Homodyne detection: understanding the laser noise amplitude transfer function Jérôme Degallaix Ilias meeting – June 2007.

Slides:



Advertisements
Similar presentations
Stefan Hild for the GEO600 team October 2007 LSC-Virgo meeting Hannover Homodyne readout of an interferometer with Signal Recycling.
Advertisements

Beyond The Standard Quantum Limit B. W. Barr Institute for Gravitational Research University of Glasgow.
Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut) HOMODYNE AND HETERODYNE READOUT OF A SIGNAL- RECYCLED GRAVITATIONAL WAVE DETECTOR.
Gravitational Wave Astronomy Dr. Giles Hammond Institute for Gravitational Research SUPA, University of Glasgow Universität Jena, August 2010.
19. October 2004 A. Freise Automatic Alignment using the Anderson Technique A. Freise European Gravitational Observatory Roma
Stefan Hild, M.Mantovani, A.Perreca and A. Freise Advanced Virgo meeting, August 2008 Automated simulations: choosing modulation frequencies à la Advanced.
Dual Recycling for GEO 600 Andreas Freise, Hartmut Grote Institut für Atom- und Molekülphysik Universität Hannover Max-Planck-Institut für Gravitationsphysik.
Status of the Virgo Commissioning G.Losurdo – INFN Firenze/Urbino for the Virgo Collaboration.
Cascina, January 25th, Coupling of the IMC length noise into the recombined ITF output Raffaele Flaminio EGO and CNRS/IN2P3 Summary - Recombined.
Optics of GW detectors Jo van den Brand
LIGO NSF review, 11/10/05 1 AdLIGO Optical configuration and control Nov 10, 2005 Alan Weinstein for AdLIGO Interferometer Sensing and Control (ISC) and.
Stefan Hild and A.Freise Advanced Virgo meeting, December 2008 Preliminary Thoughts on the optimal Arm Cavity Finesse of Advanced Virgo.
Optical simulation – March 04 1 Optical Simulation François BONDU VIRGO Tools Goals Example: tuning of modulation frequency A few questions.
Caltech 40m Current Issues University of Florida Kentaro Somiya.
LIGO-G W Where Did the LSC Signals Come From? Fred Raab 27 June 02.
LIGO- G05XXXX-00-R 40m meeting, May Experimental update from the 40m team 40m TAC meeting May 13, 2005 O. Miyakawa, Caltech and the 40m collaboration.
40m TAC, 10/13/05 1 Lock acquisition procedure towards detuned RSE Start with no DOFs controlled, all optics aligned. Re-align each 1.5 hours. ITMy ITMx.
Koji Arai – LIGO Laboratory / Caltech LIGO-G v1.
Towards dual recycling with the aid of time and frequency domain simulations M. Malec for the GEO 600 team Max-Planck-Institut für Gravitationsphysik Albert-Einstein-Institut.
Stefan Hild 1ILIAS WG1 meeting, Cascina, November 2006 Comparison of tuned and detuned Signal-Recycling Stefan Hild for the GEO-team.
G R DC Readout for Advanced LIGO P Fritschel LSC meeting Hannover, 21 August 2003.
Joshua Smith December 2003 Detector Characterization of Dual-Recycled GEO600 Joshua Smith for the GEO600 team.
Degeneracy for power-recycling and signal recycling cavities in Advanced Virgo.
Stefan Hild October 2007 LSC-Virgo meeting Hannover Interferometers with detuned arm cavaties.
GEO‘s experience with Signal Recycling Harald Lück Perugia,
Amaldi conference, June Lock acquisition scheme for the Advanced LIGO optical configuration Amaldi conference June24, 2005 O. Miyakawa, Caltech.
1 Experiences and lessons learned from interferometer simulations at GEO GWADW, Andreas Freise for Hartmut Grote, Holger Wittel and the rest.
Squeezed light and GEO600 Simon Chelkowski LSC Meeting, Hannover.
LIGO- G R Telecon on June, Mach-Zender interferometer to eliminate sidebands of sidebands for Advanced LIGO Osamu Miyakawa, Caltech.
LIGO- G R Amaldi7 July 14 th, 2007 R. Ward, Caltech 1 DC Readout Experiment at the Caltech 40m Laboratory Robert Ward Caltech Amaldi 7 July 14.
Variable reflectivity signal-recycling mirror and control Stefan Goßler for the experimental team of The ANU Centre of Gravitational Physics.
Koji Arai – LIGO Laboratory / Caltech LIGO-G v2.
RSE Experiment in Japan Feb. 20 th, 2004 Aspen Meeting LIGO-G Z K.Somiya, O.Miyakawa, P.Beyersdorf, and S.Kawamura.
1 1.Definition 2.Deliverables 3.Status of preliminary design 4.Risks 5.Tasks to be done 6.Decisions to be taken 7.Required simulations 8.Planning ISC workshop:
S. ChelkowskiSlide 1WG1 Meeting, Birmingham 07/2008.
AIGO 2K Australia - Italy Workshop th October th October 2005 Pablo Barriga for AIGO group.
Dual Recycling in GEO 600 H. Grote, A. Freise, M. Malec for the GEO600 team Institut für Atom- und Molekülphysik University of Hannover Max-Planck-Institut.
Stefan Hild 111th WG1 meeting, Hannover, January 2007 DC-Readout for GEO Stefan Hild for the GEO-team.
Paolo La Penna ILIAS N5-WP1 meeting Commissioning Progress Hannover, July 2004 VIRGO commissioning progress report.
Institute for Cosmic Ray Research Univ. of Tokyo Development of an RSE Interferometer Using the Third Harmonic Demodulation LIGO-G Z Osamu Miyakawa,
Aligning Advanced Detectors L. Barsotti, M. Evans, P. Fritschel LIGO/MIT Understanding Detector Performance and Ground-Based Detector Designs LIGO-G
1 DC readout for Virgo+? E. Tournefier WG1 meeting, Hannover January 23 rd,2007 DC vs AC readout: technical noises Output mode cleaner for DC readout.
Monica VarvellaIEEE - GW Workshop Roma, October 21, M.Varvella Virgo LAL Orsay / LIGO CalTech Time-domain model for AdvLIGO Interferometer Gravitational.
LIGO-G R DC Detection at the 40m Lab DC Detection Experiment at the 40m Lab Robert Ward for the 40m Lab to the AIC group Livingston LSC meeting.
Joshua Smith July 2004 Identifying limiting noise sources of GEO600 ILIAS WG1 Meeting Joshua Smith for the GEO team.
FINESSE FINESSE Frequency Domain Interferometer Simulation Andreas Freise European Gravitational Observatory 17. March 2004.
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.
ET-ILIAS_GWA joint meeting, Nov Henning Rehbein Detuned signal-recycling interferometer unstableresonance worsesensitivity enhancedsensitivity.
Testing Advanced LIGO length sensing and control scheme at the Caltech 40m interferometer. at the Caltech 40m interferometer. Yoichi Aso*, Rana Adhikari,
Main Interferometer Subsystem
H1 Squeezing Experiment: the path to an Advanced Squeezer
Interferometer configurations for Gravitational Wave Detectors
Detuned Twin-Signal-Recycling
Demonstration of lock acquisition and optical response on
(Some) noise hunting issues at Virgo
GEO600 Control aspects where do the error signal come from?
Nergis Mavalvala Aspen January 2005
Homodyne readout of an interferometer with Signal Recycling
GEO – VIRGO joint noise hunting project
Heterodyne Readout for Advanced LIGO
Homodyne or heterodyne Readout for Advanced LIGO?
Heterodyne Readout for Advanced LIGO
40m Laboratory Upgrade Progress Report
Variable reflectivity signal-recycling mirror and control
“Traditional” treatment of quantum noise
Advanced LIGO optical configuration investigated in 40meter prototype
Progress report from 40m team for the Advanced LIGO
Talk prepared by Stefan Hild AEI Hannover for the GEO-team
Presentation transcript:

Homodyne detection: understanding the laser noise amplitude transfer function Jérôme Degallaix Ilias meeting – June 2007

Going DC Stefan’s talk this morning Laser PRM SRM Carrier local oscillator

Measure the laser intensity noise transfer function Switch off laser power stabilisation loop Inject white noise into the laser pump Record dark port spectrum

Input ? Reflected PRC Laser After laser After MC Reflected BS output

The measured TF

Optical fields FSR = 125 kHz Laser

Optical fields FSR = 125 kHz fMI = 14.9 MHz Laser

Optical fields FSR = 125 kHz fMI = 14.9 MHz fSR = 9.01 MHz Laser

Carrier TF Simple Michelson Flat response due: Arm asymetries Dark fringe offset

Carrier TF With SRM Peak due to SRM

Carrier TF Including the higher order optical modes Increase the amplitude of the TF Flat the response at high frequency

TF with SR sidebands Resonance peak of the sidebands!

TF with SR sidebands

TF with SR sidebands Including the higher order optical modes Shape of the sidebands resonance different!

TF with MI sidebands

TF with MI sidebands Including the higher order optical modes

Changing the PRC FSR A little test to confirm what we understand...

Changing the SRC FSR Another test...

Does it match the experiment ? Adjust the overall gain of the simulated TF Thanks to Andreas for the tuning of the parameters

To sum up... Due to the signal recycling mirror Due to SR sidebands and higher order optical modes Overal magnitude depends of: arm detuning magnitude of higher order optical modes Due to second order optical modes Due to MI sidebands

So ?