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Within these run periods, the instruments are capable of detecting gravitational waves. The first run, O1, ran from September 12, 2015, to January 19, 2016, and succeeded in its first gravitational wave detection. O2 ran for a greater duration, from November 30, 2016, to August 25, 2017. [3]
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 ...
The first IPTA data release was on the 12 February 2016, which provided a 2-sigma limit on the amplitude of the Gravitational Wave Background. [5]The second data release, on 10 September 2019, resulted in the detection of the expected red noise background but not of any supermassive black hole mergers.
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 ...
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 ...
Although there are many applications for pulsar timing arrays, the best known is the use of an array of millisecond pulsars to detect and analyse long-wavelength (i.e., low-frequency) gravitational wave background. Such a detection would entail a detailed measurement of a gravitational wave (GW) signature, like the GW-induced quadrupolar ...
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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.