Note: Cover -- ADVANCED GRAVITATIONAL WAVE DETECTORS -- Title -- Copyright -- In memory of Stefano Braccini, our co-author and respected colleague. -- Contents -- Contributors -- Foreword -- Preface -- Introduction -- Part 1 An introduction to gravitational wave astronomy and detectors -- 1 Gravitational waves -- 1.1 Listening to the Universe -- 1.2 Gravitational waves in stiff-elastic spacetime -- 1.3 The luminosity of gravitational waves -- 1.4 The amplitude and frequency of gravitational wave sources -- 1.5 Gravitational waves in general relativity -- 1.6 Gravitational wave detector response and signal strength -- References -- 2 Sources of gravitational waves -- 2.1 Introduction -- 2.2 Rough guide to signal amplitudes -- 2.3 Supernovae -- 2.4 Neutron star coalescence -- 2.5 Rates of coalescing compact binaries -- 2.6 Gravitational wave standard sirens -- 2.7 Gravitational waves and gamma-ray bursts -- 2.8 Continuous gravitational wave sources -- 2.9 Low-frequency sources -- 2.10 Stochastic background from the era of early star formation -- 2.11 Cosmological gravitational waves from the Big Bang -- References -- 3 Gravitational wave detectors -- 3.1 Introduction -- 3.2 Introducing gravitational wave detectors across the spectrum -- 3.3 Key concepts in gravitational wave detection -- 3.4 Detectors from nanohertz to kilohertz -- 3.5 Introduction to terrestrial interferometers -- 3.6 Conclusion -- References -- 4 Gravitational wave data analysis -- 4.1 Introduction -- 4.2 Source amplitudes vs sensitivity -- 4.3 Matched filtering and optimal signal-to-noise ratio -- 4.4 Practical applications of matched filtering -- 4.5 Suboptimal filtering methods -- 4.6 False alarms, detection threshold and coincident observation -- 4.7 Detection of stochastic signals by cross-correlation -- 4.8 Network detection -- References. , 5 Network analysis and multi-messenger astronomy -- 5.1 Introduction -- 5.2 Network analysis -- 5.3 General approach for discretised data -- 5.4 Angular resolution of a detector network -- 5.5 Multi-messenger gravitational wave astronomy -- References -- Part 2 Current laser interferometer detectors-- three case studies -- 6 The Laser Interferometer Gravitational-Wave Observatory -- 6.1 Introduction -- 6.2 The LIGO detectors -- 6.3 Detector description -- 6.4 Instrument performance -- 6.5 Future directions -- References -- 7 The Virgo detector -- 7.1 Introduction -- 7.2 Virgo overall design -- 7.3 The Virgo subsystems -- 7.4 Interferometer commissioning -- 7.5 Virgo+ upgrades -- 7.6 Towards the next generation -- References -- 8 GEO 600 -- 8.1 A bit of history -- 8.2 GEO 600 techniques -- 8.3 The status in late 2009 -- 8.4 Upgrade plans -- 8.5 In the future -- References -- Part 3 Technology for advanced gravitationalwave detectors -- 9 Lasers for high optical power interferometers -- 9.1 Requirements on the light source of a gravitational wave detector -- 9.2 Lasers for advanced gravitational wave detectors -- 9.3 Laser stabilisation -- 9.4 Lasers for third generation interferometers -- References -- 10 Thermal noise, suspensions and test masses -- 10.1 Introduction -- 10.2 Suspension thermal noise -- 10.3 Test mass thermal noise -- 10.4 Coating loss -- References -- 11 Vibration isolation -- 11.1 Planned isolation platforms for Advanced LIGO -- 11.2 Achieving isolation -- 11.3 Conclusions -- 11.4 Design goals and philosophy -- 11.5 Cascade stages -- 11.6 Control hardware -- 11.7 Control scheme -- 11.8 Conclusion -- References -- 12 Interferometer sensing and control -- 12.1 Introduction -- 12.2 Mathematical background -- 12.3 Length sensing and control -- 12.4 Angular sensing and control -- 12.5 Local control system. , 12.6 Modulation frequencies calculations -- 12.7 Readout scheme -- References -- 13 Stabilising interferometers against high optical power effects -- 13.1 Introduction -- 13.2 Thermal lensing and control -- 13.3 Sidles--Sigg instability -- 13.4 Parametric instability -- 13.5 Parametric instability theory and modeling -- 13.6 Possible approaches to PI control -- 13.7 Conclusion -- References -- Part 4 Technology for third generation gravitational wave detectors -- 14 Cryogenic interferometers -- 14.1 Introduction -- 14.2 Material properties at low temperature -- 14.3 Reduction of mirror thermal noise -- 14.4 Elimination of thermal aberration -- 14.5 LCGT -- 14.6 Conclusion -- References -- 15 Quantum theory of laser interferometer GW detectors -- 15.1 Introduction -- 15.2 An order-of-magnitude estimate -- 15.3 Basics for analysing quantum noise -- 15.4 Quantum noise in a GW detector -- 15.5 Derivation of the SQL: A general argument -- 15.6 Beating the SQL by building correlations -- 15.7 Optical spring: Modification of test mass dynamics -- 15.8 Continuous state demolition: Another viewpoint on the SQL -- 15.9 Speed meters -- 15.10 Conclusions -- References -- 16 ET: A third generation observatory -- 16.1 Introduction to the third generation of GW observatories -- 16.2 Scientific potential of a third generation GW observatory -- 16.3 Third generation sensitivity: How to suppress the noises limiting the advanced GW detectors -- 16.4 Scenarios and timeline for the third generation -- References -- Index.