Test mass dynamics with optical springs proposed experiments at Gingin Chunnong Zhao (University of Western Australia) Thanks to ACIGA members Stefan Danilishin.

Slides:



Advertisements
Similar presentations
Ring Dampers and Gold Barrel Coatings -to control parametric instabilities Chunnong Zhao on behalf of Gingin facility, ACIGA/UWA.
Advertisements

Albert-Einstein-Institute Hannover ET filter cavities for third generation detectors ET filter cavities for third generation detectors Keiko Kokeyama Andre.
Laser Interferometer Gravitational-wave Detectors: Advancing toward a Global Network Stan Whitcomb LIGO/Caltech ICGC, Goa, 18 December 2011 LIGO-G v1.
The Threat of Parametric Instabilities in Advanced Laser Interferometer Gravitational Wave Detectors Li Ju Chunnong Zhao Jerome Degallaix Slavomir Gras.
Koji Arai – LIGO Laboratory / Caltech LIGO-G v2.
Dual Sphere Detectors by Krishna Venkateswara. Contents  Introduction  Review of noise sources in bar detectors  Spherical detectors  Dual sphere.
TeV Particle Astrophysics August 2006 Caltech Australian National University Universitat Hannover/AEI LIGO Scientific Collaboration MIT Corbitt, Goda,
Generation of squeezed states using radiation pressure effects David Ottaway – for Nergis Mavalvala Australia-Italy Workshop October 2005.
Ponderomotive Squeezing & Opto-mechanics Adam Libson and Thomas Corbitt GWADW 2015 G
Recent Developments toward Sub-Quantum-Noise-Limited Gravitational-wave Interferometers Nergis Mavalvala Aspen January 2005 LIGO-G R.
GWADW, May 2012, Hawaii D. Friedrich ICRR, The University of Tokyo K. Agatsuma, S. Sakata, T. Mori, S. Kawamura QRPN Experiment with Suspended 20mg Mirrors.
GWADW 2010 in Kyoto, May 19, Development for Observation and Reduction of Radiation Pressure Noise T. Mori, S. Ballmer, K. Agatsuma, S. Sakata,
What are GW’s ?? Fluctuation in the curvature of space time, propagating outward form the source at the speed of light Predicted by Einstein’s GTR Gravitational.
Design of Stable Power-Recycling Cavities University of Florida 10/05/2005 Volker Quetschke, Guido Mueller.
White Light Cavity Ideas and General Sensitivity Limits Haixing Miao Summarizing researches by several LSC groups GWADW 2015, Alaska University of Birmingham.
Optical Configuration Advanced Virgo Review Andreas Freise for the OSD subsystem.
Several Fun Research Projects at NAOJ for the Future GW Detectors
Optical readout for a resonant gw bar. Old setup.
Experiments towards beating quantum limits Stefan Goßler for the experimental team of The ANU Centre of Gravitational Physics.
Experimental Characterization of Frequency Dependent Squeezed Light R. Schnabel, S. Chelkowski, H. Vahlbruch, B. Hage, A. Franzen, N. Lastzka, and K. Danzmann.
Optomechanical Devices for Improving the Sensitivity of Gravitational Wave Detectors Chunnong Zhao for Australian International Gravitational wave Research.
SQL Related Experiments at the ANU Conor Mow-Lowry, G de Vine, K MacKenzie, B Sheard, Dr D Shaddock, Dr B Buchler, Dr M Gray, Dr PK Lam, Prof. David McClelland.
Sapphire Test Masses ACIGA/UWA High lights of research at UWA Alternative approach to suspensions High power test facility Cryogenic applications Mark.
Arm Length Stabilisation for Advanced Gravitational Wave Detectors Adam Mullavey, Bram Slagmolen, Daniel Shaddock, David McClelland Peter Fritschel, Matt.
Advanced Virgo Optical Configuration ILIAS-GW, Tübingen Andreas Freise - Conceptual Design -
Parametric Instabilities and Control Li Ju ( 鞠莉), Chunnnong Zhao, David Blair Jiayi Qin, Qi Fang, Carl Blair, Jian Liu University of Western Australia.
LSC August G Z Gingin High Optical Power Test Facility (AIGO) 1 High Optical Power Test Facility - Status First lock, auto-alignment and.
Quantum noise observation and control A. HeidmannM. PinardJ.-M. Courty P.-F. CohadonT. Briant O. Arcizet T. CaniardJ. Le Bars Laboratoire Kastler Brossel,
LIGO-G R Quantum Noise in Gravitational Wave Interferometers Nergis Mavalvala PAC 12, MIT June 2002 Present status and future plans.
AIGO 2K Australia - Italy Workshop th October th October 2005 Pablo Barriga for AIGO group.
LIGO LaboratoryLIGO-G R Coatings and Their Influence on Thermal Lensing and Compensation in LIGO Phil Willems Coating Workshop, March 21, 2008,
Chunnong Zhao for ACIGA
Initial and Advanced LIGO Detectors
Advanced LIGO Simulation, 6/1/06 Elba G E 1 ✦ LIGO I experience ✦ FP cavity : LIGO I vs AdvLIGO ✦ Simulation tools ✦ Time domain model Advanced.
Parametric Instabilities In Advanced Laser Interferometer Gravitational Wave Detectors Li Ju Chunnong Zhao Jerome Degallaix Slavomir Gras David Blair.
Opto-mechanics with a 50 ng membrane Henning Kaufer, A. Sawadsky, R. Moghadas Nia, D.Friedrich, T. Westphal, K. Yamamoto and R. Schnabel GWADW 2012,
The status of VIRGO Edwige Tournefier (LAPP-Annecy ) for the VIRGO Collaboration HEP2005, 21st- 27th July 2005 The VIRGO experiment and detection of.
ACIGA High Optical Power Test Facility
Advanced LIGO Status Report
Mechanical Mode Damping for Parametric Instability Control
SQL Related Experiments at the ANU Conor Mow-Lowry, G de Vine, K MacKenzie, B Sheard, Dr D Shaddock, Dr B Buchler, Dr M Gray, Dr PK Lam, Prof. David McClelland.
Optical Spring Experiments With The Glasgow 10m Prototype Interferometer Matt Edgar.
LIGO Scientific Collaboration
GEO Status and Prospects Harald Lück ILIAS / ETmeeting Cascina November 2008.
Stefan Hild 1GWADW, Elba, May 2006 Experience with Signal- Recycling in GEO 600 Stefan Hild, AEI Hannover for the GEO-team.
The Proposed Holographic Noise Experiment Rainer Weiss, MIT On behalf of the proposing group Fermi Lab Proposal Review November 3, 2009.
LIGO-G D Advanced LIGO Systems & Interferometer Sensing & Control (ISC) Peter Fritschel, LIGO MIT PAC 12 Meeting, 27 June 2002.
Lessons from CLIO Masatake Ohashi (ICRR, The University of TOKYO) and CLIO collaborators GWADW2012 Hawaii 2012/5/16.
Solar chameleon detection at CAST Part II: The optical resonator Sauman Cheng and Manwei Chan.
High Frequency Parametric Instabilities in AdvLIGO and Methods for their Control David Blair, Chunnong Zhao, Ju Li, Slawomir Gras, Pablo Barriga and Jerome.
ET-ILIAS_GWA joint meeting, Nov Henning Rehbein Detuned signal-recycling interferometer unstableresonance worsesensitivity enhancedsensitivity.
The Proposed Holographic Noise Experiment
Auxiliary Optics System (AOS)
Reaching the Advanced LIGO Detector Design Sensitivity
Overview of quantum noise suppression techniques
Nergis Mavalvala Aspen January 2005
Yet another SQL? Tobias Westphal
Gingin Advisory Committee Meeting 08 Dec 2009
Generation of squeezed states using radiation pressure effects
Quantum noise reduction techniques for the Einstein telescope
Design of Stable Power-Recycling Cavities
Quantum effects in Gravitational-wave Interferometers
Ponderomotive Squeezing Quantum Measurement Group
Advanced LIGO Quantum noise everywhere
Squeezed states in GW interferometers
Summary of Issues for KAGRA+
A. Heidmann M. Pinard J.-M. Courty P.-F. Cohadon
Squeezed Light Techniques for Gravitational Wave Detection
Advanced Optical Sensing
Measurement of radiation pressure induced dynamics
Presentation transcript:

Test mass dynamics with optical springs proposed experiments at Gingin Chunnong Zhao (University of Western Australia) Thanks to ACIGA members Stefan Danilishin and Farid Khalili (Moscow State University) Yanbei Chen (Caltech) 1 GWADW2010, May 19, 2010

2 Contents: Gingin high optical power research facility 3-mode optomechanical transducer Test mass dynamics with double optical springs (negative optical inertia) Summary

GWADW2010, May 19, Gingin high optical power test facility High optical power is necessary for improving advanced detector sensitivity, but it also introduces thermal lensing and various instabilities.

GWADW2010, May 19, Gingin high optical power test facility On this facility, we have demonstrated: Thermal lesing and thermal compensation In-situ real time thermal lensing monitoring using Hartmann sensor 3-mode opto-acoustic interactions Cavity locking using ultra-low frequency vibration isolators Current main focus: parametric instability and its control

GWADW2010, May 19, Future 80m interferometer M1 M2 M3 To Detector Bench South Fabry-Perot Cavity East Fabry-Perot Cavity Mode Cleaner Nd:YAG laser = 1064nm East-end Station South-end Station N N Signal Recycling Mirror Beam Splitter Power Recycling Cavity

GWADW2010, May 19, Currently, 2 independent 80m cavities South arm: Sapphire test masses with LIGO SOS suspension Finesse, ~1300, 10 W laser Tested thermal lensing and thermal compensation; Observed 3-mode opto-acoustic interactions; Study 3-mode optomechanical transducer. East arm: Fused silica test masses with UWA isolators and suspensions Nominal cavity finesse, W laser to be installed in August Main goals are test the parametric instability and its control.

GWADW2010, May 19, mode optomechanical transducer Test mass internal mode  m Cavity Fundamental mode (TEM 00, frequency  o ) Input light frequency  o Scattering into TEM mn, frequency  1 frequency matching and spatial overlap of acoustic and optical modes

GWADW2010, May 19, FSR   TEM 3-mode optomechanical transducer 00  0 +  m  TEM

GWADW2010, May 19, CO 2 laser thermal tuning the radius of curvature Sapphire test mass Hartmann sensor He-Ne laser CO 2 laser Probe beam (800nm) Vacuum tank Vacuum pipe Nd:YAG laser

GWADW2010, May 19, CCD Laser ITM CP ETM Spectrum Analyzer y x QPD Fundamental mode High order mode 3-mode optomechanical transducer CO 2 Laser

GWADW2010, May 19, Test mass thermal noise at ~181.6 kHz 3-mode optomechanical transducer

GWADW2010, May 19, mode optomechanical transducer potential to observe the quantum radiation pressure noise Laser 1mm x 1mm x 50nm The vibration of silicon nitride membrane excites high transverse optical mode QPD Finesse=10,000 Meff=40 ng, T=4 k,  m=2  *200 kHz Qm=10 6 Circulating power= 0.5W Radiation pressure noise ~ thermal mechanical resonance

GWADW2010, May 19, Test mass dynamics with optical springs Motivation: The SQL in terms of GW strain sensitivity: A system with larger mechanical susceptibility (  /m) has smaller SQL than the free mass SQL Y. Chen, et al, LIGO-T v1

GWADW2010, May 19, Test mass dynamics with optical springs Considering the test mass dynamics with double optical springs (DOS) F is the force applied on the test mass, x is the displacement,, Here, s=-i  ;

GWADW2010, May 19, Test mass dynamics with optical springs PM: power recycling mirror; PBS: polarization beam splitter; BS: beam splitter; PD: photodetector; ITM: input test mass; ETM: end test mass. Driving force This is achievable at Gingin with a 3-mirror cavity: The same configuration can also be used to demonstrate the local readout (optical bar)

GWADW2010, May 19, Test mass, m=0.8 kg, cavity length L=80m, cavity circulating power: I 1 = 3kW, I 2 =10kW, Cavity detuning:  1 /2  =200 Hz  2 /2  =-500 Hz Cavity linewidth:  1 /2  =36 Hz;  2 /2  =400 Hz; Test mass dynamics with optical springs Free mass With DOS

GWADW2010, May 19, Summary Gingin high optical power research facility consists: High power lasers Advanced vibration isolators and test mass suspension High finesse cavities In addition to the parametric instability research, we propose to study: High sensitivity optomechanical transducer (potential for detecting the quantum radiation pressure noise) Optical negative inertia Local readout (optical bar)