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Direct observation of gravitational waves, which commenced with the detection of an event by LIGO in 2015, [1] plays a key role in gravitational wave astronomy.LIGO has been involved in all subsequent detections to date, with Virgo joining in August 2017.
Centre for Gravitational Physics Archived 2015-09-06 at the Wayback Machine: California Institute of Technology United States: 93 LIGO Lab, Caltech LIGO Astrophysics: California State University, Fullerton United States: 15 Gravitational Wave Physics and Astronomy Center: Canadian Institute for Theoretical Astrophysics Canada: 4 Gravitational waves
The expansion of worldwide activities in gravitational-wave detection to produce an effective global network has been a goal of LIGO for many years. In 2010, a developmental roadmap [ 97 ] issued by the Gravitational Wave International Committee (GWIC) recommended that an expansion of the global array of interferometric detectors be pursued as ...
Mathematically speaking, if is the amplitude (assumed to be small) of the incoming gravitational wave and the length of the optical cavity in which the light is in circulation, the change of the optical path due to the gravitational wave is given by the formula: [9] = with being a geometrical factor which depends on the relative orientation ...
Since the 1960s, various kinds of gravitational-wave detectors have been built and constantly improved. The present-day generation of laser interferometers has reached the necessary sensitivity to detect gravitational waves from astronomical sources, thus forming the primary tool of gravitational-wave astronomy.
The signal was named GW150914 (from gravitational wave and the date of observation 2015-09-14). [3] [11] It was also the first observation of a binary black hole merger, demonstrating both the existence of binary stellar-mass black hole systems and the fact that such mergers could occur within the current age of the universe.
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The effect of a passing gravitational wave would be to perturb the local space-time metric and cause a change in the observed rotational frequency of the pulsar. Hellings and Downs [ 6 ] extended this idea in 1983 to an array of pulsars and found that a stochastic background of gravitational waves would produce a correlated signal for different ...