We present a thermal kinetic inductance detector array design for CMB polarization observation at 90/150 GHz bands. A horn-coupled planar ortho-mode transducer is used for a broadband linear polarization separation. The frequency separation is done using a fast roll-off lumped-element diplexer. Thermal kinetic inductance detectors with Al is used as the detector. The array has more than 450 optical pixels with more than 1800 detectors. The array design and preliminary measurement results will be discussed.
The Next-generation Extended Wavelength-MUltiband Sub/millimeter Inductance Camera (NEW-MUSIC) on the Leighton Chajnantor Telescope (LCT) will be a first-of-its-kind, six-band, transmillimeter-wave (“trans-mm”) polarimeter covering 2.4 octaves of spectral bandwidth to open a new window on the trans-mm time-domain frontier, in particular new frontiers in energy, density, time, and magnetic field. NEW-MUSIC’s broad spectral coverage will also enable the use of the Sunyaev-Zeldovich effects to study accretion, feedback, and dust content in the hot gaseous haloes of galaxies and galaxy clusters. Six-band spectral energy distributions, with polarization information, will yield new insights into stellar and planetary nurseries. NEW-MUSIC will employ hierarchical, phased arrays of polarization-sensitive superconducting slot-dipole antennas, coupled to photolithographic bandpass filters, to nearly optimally populate LCT’s 14′ field-of-view with six spectral bands over 80–420 GHz (1:5.25 spectral dynamic range; 2.4 octaves). Light will be routed to Al or AlMn microstripline-coupled, parallel-plate capacitor, lumped-element kinetic inductance detectors (MS-PPC-LEKIDs), an entirely new KID architecture that substantially enhances design flexibility while providing background-limited performance. Innovative, wide-bandwidth, etched silicon structures will be used to antireflection-treat the back-illuminated focal plane. NEW-MUSIC will cost-effectively reuse much of the MUSIC instrument, initially deploying a quarter-scale focal plane capable of the bulk of NEW-MUSIC science followed later by a full-FoV focal plane needed for NEW-MUSIC wide-area survey science.
Future far-infrared (FIR) astronomy missions will need large detector arrays with high sensitivity. Low noise detectors with a noise equivalent power (NEP) of 3×10−19 to 1×10−20 W/Hz1/2 for space-based continuum observations are needed, to be photon noise limited. Transition edge sensor (TES) as a type of sensitive low-temperature superconducting detector, has significant advantages in the measurement of broad band electromagnetic radiation, from millimeter waves to X-ray and gamma-rays. We propose a design of low noise TESs for FIR applications, with the NEP of lower than 3×10−19 W/Hz1/2. The key component on TES bolometer island is aluminum-manganese (AlMn) superconducting film, which has been proved that its critical temperature can be adjusted over a wide range by baking after the film deposition. We optimize the NEP of AlMn TESs by reducing the critical temperature to around 60 mK and designing the thermally isolating legs to reduce the thermal conductance effectively. The pixel design will be used as foundation in our future TES array designs and will benefit high-sensitive detector development.
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.
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.