ICRC2003 08/06/2003
description
Transcript of ICRC2003 08/06/2003
ICRC2003 08/06/2003
Current Status of TAMA300
Shuichi SatoNational Astronomical Observatory of Japan
for The TAMA collaboration
Contents
ICRC2003 08/06/2003
Overview of TAMA300 gravitational wave antenna
Detector siteIFO configuration
Current status of the detector
Power recyclingIFO control systemImproved IFO sensitivity
Site view
Aerial photograph of the TAMA site Aerial photograph of the TAMA site (NAOJ, Mitaka, Tokyo, JAPAN)(NAOJ, Mitaka, Tokyo, JAPAN)
300m
300m
Mitaka,Tokyo (NAOJ)
Mitaka campus of NAOJ, Tokyo (E 139.32.21 N 35.40.25)
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Center room
West end room
South end room
IFO Configuration
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Active air spring
Principle of Power Recycling
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Control scheme of Power Recycled FPMI
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Control scheme of Power Recycled FPMI
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Improved Sensitivity
Noise level of FPMI (Without power recycling)dx ~ 1.5 x 10-18 [m/Hz1/2 ] @ 1kHz
Dominant contribution in high frequency region Detector + Shot noiseFrequency noise
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10-20
10-19
10-18
10-17
10-16
10-15
10-14
10-13
10-12
10-11
10-10
Displacement noise [m/rHz]
101
102
103
104
105
Frequency [Hz]
2001/06/02 FPMI Phase2 theoretical limit Frequency noise (FPMI) Detector+Shot noise (FPMI)
Improved Sensitivity
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10-20
10-19
10-18
10-17
10-16
10-15
10-14
10-13
10-12
10-11
10-10
Displacement noise [m/rHz]
101
102
103
104
105
Frequency [Hz]
2001/06/02 FPMI Phase2 theoretical limit Frequency noise (FPMI) Frequency noise (PRFPMI) Detector+Shot noise (FPMI) Detector+Shot noise (PRFPMI)
Noise level of FPMI (Without power recycling)dx ~ 1.5 x 10-18 [m/Hz1/2 ] @ 1kHz
Dominant contribution in high frequency region Detector + Shot noiseFrequency noise
Improvements Incident power
enhancement byPower recycling
Highly stabilized laser frequency
Improved Sensitivity
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10-20
10-19
10-18
10-17
10-16
10-15
10-14
10-13
10-12
10-11
10-10
Displacement noise [m/rHz]
101
102
103
104
105
Frequency [Hz]
2001/06/02 FPMI 2003/7/12 Power recycled FPMI Phase2 theoretical limit
Noise level of FPMI (Without power recycling)dx ~ 1.5 x 10-18 [m/Hz1/2 ] @ 1kHz
Dominant contribution in high frequency region Detector + Shot noiseFrequency noise
Improvements Incident power
enhancement byPower recycling
Highly stabilized laser frequency
Noise level of PRFPMIdx ~ 8 x 10-19 [m/Hz1/2 ]
@ 1.5kHz
Expected Observable Distance for Binary Inspirals
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70
60
50
40
30
20
10
0
Observable Distance [kpc]
10-1
2 3 4 5 6 7 8 9
100
2 3 4 5 6 7 8 9
101
2
Member mass [Msol]
0.5Msolar - 21.4kpc
1.4Msolar - 46.6kpc
4.3Msolar - 66.0kpc
10Msolar - 35.0kpc
2001/06/02 (FPMI) 2003/07/12 (Power-recycled FPMI)
SNR=10, optimal incident angle are assumed
Noise budget (DT8)
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10-21
10-20
10-19
10-18
10-17
10-16
10-15
10-14
10-13
10-12
10-11
10-10
10-9
10-8
10-7
Displacement noise [m/rHz]
100
101
102
103
104
105
Frequency [Hz]
Displacement noise level of dL- Alignment noise Seismic noise dl- feedback noise dl+ feedback noise dL- filter noise Modulation noise Shot noise and detection system noise Shot noise (calculated) Detection system noise Laser intensity noise Laser frequency noise
Sensitivity History
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10-22
10-21
10-20
10-19
10-18
10-17
10-16
10-15
10-14
10-13
10-12
10-11
Strain sensitivity [1/rHz]
101
102
103
104
105
Frequency [Hz]
Feb. 14, 1999 Sept. 3, 1999 Oct. 15, 1999 March. 16, 2000 Sept. 4, 2000 June. 2, 2001 July 12, 2003 Phase2 limit
Summary
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Current status of TAMA300
Power recyclingOperating stablyAll mirrors are alignment-controlledRecycling gain : 4.5
Detector sensitivitydx~8 x10-19[m/rHz]@1.5kHzReaching practical shot noise limit
Future plan
Investigation of the noise issuesBetween 100Hz and 1kHz
Further automation for the observationTo operate the interferometer with less operators
Upgrade of the vibration isolation systemSeismic Attenuation System (SAS)For better stability and sensitivity