TAMA300:
current status
andthe joint observation with LIGONational Astronomical Observatory of Japan
Koji Arai (TAMA project)Overview of this talkl Introduction of TAMA300

a 300-m Fabry-Perot Michelson interferometer8 observations in pastl The 6th observation: Data Taking 6The observation for 50 days in the summber of 2001
Analyses of the 1038-hours datal The 8th observation: Data Taking 8(= LIGO S2)

LIGO-TAMA joint observation for 2 months
Detector development for DT8
Operational status

Overview of this talkof TAMA300
Fl Introduction
a 300-m Fabry-Perot Michelson interferometer8 observations in pastl The 6th observation: Data Taking 6The observation for 50 days in the summber of 2001
Analyses of the 1038-hours datal The 8th observation: Data Taking 8(= LIGO S2)

LIGO-TAMA joint observation for 2 months
Detector development for DT8
Operational status

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)
WestEndRoom

CenterRoomSouthEnd
Room
Middle of a city area ~ heavy traffic

TAMA300 detector ~ overview

300m
FP armRecycling
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
Mechanical quality
Intrinsic Q ~ 3x106

Optical quality
substrate absorption
3ppm/cm
total loss in reflection
30ppm
figure error<λ/40
surfaceo roughness<1 A

Control electronics

Control electronics

o Analog servo circuits for the most systemso Digital control/switching capabilityof the analog circuits for automatic locko Several digital servos

Data Acquisition SystemEPICS80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 - PresentOne 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 - 00/600/9 - 01/9

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

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 LIGO & GEO

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

Overview of this talkl Introduction of TAMA300

a 300-m Fabry-Perot Michelson interferometer8 observations in past

6th observation: Data Taking 6Fl The
The observation for 50 days in the summber of 2001
Analyses of the 1038-hours datal The 8th observation: Data Taking 8(= LIGO S2)

LIGO-TAMA joint observation for 2 months
Detector development for DT8
Operational status

Interferometer on DT6l DT6 ~ 50 days run (2001/8/1~9/20)
w IFO configuration: Fabry-Perot Michelson (w/o power recycling)
w Enough sensitivity to detect Galactic merger events
Enough stability for long term operation~ high duty ratio, auto lock-acquisition

Total lock time1107 h(92.3%)

Total obs. data (excl. after-lock adj.)
1038 h(86.5%)

w Coincidence with LISM 20m IFO
at Kamioka mine
Lock overlapping

709 h

300m
FP cavity(59.1%)

300m
FP cavity

Laser
10m
Mode Cleaner

Fabry-PerotMichelsonInterferometerSensitivity of IFO at DT6l Displacement noise dx = 1.5 x 10-18 m/Hz1/2 (@700Hz)
Strain sensitivity
h = dx/300= 5x10-21 /Hz1/2-11

Binary Range:
33kpc

10-1210-13

1/2

Strain sensitivity [1/Hz ]10-1410(Distance toobserve
NS inspirals
with SNR=10)

June. 2, 2001
Phase I goal

-15

10-16

10-17

10-18

10-19

10-20

10-21

10-22

10

11010

2

310

Frequency [Hz]

410

510

DT6 data analysis
l Binary inspiral search
Matched filtering search (1~2Msolar)
Coincidence analysis
between TAMA and LISM20m (1~2Msolar)l Burst search
Non-Gaussianity detection using higher-order stat.

l Periodic GW search
Possible GW wave from SN1987a (@~935Hz)GW search: compact binary inspiralsl Matched filtering analysis
Upper limit to the galactic event rate:
Revent [/h]Revent [/y]Dobs

Tobs/h=5.2x103/year

3.4kpc31h

DT4: 0.027 /h=2.4x102/year

17.9kpc

167h

DT6: 0.0095/h=8.3x101/year

33.1kpc 1038h

DT2: 0.59

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 signalFρ ≡ ( s, h ) G z
HS (f)

IJK

ρ3 ρ 4 ρ5Lf3

f5 L=2

ρ1

ρ2f1

fmin

f2~s~ ( f ) h ( f )
*dfn

f41
χ ≡ ∑ 2 ( ρ i − ρ i )2σi2

σ i 2 ≡ ( ρ i − ρ i )2 ,

ρi = ρifmax

Performance of ρ / χ selection
2

reehe
ars
la
gnists
TeSimple χ selection willproduce loss of strong
S/N events
2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%)TεLocation of TAMA and LISM

TAMA
LISM

orientation
225°
165°

latitude35.68°N
36.25°N

longitude
139.54°E
137.18°E• Distance between TAMA and LISM 〜 220km• Maximum delay of signal arrival time〜0.73msec• Relation between TAMA and LISM arms direction

Kamioka (LCGT, CLIO site)
220km west from Tokyo

Kamioka

220km
Tokyo (NAOJ)

Results of coincident event search
Results of onestep search for common lock parts
TAMA
158437 events
After t c -coincidence
70 events
After tc , M ,η -coincidence
18 events
After tc , M ,η, ρ -coincidence
13 events

LISM
142465 eventsResults of coincident event search
Results of onestep search for common lock parts
TAMA
158437 events

LISM
142465 events

After t c -coincidence
70 events

accidental coincidence ( nacc ± σ c )70.45 ±8.53

After tc , M ,η -coincidence
18 events

accidental coincidence ( nacc ± σ c )17.55 ± 4.08

After tc , M ,η, ρ -coincidence
13 event

accidental coincidence ( nacc ± σ c )12.76 ±3.51

Coincident event search upper limit (4)From above figure, we set threshold for each detector,
2
TAMA threshold : ρ tam a / χ tam a = 6.2
2
LISM threshold : ρ lism / χ lism
= 5 .3Observed number of events over threshold: Nobs=0
Expected number of fake events over threshold：Nbg=0.72
We can obtain the average number of events over threshold N=2.3 (C.L.=90%)• The second, we evaluated detection efficiency ε
we performed a Galactic event simulation (within 1kpc) .
Setting above thresholds, we can obtain the probability that we observe events overthe each detector’s threshold (namely detection efficiency)
ε= 0.22• Length of data : T=244 hours
TAMA + LISM case
Upper limit to the Galactic (within 1kpc) event rate :N/Tε= 0.042 events/hour (C.L. 90%)

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 (4)--- DT6 data analysis --Data Taking 6 (Summer 2001)
Bandwidth : 500Hz
Rejected data : 10%(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

1010–210

1–3101010–4

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 Target: possible SN1987a remnant(Middleditch, et al. New Astronomy, 5 (2000) 243)o 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: 2~3x10-10 [Hz/s])o Search result: DT6 50days data
Time-domain search:

h=3.8x10-23(False Alarm:1.8%)

Frequency domain search:

h=4.1x10-23(False Alarm:1.8%)(hupperlimit from the spindown:h=9.4x10-27)

Overview of this talkl Introduction of TAMA300

a 300-m Fabry-Perot Michelson interferometer8 observations in pastl The 6th observation: Data Taking 6

The observation for 50 days in the summber of 2001
Analyses of the 1038-hours data

Fl The 8th observation: Data Taking 8(= LIGO S2)

LIGO-TAMA joint observation for 2 months
Detector development for DT8
Operational status

Data Taking 8 (LIGO S2)
l DT8 ~ 2 months run (2003/2/14~4/15)
First full-time joint observation with LIGO S2(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

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

no light

Total dissipated power= Incident power
RecyclingMirror

Highreflectance“Dark port”
no light

Pinc = εloss Pinternal

Pinc
Pinternal =εloss

no light

g PincDT8 ~ IFO developmentl Fitting the IFO for DT8Sensitivity>> Improvement of the detection noise/shot noise levelby power recycling>> Reduction of the frequency noise
Stability>> Automatic lock system>> Automatic alignment control for 4 test masses,recycling mirror, and the mode cleaner mirrors>> Optical axis control

Automatic lock acquisition
Self-switching sub-systems (Laser&MC)
MC frequency stabilization
MC alignment control
Laser intensity stabilization
Optical axis control
Injection lock servo of the laser
Digital switching using PC and Labview
Lock acquisition
Manual mirror alignment
IFO Status monitoring
Hardware: PC + DAQ board
Software: National Instruments LabVIEWJPS Conference Spring 03 @ Tohoku Gakuin Univ.

Optical Config. and control systeml Length control for lock acq.
l Alignment control for test massl High S/N length control
10m MCEOMs
15.235 11.97
MHz MHz300m IFO

6W

Faraday Rotator

Inj. lock
Nd:YAGlaser(8.6W)

3rd
harmonicdemod.

δL−δL1
Pickoff
Signals

LOCKO p t ic a l C o n f ig . a n dc o n t r o l s y s t e ml Lengt
hcont
r
olf
orl
ockacq.
l Alignmentcont
r
olf
ort
estmassl HighS/
Nlengthcont
rol
10m MC

EOMs
15.
235 11.
97
MHz MHz

Inj.lock
Nd:
YAG
laser
(8.
6W )

300m IFO

6W

Far
adayRotator

δl+ fx3
δl− fx3

3 r dh a r m o n ic
d e m o d .
LOCKδL−δL1
P ic k o f f
S ig n a ls

LOCK

O p t ic a l C o n f ig . a n dc o n t r o l s y s t e ml Lengt
hcont
r
olf
orl
ockacq.
l Alignmentcont
r
olf
ort
estmassl HighS/
Nlengthcont
rol
10m MCEOMs
15.
235 11.
97
MHz MHzInj.lock
Nd:
YAG
laser
(8.
6W )

A lig n m e n t
C o n t r o l
QPDs

Gouyphasetelescopes

300m IFO

6W

Far
adayRot
ator

OPR
QPDs

Gouy
phasetelescopes

P ic k o f f
S ig n a ls

A lig n m e n t
C o n t r o l

O p t ic a l C o n f ig . a n dc o n t r o l s y s t e ml Lengt
hcont
r
olf
orl
ockacq.
l Alignmentcont
r
olf
ort
estmassl HighS/
Nlengthcont
rol
10m MC

EOMs
15.
235 11.
97
MHz MHzInj.lock
Nd:
YAG
laser
(8.
6W )

6W

Far
adayRotator

Alignment control
Alignment control servo for the recycling mirror
Mechanical modulation technique (Pitch 60Hz, Yaw 70Hz)
Suppress long-term drift => bandwidth < 1Hz=> All of the five mirrors are controlled
70Hz Lock in Amp2
Perpendicular Arm
Alignment Control

60Hz Lock in Amp1
Yaw Control

300-m Fabry-Perot-Michelson Interferometer

Pitch Control

QPD2

Injection-Locked
LD-pumped
Nd:YAG Laser

NSPD

EOM

15MHz

DBM2
15MHz

10-m Ring-type
Mode Clenaer

300-m FP cavity

QPD1
15MHz
DBM1

In-Line Arm
Alignment Control

Stabilizing optical axes
Control incident beam axis QPD42 QPDs / 2 PZT mirrors
on the injection table

M2
QPD2
M1

Control 300-m
optical axes
2 QPDs at both end
actuating BS
and injecting signal
to the incident axis servo
QPD3

QPD1BS+Laser=> Minimizing the alignment noise coupling to dL-.
=> Improvement of the long-term stability of the main IFO,
as well as the long-term stability of the MC.

Improved long-term stability
Longest lock stretch in the observations

Transmitted power [a.u.]54

DT8: 20h31m

32

DT7: 8h38m

1005

10Hour1520

Frequency Stabilization
Displacement noise level of TAMA300-1010-1110

With Power recycling-12

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

Displacement noise [m/Hz-1/2]

10-13Without Power recycling

10Frequency noise (2001/08/03)-1410-15

10-1610-1710-1810-1910-20

10-211011021031010410

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

5Frequency [Hz]

Sensitivty @ DT8
Displacement noise level of TAMA300(Feb, 20 2003)

-7

1/2

Displacement noise [m/Hz ]10

2003/02/20 (DT8: with recycling)
2001/08/03 (DT6: without recycling)
Phase2 limit-9

10-1110-1310-15

10-1710-1910010

Floor level:1102

31010Frequency [Hz]1/2

8x10-19 m/Hz
2.7x10-21 /Hz1/2

410510(in displacement)(in strain)Observable distance with SNR=10Observable Distance [kpc]80

2003/02/20 DT8
2001/08/03 DT6 4.3Msolor 64kpc

60
NS binary
1.4Msolar 33->42kpc
40Steller BH binary
10Msolor 34->15kpc

20Macho BH binary
0.5Msolor 14->20kpc

0-1

1023

4

5 6 7890102

3mass [Msolar]

45 6 7 891012

SNR improvement for 1.4-1.4Msolar and 0.5-0.5Msolar
Deterioration for 10-10Msolar caused by wideband alignment filters
JPS Conference Spring 03 @ Tohoku Gakuin Univ.

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

dx

LaserFrequency
Noisedxffrequency

GW
Signalportdxdxfff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 noiseLaser frequency noise-810-91/2

Displacement noise [m/Hz ]

10-10

10-11

10-12

10-13

10-14

10-15

10-16

10-17

10-18

10-19

10-20

10-21

100

10

1

102

103

10

Frequency [Hz]

410

510

Observation calendar
l 1157h51m (out of 1424 hours, duty cycle 81.3%)
Mon

TueWedThu

Date and Time in JST (UTC +9 hours)

FriFeb. 14, 2003

15

Sat

16

17

18

1920

21

22

23

24

25

26

27

28

Mar. 01

02

03

04

05

06

0708

09

10111213

14

15

16

1718

1920

21

22

23

24

25

26

27

28293031

Apr. 01

02

03

04

05

06

07

08

09

10

11

12

13

14

15

Sun

Duty cycle
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 C
W

DAQ
Trouble5

C C CCWWW

Circuit
Failure

1200

S
1000

C C CC

CC CW

Laser
TroubleC C

CCWCC C C CC C C C
Road
WW W
High Constructions
800
Sea
Waves
MC
Trouble4600PowerFailure

3400

2200
10 141516171819202122232425262728010203040506070809101112131415161718192021222324252627282930310102030405060708091011121314150FebMar

Apr

Total Obs. time [hours]

8Signal Injection
ExperimentDT8 ~ Disturbance by construction
11th May, 2003 (Tue)Observable
Distance [kpc]Seismic level[gal](Quiet weekday)

13rd May, 2003 (Thu)(Noisy weekday)

Duty cycle

Observabledistance [kpc]Daily trend of duty cycle/binary range
4030
20
1000

1.0
0.8
0.6
0.4
0.2
0.0

36

91215
Hour (JST)182124TAMA-LSC working groupl Concluded the MOU between TAMA and LSC
at GWDAW 2002 in Kyoto

Discussionsfor the joint data analysis
are now underway!
WG members- Masaki Ando (University of Tokyo)- Patrick Brady (University of Wisconsin-Milwaukee)- Sam Finn (Pennsylvania State University)- Nobuyuki Kanda (Osaka City University)- Erik Katsavounidis (MIT)- Albert Lazzarini (Caltech)- Hideyuki Tagoshi (Osaka University)- Ryutaro Takahashi (National Astronomical Observatory of Japan)- Daisuke Tatsumi (National Astronomical Observatory of Japan)- Peter Saulson (Syracuse University)

The photograph excerpted
from LIGO News

Future Planl Data Analysis of the DT8 data
In progressl IFO: sufficient stability for long-term obs.
Concentrate on the noise issuesl Further automation of the observation
To operate the interferometer with lessnumbers of the interferometer expertson the observations
Ultimately toward a contiunuous observation

Summaryl Interferometric GW detector TAMA300l Data Analysis using DT6 data
Binary ispirals: R_event<0.0095/hr
Burst search:
CW search:coincident search with LISM20m
Reduction of the IFO related noise
R_event<0.01/hr for hrms=3x10-17
Possible 1987A pulsar ~935Hz
h<4x10-23

l Data Taking 8
Full-time observation with LIGO S2Power recycling
Improvement of the sensitivity

h = 2.7 x 10-21 /sqrtHz @1.5kHz
1158 hours of 1424 hours => duty cycle 81.3%