Superconductor-Insulator-Superconductor (SIS) mixers are currently the most widely used detectors in astronomical observations in the terahertz band. To meet the demands of future large-aperture terahertz radio telescopes for multipixel applications, this work focused on the integration technology of a 660 GHz 1×4 one-dimensional linear array SIS mixers. The SIS mixers based on Nb/AlN/NbN twin tunnel junctions. We developed the uniform distribution of local oscillator power by using an integrated waveguide and multi-path local oscillator power distribution network. We also integrated the passive frequency doubler and tripler at low temperature, and integrated four low-noise amplifiers with the mixer in the same block, resulting in a more compact structure. As a result, we successfully realized the simultaneous operation of four mixers in a cryogenic Dewar. This paper will provide a detailed description of the relevant design and testing results.
The Leighton Chajnantor Telescope (LCT) project, sponsored by Shanghai Normal University in collaboration with Caltech and the University of Concepción, is seeking to relocate the Caltech Submillimeter Observatory (CSO)[1] from Mauna Kea, Hawaii to Llano de Chajnantor Observatory on the Chajnantor Plateau in Chile. The LCT will be equipped with a new 345-GHz band heterodyne array receiver of 3×3 beams and quantum-limited sensitivity. Based on superconducting Nb/Al-AlOx/Nb tunnel junction (SIS) mixers, we have developed a compact 1×3 array as one unit of the new heterodyne array receiver. Detailed design and measurement results will be presented.
Superconductor–insulator–superconductor (SIS) mixers remain the choice of heterodyne mixers for single-dish telescopes and interferometers at millimeter and submillimeter wavelengths. Compared with conventional Nb/AlOx/Nb superconducting tunnel junctions, Nb/AlN/NbN ones have larger gap voltage and may reach critical-current density beyond 10kA/cm2, which are both of particularly interest in developing broadband SIS mixers. Here we report on the design and measurement of an SIS mixer based on Nb/AlN/NbN parallel connected twin junctions (PCTJ) incorporating NbTiN/SiO2/Al microstrip circuit. The junctions have a gap voltage of 3.18mV and a critical-current density of 15kA/cm2. The measured receiver noise temperature reach 5hν/kB among 200-260GHz band, and the mixer’s fractional bandwidth is about 40% centered at 230GHz.
Fourier phase gratings play a vital role in the multi-beam heterodyne receiver in sub-millimeter astronomical instruments. In this study, a 1×4 beam grating at 660 GHz is developed, by which the surface structure is generated with an iterative algorithm. Far-field beam pattern is simulated with FEKO, where a relative high efficiency of 91% as well as a uniformity of power distribution among 4 beams of less than 1% are obtained. The grating was manufactured in aluminum material by a micro-milling machine. A PC-controlled scanning stage is employed for the beam pattern measurement. Despite the discrepancy from the manufacture of less than 6 μm, measurement results exhibit a good agreement with simulation in both power efficiency and far-field spatial distribution.
Besides the sensitivity nearly approaching the quantum limit, the intermediate-frequency (IF) bandwidth is of particular interesting for Superconductor-insulator-superconductor (SIS) mixers for radio astronomy research. In this paper, we are going to present the characteristic of IF bandwidth of two type of NbN SIS mixers, Long distributed junctions and Parallel-connected twin junctions. Firstly, the relative mixer gain are measured with different IF load impedance (25Ω, 50Ω, 75Ω) for both two SIS mixers. And also the mixers gain with different IF load impedance is simulated to get the optimum IF load impedance over a relative large IF bandwidth (2-15GHz). Finally, an IF matching circuit is designed and measured associating with SIS mixers, the measurement results show that the mixers gain are flatter over a large IF bandwidth than with 50Ω IF load impedance.
Superconductor-insulator-superconductor (SIS) mixers, with nearly quantum-limited sensitivity, have been playing an important role in Terahertz astronomy. For practical THz SIS receivers, however, the measured noise temperatures are sometimes higher than the expected value. The extra noise is mainly due to considerable RF noise contribution from the receiver components such as beam splitter, Dewar window, and infrared filter. In this paper, we mainly present the simulation and measurement results of the three components with different materials and thicknesses. Their noise contributions are also analyzed.
In this paper, we will introduce a dual-THz-band SIS (Superconductor-Insulator-Superconductor) heterodyne radiometer system developed for the atmospheric profiling synthetic observation system project (APSOS). This THz system is intended to have a durable and compact design to meet the challenging requirements of remote operation. The system as well as its major components such as antenna tipping, quasi-optics, cryogenics, SIS mixers and FFTS backend will be discussed thoroughly. Some scientific simulation focusing on the atmospheric profiling components at THz bands will also be investigated.
We report on a twin-slot antenna coupled superconducting NbN hot electron bolometer (HEB) mixer designed for 1.6
THz. Terahertz (THz) radiation is quasi-optically coupled to the HEB with an uncoated elliptical Si lens. Measured DSB
receiver noise temperatures are 1500 K at 0.85 THz, 1200 K at 1.27 THz, 1100 K at 1.31 THz, 1100 K at 1.4 THz, and
1000 K at 1.63 THz. This value at 1.63 THz is reduced to 750 K when the hot/cold loads in vacuum are used. The
frequency dependence of the noise temperature is consistent with the measured FTS spectral response. The measured farfield
beam patterns of the lens/antenna combination show nearly collimated beams with the side lobes below -16dB by
adding a 40 μm extension to a standard Si elliptical lens design, which is understood by considering a slightly lower
dielectric constant of Si (εSi) of 11.4 instead of 11.7. The good performance of such NbN HEB mixers makes it suitable
for future high-resolution spectroscopic astronomical applications.
The submillimeter (submm) regime, ranging from 100 to 1000um, is an important frequency band for radio astronomy.
A large number of astronomical spectral lines are located in this frequency region. Compared with ground-based observation,
which is limited by the atmospheric absorption of signal, space borne platform provides perfect condition for
submm observation. Here we introduce some preliminary results for a compact 500GHz SIS (Superconductor-
Insulator-Superconductor) heterodyne receiver system developed for future space borne observation. Considering
low power consumption requirement for space applications, we adopt a high critical temperature (Tc) NbN/AlN/NbN
SIS tunnel junction for the mixer, a key component of the receiver system, which may work at relatively high temperature
around 10 K. All the components, including the SIS mixer, HEMT low noise amplifier and optical lens, are assembled
into a compact system. The whole system is cooled by a close-cycled 4K cryo-cooler in laboratory and test result
shows a good noise performance, less than 250K at the 500GHz band. Detailed simulation and experimental results will
be presented in this paper.
In this paper, we present the calculation of the impedance and beam pattern of a 6×6 twin-slot antenna array combined
with an extended hemispherical silicon lens. The self and mutual impedance of the twin-slot antenna array are simulated
by High Frequency Structure Simulator (HFSS), while its radiation pattern is computed by using ray-tracing inside the
lens and electric and magnetic field integration on its surface. The distance between two neighboring antennas is set as
282μm (0.61λ0 at 650GHz) to avoid the overlap between the main-lobe beams of the antenna elements. With good
imaging quality (i.e., with a Strehl ratio no less than 0.8), the minimum diameter of the lens is found equal to 23mm
(~50λ0 at 650GHz).
Access to the requested content is limited to institutions that have purchased or subscribe to SPIE eBooks.
You are receiving this notice because your organization may not have SPIE eBooks access.*
*Shibboleth/Open Athens users─please
sign in
to access your institution's subscriptions.
To obtain this item, you may purchase the complete book in print or electronic format on
SPIE.org.
INSTITUTIONAL Select your institution to access the SPIE Digital Library.
PERSONAL Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.