status of the japanese projects kazuaki kuroda tama/clio/lcgt collaboration icrr, university of...
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Status of the Japanese Projects
Kazuaki Kuroda
TAMA/CLIO/LCGT Collaboration
ICRR, University of Tokyo
LSC-Virgo Meeting26 July, 2007G070574-00-R
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Status of TAMA
Present representative of TAMA is Emeritus Prof. Yoshihide Kozai, theformer director of NAOJ and the director of Gunma Observatory.
He also represents the gravitational wave research of Japan.Kuroda was a member of steering committee of TAMA during
1995-2003 and now Kuroda is the PI of LCGT project.
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Brief History of TAMA3001995 Project started1997 One arm cavity locked1999 FPMI operation started DT1(11hr) ,DT2(31hr)2000 World best sensitivity h = 5E-21/rHz DT4(167hr)2001 DT6(1038hr)
Power Recycled FPMI
2002 First Coincidence Run with LIGO(S1) and
GEO600 2003 DT8(1158hr) with LIGO(S2)2003/4 DT9 with LIGO(S3) and GEO600 Full Automatic
Operation
2004 - Noise hunting TAMA-SAS
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Long term operation● Operation more than 100 days / Observation data more
than 1700 hr~ Efficiency of 81.3%(Data taking run 8)
● Collaborative observation with LIGO and GEO600
● Improvement of observation system
~ Automatic (Operator free) operation~ Alarm system / remote monitoring / remote control
Time series of sensitivity
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Current best at Low Frequencies
10-20
10
-18
10
-16
10
-14
10
-12
10
-10
10
-8
Dis
pla
cem
ent n
oise
[m/H
z1/2 ]
100
101
102
103
104
105
Frequency [Hz]
Displacement noise level of TAMA300 (2003/11/04)
dL- displacement Laser frequency noise Laser intensity noise Detection+Shot noise Shot noise Detection noise mirror thermal noise Q=3e6 suspensio thermal noise Q=5e5 dl- feedback noise dl+ feedback noise dL- filter noise Alignment noise
Seismic noise dspPhase2 matrix
Noise budget of TAMA300
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To find the scattering noise source at mid-frequencies, all reflected and possible stray beams
were killed in the center Michelson part.
Identifying scattering noise in 2004
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Noise reduction by one order in Michelson part without Fabry-Perot cavities
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For Higher sensitivity at low frequencies
Alignment control noise UGF = 10Hz -> 2HzL-control ・ electric noise 1/100 @100Hzl- control noise Feedfoward with 1% accuracyIntensity noise Reduction factor = 1/5 @100Hz
Alignment control noise UGF = 10Hz -> 2HzL-control ・ electric noise 1/100 @100Hzl- control noise Feedfoward with 1% accuracyIntensity noise Reduction factor = 1/5 @100Hz
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Introduction of SAS in 2005-06
Successful lock of 300mFP cavities and a noise curve was taken as a Fabry-Perot Michelson interferometer.
Noise is suppressed at frequencies more than 1Hz
SAS
Old Suspension
Installation at center room
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Angular performance by SAS Measured by local optical lever. Angular fluctuation of the test mass was improved at >1Hz. It is possible to set the bandwidth of the alignment control to be lower
than 2Hz. → Expected reduction of the alignment noise which limited the former sensitivity of TAMA300.
Step1 By R. Takahashi at Amaldi 7
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Evaluation by Locked FP using four SASs
Locked FP with SASRFPMI in 2003
Alignment noise
• Improved displacement noise at 2~7Hz.
Step2
• Still alignment noise is dominant at 2~100Hz.
By R. Takahashi at Amaldi 7
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Possible alignment control noise reduction
4000 times improvement at 100Hz
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
Dis
pla
cem
ent n
oise
[m/H
z1/2 ]
100
101
102
103
104
105
Frequency [Hz]
Displacement noise level of TAMA300 (2003/11/04)
dL- displacement Alignment noise Phase2 Theoretical limit Expected alignment noise
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Summary of TAMA300
• Control system for SAS was established.• LengthLength fluctuation of the 300-m cavity was fluctuation of the 300-m cavity was
improved at >1Hzimproved at >1Hz..• AngularAngular fluctuation of the test mass was fluctuation of the test mass was
improved at >1Hzimproved at >1Hz..• Recycled FPMI with SAS was successfully
locked and now the final tuning is being done.
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CLIO
CLIO is a 100m baseline cryogenic interferometer placed underground at Kamioka
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Expected reduction of thermal noise by CLIO (300K – 20K)
Mirror sizeΦ10cm, t6cm
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CLIO is a locked Fabry-Perot Interferometer
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Internal view of mirror suspension
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Cryostat and 5m pipe
Radiation shieldRadiation shield
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Current sensitivity of CLIO
After reaching thermallimit, start cooling
Mirror thermal noise(300K)
Limit sensitivity
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The plots shows that thermal noise of lossy suspension wire mightbe reduced by cooling.(only three mirrors werecooled at this time)
Effort to attain ultimate sensitivity of CLIO
We have not attained roomtemperature thermal noise,yet.
We are checking suspicious noise sources one by one.
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Summary of CLIO and limiting factor of sensitivity• 30Hz-300Hz f-inversely square dependence
– Mechanical noise sources• Mirror vibration (main mirrors, pick-off mirrros, BS): not f^{-2}• Injection / detection port: detection optical line was enclosed against
acoustic noise • Optical windows: ? If so, more complicated structure may apper
– Electrical noise sources• Actuator system (amplifier noise, thermal noise of the circuit, ・・・ ) magnet bars were replaced with smaller ones• Magnetic force (bar magnets, closed loop of suspension wires) ferromagnetic parts were removed near test masses • Electrostatic force ? may depend on repeated vacuum opening process
– Physical noise sources• Stray light estimation by exciting the center part of the beam tube • Residual gas (spot sources) ? vacuum pressure changed• Radiation pressure (DC) observed repulsion of test masses by light power• Newtonian gravitational force difficult to increase to explain the present
– Data taking• 300Hz- photon shot noise / calibration• We have still no answer.
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LCGT
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LIGO (USA), VIRGO (French-Italian), GEO (Germany-England), TAMA (Japan) are in operation.
Occurrence of neutron star binary is estimated to be 10-5 for matured galaxy per year . There are 0.01 galaxies for 1 cubic Mpc. Present detectors ( km -scale) cover up to Virgo cluster ( 20Mpc). More than several years are needed to detect the event. Therefore, we need more sensitive detector. LCGT can detect an event occurring at 180Mpc on average and observes 8 events a year.
Necessity of LCGT
1pc=3.3light year
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LCGT plays an complementary role with LIGO.LCGT: grey, LIGO (Hanford): green contour
International Network of GW observation
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Optical design of LCGT
Optical design of the basic interferometer
Two interferometers are arranged not to interfere in the same vacuum system.
150W
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Design Sensitivity
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LCGT placed underground at Kamioka
Frequency Hz
Dis
plac
emen
t no
ise
m/R
Hz
Blue : MitakaRed : KamiokaGreen: estimation of seismic noise
A 20m prototype, LISM, was moved from TAMA site to Kamiokaunderground. Sensitivity was nonlinearly improved by 4 ordersat 100 Hz.
Collaborative work by NAOJ and ICRR
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• It is a direct way to reduce thermal noise• It produces less thermal lens effect
– due to high thermal conductivity and low thermal expansion rate (sapphire)
• It can avoid the optical parametric instabilities– due to higher elastic wave speed (sapphire)
and small beam size (cryogenic)
• It is free from large optical coating loss– due to low temperature
Why do we use cooled sapphire mirrors?
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Large heat production is avoided by RSE
• Broad band RSE (Resonant Side band Extraction method) is applied.
• Power recycling gain is set 11.
• Finesse of the cavity is 1550, which means that observational band becomes to be lower than required.
• RSE keeps the observation frequency band unchanged.
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Test mass of LCGT is connected to a cooling system by a heat link that possibly introduces mechanical noise. A suspension point interferometer (SPI) is introduced to maintain high attenuation of seismic and mechanical noise without degrading high heat conductivity.
Refrigerator noise is avoided by SPI
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SPI auxiliary mirror
SAS: 3 stage anti-vibration system with inverted pendulum
Main mirror
Heat links start from thisstage to inner radiation shield
Conceptual designof suspension
Radiation outer shield
Vacuum is common
Sapphire fiber suspending main mirror
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Configuration of LCGT cryostat. Two sets of towers corresponds to one arm FP cavity.
Drawn by Toshiba
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Cooling System
300K 100K
8K
5K
Absorption14K
20K
80K
T. Tomaru et al., Cryocoolers 13 (2005) 695.R. Li et al., Cryocoolers 13 (2005) 703.
Tomaru et al. Amaldi7
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New Revealed Heat Load in CLIOCryostat Beam Duct Designed heat load:
~ a few mW @ 8K shieldInitial cooling test: 12.6 K @ 8K shield → Estimated heat load > 3W ~1000 times larger than design
Cryo PipeVacuum Duct
Cryostat
Radiation Shield
Cryocooler
Thermal RadiationConduction ?
Mirror
When cryo-shield-pipe was closed, cryostat reached design temperature.
Thermal radiationfrom a 300K beamport conducted in Al cryo-pipe ?
Tomaru et al. Amaldi7
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Al baffles with aperture of1/3 of cryo-pipe diameter
Using 2 baffles
Measured result: 7.9mW
-> Reduction rate: 98%
Apply to the LCGT …
Limitation: heat conduction of a main mirror suspension (820mW)
800mm x1 case : 5W -> 700mW
250mm x2 case : 820mW -> 620mW (too small aperture)
Acceptable
Tomaru et al. Amaldi7
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International Collaborations
• TAMA-LIGO – Attachment 1 (Locking system, 1997)– Attachment 2 (Mirror imperfection, 1998)– Attachment 4 (e2e simulator, 2000)– Attachment 5 (SAS technology, 2000)– Attachment 6 (sapphire, under process, 2007)
• TAMA-VIRGO (Pwr Recycling, 1998)
• LCGT-ACIGA (R&D, 2001)
New comers are welcomed!!
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Summary
• We have acquired interferometer techniques (power recycling, Fabry-Perot Michelson, control system) by TAMA.
• LISM confirmed underground significance.• CLIO proves the feasibility of cryogenic mirror, s
oon.• LCGT will certainly detect gravitational wave eve
nts in a year.• We are doing the best for funding of FY 2008.