1 Wan Wu, Volker Quetschke, Ira Thorpe, Rodrigo Delgadillo, Guido Mueller, David Reitze, and David Tanner Noise associated with the EOM in Advanced LIGO.

Slides:



Advertisements
Similar presentations
Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut) HOMODYNE AND HETERODYNE READOUT OF A SIGNAL- RECYCLED GRAVITATIONAL WAVE DETECTOR.
Advertisements

Gravitational Wave Astronomy Dr. Giles Hammond Institute for Gravitational Research SUPA, University of Glasgow Universität Jena, August 2010.
Cascina, January 25th, Coupling of the IMC length noise into the recombined ITF output Raffaele Flaminio EGO and CNRS/IN2P3 Summary - Recombined.
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.
Optical simulation – March 04 1 Optical Simulation François BONDU VIRGO Tools Goals Example: tuning of modulation frequency A few questions.
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.
Caltech 40m Current Issues University of Florida Kentaro Somiya.
Laser Interferometer Gravitational-wave Observatory1 Characterization of LIGO Input Optics University of Florida Thomas Delker Guido Mueller Malik Rakhmanov.
Phase noise measurements in TRIUMF ISAC 2 cryomodule K. Fong, M. Laverty TRIUMF.
TeV Particle Astrophysics August 2006 Caltech Australian National University Universitat Hannover/AEI LIGO Scientific Collaboration MIT Corbitt, Goda,
LIGO-G D Advanced LIGO Systems Design & Interferometer Sensing & Optics Peter Fritschel, LIGO MIT PAC 13 Meeting, 5 June 2003.
G R DC Readout for Advanced LIGO P Fritschel LSC meeting Hannover, 21 August 2003.
RF readout scheme to overcome the SQL Feb. 16 th, 2004 Aspen Meeting Kentaro Somiya LIGO-G Z.
Design of Stable Power-Recycling Cavities University of Florida 10/05/2005 Volker Quetschke, Guido Mueller.
Test mass dynamics with optical springs proposed experiments at Gingin Chunnong Zhao (University of Western Australia) Thanks to ACIGA members Stefan Danilishin.
Interferometer Control Matt Evans …talk mostly taken from…
Amaldi conference, June Lock acquisition scheme for the Advanced LIGO optical configuration Amaldi conference June24, 2005 O. Miyakawa, Caltech.
LIGO-G D Enhanced LIGO Kate Dooley University of Florida On behalf of the LIGO Scientific Collaboration SESAPS Nov. 1, 2008.
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.
Displacement calibration techniques for the LIGO detectors Evan Goetz (University of Michigan)‏ for the LIGO Scientific Collaboration April 2008 APS meeting.
LIGO- G R Telecon on June, Mach-Zender interferometer to eliminate sidebands of sidebands for Advanced LIGO Osamu Miyakawa, Caltech.
Enhanced LIGO with squeezing: Lessons Learned for Advanced LIGO and beyond.
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.
G Z LIGO R&D1 Input Optics Definition, Function The input optics (IO) conditions light from the pre- stabilized laser (PSL) for injection into.
LIGO- G R Sensing and control, SPIE conference, June Sensing and control of the Advanced LIGO optical configuration SPIE conference at.
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 -
LIGO-G Z Guido Mueller University of Florida For the LIGO Scientific Collaboration ESF Exploratory Workshop Perugia, Italy September 21 st –23.
Advanced LIGO Sensing and Control Readout schemes for Advanced LIGO K.A. Strain University of Glasgow G & G
LIGO- G R Aspen winter conference, January Toward the Advanced LIGO optical configuration investigated in 40meter prototype Aspen winter.
Split Electrode Wedged RTP crystal To avoid the unwanted generation of amplitude modulation by polarization modulation because of imperfect alignment of.
LIGO-G R High power optical components for Enhanced and Advanced LIGO Optics/Lasers WG, March 21, 2007 Volker Quetschke, Muzammil Arain, Rodica.
AIGO 2K Australia - Italy Workshop th October th October 2005 Pablo Barriga for AIGO group.
08/24/2004 Stefan Ballmer, MIT / LIGO Hanford G I 1 Hanford 4km Recent improvements and currently limiting noise sources Stefan Ballmer Massachusetts.
Stefan Hild 111th WG1 meeting, Hannover, January 2007 DC-Readout for GEO Stefan Hild for the GEO-team.
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.
THE INPUT OPTICS OF ENHANCED AND ADVANCED LIGO D.B. Tanner, M.A. Arain, A. Lucianetti, R.M. Martin, V. Quetschke, L.F. Williams, Wan Wu, G. Mueller, and.
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 40m/AdLIGO, LSC, August Issues in sensing and control of the 40m and Advanced LIGO optical configuration LSC meeting, August.
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.
1 ILIAS WG1 meeting, Hannover The 2 nd modulation frequency project.
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.
White light Cavities University of Florida LIGO-G Z Stacy Wise, Guido Mueller, David Reitze, D.B. Tanner, California Institute of Technology April.
Laser Adaptive Optics for Advanced LIGO
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,
Complex Optical Modulation Volker Quetschke, Guido Mueller, David Reitze, David Tanner an extension of work done at UF for LIGO in 1997 by Qi-Ze Shu Department.
H1 Squeezing Experiment: the path to an Advanced Squeezer
The Proposed Holographic Noise Experiment
Progress toward squeeze injection in Enhanced LIGO
The LIGO input optics D.B. Tanner, M.A. Arain, A. Lucianetti, R. Martin, V. Quetschke, L.F. Williams, Wan Wu, G. Mueller, and D.H. Reitze University.
Output Mode Cleaners: Introduction for non-experts
The Advanced LIGO Angular Control System (ASC) (Hanford edition)
Design of Stable Power-Recycling Cavities
Heterodyne Readout for Advanced LIGO
Quantum effects in Gravitational-wave Interferometers
Homodyne or heterodyne Readout for Advanced LIGO?
Squeezed states in GW interferometers
Workshop on Gravitational Wave Detectors, IEEE, Rome, October 21, 2004
Heterodyne Readout for Advanced LIGO
A RTP crystal electro-optic modulator for next generation gravitational wave detector Wan Wu, Volker Quetschke, Ira Thorpe, Guido Mueller, David Reitze,
“Traditional” treatment of quantum noise
Advanced LIGO optical configuration investigated in 40meter prototype
Squeezed Light Techniques for Gravitational Wave Detection
RF readout scheme to overcome the SQL
Enhanced LIGO Modulator Supported by NSF grant PHY
Advanced Optical Sensing
Presentation transcript:

1 Wan Wu, Volker Quetschke, Ira Thorpe, Rodrigo Delgadillo, Guido Mueller, David Reitze, and David Tanner Noise associated with the EOM in Advanced LIGO Physics Department University of Florida Gainesville, FL Supported by NSF PHY

2 Laser noise coupling The coupling of laser noise to the readout signals arises through two mechanisms : 1. Loss difference of arm cavities ( at high frequencies ) 2. Technical radiation pressure noise ( at low frequencies ) Requirement on the laser amplitude and phase noise. The coupling effect in the DC sensing scheme is highly dependent on the readout phase ( K. Somiya, Y. Chen, S. Kawamura, and N. Mio, Phys. Rev. D, 2006) By choosing a proper readout quadrature, laser intensity noise (~ ) and laser phase noise (~ at 100 Hz) will not be a problem EOM produces additional amplitude and phase noises on the transmitted light

3 EOM to be placed in Advanced LIGO Signal recycling cavity SRM BS ETM ITM Mode Cleaner EOM PRM ETM Noise due to the Mach-Zehnder configuration not discussed here

4 Noise generation mechanism I Variation of modulation index changes the amplitude of both the carrier and the sidebands RF modulation on the laser: Carrier Sidebands Carrier light circulates inside the arm cavities and the power imbalance leads to the technical radiation pressure noise. modulation index (Guido Mueller, LIGO T )

5 Noise generation mechanism II Misalignment of the EOM imposes a phase retardation (Δ  ) between the linear polarized light orthogonal components – along the e-axis and along the o-axis of the crystal. ( S. Kawamura, A. Abramovici and M.E. Zucker, Rev.Sci.Inst, 1997 )

6 Fluctuation of Δ  in the gw band Phase noise on the light Residual amplitude modulation (laser amplitude noise) phase retardation Noise generation mechanism II

7 l Fabry-Perot cavity effect due to the reflectivity of the front and end surfaces of the crystal. Noise generation mechanism III Possible amplitude change due to the 0.2% reflectivity

8 Measurement of the intrinsic EOM noise Nd:YAG EOM PLL Phase meter f 1 f 2 Phase lock two lasers with a frequency offset Phase lock two lasers with a frequency offset Measure the beat signals – Carrier-Carrier (C-C), Carrier-Sideband (C-S) Measure the beat signals – Carrier-Carrier (C-C), Carrier-Sideband (C-S)

9 Phase meter Phase meter is the DSP instrument to have the I/Q measurement on the RF signals - developed by UF LISA group MHz sampling frequency - time series measurement on the mixture of signals - output amplitude and unwrapped phase Advantage we gain: Avoid using diode mixers!

10 Amplitude noise & phase noise

11 Noise in the beat notes Beam jitter between two laser beams Laser intensity noise Noise in two beat signals (C-C, C-S) in common mode Noise in two beat signals in differential mode (amplitude & phase noise) - produced by the EOM Common mode noise rejection analysis Amplitude Phase

12 Data analysis

13 Data analysis

14 recommendation Two important factors: n and L Acoustic vibration could also change the length of the crystal L. Temperature effect: Need temperature stabilization and possibly acoustic isolation Test a modulator made of wedged crystal.