We propose the development of a novel laser-based gyro and accelerometer, pushing the sensitivity to the fundamental limit. The device is based on two correlated frequency combs of the same repetition rate, generated in a single laser cavity. Because of this correlation, while the bandwidth of a tooth of each comb is in the Megahertz range, the bandwidth of the interference is less than 0.1 Hertz. Dispersion control of the circulating laser pulses leads to a further increase in sensitivity of this intracavity phase interferometer. In addition to the boost in sensitivity, we will reduce the noise. The classical noise limit will be reached by classical means like a high repetition rate of the measurement and additional control loops. Applying the technique of squeezed light will then be used to approach the fundamental limit of sensitivity. The results achieved in Phase I on a discrete-components OPO will be applied to two fiber-OPO prototypes. These devices are expected to be competitive with the LIGO in terms of sensitivity. Potential NASA Applications (Limit 1500 characters, approximately 150 words): Potential NASA applications include all future inertial navigation systems for which SWaP reduction is critical. A lightweight expandable gyro and miniaturized accelerometer have application in commercial navigation. Because the fiber laser can be made of very large perimeter and is of unprecedented sensitivity, it can have applications in monitoring the motion of tectonic plates. Furthermore, the ring laser gyro and linear accelerometer can be used in aerospace navigation either stand-alone or as part of Inertial Measurement Units (IMU). Potential Non-NASA Applications (Limit 1500 characters, approximately 150 words): Aerial and naval navigation, especially if included in IMU's. Emerging market segments are for instance micro- and nano- satellites (SpaceX), commercial space flight (Blue Origin, Virgin), and autonomous road vehicles. Due to the high sensitivity, the gyroscope can also have applications in basic research, for direct observation of effects in General Relativity like the Lense-Thirring precession. Duration: 6
