Local Oscillator Arrays at 1.46 THz &amp; 1.9 THz for GUSTO

Hesler, Jeffrey L.; Retzloff, Steven A.; Rowland, Cliff; Koller, Daniel; Crowe, T.W.

doi:10.1109/irmmw-thz.2018.8510181

Cited by 1 publication

(2 citation statements)

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“…However, only recent advances in some critical technologies have made receiver systems using multi-pixel arrays possible for airborne [18], balloon borne [28][29][30], and proposed instruments concepts for future space THz observatories [31][32][33]. The critical technologies include frequency multiplier-chain based multibeam LOs [34], high power QCLs [23,35], and LO multiplexing schemes based on Fourier phase gratings [36][37].…”

Section: Introductionmentioning

confidence: 99%

“…GUSTO will use compact 4x2 HEB mixer arrays. As LOs, for B1 and B2, frequency multiplier chain arrays will be used which are developed by Virginia Diodes Inc, Charlottesville in USA [34]. However, the B3 receiver will make use of a multi beam LO in a 4x2 pattern generated using a QCL developed by MIT at Cambridge in USA [23], which is multiplexed by an asymmetric Fourier phase grating developed by SRON/TUDelft [37].…”

Section: Introductionmentioning

confidence: 99%

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4×2 HEB receiver at 4.7 THz for GUSTO

Silva

Mirzaei

Laauwen

et al. 2018

Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX

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We have demonstrated three 4×2 hot electron bolometer (HEB) mixer arrays for operation at local oscillator (LO) frequencies of 1.46, 1.9 and 4.7 THz, respectively. They consist of spiral antenna coupled NbN HEB mixers combined with elliptical lenses. These are to date the highest pixel count arrays using a quasi-optical coupling scheme at supra-THz frequencies. At 1.4 THz, we measured an average double sideband mixer noise temperature of 330 K, a mixer conversion loss of 5.7 dB, and an optimum LO power of 210 nW. The array at 1.9 THz has an average mixer noise temperature of 420K, a conversion loss of 6.9 dB, and an optimum LO power of 190 nW. For the array at 4.7 THz, we obtained an average mixer noise temperature of 700 K, a conversion loss of 9.7 dB, and an optimum LO power of 240 nW. We found the arrays to be uniform regarding the mixer noise temperature with a standard deviation of 3-4%, the conversion loss with a standard deviation of 7-10%, and optimum LO power with a standard deviation of 5-6%. The noise bandwidth was also measured, being 3.5 GHz for the three arrays. These performances are comparable to previously reported values in the literature for single pixels and also other detector arrays. Our arrays meet the requirements of the Galactic/Extra-Galactic ULDB Spectroscopic Terahertz Observatory (GUSTO), a NASA balloon borne observatory, and are therefore scheduled to fly as part of the payload, which is expected to be launched in December 2023.

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