Abstract
The first detections of gravitational waves, GW150914 and GW151226, were associated with the coalescence of stellar mass black holes, heralding the opening of an entirely new way to observe the Universe. Many decades of development were invested to achieve the sensitivities required to observe gravitational waves, with peak strains associated with GW150914 at the level of 10−21. Gravitational wave detectors currently operate as modified Michelson interferometers, where thermal noise associated with the highly reflective mirror coatings sets a critical limit to the sensitivity of current and future instruments. This article presents an overview of the mirror coating development relevant to gravitational wave detection and the prospective for future developments in the field.
Highlights
Detecting gravitational waves has been one of the most challenging experimental projects ever to be undertaken
Crystalline coatings grown using molecular beam epitaxy (MBE) have been demonstrated to provide a three‐fold reduction in Brownian thermal noise [76] within an optical cavity (note that the Crystalline coatings grown using molecular beam epitaxy (MBE) have been demonstrated to title of the cited paper refers to a ten‐fold reduction in the thermal noise power: here, for consistency provide a three-fold reduction in Brownian thermal noise [76] within an optical cavity
LIGO detector are planned within the 2–3 years, a reduction in coating thermal noise is essential to reap the full benefits of future upgrades
Summary
Detecting gravitational waves has been one of the most challenging experimental projects ever to be undertaken. To achieve the sensitivities required to detect gravitational waves, significant optical power is required inside optical cavities of the interferometers in order towaves, reducedsignificant shot noise [6]. To achieve thethe sensitivities required to detect gravitational optical is a formidable challenge the required mirror specifications, in relation to the[6]. Optical required inside the opticalon cavities of the interferometers in order to reduced shot noise This sets losses associated with absorption and scatter. Optical losses will limit the achievable optical gainlosses a formidable challenge on the required mirror specifications, in relation to the optical within the cavities. Optical scatter produces stray light that may reenter the reflectivity required is >99.9%, with absorption levels of
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