1 山山 山 一 山山山山 山山山山山山 山山山山山山 鏡鏡鏡鏡鏡 鏡鏡鏡鏡鏡鏡鏡鏡鏡鏡鏡鏡鏡鏡 () 2011/6/24 @ 山山山山山山山山 山山 、
Jan 03, 2016
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山元 一広
東京大学 宇宙線研究所 重力波推進室
鏡の熱雑音(重力波検出器と周波数安定化)
2011/6/24 @ 情報通信研究機構、東京
0.Abstract
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精密測定の原理的な限界の一つである 鏡の
熱雑音について
(1)重力波検出器 (2) Cavity を用いた周波数安定化
という2つの分野にしぼって解説します。
Contents
1. Gravitational wave detection
2. Frequency stabilization
3. Summary
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1. Gravitational wave detection What is the gravitational wave ?
1915 A. Einstein : General theory of Relativity
“Gravitation is curvature of space-time.”
1916 A. Einstein : Prediction of gravitational wave
“ Gravitational wave is ripple of space-time.”
4
Wikipedia (A. Einstein, English)
A. Einstein, S. B. Preuss. Akad. Wiss. (1916) 688.
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http://spacefiles.blogspot.com
Gravitational wave
Speed is the same as that of light.
Transverse wave and two polarizations
1. Gravitational wave detection
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Interaction of gravitational wave is too weak !
Artificial generation is impossible !
No experiment which corresponds to
Hertz experiment for electromagnetic wave
Astronomical events
Strain [(Change of length)/(Length)] : h ~ 10-21
(Hydrogen atom)/(Distance between Sun and Earth)
No direct detection until now
1. Gravitational wave detection
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Indirect detection of gravitational wave
Binary pulsar
(R.A. Hulse and J.H. Taylor,
Astrophysical Journal 195 (1975) L51.)
Generation of gravitational wave
Energy emission
Change of period of binary
Observed change of period agrees with theoretical
prediction by radiation formula of gravitational wave.
J.H. Taylor et al., Nature 277 (1979) 437.
1. Gravitational wave detection
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Recent result
J.M. Weisberg and J.H. Taylor, ASP Conference Series, 328 (2005) 25 (arXiv:astro-ph/0407149).
1. Gravitational wave detection
9Web site of Nobel foundation
1. Gravitational wave detection
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What is the motivation ?
Physics : Experimental tests for theory of gravitation
Astronomy : New window for astronomical observation
Gravitational wave astronomy
No direct detection until now
1. Gravitational wave detection
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Gravitational wave astronomy: Burst source : SupernovaMechanism of the core-collapse SNe still unclear
Shock Revival mechanism(s) after the core bounce.
GWs generated by a SNe should bring information from the inner massive part of the process and could constrains on the core-collapse mechanisms.
M. Punturo, GWDAW Rome 2010
1. Gravitational wave detection
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Gravitational wave astronomy: Burst source
: Compact binary coalescence Neutron star, Black hole
msec
chirp signalcoalescence
quasi-modeoscillation
-300Hz -1kHz
K. Kuroda Fujihara seminar (2009)
New standard candle for measurement of distance
Equation of state at high density, formation black hole
1. Gravitational wave detection
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There are a lot of kinds of detectors !
Resonant detector
Interferometer (on Earth)
Interferometer (Space)
Doppler tracking
Pulsar timing
Polarization of cosmic microwave background
and so on …
Frequency range : 10-18 Hz – 108 Hz
1. Gravitational wave detection
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Interferometer (on Earth)Gravitational wave changes length difference of two arms.
Frequency : 10 Hz – 10 kHz
1. Gravitational wave detection
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All current interferometers have Fabry-Perot cavities.
1. Gravitational wave detection
World wide network for GW astronomy
Adv. LIGO (under construction since 2008 )TAMA/CLIO
LCGT, Budget request
LIGO(I) Hanford
LIGO(I) Livingston
GEO 600
Virgo
AIGO (budget request)
Adv. Virgo (design)
ET (planed)
A network of detectors is indispensable to position the source.
LCGT
By K. Kuroda (2009 May Fujihara seminar)
GEO HF
1717
LIGO (U.S.A.)
4 km, Hanford and Livingston (3000 km distance) (U.S.A.) S. Kawamura, Classical and Quantum Gravity 27 (2010) 084001.
1. Gravitational wave detection
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VIRGO (Italy and France)
3 km, Pisa (Italy) S. Kawamura, Classical and Quantum Gravity 27 (2010) 084001.
1. Gravitational wave detection
1919
GEO (Germany and U.K.)
600 m, Hannover (Germany) S. Kawamura, Classical and Quantum Gravity 27 (2010) 084001.
1. Gravitational wave detection
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TAMA (Japan)
300 m, Tokyo (Japan) S. Kawamura, Classical and Quantum Gravity 27 (2010) 084001.
1. Gravitational wave detection
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100 m, Kamioka (Japan) S. Kawamura, Classical and Quantum Gravity 27 (2010) 084001.
CLIO (Japan)
1. Gravitational wave detection
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First generation (Current)
LIGO (U.S.A.), VIRGO (Italy and France),
GEO (Germany and U.K.), TAMA (Japan), CLIO (Japan)
Second generation (Future)
Advanced LIGO, Advanced VIRGO, GEO-HF,
AIGO(Australia), LCGT (Japan)
Third generation (Future)
Einstein Telescope (Europe)
1. Gravitational wave detection
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Sensitivity of interferometer
1st generation (LIGO,VIRGO)
2nd generation
3rd generation
10 times
10 times
1. Gravitational wave detection
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Second generation Observation : 2017 ? – We can expect first detection !
Advanced LIGO, Advanced VIRGO, GEO-HF
Upgrade of LIGO, VIRGO, and GEO
AIGO (Australia)[Budget is requested.]
Similar to Advanced LIGO
LCGT (Japan)
Cryogenic technique
(Mirror temperature is 20K, small thermal motion)
Underground site (small seismic motion)
1. Gravitational wave detection
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Einstein Telescope (Europe)
30 km vacuum tube in total
Cryogenic technique Underground site (small seismic motion)
Third generation Observation : 2026 ? –
1. Gravitational wave detection
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Location of LCGTLCGT is planed to be built underground at Kamioka, where the prototype CLIO detector is placed.
By K. Kuroda (2009 May Fujihara seminar)
3 km, Kamioka (Japan)
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最近の LCGT の進展 (http://gwcenter.icrr.u-tokyo.ac.jp/)
2010 年 6 月:文部科学省「最先端研究基盤事業」の一つとして「大型低温重力波望遠鏡の整備」が承認。
2011 年 3 月:トンネル掘削予算承認(国会)。
2011 年 6 月: LCGT の愛称決定 (630 件の応募 ) 。
2011 年 7 or 8 月: LCGT の愛称公表。
1. Gravitational wave detection
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今後の予定
2010/10-2014/9 : iLCGT ( 常温干渉計の建設 ) 1 か月程度の観測運転
2014/10-2017/3 : bLCGT( 低温干渉計の建設 )
2017/4- : 長期間観測運転
1. Gravitational wave detection
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「低温工学」 2011 年 7 月号にLCGT 特集掲載予定
1. Gravitational wave detection
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Interferometric gravitational wave detector
Mirrors must be free and are suspended.
S. Kawamura, Classical and Quantum Gravity 27 (2010) 084001.
1. Gravitational wave detection
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Thermal noise of suspension and mirror
1. Gravitational wave detection
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Fluctuation-Dissipation Theorem
Relation between thermal noise
and mechanical loss in suspension and mirror
Amplitude of thermal noise is proportional to
(T/Q)1/2.In general, Q (inverse number of magnitude of Dissipation,) depends on T (temperature).
1. Gravitational wave detection
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Mirror thermal noise Two kinds of mechanical dissipation
Thermoelastic damping Inhomogeneous strain Temperature gradient (via thermal expansion) Heat flow Dissipation Structure damping Unknown mechanism Almost no frequency dependence
1. Gravitational wave detection
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Mirror consists of not only substrate,
but also reflective coating !
Thermoelastic damping
Heat flow in substrate : Substrate thermoelastic noise
Heat flow between substrate and coating :
Thermo-optic noise
Structure damping
Structure damping in substrate : Substrate Brownian noise
Structure damping in coating : Coating Brownian noise
1. Gravitational wave detection
3535
Temperature dependence of mirror thermal noise in LCGT
Below 20 K : Thermal noise is sufficiently small for LCGT.
1. Gravitational wave detection
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Thermal noise is fundamental noise of gravitational wave detection. How about the other fields ?
Cavity as reference for laser frequency stabilization
Current best laser frequency stabilization with rigid cavity at room temperature is limited by thermal noise of mirrors.
K. Numata et al., Physical Review Letters 93 (2004) 250602.
2. Frequency stabilization
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Hot paper (ISI Web of Knowledge)
1 paper every 3 weeks ! (until 18 June 2011)
2. Frequency stabilization
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2. Frequency stabilization
0.1Hz/rtHz*(1Hz/f)1/2 (10mHz-1Hz)Allan deviation :4*10-16 (10mHz-1Hz)
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世界記録( Case 1, 2011 年現在でも one of the best records ) B.C. Young et al., Physical Review Letters 82 (1999) 3799. Spacer(ULE) の散逸による熱雑音は問題にならない。鏡 (ULE) の寄与によって決まっている。鏡を fused silica で作れば coating で決まる。
2. Frequency stabilization
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世界記録( 2011 年現在でも one of best records ) B.C. Young et al., Physical Review Letters 82 (1999) 3799. これを越えるためには?
(1)Cavity を長くする。(2) ビーム径を大きくする。 離れた 2 点間の熱雑音の相関は小さいため。
但し、 factor 程度の低減。
(3)Coating mechanical loss を小さくする。(4)Cryogenic technique
2. Frequency stabilization
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(3)Coating mechanical loss を小さくする。
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Old summary of coating mechanical loss (Ta2O5/SiO2)
Loss angle : 1/Q
Similar results (same order of magnitude)
K. Yamamoto et al., Physical Review D 74 (2006) 022002.
2. Frequency stabilization
is on the order of 10-4.
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(3)Coating mechanical loss を小さくする。
(a)TiO2 doping (Ta2O5)
TiO2 ~ 20% loss 半分
G. Harry et al., Classical and Quantum Gravity 24 (2007) 405.
2. Frequency stabilization
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(3)Coating mechanical loss を小さくする。
(b)Ta2O5/SiO2 以外の材質は?
Niobia, Hafnia, Silica+Titania, Zirconia, Almina, ….
Ta2O5/SiO2 を大きくしのぐものはない。 is on the order of 10-4.
Amorphous silicon X. Liu and R.O. Pohl, Physical Review B 58(1998)9067. is on the order of 10-7~ 10-5 .
波長は 1100nm 以上。光学的特性は??
2. Frequency stabilization
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2. Frequency stabilization(3)Coating mechanical loss を小さくする。
(b)Ta2O5/SiO2 以外の材質は? AlxGa1-xAs (Small oscillator)
G.D. Cole et al., Applied Physics Letters 92 (2008) 261108. ~ 2*10-4 at 300K, 5*10-5 at 4K
~ 1*10-5 at 20KG.D. Cole et al., 2010 IEEE 23rd International Conference on Micro Electro Mechanical Systems (MEMS). Pages 847 –850
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(4)Cryogenic technique
4545
4 K : Thermal noise is 30 times smaller (Coating dominant).
2. Frequency stabilization
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世界記録( Case 1, 2011 年現在でも one of the best records )鏡 (ULE) の寄与によって決まっている。鏡の散逸が小さければ coating で決まる。 1/3 倍
Coating の散逸が温度に依存しなければ 4K まで冷却して 1/10 倍。
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300 K : 0.1Hz/rtHz*(1Hz/f)1/2 (10mHz-1Hz) Allan deviation :4*10-16 (10mHz-1Hz)
(4)Cryogenic technique
2. Frequency stabilization
4 K : Thermal noise is 30 times smaller (Coating dominant).
4 K : 3 mHz/rtHz*(1Hz/f)1/2 (10mHz-1Hz) Allan deviation :1*10-17 (10mHz-1Hz)
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2. Frequency stabilization(4)Cryogenic technique
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Material of mirror and spacerStructure damping (frequency independent) in substrate
Fused silica can not be used. Sapphire or Silicon are good.
Q value measurement T. Uchiyama et al., Physics Letters A 261 (1999) 5-11.R. Nawrodt et al., Journal of Physics: Conference Series 122 (2008) 012008. C. Schwarz et al., 2009 Proceedings of ICEC22-ICMC2008.
4848
Laser frequency stabilization with rigid cavity at 3 K
S. Seel et al., Physical Review Letters 78 (1997) 4741.
Universität Konstanz
(4)Cryogenic technique
2. Frequency stabilization
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At 3 K 2.5*10-15
Universität Konstanz
NIST
Best record at room temperature4*10-16 (limited by substrate Brownian noise)B.C. Young et al., Physical Review Letters 82 (1999) 3799.
(4)Cryogenic technique
2. Frequency stabilization
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2. Frequency stabilization(4)Cryogenic technique
At 4 K 1*10-15
H. Mueller et al., Physical Review Letters 91 (2003) 020401.
Some progress …
5151
Laser frequency stabilization with rigid cavity at cryogenic temperature should be better !Allan deviation : 1*10-17 (limited by coating Brownian noise) Experiment : 1*10-15
Development is in progress (This is not a perfect list).
Universität Konstanz, Humboldt-Universität zu Berlin,Heinrich-Heine-Universität Düsseldorf, Physikalisch-Technischen Bundesanstalt
University of Tokyo (Tsubono lab.)
(4)Cryogenic technique
2. Frequency stabilization
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(4)Cryogenic technique Coating : dominant source Temperature dependence ?
Loss angle is almost independent of temperature.
University of Tokyo
K. Yamamoto et al., Physical Review D 74 (2006) 022002.
2. Frequency stabilization
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(4)Cryogenic technique Coating : dominant source Temperature dependence ?
53I. Martin et al., Classical and Quantum Gravity 25(2008)055005.
Peak at 20 K ?
Glasgow University
2. Frequency stabilization
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Annealing suppresses (Ta2O5) peak.
Glasgow University
(4)Cryogenic technique Coating : dominant source Temperature dependence ?
I. Martin et al., Classical and Quantum Gravity 27(2010)225020.
2. Frequency stabilization
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(4)Cryogenic technique Coating : dominant source Temperature dependence ?
Vendor ?
M. Abernathy et al., CWADW 2011 http://agenda.infn.it/getFile.py/access?contribId=56&sessionId=15&resId=2&materialId=slides&confId=3351
Tokyo:JAEGlasgow:CSIRO
2. Frequency stabilization
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(4)Cryogenic technique Coating : dominant source Temperature dependence ?
データが集積されているが混乱も増している。
採用した coating の mechanical loss は当事者が測定して おさえておくべき!
LCGT 計画では再度の測定をまもなく開始する。 (JAE が供給しなくなったため )
2. Frequency stabilization
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2012 年 1 月出版予定
“Optical Coatings and Thermal Noise in Precision Measurements”, ed. by Gregory Harry, Riccardo Desalvo, and Timothy Bodiya, Cambridge University Press, in press.
重力波だけでなく、レーザー周波数安定化、量子実験などの他分野からも
2. Frequency stabilization
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目次から2. Frequency stabilization
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目次から2. Frequency stabilization
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目次から
レーザー周波数安定化について書いてます。
2. Frequency stabilization
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3.Summary(1) 鏡の熱雑音:精密測定の限界
(2)LCGT : 日本の大型重力波検出器計画 鏡の熱雑音を低減するために鏡を 20K まで冷却
(3)Cavity を用いたレーザー周波数安定化:世界記録は鏡の熱雑音で制限されている。
0.1Hz/rtHz*(1Hz/f)1/2 (10mHz-1Hz) Allan deviation :4*10-16 (10mHz-1Hz)
6262
3.Summary(4) 周波数安定化において熱雑音の壁を越えるには
(a)Coating mechanical loss を小さくする。 (i)TiO2 doped Ta2O5/SiO2 : Loss は半分程度に (ii)Ta2O5/SiO2 以外の材質は? Amorphous silicon, AlxGa1-xAs 光学特性は?
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3.Summary(4) 周波数安定化において熱雑音の壁を越えるには
(b)Cryogenic technique 4 K : Thermal noise is 30 times smaller. 4 K : 3 mHz/rtHz*(1Hz/f)1/2 (10mHz-1Hz) Allan deviation :1*10-17 (10mHz-1Hz) 鏡や spacer はサファイアもしくはシリコン。 採用した coating の mechanical loss は 当事者が測定しておさえておくべき!
まだ常温より安定度は悪い。
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ご静聴ありがとうございました。