We present the design and testing of spaceflight multiplexing kinetic inductance detector (KID) readout electronics for the PRobe far-Infrared Mission for Astrophysics (PRIMA). PRIMA is a mission proposed to the 2023 NASA Astrophysics Probe Explorer (APEX) Announcement of Opportunity that will answer fundamental questions about the formation of planetary systems, as well as the formation and evolution of stars, supermassive black holes, and dust over cosmic time. The readout electronics for PRIMA must be compatible with operation at Earth-Sun L2 and capable of multiplexing more than 1000 detectors over 2 GHz bandwidth while consuming around 30 W per readout chain. The electronics must also be capable of switching between the two instruments, which have different readout bands,: the hyperspectral imager (PRIMAger, 2.5-5.0 GHz) and the spectrometer (FIRESS, 0.4-2.4 GHz). We present the driving requirements, design, and measured performance of a laboratory brassboard system.
The EXperiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM) is a balloon-borne telescope designed to survey star formation over cosmological time scales using intensity mapping in the 420 – 540 GHz frequency range. EXCLAIM uses a fully cryogenic telescope coupled to six on-chip spectrometers featuring kinetic inductance detectors (KIDs) to achieve high sensitivity, allowing for fast integration in dark atmospheric windows. The telescope receiver is cooled to ≈ 1.7 K by immersion in a superfluid helium bath and enclosed in a superfluid-tight shell with a meta-material anti-reflection coated silicon window. In addition to the optics and the spectrometer package, the receiver contains the magnetic shielding, the cryogenic segment of the spectrometer readout, and the sub-Kelvin cooling system. A three-stage continuous adiabatic demagnetization refrigerator (CADR) keeps the detectors at 100 mK while a 4He sorption cooler provides a 900 mK thermal intercept for mechanical suspensions and coaxial cables. We present the design of the EXCLAIM receiver and report on the flight-like testing of major receiver components, including the superfluid-tight receiver window and the sub-Kelvin coolers.
Atmospheric interference, noise, and attenuation are a few limitations that arise when observing emissions of sub-millimeter wavelengths using ground-based telescopes. On-going research conducted on high-altitude balloons allow a new direction in observing these distributed emissions and eliminates all possible atmospheric interference. All sub-millimeter balloons and ground-based telescopes could benefit from a compact, re-configurable, high gain, programmable amplifier module to use in their receivers. We have designed, built, and tested an amplifier module for the Astrophysics Stratospheric Telescope for High Spectral Resolution Observations at Sub-millimeter wavelengths (ASTHROS), which is a high-altitude balloon mission that utilizes high-spectral resolution spectrometry to analyze stellar feedback by mapping ionized gas from the Milky Way galaxy and other neighboring galaxies. Using a five-stage Intermediate Frequency (IF) Low Noise Amplifier (LNA) added to a readout chain using commercial off-the-shelf components, the amplifier module yields 74 dB of gain up to 3.5 GHz with 31.75 dB of programmable attenuation with relatively linear gain flatness of ±1 dB, all while consuming 2.25 W per module (9 V at 250 mA).
While the amplification techniques and technology in this field are not new, achieving such high gain in systems usually require a significant amount of space to be allocated onboard. To alleviate this issue, this amplifier module has a unique form factor that combines the entire amplifier chain and bias system all in one module, saving space and weight on the system. The form factor design also allows the module to be stacked on top of one another to provide a higher range of gain in the system. Currently, the modules can be stacked up to eight times, and can be connected to allow for full control of the system with the use of a microcontroller. Sub-millimeter systems can have a set of 8 modules, all while saving space and reducing used weight.
KEYWORDS: Sensors, Resonators, Digital signal processing, Inductance, Data conversion, Multiplexing, Signal to noise ratio, Frequency combs, Signal attenuation
The Prime-Cam instrument on the Fred Young Submillimeter Telescope (FYST) is expected to be the largest deployment of millimeter and submillimeter sensitive kinetic inductance detectors to date. To read out these arrays efficiently, a microwave frequency multiplexed readout has been designed to run on the Xilinx Radio Frequency System on a Chip (RFSoC). The RFSoC has dramatically improved every category of size, weight, power, cost, and bandwidth over the previous generation readout systems. We describe a baseline firmware design which can read out four independent RF networks each with 500 MHz of bandwidth and 1000 detectors for ∼30 W. The overall readout architecture is a combination of hardware, gateware/firmware, software, and network design. The requirements of the readout are driven by the 850 GHz instrument module of the seven-module Prime-Cam instrument. These requirements along with other constraints which have led to critical design choices are highlighted. Preliminary measurements of the system phase noise and dynamic range are presented.
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