LCGT 詳細設計と R&D
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LCGT 詳細設計と R&D
大橋 正健東大宇宙線研
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LCGT の基本設計 - これまで -
– 感度は主に量子雑音 ( 散射雑音・輻射圧雑音 ) で決ま
る 基線長 3km
レーザー光源 100Wリサイクリングゲイン 50腕 j 共振器フィネス 100 (fcav=250Hz)
サファイアミラー 50kg, Q=108, 30Kコーティングの熱雑音を考慮懸架振り子 1Hz, Q=2x108, 10KSAS による防振系
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干渉計方式と量子雑音 • 様々な干渉計方式
• DRMI, SR, RFPMI, RSE, ExRSE
• 量子雑音 ( 散射雑音・輻射圧雑音 ) は、–腕パワーと信号帯域幅で決まる–干渉計方式には拠らない
( 水野の推論、 A. Buonanno の計算 detuning しない場合 )
• 干渉計方式の決定材料–実現可能な腕パワーと信号帯域幅–その他の要因
• 基材での発熱• 制御の容易さ
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腕パワー・信号帯域幅と量子雑音
• 量子雑音 ( 散射雑音・輻射圧雑音 ) は、腕パワーと信号帯域幅で決まる
armsigsig
arm
armsigarm
sig
sigsig
Pff
PPfP
fffff
輻射圧雑音
散射雑音1
101 102 103 104
10–24
10–22
No
ise
lev
el
[1
/Hz1/
2 ]
Frequency [Hz]
Cavity power x
10
fcutoff
fcutoffSignal b
and 1/10
101 102 103 104
10–24
10–22
No
ise
lev
el
[1
/Hz1/
2 ]
Frequency [Hz]
Cavity power x10
fcutoff
fcutoff
Signal band 1/10
散射雑音
輻射圧雑音
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設計の基本方針・境界条件 • 基本方針
– 腕パワーと信号帯域幅1.4 Mo の連星合体に対する感度を基準に決定• SNR=10 で、 200Mpc のイベントを捕らえられること• 可能ならさらに遠くまで見れるよう最適化すること
• 境界条件 (20K への冷却能力 1W)– 基材内での発熱
• 熱吸収 ( サファイア ) 20ppm/cm• 基材の厚さ 18cm
– コーティングでの発熱• 熱吸収 0.1ppm
BS 入射 < 2800W 干渉計入射パワー 100W なら PRG < 28
EM 反射パワー < 10MW
以前のデザインの PRG=50 は不可能 → RSE, ExRSE が現実的
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連星合体に対する SNR
• 連星合体を SNR=10 で検出できる距離• 1.4Mo イベントに対して、 244 Mpc
10–1 100 101 102101
102
103
Det
ecta
ble
dis
tan
ce
[Mp
c]
Mass of a star [Mo]
Old design
Optimized design
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最適化後の感度曲線 • 現実的なパラメータ範囲でほぼ最適化
• 腕内パワー 830 kW, 信号帯域幅 200 Hz
100 101 102 103 104
10–24
10–22
10–20
10–18
No
ise
lev
el
[1
/Hz1/
2 ]
Frequency [Hz]
Shot noise
Mirror thermal
Seism
ic no
ise
Suspension thermal
Radiation pressure
TAMAnoise level
Parm=830kW fsig=203 HzLCGT noise budget 腕共振器フィネス : 1250 PRG : 10 SBG : 10
68.0
72.0
99999.0
995.0
SR
R
R
R
R
E
F
100 101 102 103 104
10–24
10–22
10–20
10–18
No
ise
lev
el
[1
/Hz1/
2 ]
Frequency [Hz]
Shot noise
Mirror thermal
Seism
ic no
ise
Suspension thermal
Radiation pressure
TAMAnoise level
Parm=830kW fsig=203 HzLCGT noise budget
Old design
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連星合体に対する SNR
• 連星合体を SNR=10 で検出できる距離• 1.4Mo イベントに対して、 244 Mpc
10–1 100 101 102101
102
103
Det
ecta
ble
dis
tan
ce
[Mp
c]
Mass of a star [Mo]
Old design
Optimized design
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目標感度を達成できるか?
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目標感度が達成されれば重力波をとらえられるのか?
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同位置の 2 台でFirst detection は
可能か?
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200Mpc で 0.1events/year ?
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LISA との関係は?
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Advanced LIGO とは?
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Advanced LIGO Development Team
GroupSeismic Isolation (SEI)
Suspension(SUS)
Core Optics(COC)
Input Optics(IO)
Pre-Stab.Laser (PSL)
Aux. Optics(AOS)
Ifo Sense &Control (ISC)
SystemsEngineering
CIT requirements
requirements; Fiber & bonding research; final design; TNI noise measure
requirements; leads design; coordinates materials develop.; polishing; inhomogeneity compensation; metrology
requirements; intensity stabilization feedback to PSL
requirements; engin support & epics integration; performance eval.
requirements; photon actuation;
requirements; electronics; system identification; 40m experiment/controls testbed
requirements; standards; extend E2E simulation; system trade studies; optical layout; FFT studies
MITrequirements; LASTI prototype testing
requirements; measure coating effect on Q; LASTI prototype testing requirements
requirements; integrated IO/PSL system test
requirements; LASTI prototype & IO/PSL integrated sys test
requirements; active thermal compensation
requirements; system trade studies; bench top DC read-out exp.; PD testing; ISC design lead
requirements; define noise budget, define shared signal port power allocation, etc.
LLO engineering support
LHO
Stanford/HP Melody code
ACIGA high power system testing injection-locked, stable/unstable resonator
cavity test of active thermal compensation
GEO/Glasgow
welding; coating effect on mech Q; local control studies; triple performance in GEO-600; prelim design lead
10m signal recycling exp.; lock acq. & sensing matrix guidance
GEO/Hannover
Rod pumped system; leads PSL system design
IAP in-situ figure metrologyhigh power Faraday isolator development
PS Bench code
Iowa coating mech modeling
LSU MIMO control; SEI design lead
transient (excess) noise measure; mode coupling study & diagnostics
MSUchem & flame polishing effect on Q; surface charge measure
Stanfordhydraulic pre-isolation; ETF controls testbed
welding, bonding & coating effect on mech Q; bonding strength
low absorption sapphire development
MOPA system with LIGO 20W MO back-illuminated InGaAs detectors
Southern Utrace element identification; absorption
SMA/Lyonhigh mech Q, low absorption coatings
Syracusedirect loss measure; effect of polishing, coating, bonding
UFLIO system design; high power component tests
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スーパーカミオカンデカムランド
LISM(20m) CLIO
CLIO 建設サイト(神岡鉱山内)
暗黒物質検出器
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