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Pink noise
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===In gravitational wave astronomy=== [[Image:Gravitational-wave detector sensitivities and astrophysical gravitational-wave sources.png|thumb|upright=2|Noise curves for a selection of [[gravitational-wave detector]]s as a function of frequency]] 1/''f''<sup> Ξ±</sup> noises with Ξ± near 1 are a factor in [[gravitational-wave astronomy]]. The noise curve at very low frequencies affects [[pulsar timing array]]s, the [[European Pulsar Timing Array]] (EPTA) and the future [[International Pulsar Timing Array]] (IPTA); at low frequencies are space-borne detectors, the formerly proposed [[Laser Interferometer Space Antenna]] (LISA) and the currently proposed evolved Laser Interferometer Space Antenna (eLISA), and at high frequencies are ground-based detectors, the initial [[LIGO|Laser Interferometer Gravitational-Wave Observatory]] (LIGO) and its advanced configuration (aLIGO). The characteristic strain of potential astrophysical sources are also shown. To be detectable the characteristic strain of a signal must be above the noise curve.<ref>{{cite web|title=Gravitational Wave Detectors and Sources|url=http://rhcole.com/apps/GWplotter/|access-date=17 April 2014|author=Moore, Christopher|author2=Cole, Robert |author3=Berry, Christopher |date=19 July 2013}}</ref>
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