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Paik-1
Search for Gravitational Waves
Ho Jung PaikUniversity of Maryland
and Seoul National University
January 12, 2006Seoul, Korea
KIAS-SNU Physics Winter Camp
Paik-2
Gravitational Waves
,0),(1
2
2
22
BEtc
Tc
GG
4
π8Field equation in General Relativity:
A wave equation, in the weak-field limit.
hghtc
,01
2
2
22
Transverse, spin 1
EM wave: Gravitational wave:
Transverse, spin 2
Paik-3
Gravitational Wave Detection
Joseph Weber (c1960)
A gravitational wave will deposit energy into an elastic solid. (Weber, 1959)
Paik-4
Resonant-Mass Detector 1
)(
)(
)(
)(
2221
1211
I
u
ZZ
ZZ
V
f
22m
1221
ZM
ZZ
• Antenna Transducer Amplifier
• Transducer is characterized by an impedance matrix.
• Electromechanical energy coupling:
f() u() I() V()ijZ
Paik-5
Resonant-Mass Detector 2
• Condition to detect a GW pulse with strength h:
2
2
π
2 S
SNB
a
aa
22S2
TkQ
TkDhM B
• Optimal strategy:
noise. thermal thereduce toneeded is largeA
2 , 2
Na
aBN
S
S
S
T
Q
TkE
Signal Antenna noise Amplifier noise Thermal Wideband Backaction
Paik-6
Resonant Transducer
• To get large , a resonant mass is attached to the antenna (Paik, 1972)
Displacement gain:(M/m)1/2 102
Energy transfer time: (/a) (M/m)1/2
• An additional resonant mass with = (Mm)1/2 can be added to increase S further.
Energy transfer time: (/a) (M/m)1/4
Paik-7
S/C Inductive Transducer
MOUNTING FLANGE
ANTENNA
TEST MASS
DC SQUID
CIRCUIT BOARD
AIR FILTER
1.0~01.0
)2/(20
02
dm
AB
Paik-8
ALLEGRO
4-K antenna at LSUwith a superconducting inductive transducer
Paik-9
AURIGA
Best result obtained: h < 5 x 10-21 Hz-1/2 within ~100 Hz band
100-mK antenna in Italy with a capactive transducer coupled to a dc SQUID
Paik-10
ExplorerSwitzerland
Allegro USA NiobeAustralia
Nautilus, italy
Auriga, Italy
Resonant Bar Detectors
Paik-11
Network of Resonant Bars
Allegro Explorer Auriga
Nautilus
NiobeIGEC Network
Paik-12
Rate(y –1)
Search threshold h
h ~ 2 10-18 ~ 0.02 M⊙ converted @ 10 kpc
• Upper limit on the rate of gravitational waves bursts from the Galactic Center (1997-2000)
The area above the blue curve is excluded with a coverage > 90%
P. Astone, et al. PRD 68 (2003) 022001
IGEC Coincidence Search
• No evidence for gravity wave bursts was found.
Paik-13
Spherical Antenna
• Sphere is omni-directional.
• By detecting its 5 quadrupole modes, the source direction (, ) and wave polarization (h+, h) can be determined. (Wagoner & Paik, 1976)
• 6 radial transducers on truncated icosahedral configuration maintains “spherical” symmetry.(Johnson & Merkowitz, 1993)
TIGA (Truncated Icosahedral Gravitational Antenna)
Paik-14
Resonant Spheres
• Much larger cross-section than a bar of the same resonance frequency (up to 70 x)
MiniGrailThe Netherlands
SchenbergBrazil
Paik-15
Interferometer Concept
Laser used to measure relative lengths of two orthogonal arms
Arm lengths in LIGO are 4 km Measure difference in length to 10-19 m
Paik-16
LIGO Hardware
6-W Nd:YAG laser
Fused silica mirror
Paik-17
Limiting Noise Sources
Seismic noise limits at low frequencies.
Atomic vibrations (thermal noise) inside the components limit at mid frequencies.
Quantum nature of light (shot noise) limits at high frequencies.
Paik-18
Evolution of LIGO Sensitivity
Paik-19
Interferometer Detectors
LIGO Louisiana 4000m
TAMA Japan 300m
Virgo Italy 3000m
GEO Germany 600m
LIGO Washington 2000m & 4000m
Paik-20
Network of Interferometers
LIGO
detection confidence
GEO VirgoTAMA
AIGO?locate the sourcesdecompose the polarization of
gravitational waves
Paik-21
LIGO Science Has Begun
S1 run: 17 days (Aug - Sep 2002)Primarily methods papers Four astrophysical searches published (Phys. Rev. D 69, 2004):
Inspiraling neutron stars, bursts, known pulsar (J1939+2134) with GEO, stochastic background
S2 run: 59 days (Feb - April 2003)Analyses are mostly complete.
S3 run: 70 days (Oct 2003 – Jan 2004) Analysis is in full swing.
Paik-22
Promising Source: Compact Binaries
Paik-23
Matched Filtering
“chirps”
NS–NS: waveforms are well described
BH–BH: need better waveforms
Search: matched templates
Paik-24
Advanced LIGO
Active Seismic
Multiple Suspensions
Improved Optics
Higher Power Laser
Paik-25
Sensitivity Improvement
RateImprovement ~
104
narrow band optical
configuration
2008 +
Paik-26
Gravitational Waves in Space
Three spacecraft form an equilateral triangle with armlength of 5 million km
LISA 2012 +
Paik-27
LISA Accelerometer
The position of a reference mass is sensed by a capacitor bridge and used for drag-free control.
Paik-28
• Y-shaped payload has two identical optical assemblies with transmit/receive telescopes.
• The inertial sensor consists of a free-falling proof mass inside a reference housing.
LISA Spacecraft
Paik-29
Sources for LISA
Paik-30
LISA and LIGO
Paik-31
Status of Interferometers
Sensitivity toward gravitational wave detection is improving on many fronts.
Improved limits are being set for all major sources -- binary inspirals, periodic sources, burst sources, and stochastic background.
Data exchange and joint data analysis between detector groups is improving ability to make detections.
Need specific waveforms to improve search sensitivities!
Hopefully, detections will be made soon !!