Paul Fulda's Precision Interferometry in a New Shape: Higher-order PDF

By Paul Fulda

ISBN-10: 3319013742

ISBN-13: 9783319013749

ISBN-10: 3319013750

ISBN-13: 9783319013756

With his Ph.D. thesis, offered the following within the layout of a "Springer Theses", Paul Fulda received the 2012 GWIC thesis prize provided by way of the Gravitational Wave overseas Committee. The effect of thermal noise on destiny gravitational wave detectors is determined by the dimensions and form of the interrogating laser beam. It were recognized when you consider that 2006 that, in concept, higher-order Laguerre-Gauss modes may lessen thermal noise. Paul Fulda’s study brings Laguerre-Gauss modes an important leap forward. His paintings comprises analytical, numerical and experimental paintings on table-top setups in addition to experiments on the Glasgow 10m prototype interferometer. utilizing numerical simulations the LG33 mode used to be chosen because the optical mode to be validated. additional study via Paul and his colleagues due to the fact then focused on this mode. Paul has constructed and proven easy and potent ways to create this mode with diffractive optics and effectively confirmed its compatibility with the basic development blocks of gravitational wave detectors, specifically, optical cavities, Michelson interferometers and opto-electronic sensing and keep an eye on structures. via this paintings, Laguerre-Gauss modes for interferometers were remodeled from an basically unknown entity to a good understood alternative with an experimental basis.

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Extra resources for Precision Interferometry in a New Shape: Higher-order Laguerre-Gauss Modes for Gravitational Wave Detection

Sample text

By placing a mirror at the interferometer output it is possible to keep the light circulating in the interferometer, thus enabling very high light powers to be reached in the arms and improving the signal to shot noise ratio. Signal recycling may be considered a second generation technique, and so is described briefly in Sect. 7. GEO600 also makes use of so-called delay lines in the arms to increase the effective arm length. The LIGO, Virgo and TAMA detectors are all very similar in the principle of their design.

Rev. Lett. 45, 75–79 (1980) J. Harms, Y. Chen, S. Chelkowski, A. Franzen, H. Vahlbruch, K. Danzmann, R. Schnabel, Squeezed-input, optical-spring, signal-recycled gravitational-wave detectors. Phys. Rev. V. S. Bell, L. A. Barton, G. Cagnoli, D. Cook, L. Cunningham, M. D. M. Harry, A. Heptonstall, J. Hough, R. Jones, R. Kumar, R. A. Robertson, S. Rowan, B. A. Strain, K. Tokmakov, C. A. van Veggel, Design and development of the advanced LIGO monolithic fused silica suspension. Class. P. L. V. Kowalski, J.

The phase of light in the arms of an interferometer is dependent upon the refractive index of the medium which fills the arms. Therefore if the medium in one arm is of a higher refractive index than the medium in another arm, the interference at the beam-splitter will be affected. This very effect is used to measure refractive indices of materials in Michelson interferometers. In an interferometric gravitational wave detector however, any changes in these refractive indices will be observed at the output as noise.

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Precision Interferometry in a New Shape: Higher-order Laguerre-Gauss Modes for Gravitational Wave Detection by Paul Fulda

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