observation runs of tama300 gravitational wave detector

XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia)

Observation Runs of TAMA300 Gravitational Wave Detector

Masaki Ando Dept. of Physics, University of Tokyo

TAMA collaboration

Coalescence of a binary neutron stars

Illustration/ KAGAYA

XII-th International School on Particles and Cosmology (April 24, 2003, Baksan Valley, Russia) 2

Abstract

Japanese activities for GW detection

TAMA7 year project (April 1995 – March 2002)Construct a 300m interferometric detector : TAMA300

Several data taking runs from 1999Data analysis results

Next project : LCGT3km cryogenic interferometer at Kamioka mineResearch and development tasks

(April 2002 – March 2006)


Contents

Introduction

TAMA detector

Data taking runs with TAMA

Data analysis results

Recent results (Data Taking 8)

LCGTOverviewResearch and development tasks

Summary


Introduction (1)- Gravitational-wave astronomy -

Gravitational wave detectors

Bar detectors - network observation

Interferometric detector - finishing and starting observation

Future projects on the ground and in the space


Gravitational waves (Coalescences of compact binaries, Stellar core collapses)

　　 Change in distance between free masses (Strain about 10-18)

Introduction (2)- Detection method -

Gravitational WavesPrecise measurement

by a laser interferometer (Mirrors behave as free masses)

Michelson interferometer


Introduction (3)- Michelson interferometer -

Michelson interferometer

Detects optical-path difference caused by GWs

Long arm length for higher sensitivity


Introduction (4)- Interferometer configuration -

End mirror End mirror

Photo detector

Beamsplitter

Some mirrors are added

Sensitivity improvement

Power-recycledFabry-Perot-Michelson

interferometer(LIGO, VIRGO, TAMA)

Fabry-Perot cavityEffective arm length

Power recyclingEnhance power in the interferometer

Front mirrorFront mirror

Recycling mirror

Fabry-Perot cavity

Fabry-P

ero

t cavity

Laser source


TAMA project (1)- overview -

TAMA projectDetect gravitational waves

from local group of our galaxy

Research and development for a large-scale detector

Construct an interferometernamed TAMA300

Fabry-Perot-Michelson interferometer with 300m arms (with power recycling)

Target sensitivityh : 3x10-21

Aerial photograph of the TAMA site (NAOJ, Mitaka, Tokyo, JAPAN)

300m

300m


TAMA project (2) - Noise budget of TAMA300 -

Target sensitivity

101 102 103 104 10510–24

10–22

10–20

10–18

10–16

10–14

10–20

10–18

10–16

10–14

10–12

Str

ain

no

ise

[1

/Hz

1/2

]

Frequency [Hz]

Pendulum thermal noise

Phase I goal

Phase II goal

Dis

pla

cem

en

t no

ise

[m

/Hz

1/2

]

NS–NS

Super Novae

Seism

ic noise

Mirror thermal noise

Shot noise

Observation band

inspirals


TAMA project (3) - Photos -

Fused silica mirrorFused silica mirror

Mirror suspensionMirror suspension 300m vacuum duct300m vacuum duct

LaserLaser

RMRMMCMC BSBS

FM2FM2

FM1FM1

Center roomCenter room


Data taking runs (1)- Data taking runs with TAMA300 -

Data Taking ObjectiveObservation

timeTypical strain noise level

Total data(Longest lock)

DT1 August, 1999 Calibration test 1 night 3x10-19 /Hz 1/210 hours

(7.7 hours)

DT2 September, 1999 First Observation run 3 nights 3x10-20 /Hz 1/2 31 hours

DT3 April, 2000Observation with

improved sensitivity3 nights 1x10-20 /Hz 1/2 13 hours

DT4Aug.-Sept.,

2000100 hours'

observation data2 weeks

(night-time operation)1x10-20 /Hz 1/2

(typical)167 hours

(12.8 hours)

DT5 March, 2001100 hours' observation with high duty cycle

1 week(whole-day operation)

1.7x10-20 /Hz 1/2

(LF improvement)111 hours

DT6Aug.-Sept.,

20011000 hours' observatio

n 50 days 5x10-21 /Hz 1/21038 hours(22.0 hours)

DT7Aug.-Sept.,

2002Full operation with

Power recycling2 days 25 hours

DT8Feb.-April.,

20031000 hours

Coincidence2 months 3x10-21 /Hz 1/2

1157 hours(20.5 hours)


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 GalaxySNR of 30 for 1.4-1.4 Msolar inspiralsObservation : 1038 hours (86.5%)

Well-organized observationAutomatic lock of the detectorOnline monitor and diagnosis 65 shift participants (2 person / 8 hours’ shift)


Data taking runs (3)- Detector operation status in DT6 -

Operation status calendar Total observation : 1038 hours

Thu SunTueMon Fri SatWedAug. 01 03

08

Operated (over 10min) High–freq. data taking

Date in JST

15

22

29

05

12

191817

10

03

27

13

06 07

14

2120

28

04

11 13

06

30

23

16

09

02

10

17

24

31

07

14 15

08

Sep. 01

25

18

11

04 05

12

19

26

02

09

16

20

TyphoonLaser instabilityMeasurement+adjustmentHuman error


Data Analysis results (1)- TAMA data analysis -

GW searchBinary inspiral search

Two step searchBinary inspiral search using WaveletTAMA-LISM coincidence

Continuous wave from known pulsarBurst wave search

BH ringdown search, Stochastic background search, etc.

Detector characterization analysisCalibrationNoise veto analysisInterferometer diagnosis


Data Analysis results (2)- Binary inspiral search -

Binary inspiral event search Matched filtering

Prepare templates (predicted waveform)

Expected SNR for binary mergers

Distance: 10kpc (Galactic center)

DT6 noise spectrum

SNR : about 30 (1.4/1.4 Msolar binaries)


Data Analysis results (3) - Search results -

Matched filtering analysisDT6 1038 hours’ data1.0-2.0 Msolar events (200-1000 templates)2 event selection

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%) 10-6 events/year (prediction)

)16/( 2


Data taking 8 (1)-Data taking runs with TAMA300 -

Data Taking ObjectiveObservation

timeTypical strain noise level

Total data(Longest lock)

DT1 August, 1999 Calibration test 1 night 3x10-19 /Hz 1/210 hours

(7.7 hours)

DT2 September, 1999 First Observation run 3 nights 3x10-20 /Hz 1/2 31 hours

DT3 April, 2000Observation with

improved sensitivity3 nights 1x10-20 /Hz 1/2 13 hours

DT4Aug.-Sept.,

2000100 hours'

observation data2 weeks

(night-time operation)1x10-20 /Hz 1/2

(typical)167 hours

(12.8 hours)

DT5 March, 2001100 hours' observation with high duty cycle

1 week(whole-day operation)

1.7x10-20 /Hz 1/2

(LF improvement)111 hours

DT6Aug.-Sept.,

20011000 hours' observatio

n 50 days 5x10-21 /Hz 1/21038 hours(22.0 hours)

DT7Aug.-Sept.,

2002Full operation with

Power recycling2 days 25 hours

DT8Feb.-April.,

20031000 hours

Coincidence2 months 3x10-21 /Hz ½

1157 hours(20.5 hours)


Data taking 8 (2)- DT8 observation summary -

TAMA data taking 8 (DT8)2 month’ observation (February 14 – April 15, 2003)Full configuration (with power recycling)

Sufficient sensitivity and stability for GW events in our GalaxySNR of 40 for 1.4-1.4 Msolar inspirals Observation : 1157 hours (81.3%)

94 shift participant

Coincidence runLIGO (4km detector x2, 2km detector)


Data taking 8 (3)- Detector operation status in DT8 -

Operation status calendar Total operation : 1157 hours

Thu SunTueMon Fri SatWed

Apr. 01 03

08

Observation (continuous over 10min)

Date and Time in JST (UTC +9 hours) 15

22

05

12

191817

10

03

27

13

06

07

Feb. 14, 2003

2120

28

04

11 13

06

23

16

09

02

10

17

24

07

14 15

08

Mar. 0125

18

11

04 05

12

19

26 02

09

16

20 2221 23

27 2824 2925 26 30

31

14 15


Data taking 8 (4)- Sensitivity in DT8 -

Sensitivity for binary inspiral events

Better than DT6Longer obs. Time

Better results

Coincidence Analysis withother detectors


LCGT project (1)- Overview -

For gravitational wave astronomy Higher sensitivity (seeing further away)

More than a few events in a year

100 101 102 103 104

10-19

10-20

10-21

10-22

10-23

10-24

10-25

Frequency [Hz]

Str

ain

sen

sit

ivit

y　

[1/H

z1/2]

Illustration / S.Miyoki

LCGT project SNR : 10

for 230Mpc events

(NS-NS inspiral)


LCGT project (2) - LCGT parameters -

LCGTBaseline length : 3kmSite: Kamioka mineCryogenic interferometer

Laser : 100W50kg Sapphire mirror

(20K, Q=108)Broadband RSESeismic isolator :

SAS (300K) Cryogenic SUS

(10K, Q=2x108) Suspension point

interferometer


LCGT project (3) - CLIO100 -

CLIO100 : LCGT prototype at Kamioka mine100m cryogenic interferometerR&D for …

MirrorSuspensionCryogenics

Tunnel digging finished (July 2002)

Installing IFO for geo-phys


LCGT project (4) - Site for CLIO100 -

SuperKamiokande

CLIO100

Entrance


Summary

TAMA300Data taking runs

8 data taking runs (August 1999- ), over 2000 hours of data

Data analysisUpper limit for Galactic binary inspirals : 0.0095 /hourCoincidence analysis, burst wave, continuous wave

Data taking 8 : February 14 - April 15, 2003 just finished

Better results will be obtainedCollaboration with other detectors

For LCGTR&D tasks --- TAMA300 and CLIO100Design document


Introduction (2)- Gravitational-wave astronomy -

Gravitational waves (Ripples of space time)

Gravitational-wave astronomy

New window for astronomy and cosmology

A.Einstein

Predicted by General Relativity --- Strain of space-time which propagates at the speed of the light

(A.Einstein, 1916) Existence was proved by observation of a binary pulsar (J.H.Taylor, et.al, 1979) Generated by acceraration of masses ( Electro-Magnetic waves ： acceraration of charges) High transmissivity (Small cross section with matters) 　

Ac

cu

mu

late

d s

hif

t　

[s]

Time 　 [year]


TAMA project (1) - Optical and control configuration -


TAMA project (1) - Data acquisition and analysis -


TAMA project (1) - Basic design of TAMA300 -

Main interferometer

Fabry-Perot-Michelson with power recyclingArm cavity length : 300m

Finesse of arm cavities : 516

Light source LD-pumped Nd:YAG laserOutput power :Wavelength :

10W1064 nm

Mode cleaner Triangle ring cavityBaseline length :Finesse :

9.75m1700

Vibration isolation

Three-stage stack + Double pendulum+ Active isolation systemVibration isolation ratio : < -165 dB

Data acquisition 16 bit, 20 kHz sample, 8 channels, 160 low-freqency channels

Vacuum system < 10-6 Pa


Data Analysis results (3)--- Burst wave search ---

Burst GW event search (M.Ando, et.al. ）Poorly predicted waveform

Cannot use matched-filtering schemeMasked with non-Gaussian noises

Excess power detectionTime-scale selection

10–20 10–19 10–1810–6

10–5

10–4

10–3

10–2

10–1

100

10–3

10–2

10–1

100

101

102

103

Ra

tio

[

co

un

t/to

tal

nu

mb

er]

Strain PSD [1/Hz1/2]

DT6 total

After noise reduction

Ev

en

t R

ate

[

ev

en

ts/h

ou

r]

Gaussianity

Exc

ess

po

wer

Reject non-Gaussian noisewithout rejecting GW candidates

Event rate : 10-2 /hour (1.2x10-20 /Hz)


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.)


Data taking 8 (4)- Noise level at DT8 -


TAMA current status (1)--- Improvements after DT6 ---

Power recycling (TAMA Phase II)Mirror installation : November, 2001First lock : Dec. 24, 2001Harmonic demodulation for RM control

Longest lock : 4 hoursRecycling gain : 4

(Low gain configuration)

Improved noise level Shot noiseDetector noise levelScattered light noiseFrequency stabilization

(K.Arai, R.Takahashi S.Sato, et.al.)


TAMA current status (2)--- Current noise level ---

Latest noise levelImproved with power recycling (and the other efforts)

h : 4x10-21 /Hz1/2 around 1kHz

DT7 (Aug.31-Sept.1)

101

102

103

104

10510

–22

10–20

10–18

10–16

10–14

10–12

Str

ain

no

ise

[

1/H

z1/2]

Frequency [Hz]

Current sensitivity

June 02, 2001

Phase II goal

August 05, 2002

Improvementfactor of 3


Data taking runs (1)--- Noise level at DT6 ---

DT6 noise level h : 5x10-21 /Hz1/2

at 1kHz

Noise sources are identified

Alignment control noise Michelson phase noise Detector noise Shot noise etc.

(K.Arai, R.Takahashi, et.al.)


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)

LISM20m detector at Kamioka mineLocked 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)


Data taking 8 (5)- Stability of sensitivity in DT8 -

Sensitivity distribution

observation runs of tama300 gravitational wave detector

Documents

baksan valley

russiatama project

tama300several data

interferometer configuration

noise budget of tama300

gw detectiontama7 year

tama site naoj

observation run3 nights3x10