List of Figures

View Image Figure 1:
Some possible sources for ground based and space-borne detectors.
View Image Figure 2:
Schematic of gravitational wave detector using laser interferometry.
View Image Figure 3:
Proposed sensitivity for the LIGO 1 and planned LIGO 2 detectors.
View Image Figure 4:
Schematic view of one suspension system for use in the GEO 600 interferometer.
View Image 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.
View Image Figure 6:
Michelson interferometers with (a) delay lines and (b) Fabry–Pérot cavities in the arms of the interferometer.
View Image Figure 7:
The implementation of power and signal recycling on the two interferometers shown in the previous figure, Figure 6.
View Image Figure 8:
The 10 m prototype gravitational wave detector at Glasgow.
View Image Figure 9:
A bird’s eye view of the LIGO detector, sited in Hanford, Washington State.
View Image 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.
View Image Figure 11:
Noise contributions to the expected sensitivity of the LIGO 2 interferometer.
View Image Figure 12:
The proposed LISA detector.