1. 1 Science Opportunities for Australia Advanced LIGO Barry Barish Director, LIGO Canberra, Australia 16-Sept-03 LIGO-G030506-00-M

2. 2 Astrophysical Sources signatures  Compact binary inspiral: “chirps” »NS-NS waveforms are well described »BH-BH need better waveforms »search technique: matched templates  Supernovae / GRBs: “bursts” »burst signals in coincidence with signals in electromagnetic radiation »prompt alarm (~ one hour) with neutrino detectors  Pulsars in our galaxy: “periodic” »search for observed neutron stars (frequency, doppler shift) »all sky search (computing challenge) »r-modes  Cosmological Signal “stochastic background”

3. 3 Early Universe: “correlated noise” ‘Murmurs’ from the Big Bang Cosmic Microwave background WMAP 2003

4. 4 International Network on Earth LIGO simultaneously detect signal detection confidence GEO Virgo TAMA AIGO locate the sourcesdecompose the polarization of gravitational waves

5. 5 Detecting a passing wave …. Free masses

6. 6 Detecting a passing wave …. Interferometer

7. 7 Interferometer Concept  Laser used to measure relative lengths of two orthogonal arms As a wave passes, the arm lengths change in different ways…. …causing the interference pattern to change at the photodiode  Arms in LIGO are 4km  Measure difference in length to one part in 10 21 or 10 -18 meters Suspended Masses

8. 8 How Small is 10 -18 Meter? Wavelength of light ~ 1 micron One meter ~ 40 inches Human hair ~ 100 microns LIGO sensitivity 10 -18 m Nuclear diameter 10 -15 m Atomic diameter 10 -10 m

9. 9 International Network LIGO Hanford Observatory Livingston Observatory Caltech MIT

10. 10 LIGO Livingston Observatory

11. 11 LIGO Hanford Observatory

12. 12 LIGO Optics fused silica Caltech dataCSIRO data  Surface uniformity < 1 nm rms  Scatter < 50 ppm  Absorption < 2 ppm  ROC matched < 3%  Internal mode Q’s > 2 x 10 6

13. 13 What Limits LIGO Sensitivity?  Seismic noise limits low frequencies  Thermal Noise limits middle frequencies  Quantum nature of light (Shot Noise) limits high frequencies  Technical issues - alignment, electronics, acoustics, etc limit us before we reach these design goals

14. 14 Advanced LIGO improved subsystems Active Seismic Multiple Suspensions Sapphire Optics Higher Power Laser

15. 15 Advanced LIGO Enhanced Systems laser suspension seismic isolation test mass Rate Improvement ~ 10 4 + narrow band optical configuration 2007 +

16. 16 Advanced LIGO Cubic Law for “Window” on the Universe Initial LIGO Advanced LIGO Improve amplitude sensitivity by a factor of 10x… …number of sources goes up 1000x! Virgo cluster

17. 17 Gravitational Waves A New Window on the Universe Advanced LIGO will provide a new way to view the dynamics of the Universe