Our 10m Interferometer Prototype
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1 Our 10m Interferometer Prototype KAGRA f2f, February 14, 2014 Fumiko Kawaoze AEI 10 m Prototype 1
2 10m Prototype Interferometer Standard Quantum Limit experiment Macroscopic Quantum mechanics Thermal Noise Interferometer GEO-HF test facility (laser, control)
3 Measure Standard Quantum Limit above Classical Noise Quantum Noise Classical Noise Design sensitivity SQL-IFO with Khalili cavities and titania doped coatings Today: Direct bonded monocrystalline nultipayer coatings of AlGaAs
4 Optical Layout sub-sql Interferometer ~ 8 W 1064 nm Tap off ~260 mw Output modecleaner 10 m Fabry-Perot arm cavity Finesse :~ 670 Frequencyreference cavity: Length: 21.2 m Finesse: ~ 3000 ITM BS 100 g mirrors Triple pendulum suspensions Monolithic all-silica last stage with four filaments of 20 µm diameter Triple pendulum suspensions Mirror mass: 850 g ETM
5 Progress over the last year January 2013 January
6 Sub Projects PMC: PMC: Length: 0.53 m Finesse: ~ 1000 Frequency-ref.cav.: Length: 21.2 m Finesse: ~ 3000 Suspended 860g mirrors Substrate: Fused silica Coating: Tantala/Silica ~ 8 W 1064 nm Output modecleaner Tap off ~260 mw SPI Tap off ~100 mw ITM BS TNI: TNI: Triple pendulum suspensions Length: 0.1 m Length: Mirror mass: 850 g Finesse: ~ m Finesse: ~ m Fabry-Perot arm cavity Finesse ca. 670 AEI-SAS ETM 10 m Fabry-Perot arm cavity 100 g mirrors Finesse ca. Triple 670 pendulum suspensions Monolithic all-silica last stage with four filaments of 20 µm diameter All can be done in parallel. 6
7 Geometrical Anti-Springs GAS filter top view GAS filter side view
8 Installation of first AEI-SAS ( )
9 AEI-SAS as installed in UHV system Two out of three AEI-SAS installed, the third will be installed this year. Work done independently from other sub systems. Horizontal isolation performance: -80 db at 4 Hz
10 Suspension Platform Interferometer Installation (Spring 2013)
11 SPI as installed inside UHV system Achieved sensing noise: 10 nm/ Hz below 10 mhz 10 pm/ Hz above 1 Hz
12 LZH-AEI 35 W Laser
13 Pre Mode Cleaner 13
14 Reference Cavity Target Sensitivity: Hz/sqrt 20Hz > Hz/sqrt Hz < 1 khz Frequeny noise[hz/sqr Hz] RPquant RPclas Shot noise Substrate thermal Sus TN Seismic ver. Seismic longi. coating thermal total target Frequency[Hz] Substrate Q ~ 10^6 (wire sling suspension)
15 Ref Cavity Mirror hanging Sensor: BOSEM style shadow Control: Eddy current dampers, voice-coil actuators 15
16 Thermal Noise Interferometer Fabry Perot Interferometer Cavity length: 10cm Finesse: 3000 Tunable small spot-size Suspended 860g mirrors Substrate: Fused silica Coating: Tantala/Silica Pin = 0.1 mw The future (exchange a single mirror) AlGAs coatings, Gratings, Bonding loss 16
17 Single Arm IFO Goal: Studying cavity performance with imperfect mirrors g factor ~ 1 17
18 Program of each sub project Sub project What can be learned AEI- SAS SPI Third Table Installation, Characterization Optical Lever installation, Third SPI Installation Suspension system Optical system, suspension system, Phase meter, interferometry Ref.Cav. TNI Suspension installation, Angular control components setup Suspension installation, Angular control system setup Suspensions, Laser frequency control & CDS, interferometry, Angular Control system Thermal noise, suspension system, Gaussian optics, interferometry Sub SQL Building suspensions Interferometry, suspension system All the sub systems use the Digital Control System (CDS). 18
19 Theses completed: Alexander Wanner PhD SAS Now CEO QUEST Katrin Dahl PhD SPI Now at Diehl Christian Gräf PhD Optical simulations Now postdoc position in Glasgow Oliver Kranz Diploma SPI Now PhD student at PTB Thimotheus Alig Master Laser charactersation and PMC Now PhD student at LZH Sina Köhlenbeck Diploma Digital Interferometry Now PhD student with us Kai Voges Bachelor Calibrated IR Camera Daniel Gering Diploma Phasemeter Interface
20 Look into the future The world s first measurement below the SQL Experiences transfer to future GW detectors 20
21 Thank you for your attention. 21
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