A monolithic microwave integrated circuit (MMIC) receiver can be used as a building block for next-generation radio astronomy instruments that are scalable to hundreds or thousands of pixels. W- band (75–110 GHz) low-noise receivers are needed for radio astronomy interfer- ometers and spectrometers, and can be used in missile radar and security imagers.
These receivers need to be designed to be mass-producible to increase the sensi- tivity of the instrument. This innovation is a prototyped single-sideband MMIC receiver that has all the receiver front-end functionality in one small and planar module. The planar module is easy to assemble in volume and does not require tuning of individual receivers. This makes this design low-cost in large volumes.
This work was done by Todd C. Gaier, Lorene A. Samoska, and Pekka P. Kangaslahti of Caltech; Dan Van Vinkle, Sami Tantawi, John Fox, Sarah E. Church, Judy M. Lau, Matthew M. Sieth, and Patricia E. Voll of Stanford University; and Eric Bryerton of NRAO for NASA’s Jet Propulsion Laboratory. For more information, download the Technical Support Package (free white paper) at www.techbriefs.com/tsp under the Electronics/Computers category. NPO-47348
This Brief includes a Technical Support Package (TSP).
Ultra-Low-Noise W-Band MMIC Detector Modules
(reference NPO-47348) is currently available for download from the TSP library.
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Overview
The document is a Technical Support Package from NASA's Jet Propulsion Laboratory (JPL) detailing the development of Ultra-Low-Noise W-Band MMIC (Monolithic Microwave Integrated Circuit) Detector Modules. It serves as a technology demonstration for a future 1000-element MMIC interferometer designed to measure the polarization of the Cosmic Microwave Background (CMB). The primary goal is to enhance sensitivity and polarization purity to search for signatures of inflation and other fundamental physics processes in the B-modes of CMB polarization.
The document outlines the advantages of using MMIC interferometers, particularly their ability to reject common-mode systematic noise, which is crucial for accurate measurements in radio astronomy. It highlights the significance of previous experiments, such as the Cosmic Background Imager (CBI) and the Degree Angular Scale Interferometer (DASI), which played pivotal roles in the early detection of CMB polarization and the measurement of acoustic peaks in the polarization power spectrum. However, it notes that a significant increase in capability beyond these experiments is necessary to detect the faint B-mode component effectively.
The document describes the development of key technologies for the interferometer, including the design, fabrication, and assembly of four W-band prototype modules equipped with orthomode transducers. These transducers are essential for splitting the receiver signal into left- and right-hand circular polarization, which is critical for accurate polarization measurements.
The document emphasizes that while raw sensitivity is important, the real challenge for the next generation of CMB measurements lies in minimizing systematic effects. It suggests that the interferometric approach, despite having fallen out of favor due to the complexity and cost of larger experiments, offers unique advantages in reducing systematics and improving measurement accuracy.
Overall, the Technical Support Package provides a comprehensive overview of the advancements in MMIC technology and its applications in CMB research, highlighting the ongoing efforts to push the boundaries of our understanding of the universe through improved observational techniques. The document serves as a resource for those interested in the intersection of aerospace technology and fundamental physics, showcasing NASA's commitment to innovation and exploration.
