List of Figures

	Figure 1: Some possible sources for ground based and space-borne detectors.
	Figure 2: Schematic of gravitational wave detector using laser interferometry.
	Figure 3: Proposed sensitivity for the LIGO 1 and planned LIGO 2 detectors.
	Figure 4: Schematic view of one suspension system for use in the GEO 600 interferometer.
	Figure 5: Prototype ‘monolithic’ fused silica test mass suspension. The mass (3 kg) here is of 12.5 cm diameter. Note final suspension will use four fibres.
	Figure 6: Michelson interferometers with (a) delay lines and (b) Fabry–Pérot cavities in the arms of the interferometer.
	Figure 7: The implementation of power and signal recycling on the two interferometers shown in the previous figure, Figure 6.
	Figure 8: The 10 m prototype gravitational wave detector at Glasgow.
	Figure 9: A bird’s eye view of the LIGO detector, sited in Hanford, Washington State.
	Figure 10: Sensitivity curves for VIRGO showing the total contribution of the important noise sources. The signal levels expected from a number of pulsars after six months of integration are shown as are signal levels from some compact binary systems of different mass and at different distances.
	Figure 11: Noise contributions to the expected sensitivity of the LIGO 2 interferometer.
	Figure 12: The proposed LISA detector.