Status of TAMA
National Astronomical ObservatoryofJapan
Koji Arai (TAMA project)Overview of this talkl Introduction
Laser interferometric gravitational-wave detector
Worldwide statusl TAMA300 detector

Overview of the detector

Activity1: 1000hours observation
Activity2: Recycling experimentl Analysis of TAMA300 data

(2001/8-9)(2001/12~)

Inspiral search, burst search, and pulsar searchOverview of this talkl Introduction

F Laser interferometric gravitational-wave detector
F Worldwide statusl TAMA300 detector

Overview of the detector

Activity1: 1000hours observation
Activity2: Recycling experimentl Analysis of TAMA300 data(2001/8-9)(2001/12~)

Inspiral search, burst search, and pulsar search

Gravitational wave detection (1)l Direct detection of GW
Binary pulsar observation[ Indirect proof of GWs
Direct observation of GWs[ Confirmation of General Relativity
in a strong gravitational field[ Information of astrophysical objects

which is different from that with EM observation

Gravitational wave detection (2)l Resonant mass detector
GWvibration
sensormetallic bar

Excitation of quadrupolemodes of the bar[ Narrow-band detection~ only at the resonant
frequencyl Interferometric detector
Suspended
mirrorGW
Beamsplitter

Differential pathlengthchange of two arms
[ Wide-band detection~ waveform is preserved

Suspended
mirrorLaser
Photodetector

Interferometric GW detector
throughout the world
l 4 projects, 6 large-scale interferometers
VIRGO(Italy & France)

GEO
Germany & Great Britain

TAMAJapan

LIGO
U.S.A.

Site: Pisa
L=3km

Site: Hannover
L=600mSite: Tokyo
L=300mSite:
Hanford 1
L=2km
Hanford 2
L=4km
Louisiana
L=4km

LIGO

LIGO Hanford

First light 1999
Improving the sensitivity
and the stability
8 engineering runs
Run into Scientific runs from 2002

LIGO Louisiana

GEOEngneering and Science runs from 2002
Changing the optical configuration (Signal Recycling)VIRGO

5 engneering runs
End commissioning of CITF (Short interferometer),
Arm construction finishedMove to Full 3k IFO

Overview of this talkl Introduction
Laser interferometric gravitational-wave detector
Worldwide statusl TAMA300 detector

F Overview of the detector
Activity1: 1000hours observation
Activity2: Recycling experimentl Analysis of TAMA300 data(2001/8-9)(2001/12~)

Inspiral search, burst search, and pulsar search

TAMA300l Laser interferometric GW detector
with arm length of 300m
Site: National Astronomical Observatory of Japan,(Mitaka, Tokyo)l Object of the project
To develop a detector capable to detect GW eventsin nearby galaxies.
To establish techniques for a future km-class interferometer
Designed sensitivity ~hRMS = 3 x 10-21 @300Hz (BW300Hz)

Bird’s view of the TAMA sitel National Astronomical Observatory of JapanTokyo, Mitaka Campus (E139.32.21 N35.40.25)
WestEndRoomCenterRoomSouthEnd
RoomMiddle of a city area ~ heavy traffic

TAMA300 detector ~ overview

300mFP arm

Recycling
Mirror10m
ModeCleaner

Gravitational
Wave

300m FP arm

Vacuum Chamber /Vacuum Duct
Suspension
SystemPhotodetector

10W
Laser
Data Acquisition
Storage/Analysis

MirrorVibration
isolation
stackCenter room

300m vacuum tube

Vibration Isolation Systeml 3 layer system
Actively-controlled
air spring+
Stack(Sandwitches of rubbers
and metal blocks)+
Double pendulum
suspension

Achieved performance~ better than 10-8
at 150HzMirrorl Fused silica (SiO2) φ 100mm x 60mm
High mechanicalquality~ to suppress thermal
vibration in the observation
bandHigh optical quality~ ultra low loss (~30ppm)
in reflection.

Control electronics

History of TAMA development
1995
1996

Recombine I
98/5 - 99/1

1997

Mode Cleaner
97/4 - 97/12

300m
FP cavity

10W Laser

Mode Cleaner+ 10W Laser
98/1 - 99/1

300m
FP cavity

Project started
Facility construction
completed
Vacuum systemcompleted

1999/8
Data Taking 111h
1999/9
Data Taking 231h
2000/4
Data Taking 313h
2000/8,9 Data Taking 4 167h
2001/3
Data Taking 5 111h
2001/8,9 Data Taking 6 1038h2001/10- Recycling experiment

Recycling I
01/10 - PresentOne Arm
2002/8-9 Data Taking 7
97/8 - 98/410m
Mode Cleaner

Recombine II
Recombine III

99/2 - 00/6
00/9 - 01/925h

Overview of this talkl Introduction
Laser interferometric gravitational-wave detector
Worldwide statusl TAMA300 detector

Overview of the detector

Activity1: 1000hours observation
F Activity2:
Recycling experimentl Analysis of TAMA300 data

(2001/8-9)(2001/12~)

Inspiral search, burst search, and pulsar searchPast data taking (DT) runs
[Without power reycycling]DT1 1999 Aug. 6-7

1 night

11 hours

DT2 1999 Sep. 17~20

3 nights

31 hours

DT3 2000 Apr. 20~23

3 nights

13 hours

13 nights

167 hours

6 days111 hours

50 days1038 hours

1 day

25 hours

DT4 2000 Aug. 21~Sep. 4
DT5 2001 Mar. 2~8
DT6 2001 Aug. 1~Sep. 20[With power recycling]DT7 2002 Aug, 31~Sep. 2

Data runs have been held prior to the other projects.

Achievements on DT6l Sensitivity enough to detect Galactic GW events
Strain sensitivity:

h = 5 x 10-21 /sqrtHz

NS ispirals with SNR=10:33kpc

l Stable operation ~ high duty ratio
Total amount of observation data:

1038 h (86.5%)(adjustment period excluded)l Coincident run with Kamioka 20m prototype
Total amount of coincident operation:

709 h(59.1%)

Achieved sensitivity (at DT6)l Displacement noise dx = 1.5 x 10-18 m/Hz1/2(@700Hz)
Strain sensitivity
h = dx/300= 5x10-21 /Hz1/2
-11

10-12

10-13

1/2

Strain sensitivity [1/Hz ]

10-14

10

June. 2, 2001
Phase I goal

-15

10-1610-17

10-1810-19

10-20

10-2110-2210

110102

310

Frequency [Hz]410510DT6: SNR to compact binaries
l Observable distance with SNR=10
using matched filtering
60

2001/8/3
DT6Observable Distance [kpc]50

Steller BH binary
10Mo ~34kpc

40

NS binary
1.4Mo ~33kpc

30
20

Macho BH binary
0.5Mo ~17kpc

100
10-1

2

3

4

5 6 7 80234

5 6 7 810
mass of a member star [Msolar]

1012Observation calendar
Date in JST
Mon

Tue

06

WedThuFriSat

Sun

07

08

09

10111213

1415

16

1718

19

20

21

2223

24

25

2627

28

29

30

31

Sep. 0102030405

06070809

1011121314151617181920Aug. 01

02

Operated (over 10min)

03

04

05

High–freq. data taking

Causes of obs. time loss

32iiiii

Laseri

Human errori
LaseriTape exchange

Typhoon + Laser

4i

Human error + Laser

5i

Laser
Typhoon + Human error + Laser

6i

Human error
Human error

7Obs. time in each shift [hours]i

Preparation
HDAQ + Prep.
Measurement

8Construction
Measurement
Fire detector check

Total obs. time: 1038:07:35, Duty cycle: 86.5105%

10010203040506070809101112131415161718192021222324252627282930310102030405060708091011121314151617181920AugSep
Observation date

SNR trend during DT6SNR

SNR

SNRSNRl About 80% is adequate to analyses
40
35
30
25
20
15
10
50
08/01

08/02

08/03

08/04

08/05

08/06

08/07

08/08

08/09

08/10

08/11

08/12

08/13

08/14

08/15

40
35
30
25
20
15
10
5
0
08/15

08/16

08/17

08/18

08/19

08/20

08/21

08/22

08/23

08/24

08/25

08/26

08/27

08/28

08/29

40
35
30
25
20
15
10
5
0
08/29

08/30

08/31

09/01

09/02

09/03

09/04

09/05

09/06

09/07

09/08

09/09

09/10

09/11

09/12

09/24

09/25

09/26

40
35
30
252015105009/12

10-10 Msolar
1.4-1.4 Msolar
0.5-0.5 Msolar
09/13

09/14

09/15

09/16

09/17

09/18

09/19

=> To data analysis

09/20

09/21

09/22

09/23

Overview of this talkl Introduction
Laser interferometric gravitational-wave detector
Worldwide statusl TAMA300 detector

Overview of the detector

FActivity1: 1000hours observation
Activity2: Recycling experimentl Analysis of TAMA300 data

(2001/8-9)(2001/12~)

Inspiral search, burst search, and pulsar searchPower recycling
l Enhancing light power in the interferometer
Partial mirror(Power recycling mirror)

300m arm

300m arm

Laser

Principle of power recycling
l Why recycling mirror increases the light
power in the interferometer?
e.g. Michelsoninterferometer“Bright”
interference“Dark”
interference(no light coming out)Principle of power recycling
l Why recycling mirror increases the light
power in the interferometer?
no light“Dark”
interference(no lightreflected)

Highreflectance
Recycling
Mirror“Bright”
interferenceHighreflectanceno light

no light

Q. The light has no way out from the interferometer.
Where does the light go?

Principle of power recyclingl Laser light is enclosed in the interferometer
This condition is so-called “resonant”, “impedancematched”, or “recycled”
Total dissipated power= Incident power

Pinc = εloss PinternalPower in the arms
Low loss optics

Pinc
Pinternal =εloss

g Pincenhanced
High recycling gain

Displacement noise level of TAMA300(August, 31 2002)

-7

10-8

10-9

1/2

Displacement noise [m/Hz ]10

2001/06/02 (Recombine3)
2002/08/31 (Recycling1 HP)
Phase2 limit-10

10-1110-1210-1310-1410-15

10-16

10-1710-18

10-1910-20

100

10

110210310

Frequency [Hz]410510-11

10Feb. 14, 1999
Sept. 3, 1999
Oct. 15, 1999
March. 16, 2000
Sept. 4, 2000
June. 2, 2001
Aug. 31, 2002
Phase2 Limit-12

10-13

1/2

Strain sensitivity [1/Hz ]

10-14

10-15

10-16

10-17

10-18

10-19

10-20

10-21

10-22

10

1

1010

2

3

10

Frequency [Hz]410510Expected SNR to inspiralsl Observable distance with SNR=10
using matched filtering
Observable Distance [kpc]80

2002/09/29
With power recycling

60

Steller BH binary
10Mo40NS binary
1.4Mo
20Macho BH binary
0.5Mo0-1102345 6 7801023

mass of a member star

45 6 7 81102

Estimation of noise contributionsl Noise estimation based on signal injection
Artificial
Sinusoidal
Signal

dx

dx

Laser
Frequency
Noisedxffrequency

GW
SignalportdxdxfffDisplacement noise level of TAMA300-7(September, 29 2002)

Preliminary

10-8

10-9102002/9/29 Displacement sensitivity
Alignment noise (2001/06/03)
Detector noise
Shot+Detector noise
Modulation noise
Recycled Michelson noise
Intensity noise
Frequency noise
Filter noise (feedback)
Seismic noisedl- feedback noisedl+ feedback noise

-10

1/2

Displacement noise [m/Hz ]10-1110-1210-13

10-14

10-15

10-1610-1710-1810-19

10-20

100

10110231010
Frequency [Hz]410510Stabilityl Recycling also increases complicationof the system
Internal power becomes sensitive to mirror motions

Transmitted
light level [a.u.]

3.0
2.5
2.0
1.5

8h 38mminavg
max

1.0
0.5
0.0

21:00 22:00 23:00
2002/08/31

0:00

1:00
Time

2:00 3:00 4:00
2002/09/01

Longest continuous operation
with power recycling:
8h 38m(without power recycling: 24h 50m)

5:00

Concident observations
l large-scale interferometers in operationu S1 (Scientific run 1)
2002/8/22-2002/9/9
Coincident run by LIGO and GEO
Partial participation of TAMAu S2 (Scientific run 2)
2003/2/14-2002/4/14
Full coincident run by LIGO, GEO and TAMATAMA, LIGO (and GEO) detectors enter theobservation phase in 2002 - 2003.
••

5 detectors are operating in Comparable Sensitivity
TAMA: 300m at Mitaka Tokyo
LIGO: Livingston 4km, Hanford 4km, 2kmGEO: 600m
Benefit
Increase of whole sky coverage
Statistical Treatment• More strict rejection for fake events• Efficient criteria with same fake rate of single detector analysis•

Stable run scheduling
LIGO(+GEO) S1<-> TAMA DT7• 2002, summer. 2 weeks <-> 3 days
• Actual 9hrs 50min. common locking data

LIGO(+GEO) S2 run <-> TAMA DT8• Duration: 2/14/2002 - 4/14/2002

S1 & DT7
Common Lock of 5 interferometers: 9hrs 50min
Longest Common Lock stretch:2hrs 24min
Coincidence Run (TAMA300, LIGO, and GEO600)

T1

G1

L1

H2H112:00 14:00 16:00 18:00 20:00 22:00

0:00

2:00

4:00

6:00

8:00

10:00 12:00 14:00 16:00 18:00 20:00 22:00

Time [hour] (from 31 Aug. 12:00 UTC)

Overview of this talkl Introduction
Laser interferometric gravitational-wave detector
Worldwide statusl TAMA300 detector

Overview of the detector

Activity1: 1000hours observation
Activity2: Recycling experiment

Fl Analysis of TAMA300 data

(2001/8-9)(2001/12~)

Inspiral search, burst search, and pulsar search

Gravitational wave search:
Compact binary Inspiral
Matched filtering analysis （Tagoshi, et al.)
We analyzed 1000 hours data of DT6 by matched filtering to searchfor compact binary inspirals
Upper limit to the event rate:•DT2: 0.59/hours (0.3-10Msolar) (Phys.Rev.D63,062001(2001))•DT4: 0.027/hours (0.3-4.7Msolar)•DT6: Upper limit to Galactic event rate:
0.0095/hours (1-2Msolar)

TAMA-LISM coincidence analysis (Takahashi’s talk)is also doneMatched filter• Detector outputs: s ( t ) = A h ( t ) + n ( t )h(t ) ： known gravitational waveform (template)Post-Newtoniann(t ) ： noise.
approximation• Outputs of matched filter:z~*~s ( f )h ( f )ρ ( m 1 , m 2 , tc , . . . ) = 2df
Sn ( f )•Sn ( f ) noise spectrum density• signal to noise ratio SNR = ρ / 2• Matched filtering is the process to find optimal
parameters which realize

FH max ρ(m , m , t ,...)IK
m1 , m2 ,tc ,...

12c

Log10[Number of events]ρ / χ 2 = 16)2
ρ/ χUpper limit to the Galactic event rate
threshold=16 (〜S/N=11) (fake event rate=0.8/year)
Efficiency for Galactic events ε = 0.23 (from simulation)•We also obtain upper limit to the average number ofevents over threshold by standard poisson statistics analysis
N=2.3 (C.L.=90%)•Data length used : T＝1039 hours
Upper limit to the Galactic event rate

N==0.0095 [1/ hour] (C.L. = 90%)Tεc.f.

Caltech 40m : 0.5/hour(C.L.=90%)

Allen et al. Phys. Rev. Lett. 83, 1498 (1999).

Burst wave analysis (1)(Ando, et al.)--- Burst gravitational wave search --Burst gravitational wave analysis (Super novae, etc.)
Waveforms are poorly predicted
Cannot use matched filtering method
Look for ‘something unusual’ events
Detection efficiency is limited bynon-Gaussian noises in a GW detector

Rejection of non-Gaussian noise is indispensable
Single detector
Detector improvement
Data processing
Correlation with other detectors
Other GW detectors
Other astronomical channels(Super novae, Gamma-ray burst, etc.)
1

Burst wave analysis (2)--- Reduction of non-stationary noise --Non-Gaussian noise reduction
Distinguish GW signal from non-Gaussian noises
with time-scale of the ‘unusual signals’
GW from gravitational core collapse < 100 msec,
Noise caused by IFO instability > a few sec
2 statistics in detector output
Averaged noise power
2nd-order moment of noise power
Estimate parameter : ‘GW likelihood’C1 = Pj 2
1  Pj−2C2 = 
2  Pj 2Reduce non-stationary and non-Gaussian noises
without rejecting GW signals

2

Burst wave analysis (3)--- Data processing --Data Processing
1. Calculate Spectrogram by FFT
2. Extract a certain time-frequency region
to be evaluated
3. Evaluate GW likelihood at each frequency
4. Reject given time region
if it has large ‘non-GW like’ ratio

Raw data

Spectrogram

5. Calculate total power for given T-F region

Evaluation‘Filter’ outputs
Survived --- Stable detector operation
Data may be used for GW search
Large power : event candidates
Rejected --- Detector instability
Detector ‘dead time’

Rejection, Total power3

Burst wave analysis (4)--- DT6 data analysis --Data Taking 6 (Summer 2001)
Analyze last 1-week data
Bandwidth : 500Hz
Rejected data : 20%(False dismissal rate : 1ppm)

Event rate for 10msec GWs
hrms〜 1x10-17 : 1 events/hour
hrms〜 3x10-17 : 10-2 events/hour

Event Rate [Ratio]

Still worse than stable hours
in DT4, and Gaussian noise level03

1010–1

2

Original data

1010–2

10

1–3

10

10
10–4

10–5

100

1/1000DT4 stable(10hours)–1

After noise rejection 10–2

10Gaussian noise

10–20

10–19

10–18

1/2

Noise level [1/Hz ]4

Event Rate [events/hour]

Improvement offalse event rate : 1/1000

Continuous wave from SN1987A
l Continuous GW wave searchat around 935Hz from SN1987a remnant(Soida, et al.)
Expected Waveform: Sinusoidal(f=934.908Hz +/- 0.05Hz)+ time dependence of the sensitivity+ doppler correction(the earth's daily/yearly round)+ spindown correction(assume spindown rate: 2.5x10-10 [Hz/s])

Search: DT6 50days data

Search result

h=3.8x10-23(False alarm rate 1.8%)
Theoretical upper limit from spindown rate: h=9.4x10-27

Online analysis
l Further development on data analysis system
Requirement for long / coincident observation
Real-time/online GW event search-> PC clusters on each institute(NAO, Osaka Univ, Osaka City Univ., Univ. of Tokyo, ICRR)
Systematic search-> Use of unified software
Network data distribution-> connect each institute with Super SINET (>10Gbps)

Summaryl Interferometric GW detector TAMA300
Observation: 50 days, more than 1000 hours
Power recycling: Improvement of the sensitivity
h = 3.3 x 10-21 /sqrtHz @1.5kHz

l Data Analysis using DT6 data
Binary ispirals
Burst searchContinuous wave searchl Future plan
Continue to improve the performance
Online/real-time analysis
Coincident observation with LIGO and GEO