Development of large terahertz heterodyne receiver arrays for future space observations

Gan, Y.

doi:10.33612/diss.193635266

Cited by 1 publication

(1 citation statement)

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“…The mixer array is formed by aligning two wafers, that may offer a reliable and cheap technology for future large heterodyne arrays. The concept study of this new approach, including the choices of low noise amplifiers and spectrometers, has been described in detail in [71]. However, until such a solution is available, our approach can provide a feasible route for larger heterodyne HEB arrays, for example, for the proposed concept instruments HERO [32] or the farinfrared spectroscopic surveyor (FIRSS) [33].…”

Section: Scaling the Pixel Count In Heb Mixer Arraysmentioning

confidence: 99%

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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Section: Scaling the Pixel Count In Heb Mixer Arraysmentioning

confidence: 99%