1 science opportunities for australia advanced ligo barry barish director, ligo canberra, australia...
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![Page 1: 1 Science Opportunities for Australia Advanced LIGO Barry Barish Director, LIGO Canberra, Australia 16-Sept-03 LIGO-G030506-00-M](https://reader030.vdocuments.us/reader030/viewer/2022032800/56649d2b5503460f94a0040c/html5/thumbnails/1.jpg)
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Science Opportunities for Australia
Advanced LIGO
Barry BarishDirector, LIGO
Canberra, Australia16-Sept-03
LIGO-G030506-00-M
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Astrophysical Sourcessignatures
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”
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Early Universe: “correlated noise”
‘Murmurs’ from the Big Bang
Cosmic Microwave
background
WMAP 2003
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International Network on Earth
LIGO
simultaneously detect signal
detection confidence
GEO VirgoTAMA
AIGOlocate the sourcesdecompose the polarization of
gravitational waves
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Detecting a passing wave ….
Free masses
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Detecting a passing wave ….
Interferometer
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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 1021 or 10-18 meters
SuspendedMasses
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How Small is 10-18 Meter?
Wavelength of light ~ 1 micron
100
One meter ~ 40 inches
Human hair ~ 100 microns000,10
LIGO sensitivity 10-18 m000,1
Nuclear diameter 10-15 m
000,100
Atomic diameter 10-10 m000,10
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International NetworkLIGO
Hanford Observatory
LivingstonObservatory
Caltech
MIT
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LIGO Livingston Observatory
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LIGO Hanford Observatory
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LIGO Opticsfused silica
Caltech data CSIRO data
Surface uniformity < 1 nm rms Scatter < 50 ppm Absorption < 2 ppm ROC matched < 3% Internal mode Q’s > 2 x 106
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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
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Advanced LIGOimproved subsystems
Active Seismic
Multiple Suspensions
Sapphire Optics
Higher Power Laser
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Advanced LIGO
Enhanced Systems• laser• suspension• seismic isolation• test mass Rate
Improvement
~ 104
+narrow band
optical configuration
2007 +
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Advanced LIGOAdvanced LIGOCubic Law for “Cubic Law for “WindowWindow” on the Universe” on the Universe
Initial LIGO
Advanced LIGO
Improve amplitude sensitivity by a factor of 10x…
…number of sources goes up 1000x!
Virgo cluster
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Gravitational Waves A New Window on the
Universe
Advanced LIGO will provide a new way to view the dynamics of the
Universe