Integrated Silicon Micromachined SIS-Heterodyne Array Instrument at 557 GHz

We propose to develop a highly integrated low power and low-mass 450-570 GHz silicon micromachined 16-pixel SIS-mixer based high-resolution spectrometer. This integrated component development technology at submillimeter wavelengths that will dramatically simplify the fabrication, assembly, and integration of large focal plane arrays. This technology has the potential to significantly increase the pixel count of detector arrays and reduce the mass, volume, and complexity of arrays for a broad range of applications in astrophysics. Since it is getting increasingly difficult to field submillimeter-wave heterodyne array instruments due to the lack large mission opportunities, it is high time we demonstrate the technology viability using SmallSat and CubeSat platforms. Towards that goal, this development will also include a ~15 cm aperture diameter spiral leaky-wave planar metasurface-based antenna with a circular waveguide feed, which can easily be integrated on the sidewalls of a CubeSat or SmallSat. The 16-pixel array spectrometer development includes SIS mixer-based receiver front end, integrated low-loss waveguide switch for differential radiometric calibration, and will use existing CMOS based low-power synthesizer and spectrometer. The scientific importance of high-resolution spectroscopic observations at submillimeter wavelengths is underscored by the key role of heterodyne spectrometers in the ESA cornerstone Herschel Space Observatory as well as the ground-based ALMA and airborne SOFIA. Star formation and key phases of galaxy evolution occur in region enshrouded by dust that obscures them at infrared and optical wavelengths, while the temperature range of the interstellar medium of ten to a few thousand Kelvin in these regions excites a wealth of submillimeter-wave spectral lines. With high-resolution spectroscopy, resolved line profiles reveal the dynamics of star formation, directly revealing details of turbulence, outflows, and core collapse. Observations of emission from ionized species such as water (557 GHz) and carbon (490 GHz) with a high-resolution array instrument with hundreds of pixel will change the way mapping is done for this important species. While the primary motivation to develop multi-pixel array technology arises from the need for future missions to study a wide range of astrophysical topics ranging from planet formation to the large-scale structure of the universe to the monitoring of the earth's atmosphere, this technology effort will also spawn synergistic systems involving other imaging sensors for reconnaissance usage and will help pioneer the emerging uses of the submillimeter-wave spectrum in the homeland security applications. Possible Reviewers: (i) Prof. Philip Mauskopf – Arizona State University (Philip.Mauskopf@asu.edu), (ii) Dr. Sander Weinreb – Caltech (sweinreb@caltech.edu), (iii) Dr. Theodore Reck – Virginia Diodes Inc. (theodore.reck@vadiodes.com), (iv) Dr. Berhanu Bulcha – NASA Goddard Space Flight Center (berhanu.t.bulcha@nasa.gov)

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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