Observation runsof
an interferometric gravitational
wave detector TAMA300
National Astronomical Observatory of Japan
Koji Arai (TAMA project)

MG10 Plenary

Overview of this talkl Introduction of TAMA300

a 300-m Fabry-Perot Michelson interferometer8 observations since 1999l Long-term observations: Data Taking 6 & 8
DT6: 50 days' observation in the summer of 2001
DT8: 59 days’ observation in the winter-spring of 2003
(LIGO-TAMA joint observation)l TAMA Data Analysis

Results with DT6 data
Preliminary result of NS inspiral search with DT8 datal Future Plans

LCGT: 3km cryogenic interferometer in a mineOverview of this talkof TAMA300
F l Introduction
a 300-m Fabry-Perot Michelson interferometer8 observations since 1999l Long-term observations: Data Taking 6 & 8
DT6: 50 days' observation in the summer of 2001
DT8: 59 days’ observation in the winter-spring of 2003
(LIGO-TAMA joint observation)l TAMA Data Analysis

Results with DT6 data
Preliminary result of NS inspiral search with DT8 datal Future Plans

LCGT: 3km cryogenic interferometer in a mine

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)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TAMA300 detector overview
Aerial view

West EndRoom

Light source
Center room

CenterRoom

300-m tubes
Vibration
isolation
Mirrors
Controlelectronics

South EndRoom

National Astronimical Observatory of Japan(Tokyo, Mitaka Campus (E139.32.21 N35.40.25)

Middle of the city area ~ convenient for detector development~ heavy traffic

TAMA300 detector overview
Aerial view
Light source

Master Laser

Center room
300-m tubes
Vibration
isolation
Mirrors
Controlelectronics
Injection locked Nd:YAG laser
λ=1064nm, Output of 10W
Pre-stabilized by 10-m mode cleaner

Slave cavity

TAMA300 detector overview
Aerial viewLight source
Center room

Beamsplitter
Chamber

Front Mirror
Chamber

300-m tubes
Vibration
isolation
Mirrors
Controlelectronics

Detection port

Beamsplitter~ divides the incident beams into two beams~ recombines the two reflected beams

Photodetectors receive recombined beam at the detection port

TAMA300 detector overview
Aerial view
Light source
Center room
300-m tubes
Vibration
isolation
Mirrors
Controlelectronics
300-m arms:
Electro-Chemical Polishing of internal surface~ realizes vacuum pressure of 10-8 Pa without baking

TAMA300 detector overview
Aerial view
Light source
Center room300-m tubes
Vibration
isolation
Mirrors
Controlelectronics
3-layer system:

Active air spring + Stack + Double pendulum suspension

Achieved performance~ better than 10-8 at 150Hz

TAMA300 detector overview
Aerial view
Light source
Center room
300-m tubes
Vibration
isolation
Mirrors
Controlelectronics
Fused Silica φ100mm x 60mm, m=1kg
Polished / Dielectric coating

TAMA300 detector overview
Aerial view
Light source
Center room
300-m tubes
Vibration
isolation
Mirrors
Controlelectronics
Analog control circuitswith capability of digital switching for automatic operation

Overview of this talkl Introduction of TAMA300

a 300-m Fabry-Perot Michelson interferometer8 observations since 1999

observations: Data Taking 6 & 8
F l Long-term
DT6: 50 days' observation in the summer of 2001
DT8: 59 days’ observation in the winter-spring of 2003
(LIGO-TAMA joint observation)l TAMA Data Analysis

Results with DT6 data
Preliminary result of NS inspiral search with DT8 datal Future Plans

LCGT: 3km cryogenic interferometer in a mine

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

Interferometer on Data Taking 6l 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 NS merger events
Enough stability for long-term operation
Best sensitivity:
5x10-21 [/Hz1/2]
Accumulated data: 1038 hours
Duty Cycle:
86.5%
Longest lock:22 hours
w Coincidence with LISM 20m IFO
at Kamioka mine
Lock overlapping

300m
FP cavity
300m
FP cavity

Laser

709 h (59.1%)

10m
ModeCleaner

Fabry-Perot
Michelson
Interferometer

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

(Called S2 in LIGO)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:

PowerRecycling
mirror300m arm

1158 hours

Duty cycle:

81.3 %

Longest lock:20.5 hours

300m arm

Laser

Principle of power recyclingl Laser light is enclosed in the interferometerHighreflectance“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 Pincεloss(GTAMA=4.5)

Sensitivty in DT6 & DT8
Strain sensitivity of TAMA300(Feb, 20 2003)-1210-13

10DT8 with power recycling
DT6 without power recycling

1/2

Strain sensitivity [1/Hz ]

-14

10-15

10-16

10-17

10-18

10-19

10-20

10-21

10

1

102

103

10
Frequency [Hz]410510Sensitivty in DT6 & DT8
Strain sensitivity of TAMA300(Feb, 20 2003)

-12

10-13

10

DT8 with power recycling
DT6 without power recycling

1/2

Strain sensitivity [1/Hz ]

-14

10-15

10

Noise frommirror alignment
control-1610-1710Power increase
by recycling-1810-1910-20

10-2110110210310
Frequency [Hz]410Floor level: DT6 5 x10-21 /Hz1/2
DT8 2.7x10-21 /Hz1/2

510

Displacement noise level of TAMA300 (May 21, 2003)-710

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 ]10-1010-11

10-12

10-13

10-14

10-15

10-16

10-17

10-18

10-19

10-20

10-21

100

101102103

10

Frequency [Hz]410510History of the sensitivity
l Improvement by a factor of 103 ~ 104~ operation since 1999
Strain sensitivity of TAMA300

-11

10

Feb. 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

10-2210110102310Frequency [Hz]410510Observable distance
Distance for an optimally oriented m+m system,
to yield SNR=10DT6DT8
m=0.5
m=1.4
m=10

(Macho BH):
(NS):(BH):

Observable Distance [kpc]80

14 kpc33 kpc34 kpc20 kpc42 kpc15 kpc2003/02/20 DT8
2001/08/03 DT660
40
20010 -1

2

3

5

7

100

2

3572

10 1 mass [Msolar]

Duty cyclel DT6: 1038h07m (out of 1200 hours, duty cycle 86.5%)
l DT8: 1157h51m (out of 1424 hours, duty cycle 81.3%)Observation Calendar for DT8
Mon

TueWedThu

Date and Time in JST (UTC +9 hours)

FriSatSun

Feb. 14, 2003

15

161718

1920

21

22

23

24

25

26

27

28

Mar. 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

Apr. 01

02

03

04

05

06

07

08

09

10

11

12

13

14

15

DT8: Disturbance by construction

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

13rd May, 2003 (Thu)(Noisy weekday)
30
25
2015
1050

Construction works
near the siteOverview of this talkl Introduction of TAMA300

a 300-m Fabry-Perot Michelson interferometer8 observations since 1999l Long-term observations: Data Taking 6 & 8
DT6: 50 days' observation in the summer of 2001
DT8: 59 days’ observation in the winter-spring of 2003
(LIGO-TAMA joint observation)

Data Analysis
F l TAMA
Results with DT6 dataPreliminary result of NS inspiral search with DT8 datal Future Plans

LCGT: 3km cryogenic interferometer in a mine

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 possible GW from SN1987a remnant

NS ispirals: Matched Filtering

signall 2.5PN templatetimeselected!

chirp templatesl Each data segment has two outputs
ρ:signal amplitude ~ correlation with the template
χ2:deviation of the signal from the selected template

Event distrib. / detection efficiency

ρ/(χ2)1/2=12.5210alsngisest

Tdetection efficiency
ε = 0.61

10 20 30 40 50 60 70 80 90 100

Signal amplitude ρLog10(number of events)

3events

4

TAMA DT8 results

8TAMADeviation from the template

5TAMA events and Galactic event
7

Fitting range

65Threshold

4r / c 2 =12.5

32
1
0
3

4

5

6

7

8

9 10 11 12 13 14 15Set "False Alam rate"
to 0.8 event/yearUpper limit to the Galactic NS mergerl Observation time
Tobs = 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

DT6: TAMA-LISM20m coincidence runl Location of TAMA and LISM20m prototype• Distance between TAMA and LISM 〜 220km=> Max delay of signal arrival time = 0.73msec• Sensitivity h = 8 x 10-20 /Hz1/2• Analyzed 244 hours of commonly-locked data
• Relation between TAMA and LISM arms direction
TAMA
LISM

orientation
225°
165°

latitude35.68°N
36.25°N

longitude
139.54°E
137.18°E

Kamioka

220km
Tokyo (NAOJ)

Results of coincident event search
Results of onestep search for common lock partsTAMA
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 events

accidental coincidence ( nacc ± σ c )12.76 ±3.51

Burst GW analysis
l Distinguish burst signals with a certain time-scaleusing higher-order statistics
The detector output:
Full of bursts ~ essentially indistingushable from GWs=> assume time-scale of the GW bursts(c.f. Supernova)
Two statistics of each data segment:
Averaged noise power:
Averaged noise level2nd-order moment of noise power: Gaussianity
Bursts with different time-scale have different behavioursin terms of those two statistics=> Select bursts only with target time-scaleBurst GW analysis
l Analysis of DT6 data
Rejected 10% of data by the time-scale filter=> Improvement offalse event rate 1/1000(False dismissal rate = 1ppm)

Event rate for 10msec GWs

hrms:~ 3x10-17 : 4 ev/hr

310–1

102

10

Original data

–2

10

1–3

10

10
10

1/1000

–4–1

10–5

100

After noise rejection 10–2

10Gaussian noise

10–20

10–19
1/2

Noise level [1/Hz ]10–18

Event Rate [events/hour]~ 3x10-17 : 10-2 ev/hr
Event rate for 1msec GWs

010
Event Rate [Ratio]hrms:~ 1x10-17 : 1 ev/hr

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
Upper limit:

h=5x10-23(hupperlimit from the spindown:

h=9.4x10-27)(C.L. 99%)

Overview of this talkl Introduction of TAMA300

a 300-m Fabry-Perot Michelson interferometer8 observations since 1999l Long-term observations: Data Taking 6 & 8
DT6: 50 days' observation in the summer of 2001
DT8: 59 days’ observation in the winter-spring of 2003
(LIGO-TAMA joint observation)l TAMA Data Analysis

Results with DT6 data
Preliminary result of NS inspiral search with DT8 dataPlans
F l Future
LCGT: 3km cryogenic interferometer in a mineLCGT: Japanese future projectl Large-scale Cryogenic
Gravitational wave Telescope
3-km interferometer at Kamioka mine
Cryogenic (~20K) mirror to reduce thermal noiseDesign sensitivity of LCGTLCGT noise budget
Power in the arms
Signal bandwidth–18

Noise level [1/Hz1/2]

10800 kW200 HzTAMA
theoreticallimit

–20

10–22

10–24

10010

10

1210
Frequency [Hz]103410Sensitivity of LCGT will be quantum-noise limited
LCGT will be capable of detecting
NS binary inspiral at 200Mpc with SNR of 10

CLIO: Cryogenic laser interferometer Observatory
100-m cryogenic interferometer detector in Kamioka
Pilot program to demonstrate feasibility of LCGT technologies
The constructionis underway

KLIS:
Kamioka Laser
InterferometricStrainmeter~ for geophysical purposes

Summaryl Interferometric GW detector TAMA300
A 300-m Fabry-Perot Michelson interferometer8 observations from 1999 to 2003l Long-term (>1000h) observation DT6 / DT8
DT6:

h= 5 x10-21/sqrtHz
1038h => duty cycle 86.5%

DT8:First long-term operation with power recycling
Full-time joint observation with LIGO
h=2.7x10-21/sqrtHz
1158h => duty cycle 81.3%

Summaryl Data Analysis using DT6 / DT8 data
>NS ispirals: Galactic event rate
DT6 R < 0.0095 event/hr (C.L.90%) for 1<m<2Msolar
DT8 R < 0.0033 event/hr (C.L.90%) for 1<m<3Msolar>Coincidence analysis between multiple detectors
TAMA300 & LISM (20m)>Burst search
Rejection of non-gaussian noise by time-scale selection
R = 0.01 event/hr for hrms>3x10-17 (10ms pulse)>Continuous wave from possible SN1987a remnant
h < 5 x 10-23 (C.L. 90%)l LCGT: Large-scale Cryogenic
Gravitational wave Telescope