One of the fundamental limits associated with an instrument of this type is the ability to detect differential phase shifts between the beams returning to the beamsplitter from the Fabry-Perot arm cavities. To achieve the planned sensitivity to gravitational radiation, this detection should be limited only by photon counting statistics (“shot noiseâ€) at a level of 8 x 10-11 radians/Hz between 150 Hz and 10 kHz.
The goal of this work is to develop and demonstrate the techniques which are necessary to achieve this optical phase sensitivity. A prototype recycled Michelson interferometer was constructed which reached an optical phase sensitivity of 12 x 10-11 radians/Hz above 600 Hz.
This thesis describes the methods used to achieve this optical phase sensitivity, and details the lessons learned from operating the prototype instrument. We pay particular attention to interferometric control of suspended optics, laser frequency control, and thermal lensing.
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