LIGO Document G2100582-v1
- The seismic isolation in aLIGO attenuates seismic noise very well in the GW band. Nevertheless noise around 10 Hz prevents aLIGO to reach its theoretical limit and therefore reduces the observational volume. The main causes for access noise are auxiliary control loops from the power and signal recycling cavities as well as stray light. An additional stabilization at the HAM-ISI level could reduce the noise by successively adapting the control loop to the reduced input noise. A set of interferometers and optical levers is a suitable candidate for sensors at the HAM-ISI level. This talks presents the general idea and some preliminary work on the interferometer readout.
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