

This proposal seeks to develop a technology that enables selective high-resolution (1-3 nm) infrared (IR) spectroscopy, in order to achieve higher science return on future NASA Planetary Science missions. We seek to advance, from a technology readiness level (TRL) of 3 to 4, a metamaterial spectral filter (MSF) which would open up access to higher spectral resolution than is typical of the state-of-the-art IR spectrometers (e.g. L’Ralph/Linear Etalon Imaging Spectral Array (LEISA), Mapping Imaging Spectrometer for Europa (MISE) or Moon Minerology Mapper (M3)) without increasing instrument size. IR spectroscopy is a critical element of planetary science missions, providing essential information about both planetary surfaces and atmospheres. An IR spectrometer equipped with this MSF would benefit science objectives of multiple New Frontiers (NF) and Flagship missions, as detailed below. This work needs to be funded now so there is sufficient time to advance this technology prior to the NF5 and Uranus Orbiter Probe (UOP) opportunities. This MSF technology has been previously developed with Small Business Innovation Research (SBIR), Earth Science Technology Office (ESTO)/ Advanced Component Technology (ACT) and ESTO/ Instrument Incubator Program (IIP) funding for central wavelengths longer than 3 µm, and has demonstrated high optical collection (f/#) and narrowband spectroscopy unattainable with other state of the art techniques. In the proposed effort we will develop the MSF fabrication technique for shorter wavelengths to enable the full bandpass of typical planetary science IR spectrometers (1-5 µm). We will carry out a detailed science/instrument trade study, where we will simulate data from various mission scenarios and determine the improved science return from higher resolution. We will trade which wavelength bands have high resolution, how high a resolution is beneficial, and how many channels in each band are necessary to obtain optimal signal-to-noise ratio (SNR) and science return relative to instrument size. We will determine the best set of spectral bands for each mission in a compact instrument volume, and then decide on what wavelength bands and bandwidths to use for fabricating our test filters at wavelengths shorter than 3 µm. We will then modify our fabrication method from the previous filter development programs to develop the process for shorter wavelengths. The fabrication process applies photolithograph, thin film deposition, and material etching in a multi-step process that produces predesignated spectral band active areas on the filter. We will measure transmission vs. wavelength and band central wavelength vs. angle of incidence. We will iterate between filter test and fabrication to optimize the fabrication process for the chosen bands. This will advance the MSF fabrication process TRL to 4 for λ < 3 μm. Further component development to TRL 6 in time for the UOP and NF 6 opportunities is considered low risk due to the substrate and meta-layer materials (Si, SiO2, ZnS and Ge, used as spaceflight optics previously).

Development of new proof-of-concept instruments, systems or components, including sampling technologies, that significantly improve instrument measurement capabilities to address high priority science goals of planetary missions.

This is a mature technology (TRL 7+) — the realistic path in is usually NASA's Technology Transfer Program: licensing an existing NASA patent, or a Space Act Agreement to use NASA facilities/expertise directly. NASA also runs a startup licensing program with no upfront fee for companies formed to commercialize a specific NASA technology.

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