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No full textInterferometric gravitational wave antennas are based on Michelson interferometers whose sensitivity to small differential length changes has been enhanced by adding multiple coupled optical resonators. The use of optical cavities is essential for reaching the required sensitivity, but sets challenges for the control system which must maintain the cavities near resonance. The goal for the strain sensitivity of the Laser Interferometer Gravitational-wave Observatory (LIGO) is 10 −21 rms, integrated over a 100 Hz bandwidth centered at 150 Hz. We present the major design features of the LIGO length and frequency sensing and control system which will hold the differential length to within 5×10 −14 m of the operating point. We also highlight the restrictions imposed by couplings of noise into the gravitational wave readout signal and the required immunity against them.
file C:\User\Daniel\Papers\ICALEPCS\Title.fm- printed November 26, 2001READOUT AND CONTROL OF A POWER-RECYCLED INTERFEROMETRIC GRAVITATIONAL WAVE ANTENNA ∗
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No full textPublication LIGO-P010038-00- D 11/8/01 Readout and control of a power-recycled interferometric gravitational wave antenn
The population of merging compact binaries inferred using gravitational waves through GWTC-3 - Data release
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- Écl. Norm. Supérieure
- Publication venue
- ZENODO
- Publication date
- 19/04/2023
- Field of study
No full textData associated with Figures, Tables, and population parameter samples associated with The population of merging compact binaries inferred using gravitational waves through GWTC-3 , LIGO DCC, arXiv, PRX. This is v2, superseding v1. Please see the README.md for more information
