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Observation Runs of TAMA300 Gravitational Wave Detector. Masaki Ando Dept. of Physics, University of Tokyo TAMA collaboration. Coalescence of a binary neutron stars Illustration/ KAGAYA. Abstract. Japanese activities for GW detection TAMA - PowerPoint PPT Presentation
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XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)
Observation Runs of TAMA300 Gravitational Wave Detector
Masaki Ando Dept. of Physics, University of Tokyo
TAMA collaboration
Coalescence of a binary neutron stars
Illustration/ KAGAYA
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 2
Abstract
Japanese activities for GW detection
TAMA7 year project (April 1995 – March 2002)Construct a 300m interferometric detector : TAMA300
Several data taking runs from 1999Data analysis results
Next project : LCGT3km cryogenic interferometer at Kamioka mineResearch and development tasks
(April 2002 – March 2006)
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 3
Contents
Introduction
TAMA detector
Data taking runs with TAMA
Data analysis results
Recent results (Data Taking 8)
LCGTOverviewResearch and development tasks
Summary
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 4
Introduction (1)- Gravitational-wave astronomy -
Gravitational wave detectors
Bar detectors - network observation
Interferometric detector - finishing and starting observation
Future projects on the ground and in the space
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 5
Gravitational waves (Coalescences of compact binaries, Stellar core collapses)
Change in distance between free masses (Strain about 10-18)
Introduction (2)- Detection method -
Gravitational WavesPrecise measurement
by a laser interferometer (Mirrors behave as free masses)
Michelson interferometer
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 6
Introduction (3)- Michelson interferometer -
Michelson interferometer
Detects optical-path difference caused by GWs
Long arm length for higher sensitivity
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 7
Introduction (4)- Interferometer configuration -
End mirror End mirror
Photo detector
Beamsplitter
Some mirrors are added
Sensitivity improvement
Power-recycledFabry-Perot-Michelson
interferometer(LIGO, VIRGO, TAMA)
Fabry-Perot cavityEffective arm length
Power recyclingEnhance power in the interferometer
Front mirrorFront mirror
Recycling mirror
Fabry-Perot cavity
Fabry-P
ero
t cavity
Laser source
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 8
TAMA project (1)- overview -
TAMA projectDetect gravitational waves
from local group of our galaxy
Research and development for a large-scale detector
Construct an interferometernamed TAMA300
Fabry-Perot-Michelson interferometer with 300m arms (with power recycling)
Target sensitivityh : 3x10-21
Aerial photograph of the TAMA site (NAOJ, Mitaka, Tokyo, JAPAN)
300m
300m
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 9
TAMA project (2) - Noise budget of TAMA300 -
Target sensitivity
101 102 103 104 10510–24
10–22
10–20
10–18
10–16
10–14
10–20
10–18
10–16
10–14
10–12
Str
ain
no
ise
[1
/Hz
1/2
]
Frequency [Hz]
Pendulum thermal noise
Phase I goal
Phase II goal
Dis
pla
cem
en
t no
ise
[m
/Hz
1/2
]
NS–NS
Super Novae
Seism
ic noise
Mirror thermal noise
Shot noise
Observation band
inspirals
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 10
TAMA project (3) - Photos -
Fused silica mirrorFused silica mirror
Mirror suspensionMirror suspension 300m vacuum duct300m vacuum duct
LaserLaser
RMRMMCMC BSBS
FM2FM2
FM1FM1
Center roomCenter room
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 11
Data taking runs (1)- Data taking runs with TAMA300 -
Data Taking ObjectiveObservation
timeTypical strain noise level
Total data(Longest lock)
DT1 August, 1999 Calibration test 1 night 3x10-19 /Hz 1/210 hours
(7.7 hours)
DT2 September, 1999 First Observation run 3 nights 3x10-20 /Hz 1/2 31 hours
DT3 April, 2000Observation with
improved sensitivity3 nights 1x10-20 /Hz 1/2 13 hours
DT4Aug.-Sept.,
2000100 hours'
observation data2 weeks
(night-time operation)1x10-20 /Hz 1/2
(typical)167 hours
(12.8 hours)
DT5 March, 2001100 hours' observation with high duty cycle
1 week(whole-day operation)
1.7x10-20 /Hz 1/2
(LF improvement)111 hours
DT6Aug.-Sept.,
20011000 hours' observatio
n 50 days 5x10-21 /Hz 1/21038 hours(22.0 hours)
DT7Aug.-Sept.,
2002Full operation with
Power recycling2 days 25 hours
DT8Feb.-April.,
20031000 hours
Coincidence2 months 3x10-21 /Hz 1/2
1157 hours(20.5 hours)
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 12
Data taking runs (2)- DT6 observation summary -
TAMA data taking 6 (DT6)50 days’ observation (August 1 – September 20, 2001)Phase I configuration (without power recycling)
Sufficient sensitivity and stability for GW events in our GalaxySNR of 30 for 1.4-1.4 Msolar inspiralsObservation : 1038 hours (86.5%)
Well-organized observationAutomatic lock of the detectorOnline monitor and diagnosis 65 shift participants (2 person / 8 hours’ shift)
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 13
Data taking runs (3)- Detector operation status in DT6 -
Operation status calendar Total observation : 1038 hours
Thu SunTueMon Fri SatWedAug. 01 03
08
Operated (over 10min) High–freq. data taking
Date in JST
15
22
29
05
12
191817
10
03
27
13
06 07
14
2120
28
04
11 13
06
30
23
16
09
02
10
17
24
31
07
14 15
08
Sep. 01
25
18
11
04 05
12
19
26
02
09
16
20
TyphoonLaser instabilityMeasurement+adjustmentHuman error
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 14
Data Analysis results (1)- TAMA data analysis -
GW searchBinary inspiral search
Two step searchBinary inspiral search using WaveletTAMA-LISM coincidence
Continuous wave from known pulsarBurst wave search
BH ringdown search, Stochastic background search, etc.
Detector characterization analysisCalibrationNoise veto analysisInterferometer diagnosis
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 15
Data Analysis results (2)- Binary inspiral search -
Binary inspiral event search Matched filtering
Prepare templates (predicted waveform)
Expected SNR for binary mergers
Distance: 10kpc (Galactic center)
DT6 noise spectrum
SNR : about 30 (1.4/1.4 Msolar binaries)
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 16
Data Analysis results (3) - Search results -
Matched filtering analysisDT6 1038 hours’ data1.0-2.0 Msolar events (200-1000 templates)2 event selection
No GW event Simulation
Assumed Galactic source distribution
DT6 detector direction
Detection efficiency: 23%
Upper limit Galactic event rate:
0.0095 events/hour (C.L. 90%) 10-6 events/year (prediction)
)16/( 2
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 17
Data taking 8 (1)-Data taking runs with TAMA300 -
Data Taking ObjectiveObservation
timeTypical strain noise level
Total data(Longest lock)
DT1 August, 1999 Calibration test 1 night 3x10-19 /Hz 1/210 hours
(7.7 hours)
DT2 September, 1999 First Observation run 3 nights 3x10-20 /Hz 1/2 31 hours
DT3 April, 2000Observation with
improved sensitivity3 nights 1x10-20 /Hz 1/2 13 hours
DT4Aug.-Sept.,
2000100 hours'
observation data2 weeks
(night-time operation)1x10-20 /Hz 1/2
(typical)167 hours
(12.8 hours)
DT5 March, 2001100 hours' observation with high duty cycle
1 week(whole-day operation)
1.7x10-20 /Hz 1/2
(LF improvement)111 hours
DT6Aug.-Sept.,
20011000 hours' observatio
n 50 days 5x10-21 /Hz 1/21038 hours(22.0 hours)
DT7Aug.-Sept.,
2002Full operation with
Power recycling2 days 25 hours
DT8Feb.-April.,
20031000 hours
Coincidence2 months 3x10-21 /Hz ½
1157 hours(20.5 hours)
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 18
Data taking 8 (2)- DT8 observation summary -
TAMA data taking 8 (DT8)2 month’ observation (February 14 – April 15, 2003)Full configuration (with power recycling)
Sufficient sensitivity and stability for GW events in our GalaxySNR of 40 for 1.4-1.4 Msolar inspirals Observation : 1157 hours (81.3%)
94 shift participant
Coincidence runLIGO (4km detector x2, 2km detector)
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 19
Data taking 8 (3)- Detector operation status in DT8 -
Operation status calendar Total operation : 1157 hours
Thu SunTueMon Fri SatWed
Apr. 01 03
08
Observation (continuous over 10min)
Date and Time in JST (UTC +9 hours) 15
22
05
12
191817
10
03
27
13
06
07
Feb. 14, 2003
2120
28
04
11 13
06
23
16
09
02
10
17
24
07
14 15
08
Mar. 0125
18
11
04 05
12
19
26 02
09
16
20 2221 23
27 2824 2925 26 30
31
14 15
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 20
Data taking 8 (4)- Sensitivity in DT8 -
Sensitivity for binary inspiral events
Better than DT6Longer obs. Time
Better results
Coincidence Analysis withother detectors
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 21
LCGT project (1)- Overview -
For gravitational wave astronomy Higher sensitivity (seeing further away)
More than a few events in a year
100 101 102 103 104
10-19
10-20
10-21
10-22
10-23
10-24
10-25
Frequency [Hz]
Str
ain
sen
sit
ivit
y
[1/H
z1/2]
Illustration / S.Miyoki
LCGT project SNR : 10
for 230Mpc events
(NS-NS inspiral)
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 22
LCGT project (2) - LCGT parameters -
LCGTBaseline length : 3kmSite: Kamioka mineCryogenic interferometer
Laser : 100W50kg Sapphire mirror
(20K, Q=108)Broadband RSESeismic isolator :
SAS (300K) Cryogenic SUS
(10K, Q=2x108) Suspension point
interferometer
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 23
LCGT project (3) - CLIO100 -
CLIO100 : LCGT prototype at Kamioka mine100m cryogenic interferometerR&D for …
MirrorSuspensionCryogenics
Tunnel digging finished (July 2002)
Installing IFO for geo-phys
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 24
LCGT project (4) - Site for CLIO100 -
SuperKamiokande
CLIO100
Entrance
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 25
Summary
TAMA300Data taking runs
8 data taking runs (August 1999- ), over 2000 hours of data
Data analysisUpper limit for Galactic binary inspirals : 0.0095 /hourCoincidence analysis, burst wave, continuous wave
Data taking 8 : February 14 - April 15, 2003 just finished
Better results will be obtainedCollaboration with other detectors
For LCGTR&D tasks --- TAMA300 and CLIO100Design document
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 26
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 27
Introduction (2)- Gravitational-wave astronomy -
Gravitational waves (Ripples of space time)
Gravitational-wave astronomy
New window for astronomy and cosmology
A.Einstein
Predicted by General Relativity --- Strain of space-time which propagates at the speed of the light
(A.Einstein, 1916) Existence was proved by observation of a binary pulsar (J.H.Taylor, et.al, 1979) Generated by acceraration of masses ( Electro-Magnetic waves : acceraration of charges) High transmissivity (Small cross section with matters)
Ac
cu
mu
late
d s
hif
t
[s]
Time [year]
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 28
TAMA project (1) - Optical and control configuration -
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 29
TAMA project (1) - Data acquisition and analysis -
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 30
TAMA project (1) - Basic design of TAMA300 -
Main interferometer
Fabry-Perot-Michelson with power recyclingArm cavity length : 300m
Finesse of arm cavities : 516
Light source LD-pumped Nd:YAG laserOutput power :Wavelength :
10W1064 nm
Mode cleaner Triangle ring cavityBaseline length :Finesse :
9.75m1700
Vibration isolation
Three-stage stack + Double pendulum+ Active isolation systemVibration isolation ratio : < -165 dB
Data acquisition 16 bit, 20 kHz sample, 8 channels, 160 low-freqency channels
Vacuum system < 10-6 Pa
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 31
Data Analysis results (3)--- Burst wave search ---
Burst GW event search (M.Ando, et.al. )Poorly predicted waveform
Cannot use matched-filtering schemeMasked with non-Gaussian noises
Excess power detectionTime-scale selection
10–20 10–19 10–1810–6
10–5
10–4
10–3
10–2
10–1
100
10–3
10–2
10–1
100
101
102
103
Ra
tio
[
co
un
t/to
tal
nu
mb
er]
Strain PSD [1/Hz1/2]
DT6 total
After noise reduction
Ev
en
t R
ate
[
ev
en
ts/h
ou
r]
Gaussianity
Exc
ess
po
wer
Reject non-Gaussian noisewithout rejecting GW candidates
Event rate : 10-2 /hour (1.2x10-20 /Hz)
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 32
Data Analysis results (4)--- Continuous wave search ---
Continuous wave search (K.Soida, M.Ando, et.al. )Target : pulsar at SN1987A remnant (935 0.1 Hz)DT6 1038 hours’ data
Threshold : 14P0 (False alarm: 2.6%)
No GW signal, hupperlimit : 3.4x10-23 (Preliminary: fixed spindown param.)
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 33
Data taking 8 (4)- Noise level at DT8 -
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 34
TAMA current status (1)--- Improvements after DT6 ---
Power recycling (TAMA Phase II)Mirror installation : November, 2001First lock : Dec. 24, 2001Harmonic demodulation for RM control
Longest lock : 4 hoursRecycling gain : 4
(Low gain configuration)
Improved noise level Shot noiseDetector noise levelScattered light noiseFrequency stabilization
(K.Arai, R.Takahashi S.Sato, et.al.)
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 35
TAMA current status (2)--- Current noise level ---
Latest noise levelImproved with power recycling (and the other efforts)
h : 4x10-21 /Hz1/2 around 1kHz
DT7 (Aug.31-Sept.1)
101
102
103
104
10510
–22
10–20
10–18
10–16
10–14
10–12
Str
ain
no
ise
[
1/H
z1/2]
Frequency [Hz]
Current sensitivity
June 02, 2001
Phase II goal
August 05, 2002
Improvementfactor of 3
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 36
Data taking runs (1)--- Noise level at DT6 ---
DT6 noise level h : 5x10-21 /Hz1/2
at 1kHz
Noise sources are identified
Alignment control noise Michelson phase noise Detector noise Shot noise etc.
(K.Arai, R.Takahashi, et.al.)
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 37
Data Analysis results (5)--- Coincidence search ---
TAMA-LISM coincidence analysis for binary events (paper in
preparation)(H.Takahashi, H.Tagoshi, N.Kanda, D.Tatsumi, T.Tanaka)
LISM20m detector at Kamioka mineLocked Fabry-Perot configuration
Sensitivity h : 8x10-20 /Hz1/2
Simultaneous operation with TAMA DT6: 709 hours
Compare candidate event list 244 hours of commonly lock data.Check parameter consistency
1. Significant reduction of fake event rate.2. Number of survived events :
Consistent with the accidental coincident rate. 3. Upper limit to the Galactic event rate within 1kpc :
0.064/hours (1.0-2.0 Msolar)
XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 38
Data taking 8 (5)- Stability of sensitivity in DT8 -
Sensitivity distribution