Low Noise Receivers for Future Observatories

There are many competing requirements for low noise receivers, including ultra-low noise performance, wide frequency bandwidth, low power consumption, low cost, reliability, high gain and stability. Not all of these requirements can be fulfilled by one design approach, choice of semiconductor technology or type of low noise amplifier; different applications will have different requirements and therefore require different approaches to the design. The aim of the PhD programme is to design the low noise receivers needed for near future astronomy instrumentation at radio and other wavelengths. A major part of the design challenge is the choice of semiconductor technology for the receiver components based on the intended application and required performance. This technology is continually evolving and producing receivers with state-of-the-art performance requires keeping abreast of the next generation of semiconductor technology that can be exploited for astronomy applications, from newly commercially available transistor technologies to forefront and emerging research technologies. In addition, the precision characterisation of low noise amplifiers as well as the transistors and other components within the receiver is an essential aspect of the design and testing process. This is not only to ensure the correct receiver behaviour after manufacture, but also during the design phase to ensure that the most accurate component models possible are being utilised in the simulations. Accurate and repeatable characterization of cryogenic receivers and components is very challenging but is of critical importance. It is the aim to work with the fore most technologies and processes with the goal of designing, building and testing improved devices, and to contribute, where astronomically relevant, to advancing device and process technologies.