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Abstract

Control of Scattered Light in Advanced LIGO

The phase shifts of the light fields scattered into the interferometer optical mode from baffles, beam dumps, optical elements, or from the vacuum enclosure walls that have seismic motion, will cause an apparent differential arm signal. The magnitude of the scattered light noise depends upon the particular location into which the light is injected; and for small phase angles, the phase noise is proportional to the rms amplitude of the horizontal displacement of the scattering surface and to the electric field amplitude of the scattered light. For Advanced LIGO, the total scattered light phase noise, expressed in equivalent displacement noise, must be < 1/10th of the quadrature sum of the suspension thermal noise and the test mass thermal noise.

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