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Observation run of TAMA GW
detector
Masaki Ando
Department of Science, University of Tokyo
and
the TAMA Collaboration
Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)
Abstract
Japanese activities for GW detection
TAMA
7 year project (April 1995 – March 2002)
Construct a 300m interferometric detector : TAMA300
Several data taking runs from 1999
Operation with final configuration
Data analysis results
Next project : LCGT
3km cryogenic interferometer at Kamioka mine
Research and development tasks
(April 2002 – March 2006)
Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)
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Contents
TAMA
Overview
Data taking runs
Data analysis results
Current status
LCGT
Overview
Research and development tasks
Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)
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TAMA project (1)
--- Targets of TAMA ---
TAMA project
Detect gravitational waves
from local group of our galaxy
Research and development
for a large-scale detector
Construct an interferometer
named TAMA300
Fabry-Perot-Michelson
interferometer with 300m arms
Target sensitivity
h : 3x10-21
Aerial photograph of the TAMA site
(NAOJ, Mitaka, Tokyo, JAPAN)
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TAMA project (2)
--- Noise budget of TAMA300 ---
1/2
10
10
10
10
–16
Observation band
–18
–20
10
I goal
Phase ase II goal
Ph
NS–N
inspir S
als
Super Novae
10
10
oise
Shot n
–22
Pend
–24
10
1
10
2
ulum
therm
al no
3
ise
10
Mirror therma
l no
10
Frequency [Hz]
ise
10
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–12
–14
–16
–18
–20
1/2
10
e
ois
ic n
ism
10
–14
Se
Strain noise [1/Hz ]
10
Displacement noise [m/Hz ]
Target sensitivity
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5
TAMA project (3)
--- Basic design of TAMA300 --Main
interferometer
Light source
Fabry-Perot-Michelson with power recycling
Arm cavity length :
300m
Finesse of arm cavities :
516
LD-pumped Nd:YAG laser
Output power :
Wavelength :
Mode cleaner
Triangle ring cavity
Baseline length :
Finesse :
Vibration
isolation
Vacuum system
9.75m
1700
Three-stage stack + Double pendulum
+ Active isolation system
Vibration isolation ratio :
Data acquisition
10W
1064 nm
< -165 dB
16 bit, 20 kHz sample, 8 channels,
160 low-freqency channels
< 10-6 Pa
Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)
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TAMA project (4)
--- Photos --Mirror suspension
300m vacuum duct
FM2
Laser
MC
RM
Fused silica mirror
Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)
BS
FM1
Center room
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TAMA project (5)
--- Optical and control configuration ---
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TAMA project (6)
--- Data acquisition and analysis ---
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Data taking runs (1)
--- Data taking runs with TAMA300 --Data Taking
Objective
Observation
time
Typical strain
noise level
Total data
(Longest
lock)
DT1
August,
1999
Calibration test
1 night
3x10-19 /Hz 1/2
10 hours
(7.7 hours)
DT2
September,
1999
First Observation
run
3 nights
3x10-20 /Hz 1/2
31 hours
DT3
April, 2000
Observation with
improved sensitivity
3 nights
1x10-20 /Hz 1/2
13 hours
DT4
Aug.-Sept.,
2000
100 hours'
observation data
2 weeks
(night-time
operation)
1x10-20 /Hz 1/2
(typical)
167 hours
(12.8 hours)
DT5
March, 2001
100 hours'
observation
with high duty
cycle
1 week
(whole-day
operation)
1.7x10-20 /Hz 1/2
(LF
improvement)
(TR1)
June, 2001
DT6
Aug.-Sept.,
2001
2 days
1000 hours'
observation
50 days
111 hours
(24.8 hours)
5x10-21 /Hz 1/2
Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)
1038 hours
(22.0 hours)
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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 Galaxy
SNR of 30 for 1.4-1.4 Msolar inspirals
Operation : 1107 hours (92.3%) , longest cont. operation : 22 hours
Observation : 1038 hours (86.5%)
Well-organized observation
Automatic lock of the detector
Online monitor and diagnosis
65 shift participants (2 person / 8 hours’ shift)
Coincidence run
LISM (20m detector at Kamioka mine)
Simultaneous operation : 709 hours
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Data taking runs (3)
--- Detector operation status in DT6 --Operation status calendar
Total operation : 1107 hours
Date in JST
Mon
Tue
Wed
Typhoon
Laser instability
Measurement+adjustment
Human error
Thu
Fri
Sat
Sun
Aug. 01
02
03
04
05
06
07
08
09
10
11
12
13
14
15
16
17
18
19
20
21
22
23
24
25
26
27
28
29
30
31
Sep. 01
02
03
04
05
06
07
08
09
10
11
12
13
14
15
16
17
18
19
20
Operated (over 10min)
High–freq. data taking
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Data taking runs (4)
--- Noise level at DT6 --DT6 noise level
h : 5x10-21 /Hz1/2
(K.Arai, R.Takahashi, et.al.)
at 1kHz
Noise sources
are identified
Alignment control noise
Michelson phase noise
Detector noise
Shot noise
etc.
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Data Analysis results (1)
--- TAMA data analysis --GW event search
Binary inspiral search
One step search (H.Tagoshi, D.Tatsumi, H.Takahashi)
Two step search (H.Tagoshi, T.Tanaka)
Binary inspiral search using Wavelet (N.Kanda)
TAMA-LISM coincidence (H.Takahashi, H.Tagoshi, D.Tatsumi,…)
Continuous wave from known pulsar (K.Soida, M.Ando,…)
Burst wave search (M.Ando,…)
BH ringdown search, Stochastic background search, etc.
Detecor characterization analysis
Calibration (D.Tatsumi, S.Telada,…)
Noise veto analysis (Y.Watanabe, N.Kanda,…)
Interferometer diagnosis (M.Ando,…)
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Data Analysis results (2)
--- Inspiral search --Binary inspiral event search
(H.Tagoshi, D.Tatsumi, N.Kanda, H.Takahashi, T.Tanaka, M.Sasaki)
Expected SNR
for binary mergers
Distance: 10kpc
(Galactic center)
DT6 noise spectrum
SNR : about 30
(1.4/1.4 Msolar binaries)
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--- Inspiral search (contd.) --Matched filtering analysis
(paper in preparation)
DT6 1038 hours’ data
1.0-2.0 Msolar events (200-1000 templates)
c2 event selection (  /  2  16)
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%)
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Data Analysis results (3)
--- Burst wave search --Burst GW event search
(M.Ando, et.al.）
Poorly predicted waveform
Cannot use matched-filtering scheme
Masked with non-Gaussian noises
Reject non-Gaussian noise
without rejecting GW candidates
Event rate : 10-2 /hour (1.2x10-20 /Hz)
3
0
10
–1
10
10
2
10
1
–2
10
10
DT6 total
0
–3
10
10
–4
10
–1
After noise reduction
10
–2
–5
10
10
–6
10
Gaussianity
–20
10
–19
10
1/2
Strain PSD [1/Hz ]
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Event Rate [events/hour]
Excess power
Ratio [count/total number]
Excess power detection
Time-scale selection
–3
10
–18
10
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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.)
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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)
LISM
20m detector at Kamioka mine
Locked 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)
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TAMA current status (1)
--- Improvements after DT6 --Power recycling (TAMA Phase II)
Mirror installation : November, 2001
First lock : Dec. 24, 2001
Harmonic demodulation for RM control
Longest lock : 4 hours
Recycling gain : 4
(Low gain configuration)
Improved noise level
Shot noise
Detector noise level
Scattered light noise
Frequency stabilization
(K.Arai, R.Takahashi S.Sato, et.al.)
Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)
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TAMA current status (2)
--- Current noise level --Latest noise level
Improved with power recycling (and the other efforts)
h : 4x10-21 /Hz1/2 around 1kHz
–12
10
June 02, 2001
1/2
Strain noise [1/Hz ]
–14
10
Improvement
Current sensitivity factor of 3
August 05, 2002
–16
10
–18
10
–20
10
oal
e II g
s
a
h
P
–22
10
1
10
2
10
3
4
10
10
Frequency [Hz]
5
10
DT7 (Aug.31-Sept.1)
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Current and future tasks
--- LCGT project --TAMA project
7years’ project (April 1995 – March 2002)
LCGT
Baseline length : 3km
Site: Kamioka mine
Cryogenic interferometer
Laser : 100W
50kg Sapphire mirror
(20K, Q=108)
Broadband RSE
Seismic isolator :
SAS (300K)
Cryogenic SUS (10K, Q=2x108)
Suspension point interferometer
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Current and future tasks
--- Status --Research and development for LCGT
Observation runs with TAMA detector
Development of cryogenic techniques
100m cryogenic interferometer : CLIO
Seismic isolation system : SAS
Thermal noise investigation
Resonant sideband extraction, Suspension point
interferometer
Design document will be finished in this year
DECIGO (Interferometer in space)
Working group
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R&D tasks (1)
--- CLIO100 --CLIO100 : 100m cryogenic interferometer
Development and test of …
Mirror
Suspension
Cryogenics
(S.Miyoki, M.Ohashi, et. al.)
Tunnel digging
finished
(July 2002)
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R&D tasks (2)
--- TAMA SAS --TAMA SAS
Low-freq. seismic attenuation system
To be installed in TAMA300
Pre-isolator of LCGT
(A.Takamori, et. al.)
Full Scale Prototype Test
Two Test Towers
For a 3m Prototype Interferometer
Established Local Control
Characterization of
Attenuation Performance
Introducing New Control Method
Commissioning a Fabry-Perot Cavity
2 SAS Prototypes Completed
Acquired lock of the cavity
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--- TAMA SAS (contd.) --(A.Takamori, et. al.)
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--- TAMA SAS (contd.) ---
10
1/2
Displacement [m/Hz ]
10
10
10
10
10
10
10
10
10
10
-4
Cavity Motion
Ground Motion
DAC Noise
Frequency Noise (Free Run)
Estimated FP displacement
-5
-6
-7
-8
Alignment Noise
-9
-10
-11
-12
-13
-14
0.01
0.1
1
10
Frequency [Hz]
Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)
100
(A.Takamori, et. al.)
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R&D tasks (3)
--- Direct measurement of TN --Reference Cavity
Rigid cavity (suspended)
Frequency stabilization
Length : 11cm
Finesse : 19000
Test Cavity
Displacement sensor
Independent mirror
Length : 1cm
Finesse : 500
Spot size : 50um
Material : BK7
(K.Numata, et. al.)
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--- contd. --Approaching TN
Future works
10
10
10
Sensitivity[m/rtHz]
…or looking at TN
Unidentified noise : f-1/2
10-16m/rtHz@~100Hz
~TAMA
Could be updated by
Low noise driver
Stack
Alignment
Shot noise
New mirror
CaF2/Sapphire/Silica…
Differential measurement
Frequency/seismic noise
Electric noise
Ground loop
Low noise filter
10
10
10
10
10
10
10
10
10
-7
Sensitivity (02/06/29)
Sensitivity(W/O stabilization)
-8
-9
Total
Brownian
Thermoelastic
-10
-11
-13
Frequency noise(Stabilized)
Frequency noise(Freerun)
Demodulation system noise
Servo system noise
Driver noise
-14
Seismic noise(W/ z-coupling)
-12
-15
-16
-17
-18
10
0
10
1
10
2
10
3
10
4
10
5
Frequency[Hz]
Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)
(K.Numata, et. al.)
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Summary
TAMA300
Data taking runs
6 data taking runs (August 1999- ), over 1000 hours of data
Data analysis
Upper limit for Galactic binary inspirals : 0.0095 /hour
Coincidence analysis, burst wave, continuous wave
Data taking 7 : August 31 - September 1
Detector updates
Power recycling
Recycling gain : 4
Longest cont. lock : 4 hours
(over 24 hours without power recycling)
Improved sensitivity : h : 4x10-21 /Hz1/2
For LCGT
R&D tasks
Design document in this year
Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)
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