gravitational waves laser interferometric detectors barry barish 5 july 2000 the ninth marcel...
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Gravitational Waves Laser Interferometric Detectors
Barry Barish
5 July 2000
The Ninth Marcel Grossmann Meeting
University of Rome “La Sapienza”
Rome, July 2 - 8, 2000
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Suspended mass Michelson-type interferometerson earth’s surface detect distant astrophysical sources
International network (LIGO, Virgo, GEO, TAMA and AIGO) enable locating sources and decomposing polarization of gravitational waves.
Interferometersterrestrial
Suspended test masses
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Interferomersinternational network
LIGO
Simultaneously detect signal (within msec)
detection confidence locate the sources
decompose the polarization of gravitational waves
GEO VirgoTAMA
AIGO
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LIGO (Washington) LIGO (Louisiana)
Interferometersinternational network
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GEO 600 (Germany) Virgo (Italy)
Interferometersinternational network
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TAMA 300 (Japan) AIGO (Australia)
Interferometersinternational network
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Astrophysics Sourcesfrequency range
EM waves are studied over ~20 orders of magnitude» (ULF radio HE rays)
Gravitational Waves over ~8 orders of magnitude» (terrestrial + space)
Audio band
space groundbased
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Interferometers the noise floor
Interferometry is limited by three fundamental noise sources
seismic noise at the lowest frequencies thermal noise at intermediate frequencies shot noise at high frequencies
Many other noise sources lurk underneath and must be controlled as the instrument is improved
Sensitive region
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Noise Floor40 m prototype
• displacement sensitivityin 40 m prototype. • comparison to predicted contributions from various noise sources
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Noise FloorTAMA 300
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LIGO II
Vacuum Systemsbeam tube enclosures
LIGO minimal enclosures
no services
Virgopreparing arms
GEOtube in the trench
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Beam Tubes
LIGO 4 km beam tube (1998)
TAMA 300 m beam pipe
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Beam Tube Bakeout
LIGO bakeout
standard quantum limit
phase noise
residual gas
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BakeoutLIGO performance
Livingston
Species Goal b HY2 HY1 HX1 HX2 LX2
H 2 4.7 4.8 6.3 5.2 4.6 4.3x 10 -14
torr liters/sec/cm 2
CH 4 48000 < 900 < 220 < 8.8 < 95 < 40x 10 -20
torr liters/sec/cm 2
H 2O 1500 < 4 < 20 < 1.8 < 0.8 < 10x 10 -18
torr liters/sec/cm 2
CO 650 < 14 < 9 < 5.7 < 2 < 5x 10 -18
torr liters/sec/cm 2
CO 2 2200 < 40 < 18 < 2.9 < 8.5 < 8x 10 -19
torr liters/sec/cm 2
NO+C 2H 6 7000 < 2 < 14 < 6.6 < 1.0 < 1.1x 10 -19
torr liters/sec/cm 2
H nC pOq 50-2 c < 15 < 8.5 < 5.3 < 0.4 < 4.3x 10 -19
torr liters/sec/cm 2
air leak 1000 < 20 < 10 < 3.5 < 16 < 7x 10 -11
torr liter/sec
c Goal for hydrocarbons depends on weight of parent molecule; range given corresponds with 100-300 AMU
Hanford
Beam Tube Bakeout Results a
a Outgassing results correct to 23 C
NOTE: All results except for H 2 are upper limits
b Goal: maximum outgassing to achieve pressure equivalent to 10 -9 torr H 2 using only pumps at stations
Achieved Design Requirements(< 10-9 torr)
partial pressures during bakeout
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Vacuum Chamberstest masses, optics
TAMA chambers
LIGO chambers
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Interferometers the noise floor
Interferometry is limited by three fundamental noise sources
seismic noise at the lowest frequencies thermal noise at intermediate frequencies shot noise at high frequencies
Many other noise sources lurk underneath and must be controlled as the instrument is improved
Sensitive region
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Suspension vertical transfer function measured and simulated (prototype)
Seismic IsolationVirgo
“Long Suspensions”• inverted pendulum• five intermediate filters
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Long SuspensionsVirgo installation at the site
Beam Splitter and North Input mirror
All four long suspensions for the entire central interferometer will be complete by October 2000.
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SuspensionsGEO triple suspension
lower cantilever stage (view from below)
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Suspensions GEO triple pendulum
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Test Massesfibers and bonding - GEO
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LIGO II
Interferometers basic optical configuration
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Opticsmirrors, coating and polishing
All optics polished & coated» Microroughness within spec.
(<10 ppm scatter)» Radius of curvature within
spec. R/R 5%)» Coating defects within spec.
(pt. defects < 2 ppm, 10 optics tested)
» Coating absorption within spec. (<1 ppm, 40 optics tested)
LIGO
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LIGOmetrology
Caltech
CSIRO
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SputteredAtoms
Mask
X
YRobot
Sputtered Atoms
SiO2 target
Ion Source
Mirror
InterferometerWavefront control
Corrective CoatingVirgo
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Corrective Coating results
38
0
P.V
. in
nm
6 nm R.M.S.
12
0
P.V
. in
nm
1,5 nm R.M.S.
Before After
80 mm high reflectivity mirror @633 nm
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Interferometers the noise floor
Interferometry is limited by three fundamental noise sources
seismic noise at the lowest frequencies thermal noise at intermediate frequencies shot noise at high frequencies
Many other noise sources lurk underneath and must be controlled as the instrument is improved
Sensitive region
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Interferometers Lasers
Nd:YAG (1.064 m) Output power > 8W in
TEM00 mode
GEO Laser
LIGO Lasermaster oscillator power amplifier
Master-Slave configuration with 12W output power
Virgo Laser
residual frequency noise
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Laser pre-stabilization
intensity noise: dI(f)/I <10-6/Hz1/2, 40 Hz<f<10 KHz
frequency noise: dn(f) < 10-2Hz/Hz1/2 40Hz<f<10KHz
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Phase Noisesplitting the fringe
• spectral sensitivity of MIT phase noise interferometer
• above 500 Hz shot noise limited near LIGO I goal
• additional features are from 60 Hz powerline harmonics, wire resonances (600 Hz), mount resonances, etc
shot noise
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1 10 100 100010
-23
10-22
10-21
10-20
10-19
10-18
C85 steel wire (total) Fused Silica wire (total) FS pendulum thermal noise Mirror thermal noise
h [1
/sqr
t(H
z)]
Frequency [Hz]
Virgo sensitivity curveInterferometerssensitivity curves
TAMA 300
GEO 600
Virgo
LIGO
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Interferometerstesting and commissioning
TAMA 300» interferometer locked; noise studies
LIGO» input optics commissioned; » 2 km single arm locked/tested
Geo 600» commissioning tests
Virgo» testing isolation systems; input optics
AIGO» setting up central facility
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TAMA 300optical configuration
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TAMA Commissioningcontrol error signals
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TAMA Performancenoise source analysis
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LIGOschematic of interferometer system
LASER
Mode Cleaner
2 km cavity
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2km Fabry-Perot cavity Includes all interferometer subsystems
» many in definitive form; analog servo on cavity length for test configuration
confirmation of initial alignment» ~100 microrad errors; beams easily found in both arms
ability to lock cavity improves with understanding » 0 sec 12/1 flashes of light
» 0.2 sec 12/9
» 2 min 1/14
» 60 sec 1/19
» 5 min 1/21 (and on a different arm)
» 18 min 2/12
» 1.5 hrs 3/4 (temperature stabilize pre modecleaner)
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2km Fabry-Perot cavity
models of environment» temperature changes on laser frequency
» tidal forces changing baselines
» seismometer/tilt correlations with microseismic peak
mirror characterization» losses: ~6% dip,
excess probably due to poor centering
» scatter: appears to be better than requirements
» figure 12/03 beam profile
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2km Fabry-Perot cavity 15 minute locked stretch
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Interferometersastrophysical sources
Compact binary mergers
Sensitivity to coalescing binaries
Binary inspiral ‘chirp’ signal
2002
2007
future
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Interferometerdata analysis
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
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Interferometer Data40 m
Real interferometer data is UGLY!!!(Gliches - known and unknown)
LOCKING
RINGING
NORMAL
ROCKING
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The Problem
How much does real data degrade complicate the data analysis and degrade the sensitivity ??
Test with real data by setting an upper limit on galactic neutron star inspiral rate using 40 m data
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“Clean up” data stream
Effect of removing sinusoidal artifacts using multi-taper methods
Non stationary noise Non gaussian tails
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Inspiral ‘Chirp’ Signal
Template Waveforms
“matched filtering”687 filters
44.8 hrs of data39.9 hrs arms locked25.0 hrs good data
sensitivity to our galaxyh ~ 3.5 10-19 mHz-1/2
expected rate ~10-6/yr
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Detection Efficiency
• Simulated inspiral events provide end to end test of analysis and simulation code for reconstruction efficiency
• Errors in distance measurements from presence of noise are consistent with SNR fluctuations
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Setting a limit
Upper limit on event rate can be determined from SNR of ‘loudest’ event
Limit on rate:R < 0.5/hour with 90% CL = 0.33 = detection efficiency
An ideal detector would set a limit:R < 0.16/hour
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TAMA 300search for binary coalescence
• 2-step hierarchical method
• chirp masses (0.3-10)M0
• strain calibrated h/h ~ 1 %
Matched templates
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TAMA 300preliminary result
For signal/noise = 7.2
Expect: 2.5 eventsObserve: 2 events
Note: for a 1.4 M0 NS-NS inspiral this limit corresponds to a max distance = 6.2 kpc
Rate < 0.59 ev/hr 90% C.L.
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Interferometersastrophysical sources
SN1987Asensitivity to burst sources
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LIGOastrophysical sources
Pulsars in our galaxy»non axisymmetric: 10-4 < e < 10-6»science: neutron star precession; interiors»narrow band searches best
Continuous wave sources
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Conclusions a new generation of long baseline suspended mass interferometers are
being completed with h ~ 10-21
commissioning, testing and characterization of the interferometers is underway
data analysis schemes are being developed, including tests with real data from the 40 m prototype and TAMA (see Tsubono)
science data taking to begin within two years
plans and agreements being made for exchange of data for coincidences between detectors (GWIC)
significant improvements in sensitivity (h ~ 10-22) are anticipated about
2007+ (see Danzmann)