Kinetic inductance detectors (KID) have great potential in astronomical observation, such as searching for exoplanets, because of their low noise, fast response and photon counting characteristics. In this paper, we present the design process and simulation results of a microstrip line coupled KIDs array for near-infrared astronomical observation. Compared with coplanar waveguide (CPW) feedlines, microstrip feedlines do not require air bridges, which simplify fabrication process. In the design part, we mainly focus on the impedance transforming networks, the KID structure, and the frequency crosstalk simulations. The test array has a total of 104 resonators with 8 rows and 13 columns, which ranges from 4.899 GHz to 6.194 GHz. The pitch size is about 200 µm and the frequency crosstalk is less than 50 kHz in simulation.
Aaron Steiger, Ritoban Basu Thakur, Nikita Klimovich, Shibo Shu, Eitan Rapaport, Junhan Kim, Peter Day, Tzu-Ching Chang, Olivier Dore, Erik Shirokoff, Pete Barry, Philip Mauskopf, Farzad Faramarzi, Emily Linden, Christina Bell
Kinetic Inductance Detectors fulfil their great promise of large pixel numbers due to their easiness of multiplexing, as has been witnessed by the astronomic instruments that have become available over the last years. However, the number of available pixels is currently limited by unavoidable scatter in the resonance frequency of individual pixels. We have studied this frequency scatter, and show that it is largely caused by fabrication inhomogeneities, giving rise to variations in critical dimensions on the 10% level. We discuss the intrinsic causes of these inhomogeneities, and possible solutions to avoid them. Moreover, we show that by performing a post-characterisation adaptation step of all individual pixels, we can recover the lost pixels. This result brings 10 kilopixel class KID arrays for mm-wave observation within reach.
The Kinetic Inductance Traveling-Wave Parametric Amplifier (KI-TWPA) has been demonstrating promise as a versatile amplifier that can provide wide instantaneous bandwidth, near quantum limited sensitivity and dynamic range high enough for use in a variety of practical applications including astronomical instruments. Until recently, work on these devices has concentrated on the microwave frequency range below about 10 GHz. Here will discuss a KI-TWPA design based on a microstrip transmission line that is compatible with operation throughout the millimeter-wave band. We present measurements characterizing nonlinearity and loss in the NbTiN microstrip lines used for the new KI-TWPAs as well as results on a waveguide-coupled implementation that shows gain in W-band in good agreement with a model calculation. This model suggests that wideband, quantum limited amplifiers operating up to several hundred GHz should be realizable.
LiteBIRD is a next generation satellite aiming for the detection of the Cosmic Microwave Background (CMB) B-mode polarization imprinted by the primordial gravitational waves generated in the era of the inflationary universe. The science goal of LiteBIRD is to measure the tensor-to-scaler ratio r with a precision of δr < 10-3♦, offering us a crucial test of the major large-single-field slow-roll inflation models. LiteBIRD is planned to conduct an all sky survey at the sun-earth second Lagrange point (L2) with an angular resolution of about 0.5 degrees to cover the multipole moment range of 2 ≤ ℓ ≤ 200. We use focal plane detector arrays consisting of 2276 superconducting detectors to measure the frequency range from 40 to 400 GHz with the sensitivity of
3.2 μK·arcmin. including the ongoing studies.
A focal plane based on MKID has been designed for cosmic microwave background (CMB) B-mode
polarization experiments. We are designing and developing a focal plane with broadband corrugated
horn array, planar OMT, 180 degree hybrid, bandpass filters, and MKIDs. The focal plane consists of 3
octave bands (55 - 108 GHz, 80 - 160 GHz, 160 - 320 GHz), 10 hexagonal modules. Broadband corrugated
horn-array has been directly machined from an Al block and measured to have a good beam shape which
is consistent with electromagnetic field simulations in octave bands. The horn array is designed to be low
standing-wave, light weight, and electromagnetic shield. The broadband 4 probes ortho-mode transducer
(OMT) is fabricated on Si membrane of an SOI wafer. A broadband 180 degree hybrid made with
coplanar waveguide (CPW) is used to reduce higher modes of the circular waveguide. Two bandpass
filters of each polarization are patterned with Nb microstrip. A prototype of the broadband corrugated
horn coupled MKIDs has been fabricated and tested.
We demonstrate a design of octave-band circular waveguide coupled planar ortho-mode transducer (OMT)
with Microwave Kinetic Inductance Detector (MKID) for LiteBIRD mission, a small-size satellite for cosmic
microwave background (CMB) polarization signal full-sky mapping. In our 4-pixel prototype design, each single
pixel is sensitive to two frequency bands (90 GHz and 150 GHz) corresponding to atmospheric window. Silicon
on insulator (SOI) has been selected for OMT structure and a broadband coplanar waveguide (CPW) 180-degree
hybrid is designed to cancel higher modes of a circular waveguide and add two signals from the fundamental
mode together. After a microstrip bandpass diplexer, a microstrip line to coplanar waveguide transition structure
couples signal to MKID. MKIDs are designed with Nb ground plane and Al/Ti bilayer center strip line to achieve
low frequency response and high sensitivity. A 4-pixel module is under test and we plan to deploy these multi-
chroic polarimeters on Nobeyama 45m telescope.
Wide field cryogenic optics and millimeter-wave Microwave Kinetic Inductance Detector (MKID) cameras with Si lens array have been developed. MKID is a Cooper-pair breaking photon detector and consists of supercon- ducting resonators which enable microwave (~GHz) frequency multiplexing. Antenna-coupled Aluminum CPW resonators are put in a line on a Si substrate to be read by a pair of coaxial cables. A 220 GHz - 600 pixels MKID camera with anti-reflection (AR) coated Si lens has been demonstrated in an 0.1 K cryostat. A compact cryogenic system with high refractive index materials has been developed for the MKID camera.
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