Preface to the Second Edition |
Preface |
The Search for Gravitational Waves / 1: |
The Importance of the Search / 1.1: |
A Bit of History / 1.2: |
The Practice of Gravitational Wave Detection / 1.3: |
A Guide for the Reader / 1.4: |
The Nature of Gravitational Waves / 2: |
Waves in General Relativity / 2.1: |
The Michelson-Morley Experiment / 2.2: |
A Schematic Detector of Gravitational Waves / 2.3: |
Description of Gravitational Waves in Terms of Force / 2.4: |
Sources of Gravitational Waves / 3: |
Physics of Gravitational Wave Generation / 3.1: |
In the Footsteps of Heinrich Hertz? / 3.2: |
Observation of Gravitational Wave Emission / 3.3: |
Astronomical Sources of Gravitational Waves / 3.4: |
Neutron star binaries / 3.4.1: |
Super novae / 3.4.2: |
Pulsars / 3.4.3: |
"Wagoner stars" / 3.4.4: |
Black holes / 3.4.5: |
Stochastic backgrounds / 3.4.6: |
Discussion / 3.4.7: |
Linear Systems, Signals and Noise / 4: |
Characterizing a Time Series / 4.1: |
The Fourier transform / 4.1.1: |
Cross-correlation and autocorrelation / 4.1.2: |
Convolution / 4.1.3: |
The power spectrum / 4.1.4: |
The Periodogram / 4.1.5: |
Interpretation of power spectra / 4.1.6: |
The amplitude spectral density / 4.1.7: |
Linear Systems / 4.2: |
Bode plots / 4.2.1: |
Frequency response example / 4.2.2: |
The Signal-to-Noise Ratio / 4.3: |
Noise statistics / 4.3.1: |
Matched templates and matched filters / 4.3.2: |
SNR rules of thumb / 4.3.3: |
The characteristic amplitude / 4.3.4: |
Optical Readout Noise / 5: |
Photon Shot Noise / 5.1: |
Radiation Pressure Noise / 5.2: |
Shot Noise in Classical and Quantum Mechanics / 5.3: |
The Remarkable Precision of Interferometry / 5.4: |
Folded Interferometer Arms / 6: |
Herriott Delay Line / 6.1: |
Beam Diameter and Mirror Diameter / 6.2: |
Fabry-Perot Cavities / 6.3: |
A Long Fabry-Perot Cavity / 6.4: |
Hermite-Gaussian Beams / 6.5: |
Scattered Light in Interferometers / 6.6: |
Comparison of Fabry-Perot Cavities with Delay Lines / 6.7: |
Optical Readout Noise in Folded Interferometers / 6.8: |
Transfer Function of a Folded Interferometer / 6.9: |
To Fold, or Not to Fold? / 6.10: |
Thermal Noise / 7: |
Brownian Motion / 7.1: |
Brownian Motion of a Macroscopic Mass Suspended in a Dilute Gas / 7.2: |
The Fluctuation-Dissipation Theorem / 7.3: |
Remarks on the Fluctuation-Dissipation Theorem / 7.4: |
The Quality Factor, Q / 7.5: |
Thermal Noise in a Gas-Damped Pendulum / 7.6: |
Dissipation from Internal Friction in Materials / 7.7: |
Special Features of the Pendulum / 7.8: |
Thermal Noise of the Pendulum's Internal Modes / 7.9: |
Seismic Noise and Vibration Isolation / 8: |
Ambient Seismic Spectrum / 8.1: |
Seismometers / 8.2: |
Vibration Isolators / 8.3: |
Myths About Vibration Isolation / 8.4: |
Isolation in an Interferometer / 8.5: |
Stacks and Multiple Pendulums / 8.6: |
Q: High or Low? / 8.7: |
A Gravitational "Short Circuit1' Around Vibration Isolators / 8.8: |
Beyond Passive Isolation / 8.9: |
Design Features of Large Interferometers / 9: |
How Small Can We Make a Gravitational Wave Inteferometer? / 9.1: |
Noise from Residual Gas / 9.2: |
Simple model / 9.2.1: |
Exact result / 9.2.2: |
Implications for Interferometer Design / 9.2.3: |
The Space-Borne Alternative / 9.3: |
Null Instruments / 10: |
Some Virtues of Nullity / 10.1: |
Null hypotheses / 10.1.1: |
Null experiments / 10.1.2: |
Null instruments / 10.1.3: |
Null features of a gravitational wave interferometer / 10.1.4: |
Active null instruments / 10.1.5: |
The Advantages of Chopping / 10.2: |
The Necessity to Operate a Gravitational Wave Interferometer as an Active Null Instrument / 10.3: |
The need to chop / 10.3.1: |
The need to actively null the output / 10.3.2: |
Feedback Control Systems / 11: |
The Loop Transfer Function / 11.1: |
The Closed Loop Transfer Function / 11.2: |
Designing the Loop Transfer Function / 11.3: |
Instability / 11.4: |
Causes of instability / 11.4.1: |
Stability-tests / 11.4.2: |
The Compensation Filter / 11.5: |
Active Damping: A Servo Design Example / 11.6: |
Feedback to Reduce Seismic Noise Over a Broad Band / 11.7: |
Suspension point interferometer / 11.7.1: |
Active isolation / 11.7.2: |
An Interferometer as an Active Null Instrument / 12: |
Fringe-Lock in a Non-Resonant Interferometer / 12.1: |
Shot Noise in a Modulated Interferometer / 12.2: |
Rejection of Laser Output Power Noise / 12.3: |
Locking the Fringe / 12.4: |
Fringe Lock for a Fabry-Perot Cavity / 12.5: |
A Simple Interferometer with Fabry-Perot Arms / 12.6: |
Beyond the Basic Interferometer / 12.7: |
Power recycling / 12.7.1: |
Signal recycling / 12.7.2: |
Resonant sideband extraction / 12.7.3: |
Resonant Mass Gravitational Wave Detectors / 13: |
Does Form Follow Function? / 13.1: |
The Idea of Resonant Mass Detectors / 13.2: |
A Bar's Impulse Response and Transfer Function / 13.3: |
Resonant Transducers / 13.4: |
Thermal Noise in a Bar / 13.5: |
Bandwidth of Resonant Mass Detectors / 13.6: |
When are narrow bandwidths optimum? / 13.6.1: |
Interpreting narrow-band observations / 13.6.2: |
A Real Bar / 13.7: |
Quantum Mechanical Sensitivity "Limit" / 13.8: |
Beyond the Quantum "Limit"? / 13.9: |
Detecting Gravitational Wave Signals / 14: |
The Signal Detection Problem / 14.1: |
Probability Distribution of Time Series / 14.2: |
Coincidence Detection / 14.3: |
Optimum Orientation / 14.4: |
Local Coincidences / 14.5: |
Searching for Periodic Gravitational Waves / 14.6: |
When is a spectral peak improbably strong? / 14.6.1: |
Signatures of periodic gravitational waves / 14.6.2: |
Frequency noise in the source and elsewhere / 14.6.3: |
Searching for a Stochastic Background / 14.7: |
Gravitational Wave Astronomy / 15: |
Gravitational Wave Source Positions / 15.1: |
Network figure of merit / 15.1.1: |
Why measure positions? / 15.1.2: |
Inferences from precise positions / 15.1.3: |
Temporal coincidence with non-gravitational observations / 15.1.4: |
Interpretation of Gravitational Waveforms / 15.2: |
Core collapse / 15.2.1: |
Binary coalescences / 15.2.2: |
A gravitational standard candle / 15.2.3: |
Recognizing signals from black holes / 15.2.4: |
Previous Gravitational Wave Searches / 15.3: |
Room temperature bars / 15.3.1: |
Cryogenic bars / 15.32: |
The Strange case of Supernova 1987A / 15.3.3: |
Gravitational wave searches with interferometers / 15.3.4: |
Other observational upper limits / 15.3.5: |
Prospects / 16: |
A Prototype Interferometer / 16.1: |
LIGO / 16.2: |
Proposed Features of 4 km Interferometers / 16.3: |
Epilogue / 17: |
Introduction / 17.1: |
Physics/Engineering Background (Chapters 4, 10, 11) / 17.2: |
Prehistory of Gravitational Wave Detection (Chapter 1) / 17.3: |
Gravitational Waves and their Interactions with Detectors (Chapter 2) / 17.4: |
Sources of Gravitational Waves (Chapter 3) / 17.5: |
Quantum Measurement Noise (Chapter 5) / 17.6: |
Interferometer Configurations (Chapters 6 and 12) / 17.7: |
Thermal Noise (Chapter 7) / 17.8: |
Seismic Noise (Chapter 8 and Section 11.7.2) / 17.9: |
Resonant Mass Detectors (Chapter 13) / 17.10: |
Large Interferometers (Chapters 9 and 16) / 17.11: |
Data Analysis (Chapter 14) / 17.12: |
Gravitational Wave Astronomy (Chapter 15) / 17.13: |
References |
Preface to the Second Edition |
Preface |
The Search for Gravitational Waves / 1: |
The Importance of the Search / 1.1: |
A Bit of History / 1.2: |
The Practice of Gravitational Wave Detection / 1.3: |