Low-noise 0.8-0.96- and 0.96-1.12-THz superconductor-insulator-superconductor mixers for the herschel space observatory

Jackson, B. D.; Lange, Gert de; Zijlstra, T.; Kroug, M.; Kooi, J.; Stern, Jeffrey A.; Klapwijk, T. M.

doi:10.1109/tmtt.2005.862717

Cited by 65 publications

(46 citation statements)

References 17 publications

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“…The invention of the superconducting tunnel junction or "SIS" mixer [25], [26], the development of a detailed quantum theory of its operation [27], and the discovery of a method for producing robust, high quality tunnel junctions using the refractory metal niobium [28] have resulted in the development far more sensitive submillimeter mixers, often approaching the quantum limit [15], and extending up to frequencies as high as 1.25 THz [29], [30]. The "photodiode picture" [10] provides the easiest way to understand the operation of SIS mixers.…”

Section: Coherent Vs Direct Detectionmentioning

confidence: 99%

“…Meanwhile, low leakage currents are possible using modern junction fabrication technologies incorporating either aluminum oxide [28] or aluminum nitride [30], [31] barriers. SIS receivers have transformed submillimeter astronomy, and provided much of the motivation for pursuing largescale projects such as the ALMA interferometer [32] and the Herschel Space Observatory [29], [33].…”

Section: Coherent Vs Direct Detectionmentioning

confidence: 99%

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Technology for Submillimeter Astronomy

Žmuidzinas

2007

2007 IEEE/MTT-S International Microwave Symposium

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Abstract-Despite about three decades of progress, the field of submillimeter astronomy remains quite challenging, because the detection technology is still under development and the transmission of the atmosphere is poor. The latter problem has been overcome by constructing submillimeter telescopes at excellent sites, first on Mauna Kea and later in Chile and Antarctica, and also by using airborne and space telescopes. Meanwhile, the improvements in technology over the past several decades have been remarkable. While considerable opportunities for improvement remain, existing detector and receiver technologies now often approach fundamental limits. This technological revolution has brought submillimeter astronomy from the fringes to the forefront of modern astrophysics and has stimulated major investments such as the 50-element ALMA interferometer and the ESA/NASA Herschel Space Observatory.

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Section: Coherent Vs Direct Detectionmentioning

confidence: 99%

Section: Coherent Vs Direct Detectionmentioning

confidence: 99%

Technology for Submillimeter Astronomy

Žmuidzinas

2007

2007 IEEE/MTT-S International Microwave Symposium

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“…14 ͑As is discussed in detail in Ref. 15, the 1.04-THz mixer design is a scaled version of the 650-GHz design, but with the substrate suspended in the substrate channel to reduce the magnitude and reactance of the waveguide probe impedance.͒ Waveguide mixers A and B described here make use of twin-junction tuning circuits that are similar to that used in Ref. 12 ͑see Fig.…”

Section: Mixer Design and Sis Device Fabricationmentioning

confidence: 99%

Niobium titanium nitride-based superconductor-insulator-superconductor mixers for low-noise terahertz receivers

Jackson

Lange

Zijlstra

et al. 2005

Journal of Applied Physics

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Integrating NbTiN-based microstrip tuning circuits with traditional Nb superconductorinsulator-superconductor ͑SIS͒ junctions enables the low-noise operation regime of SIS mixers to be extended from below 0.7 to 1.15 THz. In particular, mixers incorporating a NbTiN / SiO 2 / NbTiN microstrip tuning circuit offer low-noise performance below 0.8-0.85 THz, although their sensitivities drop significantly at higher frequencies. Furthermore, a microstrip geometry in which NbTiN is used as the ground plane material only ͑NbTiN / SiO 2 /Al͒ yields significant improvements in the sensitivities of SIS mixers operating up to 1.15 THz, with an upper operating frequency that depends upon the quality of the NbTiN layer, and thus its deposition process. Films deposited at room temperature have T c = 14.4 K and n,20 K ϳ 60 ⍀ cm, and offer low-noise performance up to 1 THz, whereas films deposited at 400°C have T c = 16 K and n,20 K ϳ 110 ⍀ cm, and offer low-noise performance up to 1.15 THz. Taken together, these results demonstrate that the high-frequency surface resistance of a NbTiN layer depends upon the film's structural properties. Most significantly, the drop in performance that is seen at F Ͼ 1 THz in mixers incorporating NbTiN ground planes deposited at room temperature is attributed to nonhomogeneities in the structural and electrical properties of these films, as is the poor performance of mixers that incorporate NbTiN wiring layers at F Ͼ 0.85 THz. The development of these NbTiN-based microstrip tuning circuits will enable the production of low-noise SIS mixers for the 0.8-0.96-and 0.96-1.12-THz frequency bands of the Heterodyne Instrument for the Far Infrared on board the European Space Agency's Herschel Space Observatory.

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“…Earlier works on 1 THz SIS mixer has been done using on-chip normal metal circuits and having a relatively narrow operation band [6], [7]. Recently a waveguide SIS mixer design with Nb/Al-AlO/Nb junctions and NbTiN circuit has been explored with a big success in order to provide a 0.96-1.12 THz SIS receiver for Herschel Space Observatory (HSO) HIFI instrument [8]. In our work for CASIMIR project the goal is to develop a quasi-optical SIS mixer with a broader RF band centered at 1 THz.…”

Section: Introductionmentioning

confidence: 99%