Progress Toward a Laser Interferometer Gravitational-Wave Observatory.

Physics

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The Laser Interferometer Gravitational-Wave Observatory ( Supported by the National Science Foundation under Cooperative Agreement No. PHY-9210038.) (LIGO) is being constructed to observe gravitational waves of cosmic origin by measuring the small apparent displacements that such waves produce between suspended test masses. This technique is inherently capable of providing broad-band information about the gravitational waveforms, from which the dynamical evolution of the sources may be inferred. Among the possible sources to be observed by LIGO are the non-axisymmetric collapse of a stellar core to form a neutron star or black hole, the inspiral and coalescence of orbiting neutron stars or black holes, the rotation of neutron stars with deformed crusts and a stochastic background of gravitational radiation. Construction has begun at the two LIGO observatory sites in Hanford, WA and Livingston, LA. Each facility will house laser interferometers consisting of two 4-km-long Fabry-Perot optical resonators in an L-shaped geometry. The interferometers will sense the apparent displacements between the mirrored test masses of the optical resonators, which are expected to be of the order of a thousandth of a fermi. A test interferometer with 38.5-m-long resonators has been built and has succeeded in demonstrating sensitivity to displacements of approximately 10-17 meters over a bandwidth of 2500 Hz. This talk will review the physical principles behind LIGO and present results from the ongoing interferometer R&D effort.

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