Sensitive Mid and Far-IR Kinetic Inductance Detector Arrays for Space Astronomy

Over the past several years, NASA has been intensively studying future astrophysics missions at mid- and far-infrared wavelengths, including the flagship-class Origins Space Telescope (OST) and the probe-class Galaxy Evolution Probe (GEP). These mission studies follow the broad endorsement of a "Far-Infrared Surveyor" mission in the 2013 30-year roadmap study chartered by NASA, and the 2010 Decadal Survey recommendation for NASA participation in the JAXA/ESA SPICA far-IR mission. Not surprisingly, the OST and GEP studies have identified detector arrays as the highest-priority technology needing development. In this proposal, we offer to address essentially all of the fundamental detector needs for OST and GEP and for sub-orbital precursors, including the full 10-400 micron wavelength range, the varied sensitivity requirements, scalability to the desired array formats, and even to open a path toward highly stable photon-counting detectors needed for mid-IR biosignature characterization of terrestrial exoplanets with OST. We address all of these needs in a timely, integrated, highly efficient program by focusing on a single underlying technology, namely direct-absorption (microwave) kinetic inductance detectors (MKIDs or KIDs) using aluminum as the superconducting material. Our proposal aims squarely at the needs for OST and GEP: 1) sensitivity at or below 1e-19 W/root(Hz); 2) array architecture that enables efficient absorption at wavelengths from 10 to 350 micron, and 3) scalability to focal planes of >10^5 pixels. We will begin by increasing the sensitivity of our existing 350 micron feedhorn-coupled devices (which comfortably meet sub-orbital sensitivity requirements) by 1.5 orders of magnitude with a combination of lower operating temperature, higher quality films, and a reduced volume absorber. We will also push to shorter wavelengths, targeting first 30 micron and then 10 micron detectors, through use of new, efficient, and practical absorber geometries illuminated by scalable microlens arrays. This mid-IR capability will substantially reduce the cost and complexity of GEP and provide photon counting capability for high-stability mid-IR spectroscopic characterization of terrestrial exoplanets with OST, extending the initial work with JWST/MIRI. A successful conclusion to our proposed program would represent a substantial reduction of technological risk for future NASA mid- and far-IR missions such as OST and GEP, with demonstration of the sensitivity, wavelength range, and array formats needed for the baseline designs developed by these study teams. It would also open a path to high-stability mid-IR exoplanet characterization with OST via photon counting.

The Astrophysics Research and Analysis program (APRA) supports suborbital and suborbital-class investigations, development of detectors and supporting technology, laboratory astrophysics, and limited ground based observing. Basic research proposals in these areas are solicited for investigations that are relevant to NASA's programs in astronomy and astrophysics, including the entire range of photons, gravitational waves, and particle astrophysics. The emphasis of this solicitation is on technologies and investigations that advance NASA astrophysics missions and goals.

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