The optical loss study of molecular layer for a cryogenic interferometric gravitational-wave detector
arXiv:2006.16772 · doi:10.1103/PhysRevD.102.022009
Abstract
The detection of gravitational-waves provides us with a deep insight into the universe. In order to increase the number of detectable gravitational-wave sources, several future gravitational-wave detectors will operate with cryogenic mirrors. Recent studies, however, showed residual gas molecules inside the vacuum chamber adhere to the cryogenic mirror surface and form a molecular layer which grows with time. The growing molecular layer introduces an additional optical loss in the mirror which can decrease the detector's performance. We theoretically estimate the optical loss by the molecular layer in a cryogenically operated gravitational-wave detector. The impacts on a cryogenic gravitational-wave detector is discussed based on the results of optical loss estimation.
References in corpus (12)
- Observation of Gravitational Waves from a Binary Black Hole Merger
- Gravitational Waves and Gamma-rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A
- Characterization of the LIGO detectors during their sixth science run
- Interferometer design of the KAGRA gravitational wave detector
- Detector configuration of KAGRA - the Japanese cryogenic gravitational-wave detector
- J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817
- A Cryogenic Silicon Interferometer for Gravitational-wave Detection
- Theory of amorphous ices
- First cryogenic test operation of underground km-scale gravitational-wave observatory KAGRA
- Adaptive thermal compensation of test masses in advanced LIGO
- Quantum noise of non-ideal Sagnac speed meter interferometer with asymmetries
- Molecular adsorbed layer formation on cooled mirrors and its impacts on cryogenic gravitational wave telescopes