The LIGO interferometers collect enormous amounts of data, in addition to the primary gravitational wave strain channel. I will discuss ways in which we can use this auxiliary information to improve the controls topology of the detectors, which can lead directly to improvements in sensitivity to gravitational waves. I will also discuss areas where we could be collecting and utilizing even more data than we do currently, to remove noise sources that will limit the low frequency sensitivity of future ground-based detectors.
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