OperationofTAMA300 detector
National Astronomical Observatory of Japan
Koji Arai (TAMA project)

MG10 GW3 session

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.

WestEndRoomSouthEnd
RoomTo establish techniques
for a future km-class interferometer
Designed sensitivity ~hRMS = 3 x 10-21 @300Hz (BW300Hz)

CenterRoomTAMA300 detector ~ overview

300m
FP armRecyclingMirror

10m
ModeCleaner

GravitationalWave

300m FP arm

Vacuum Chamber /Vacuum Duct
Suspension
SystemPhotodetector

10W
Laser
Data Acquisition
Storage/Analysis

MirrorVibration
isolation
stack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 1038h
2001/10- Recycling experiment

Recycling I
01/10 - Present

One Arm
2002/8-9 Data Taking 7
97/8 - 98/425h
2003/2-4 Data Taking 8 1158h

10mMode Cleaner

Recombine II
Recombine III

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

Principle of power recyclingl Laser light is enclosed in the interferometer
Highreflectance“Dark”
interference
no light
reflected

no light

Total dissipated power= Incident power
Recycling
MirrorHigh
reflectance“Dark port”
no light

Pinc = εloss Pinternal

no light

Pinc
Pinternal =G Pinc
εloss
(GTAMA=4.5)

Frequency Stabilization
Displacement noise level of TAMA300-1010-1110With Power recycling-12

Displacement noise (2003/02/20)
Frequency noise (2003/12/04)

Displacement noise [m/Hz-1/2]

10-13

Without Power recycling

10Frequency noise (2001/08/03)

-14

10-15

10-16

10-17

10-18

10-19

10-20

10-21

10

1

102

10

3

10

10

4

105

Control bandwidths extended:MC servo(300kHz -> 600kHz)
Common-mode servo( 20kHz -> 40kHz)

Frequency [Hz]

Power recyclingl Sensitivity improved by power recycling
Reduction of detector noise, shot noise, and frequency noise
Displacement noise level of TAMA300(July 12, 2003)-710-810-9

July 12, 2003 with recycling
June 2, 2001 without recycling
Phase2 theoretical limit

101/2

Displacement noise [m/Hz ]-1010-1110-12

10-13

10-14

10-15

10-1610-17

10-18

10-19

10-20

10010

Floor level:

1102

10
10
Frequency [Hz]8 x10-19 m/Hz1/2
2.7x10-21 /Hz1/2

310

4

105

(in displacement)(in strain)

History of the sensitivity
l Improvement by a factor of 103 ~ 104~ operation since 1999
Strain sensitivity of TAMA300-1110Feb. 14, 1999
Sept. 3, 1999
Oct. 15, 1999
March. 16, 2000
Sept. 4, 2000
June. 2, 2001
July 12, 2003
Phase2 limit

-12

10-13

10
1/2

Strain sensitivity [1/Hz ](July 12, 2003)

-14

10-15

10-16

10-17

10-18

10-19

10-20

10-21

10-22

10

110

10

2

3

10

Frequency [Hz]

4

10

5

10

Observable distancel Distance of binary inspirals~ expecting SNR=10, optimal incident angle assumed

Observable Distance [kpc]70

4.3Msolar
66.0kpc

60
1.4Msolar
46.6kpc

50
4030

10Msolar
35.0kpc

0.5Msolar
21.4kpc

20July 12, 2003
with recycling
June 2, 2001
without recycling

10010 -1

23

4 5 6 7 892310 0mass [Msolar]

4 5 6 7 89

10 1

2

Sufficiently sensitive to galactic inspiral events

Displacement noise level of TAMA300 (May 21, 2003)-7

10

Displacement noise level of dLAlignment noise
Seismic noisedl- feedback noisedl+ feedback noisedL- filter noise
Modulation noise
Shot noise and detection system noise
Shot noise (calculated)
Detection system noise
Laser intensity noise
Laser frequency noise-810-91/2

Displacement noise [m/Hz ]10-1010-1110-1210-1310-1410-1510-1610-1710-1810-1910-20

10-21

100101102103

10Frequency [Hz]410510Data taking (DT) runs in past
6 observations without power recycling
2 observations with power recycling[Without power recycling]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

DT4 2000 Aug. 21~Sep. 4 13 nights 167 hours
DT5 2001 Mar.

2~ 8

6 days111 hours Coincidence

DT6 2001 Aug. 1~Sep. 20 50 days 1038 hours

LISM(20m)[With power recycling]DT7 2002 Aug, 31~Sep. 2

1 day

25 hours

DT8 2003 Feb. 14~Apr. 15 59 days 1158 hours

LIGO & GEO
LIGO

Data Taking 8 (LIGO S2)
l DT8 ~ 2 months run (2003/2/14~4/15)
First full-time joint observation with LIGO
(c.f. DT7: partial participation of TAMA to S1)First long-term observation with power recycling
Power recycling of TAMA300 (2001/10~Present)
Power recycling gain of 4.5
Best sensitivity: 2.7x10-21[/Hz1/2]
IFO operation
Accumulated data:

1158 hours

Duty cycle:81.3 %Longest lock:20.5 hours

Power-recycled
Fabry-Perot
Michelson
Interferometer

300m arm

300m arm

Laser

Improved long-term stability
Longest lock stretch in the observations

Transmitted power [a.u.]54

DT8: 20h31m

32

DT7: 8h38m

100

510Time [hour]

1520

Improved long-term stability
Longest lock stretch in the observations

Transmitted power [a.u.]54

DT8: 20h31m

3l Length drift control
l WFSs for the test masses
DT7:
8h38m
l Recycling
mirror alignmentl Optical axis control

2100510Time [hour]

1520

Duty cyclel 1157h51m (out of 1424 hours, duty cycle 81.3%)
Start: Feb 14, 2003, Fri, 23:00:00 JST, End: Apr 15, 2003, Tue, 07:00:00 JST (Total run time: 1424:00:01)
Total long obs. time: 1157:51:26, Duty cycle: 81.3102%

7

S S

Avg duty cycle (81.3%)
CC C

Obs. time in each shift [hours]

6C CW

DAQ
Trouble5

C C CCWWW

Circuit
Failure

1200

S1000

C C CC

CC CW

Laser
TroubleC C

CCWCC C C CC C C CRoad
WW W
High Constructions
800
SeaWaves
MCTrouble

4600

PowerFailure

34002200
10 141516171819202122232425262728010203040506070809101112131415161718192021222324252627282930310102030405060708091011121314150FebMar

Apr

Total Obs. time [hours]

8Signal Injection
ExperimentDT8 ~ Disturbance by construction

Observable
Distance [kpc]Seismic level[mgal (=10-5m/s2)]

13rd May, 2003 (Thu)(Noisy weekday)
30
25
20
15
1050

Construction works
near the site

Duty cycle

Daily trend of duty cycle/sensitivity
1.0
0.8
0.6
0.4
0.2
0.00

Lunchtime3691215
Hour (JST)

18

21

24

Observabledistance [kpc]With construction ~ IFO didn't work => Duty cycle about 60%
40
30
2010003691215Hour (JST)182124

Even without construction ~ sensitivity reduction of about 20%

Seismic level vs Duty cycle
Duty cycle vs Seismic motion

1Duty Cycle

0.8
0.6
0.4
0.2
005101520
Seismic Motion (mgal)

25

Data analysis activitiesl Matched filtering analysis> NS binary inspirals> Coincidence analysis between multiple detectors> 0.5Msolar Macho BH binary inspirals> BH ringdown analysis

l Burst analysis> Rejection of non-gaussian noiseby time-scale selectionl Continuous wave
> Search for GW from possible SN1987a remnant

Matched Filtering analysis• Detector outputs: s ( t ) = A h ( t ) + n ( t )h(t) ： known gravitational waveform (2.5PN template)n(t) ： noise.
• Correlation of the detector output and the templatein the frequency domain:~*~s( f )h ( f)
ρ ( m 1 , m 2 , tc , . . . ) = 2
df
Sn ( f )• Weighted by Sn ( f ) noise spectrum density• Signal to noise ratio SNR = ρ /2

• Find the optimal parameters

m1, m2 , tc ,...

in a data chunk which maximizes ρχ test
2

Divide frequency region into bins.
Test whether the contribution to ρ from eachbins agree with that expected from chirp signalF
ρ ≡ ( s, h ) G z
HS (f)

IJK

ρ3 ρ 4 ρ5L

f3

f5 L=2

ρ1

ρ2
f1

fmin

f2

~s~ ( f ) h ( f )
*dfn

f4

1
χ ≡ ∑ 2 ( ρ i − ρ i )2σi2

σ i 2 ≡ ( ρ i − ρ i )2 ,

ρi = ρifmax

Event distrib. / detection efficiency
TAMA events and Galactic event

5ents

4.5

3(χ2)1/2 2.5
2

ρ/(χ2)1/2=12.5

TAM

3.5A ev

4slaignsts
Te

1.5
1detection efficiency
ε = 0.61

0.5
010

2030

4050
ρ60

70

80

90100

Event distribution / threshold
TAMA DT8 results

Log10(number of events)

87

Fitting range

65Threshold

4r / c 2 =12.5

32
103

456

7

8

9 10 11 12 13 14 15r/(c2)1/2

Set "False Alam rate"
to 0.8 event/yearUpper limit to the Galactic NS mergerl Observation timeTobs = 1163 hours (for lock longer than 520sec)
l Event threshold
1039 hours for DT6
ρ/(χ2)1/2 = 12.5
(for false alerm rate = 0.8 / year)
ρ/(χ2)1/2 = 16 for DT6l Detection efficiency
ε = 0.61(from Galactic event monte-carlo simulation)l Upper limit to the avg # of events 0.23 for DT6
Observed # of event = 0
over the threshold=> N=2.3 (C.L.: 90%) (from standard Poisson statistics analysis)
Preliminary search result for DT8=> N / Tobs / ε = 0.0033 [event/hr]= 2.9x101 [event/yr]
for 1.0 Msolar < m1, m2 < 3.0Msolar

For DT6=0.0095[1/hr]=8.3x101 [1/yr]
1 < m < 2Msolar

Future Planl Data Analysis of the DT8 data other than NS inspirals
In progressl Investigation on the noise issues
In particular, noises between 100Hz and 1kHz.
l Further automation of the observation
To operate the interferometer with less operatorsl Upgrade of the vibration isolation system
Seismic attenuation system (SAS)Isolation from low frequency (~0.1Hz)
R&D with Caltech and Univ. of Pisa
Installation in early 2005l More power in the arms
High gain (G=10) recycling

Summaryl Interferometric GW detector TAMA300l Data Taking 8
Full-time joint observation with LIGOFirst long-term operation with power recycling
With improved sensitivity by power recyclingh = 2.7 x 10-21 /sqrtHz @1.5kHz
1158 hours of 1424 hours => duty cycle 81.3%

l Data Analysis using DT8 data
NS ispirals: Galactic event rate
R < 0.0033 event/hr (C.L.90%)
for 1.0 Msolar < m1, m2 < 3.0Msolar