Gravitational Wave Astronomy: Listening To The Universe

Giles Hammond, University of Glasgow, Physics and Astronomy, Glasgow, United Kingdom

Contact First Author: Giles Hammond; giles.hammond@glasgow.ac.uk

Previously Published Material: 1. C. Bell et al., Experimental results for nulling the effective thermal expansion coefficient of fused silica fibres under a static stress, Classical and Quantum Gravity, 065010, 2014      2. S. Aston, et al., Update on quadruple suspension design for Advanced LIGO, Classical and Quantum Gravity, 235004, 2012     3. K. Tokmakov et al., A study of the fracture mechanisms in pristine fused silica fibres using high speed imaging techniques, Journal of Non-Crystalline Solids, 358, 1699-1709, 2012     4. G.D Hammond et al., Reducing the Suspension Thermal Noise of Advanced Gravitational Wave Detectors, Classical and Quantum Gravity, Vol. 29, 124009, 2012      5. A.V. Cumming et al., Design and development of the advanced LIGO monolithic fused silica suspension, Classical and Quantum Gravity, Vol. 29, 035003, 2012.

Abstract ID#: 35317

 

English Abstract:
Gravitational wave detectors are the most sensitive length measuring devices in the world. They are broadband long baseline interferometers capable of achieving 10-19m/√Hz at a frequency of 10Hz, and operating up to a few kHz. A worldwide network of 2nd generation detectors is currently under construction/commissioning. This includes the US LIGO detectors with 4km long arms, the 3km VIRGO detector in Italy, GEO-HF in Germany and the KAGRA 3km detector in the Kamioke mine. The goal of these detectors is to measure gravitational waves, tiny ripples in spacetime which are produced by the most extreme environments in the universe; including supernova, coalescing neutron stars and black holes. This will open a new window on the universe which is complimentary to our current electromagnetic view.

The detectors are limited by a variety of fundamental noise sources including gravity gradient noise, seismic noise, thermal noise and quantum noise. The latter is the effect of the Heisenberg uncertainly principle as applied to the free test masses of the interferometer. In this talk I will provide an overview of the science & sources which are being pursued and some of the technical challenges & hardware development necessary to push the limits of detection sensitivity; this will include the technology to hang 40kg mirrors on fused silica fibres for ultra low thermal noise systems and low scatter optical coatings. Many of these technologies have spin-offs in the field of precision measurement and gravity sensing, including fused silica borehole meters and low frequency MEMS gravimeters. I will further describe the future opportunities in the field, plans for future ground-based and space-based detectors, and the remarkable potential of gravitational wave astronomy.

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