observation run of tama gw detector

Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA)

Observation run of TAMA GW detector

Masaki AndoDepartment of Science, University of Tokyo

and the TAMA Collaboration

Astronomical Telescopes and Instrumentation (August 25, 2002, Hawaii USA) 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 1999Operation with final configurationData analysis results

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

(April 2002 – March 2006)


Contents

TAMAOverviewData taking runsData analysis resultsCurrent status

LCGTOverviewResearch and development tasks


TAMA project (1)--- Targets of TAMA ---

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

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)--- 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


TAMA project (4)--- Photos ---

Fused silica mirrorFused silica mirror

Mirror suspensionMirror suspension 300m vacuum duct300m vacuum duct

LaserLaser

RMRMMCMC BSBS

FM2FM2

FM1FM1

Center roomCenter room


TAMA project (5)--- Optical and control configuration ---


TAMA project (6)--- Data acquisition and analysis ---


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 1/2

10 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, 2001

100 hours' observation

with high duty cycle

1 week(whole-day operati

on)

1.7x10-20 /Hz 1/2

(LF improvement)

111 hours

(TR1) June, 2001 2 days (24.8 hours)

DT6Aug.-Sept.,

20011000 hours' observa

tion 50 days 5x10-21 /Hz 1/21038 hours(22.0 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 inspiralsOperation : 1107 hours (92.3%) , longest cont. operation : 22 hours Observation : 1038 hours (86.5%)

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

Coincidence runLISM (20m detector at Kamioka mine)

Simultaneous operation : 709 hours


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

Operation status calendar Total operation : 1107 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 taking runs (4)--- 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 (1)--- TAMA data analysis ---

GW event searchBinary inspiral search

One step search (H.Tagoshi, D.Tatsumi, H.Takahashi)

Two step search (H.Tagoshi, T.Tanaka)

Binary inspiral search using Wavelet (N.Kanda)

TAMA-LISM coincidence (H.Takahashi, H.Tagoshi, D.Tatsumi,…)

Continuous wave from known pulsar (K.Soida, M.Ando,…)

Burst wave search (M.Ando,…)

BH ringdown search, Stochastic background search, etc.

Detecor characterization analysisCalibration (D.Tatsumi, S.Telada,…)

Noise veto analysis (Y.Watanabe, N.Kanda,…)

Interferometer diagnosis (M.Ando,…)


Data Analysis results (2)--- Inspiral search ---

Binary inspiral event search (H.Tagoshi, D.Tatsumi, N.Kanda, H.Takahashi, T.Tanaka, M.Sasaki)

Expected SNR for binary mergers

Distance: 10kpc (Galactic center)

DT6 noise spectrum

SNR : about 30 (1.4/1.4 Msolar binaries)


--- Inspiral search (contd.) ---

Matched filtering analysis (paper in preparation)DT6 1038 hours’ data1.0-2.0 Msolar events (200-1000 templates)c2 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%)

)16/( 2


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 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)


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


Current and future tasks--- LCGT project ---

TAMA project 7years’ project (April 1995 – March 2002)

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


Current and future tasks--- Status ---

Research and development for LCGTObservation runs with TAMA detectorDevelopment of cryogenic techniques

100m cryogenic interferometer : CLIOSeismic isolation system : SASThermal noise investigationResonant sideband extraction, Suspension point interferometer

Design document will be finished in this year

DECIGO (Interferometer in space)Working group


R&D tasks (1)--- CLIO100 ---

CLIO100 : 100m cryogenic interferometerDevelopment and test of …

MirrorSuspensionCryogenics

Tunnel digging finished (July 2002)

(S.Miyoki, M.Ohashi, et. al.)


R&D tasks (2)--- TAMA SAS ---

TAMA SASLow-freq. seismic attenuation system

To be installed in TAMA300Pre-isolator of LCGT

Full Scale Prototype TestTwo Test Towers

For a 3m Prototype InterferometerEstablished Local ControlCharacterization of

Attenuation PerformanceIntroducing New Control Method

Commissioning a Fabry-Perot Cavity2 SAS Prototypes CompletedAcquired lock of the cavity

(A.Takamori, et. al.)


　--- TAMA SAS (contd.) ---



　--- TAMA SAS (contd.) ---

10-14

10-13

10-12

10-11

10-10

10-9

10-8

10-7

10-6

10-5

10-4

Dis

plac

emen

t [m

/Hz1/

2 ]

0.01 0.1 1 10 100

Frequency [Hz]

Alignment Noise

Cavity Motion Ground Motion DAC Noise Frequency Noise (Free Run) Estimated FP displacement



R&D tasks (3)--- Direct measurement of TN ---

Reference CavityRigid cavity (suspended)Frequency stabilization

Length : 11cmFinesse : 19000

Test CavityDisplacement sensorIndependent mirror

Length : 1cmFinesse　 : 500Spot size : 50um

Material : BK7

(K.Numata, et. al.)


--- contd. ---

Approaching TN…or looking at TN

Unidentified noise : f-1/2

10-16m/rtHz@~100Hz~TAMACould be updated by

Low noise driverStack

Future worksAlignment

Shot noiseNew mirror

CaF2/Sapphire/Silica…Differential measurement

Frequency/seismic noiseElectric noise

Ground loopLow noise filter

10-18

10-17

10-16

10-15

10-14

10-13

10-12

10-11

10-10

10-9

10-8

10-7

Se

ns

itiv

ity

[m/r

tHz]

100

101

102

103

104

105

Frequency[Hz]

Sensitivity (02/06/29) Sensitivity(W/O stabilization)

Total Brownian Thermoelastic

Frequency noise(Stabilized) Frequency noise(Freerun) Demodulation system noise Servo system noise Driver noise

Seismic noise(W/ z-coupling)

(K.Numata, et. al.)


Summary

TAMA300Data taking runs

6 data taking runs (August 1999- ), over 1000 hours of data Data analysis

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

Data taking 7 : August 31 - September 1Detector updates

Power recyclingRecycling gain : 4Longest cont. lock : 4 hours

(over 24 hours without power recycling) Improved sensitivity : h : 4x10-21 /Hz1/2

For LCGTR&D tasksDesign document in this year

observation run of tama gw detector

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