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arXiv:2610.24838

An Enhanced Intersecting-Lines Method for Optical Loss Characterization in SIS Heterodyne Receivers

François Joint, Magnus Strandberg, Denis Meledin, Igor Lapkin, Sven-Erik Ferm, Mathias Fredrixon, Leif Helldner, Alexei Pavolotsky, Erik Sundin, Victor Y. Belitsky, Vincent Desmaris

Published Oct 17, 2026• 0 citations
arXivHTMLPDF

Abstract

Accurate knowledge of radio-frequency (RF) losses in front of superconductor--insulator--superconductor (SIS) mixers is essential for optimizing millimeter- and terahertz heterodyne receivers. However, such losses are difficult to extract from conventional hot/cold-load measurements because the measured receiver noise combines contributions from the input optics, the mixer, and the intermediate-frequency chain. In this work, we present a numerical implementation of the straight-line, or intersecting-lines, method for estimating input-referred RF noise and optical loss from standard Y-factor measurements. Hot/cold IF spectra are acquired while sweeping the local oscillator (LO) pumping level from under-pumped to over-pumped operation, so that each IF frequency bin gives a family of linear relations between receiver output power and input load temperature. We evaluate all pairwise intersections between these lines and analyze the crossing cloud to obtain the effective RF input noise. We repeat the analysis across the IF band and multiple LO tunings which provides a frequency-resolved characterisation of the input losses over the full band. Our implementation turns the straight-line technique into a reproducible framework for receiver characterisation and relative optical-loss comparison in low-loss front-end configurations.

DOI
10.48550/arxiv.2610.24838

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The development of quantum limited heterodyne receivers requires that you understand and are able to measure the major sources of noise in the receiver system. The major sources of noise in millimeter- and submillimeter-wave SIS heterodyne receivers are the optical front end losses, vacuum fluctuation noise associated with the RF coupling efficiency to the SIS tunnel junction and IF amplifier noise. Although there are several methods for estimating the optical losses and IF amplifier noise, the RF coupling efficiency or quantum efficiency has been much more difficult to ascertain. This paper describes in situ techniques for measuring all three noise contributions in a standard receiver used for astronomical observations. Results are presented for the receivers operating in the Owens Valley Millimeter Interferometer Array.>

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Accurate knowledge of radio-frequency (RF) losses in front of superconductor--insulator--superconductor (SIS) mixers is essential for optimizing millimeter- and terahertz heterodyne receivers. However, such losses are difficult to extract from conventional hot/cold-load measurements because the measured receiver noise combines contributions from the input optics, the mixer, and the intermediate-frequency chain. In this work, we present a numerical implementation of the straight-line, or intersecting-lines, method for estimating input-referred RF noise and optical loss from standard Y-factor measurements. Hot/cold IF spectra are acquired while sweeping the local oscillator (LO) pumping level from under-pumped to over-pumped operation, so that each IF frequency bin gives a family of linear relations between receiver output power and input load temperature. We evaluate all pairwise intersections between these lines and analyze the crossing cloud to obtain the effective RF input noise. We repeat the analysis across the IF band and multiple LO tunings which provides a frequency-resolved characterisation of the input losses over the full band. Our implementation turns the straight-line technique into a reproducible framework for receiver characterisation and relative optical-loss comparison in low-loss front-end configurations.
We present measurements on two high frequency S(uperconductor)I(nsulator) S(uperconductor) heterodyne receivers at 660 GHz and 810 GHz. Their noise temperatures are 163 K and 860 K, respectively. The contribution of the high frequency (RF) input loss to this number is measured with the commonly used method of intersecting lines. The result is compared to a more rigorous analysis using the full quantum theory of mixing. We will show that in this frequency range the method of intersecting lines in general leads to an overestimation of the RF input loss. Even at 660 GHz, with a well matched SIS junction, the input noise contribution is overestimated by about 25 percent. This is due to the summation of the contributions due to the vacuum fluctuations, which is the highest contribution, the mismatch at the intermediate frequency (IF), and the fact that the mixer output noise is not completely independent of local oscillator (LO) power. At 810 GHz, due to a much stronger loss-induced mismatch of the SIS junction, the mixer output noise varies considerably with LO-power. The large loss of approximately 8 dB directly in front of the mixer enhances this contribution to the measured RF input loss. The contribution of the IF-mismatch is likewise enhanced. Together with the contribution of the vacuum fluctuations, this can lead to an overestimation of the RF input noise by more than 100 percent, depending on the actual mismatch of the mixers. We therefore conclude that, for the severe mismatch that occurs in Nb based SIS mixers above 700 GHz, the method of intersecting lines gives incorrect results and the full analysis should be applied.
In the assessment of a superconductor-insulator-superconductor (SIS) mixer, the breakdown of the overall receiver noise into intrinsic mixer noise and noises from other components is indispensable. The input noise due to losses in front of the mixer is conventionally measured by assessing the receiver noise as a linear function of mixer conversion loss at low local oscillator power and extrapolating the line to an infinite gain. However, it has been observed that this method tends to overestimate the input noise. To address this, the underlying theory of the input noise measurement method was revisited. It was found that the product of mixer gain and noise, i.e., the output noise of the mixer, is not a constant with respect to LO power. Therefore, extrapolating the linear relation to a large gain, where the input noise is inferred, becomes problematic. Numerical simulations were conducted to validate this analysis. Finally, a two-step measurement approach is introduced, in which an attenuator is inserted in front of the SIS mixer at the 4-K cold stage, to obtain the actual RF input noise.
A good understanding of input radio-frequency (RF) noise contribution is of particular importance to the development of high-sensitivity superconducting hot electron bolometer (HEB) receivers. In terms of simulation results based on the hot spot model, we found that the output noise of HEB mixers is nearly linearly decreased with the mixer's bath temperature when the HEB mixer is operated at its optimum DC-bias regime under appropriate local-oscillator signal pumping, and the effect of this decrease on the receiver output power can be well corrected. Thus, we used an intersecting lines technique to measure the input RF noise temperature of a quasi-optical superconducting NbN HEB receiver, and the measured input RF noise temperature of the HEB receiver is around 300 K at 850 GHz. For comparison, we also evaluated the losses and equivalent noise temperatures of the quasi-optical components in the RF signal path. The evaluated input RF noise temperature is found to be smaller than the measured one.
This thesis describes the development of low-noise heterodyne receivers at THz frequencies for submillimeter astronomy using Nb-based superconductor-insulator-superconductor (SIS) tunneling junctions. The mixers utilize a quasi-optical configuration which consists of a planar twin-slot antenna and antisymmetrically-fed two-junctions on an antireflection-coated silicon hyperhemispherical lens. On-chip integrated tuning circuits, in the form of microstrip lines, are used to obtain maximum coupling efficiency in the designed frequency band. To reduce the rf losses in the integrated tuning circuits above the superconducting Nb gap frequency (~ 700 GHz), normal-metal Al is used to replace Nb as the tuning circuits. To account the rf losses in the micros trip lines, we calculated the surface impedance of the AI films using the nonlocal anomalous skin effect for finite thickness films. Nb films were calculated using the Mattis-Bardeen theory in the extreme anomalous limit. Our calculations show that the losses of the Al and Nb microstrip lines are about equal at 830 GHz. For Al-wiring and Nb-wiring mixers both optimized at 1050 GHz, the RF coupling efficiency of Al-wiring mixer is higher than that of Nb-wiring one by almost 50%. We have designed both Nb-wiring and Al-wiring mixers below and above the gap frequency. A Fourier transform spectrometer (FTS) has been constructed especially for the study of the frequency response of SIS receivers. This FTS features large aperture size (10 inch) and high frequency resolution (114 MHz). The FTS spectra, obtained using the SIS receivers as direct detectors on the FTS, agree quite well with our theoretical simulations. We have also, for the first time, measured the FTS heterodyne response of an SIS mixer at sufficiently high resolution to resolve the LO and the sidebands. Heterodyne measurements of our SIS receivers with Nb-wiring or Al-wiring have yielded results which arc among the best reported to date for broadband heterodyne receivers. The Nb-wiring mixers, covering 400 - 850 GHz band with four separate fixed-tuned mixers, have uncorrected DSB receiver noise temperature around 5hv/kb to 700 GHz, and better than 540 K at 808 GHz. An Al-wiring mixer designed for 1050 GHz band has an uncorrected DSB receiver noise temperature 840 K at 1042 GHz and 2.5 K bath temperature. Mixer performance analysis shows that Nb junctions can work well up to twice the gap frequency and the major cause of loss above the gap frequency is the rf losses in the microstrip tuning structures. Further advances in THz SIS mixers may be possible using circuits fabricated with higher-gap superconductors such as NbN. However, this will require high-quality films with low RF surface resistance at THz frequencies.
A heterodyne receiver equipped with fixed-tuned superconductor-insulator-superconductor (SIS) mixer is developed and characterized. A Martin-Puplett interferometer is used in the receiver as diplexer to combine the RF/LO signal. The receiver noise measurement indicates the lowest receiver noise temperature including the optical loss of the MPI is as low as 250K. The receiver noise temperature is below 400K in the IF center frequency and below 500K over whole IF passband for LO frequency tuned between 624-696GHz.
The development of quantum limited heterodyne receivers requires that you understand and are able to measure the major sources of noise in the receiver system. The major sources of noise in millimeter- and submillimeter-wave SIS heterodyne receivers are the optical front end losses, vacuum fluctuation noise associated with the RF coupling efficiency to the SIS tunnel junction and IF amplifier noise. Although there are several methods for estimating the optical losses and IF amplifier noise, the RF coupling efficiency or quantum efficiency has been much more difficult to ascertain. This paper describes in situ techniques for measuring all three noise contributions in a standard receiver used for astronomical observations. Results are presented for the receivers operating in the Owens Valley Millimeter Interferometer Array.>