We present an overview of quantum noise in gravitational wave
interferometers. Gravitational wave detectors are extensively
modified variants of a Michelson interferometer and the quantum
noise couplings are strongly influenced by the interferometer
configuration. We describe recent developments in the treatment of
quantum noise in the complex interferometer configurations of
present-day and future gravitational-wave detectors. In addition,
we explore prospects for the use of squeezed light in future
interferometers, including consideration of the effects of losses,
and the choice of optimal readout schemes.
The LIGO project has completed the installation of large fused silica optical components in the vacuum systems of its observatories. Commissioning work on the Hanford 2 km interferometer has determined an upper limit to the optics losses, allowing comparison with design and pre-installation testing. Planning and development of sapphire optics for the next generation, advanced LIGO detector is now underway, including polishability, optical homogeneity, absorption, and birefringence. The advanced optics development also includes research aimed at lowering coating loss.
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