Polarization Techniques for Interferometer Control Peter Beyersdorf National Astronomical Observatory of Japan LSC March 2002 Advanced Configurations LIGO-G020024-00-Z.

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.
FINESSE FINESSE Frequency Domain Interferometer Simulation Versatile simulation software for user-defined interferometer topologies. Fast, easy to use.
19. October 2004 A. Freise Automatic Alignment using the Anderson Technique A. Freise European Gravitational Observatory Roma
Dual Recycling for GEO 600 Andreas Freise, Hartmut Grote Institut für Atom- und Molekülphysik Universität Hannover Max-Planck-Institut für Gravitationsphysik.
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.
Optics of GW detectors Jo van den Brand
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.
Marcus Benna, University of Cambridge Wavefront Sensing in Dual-Recycled Interferometers LIGO What is Wavefront Sensing? How does it work? –Detection of.
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.
Marcus Benna, University of Cambridge Wavefront Sensing in Dual-Recycled Interferometers LIGO What is Wavefront Sensing? How does it work? –Detection of.
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.
Design of Stable Power-Recycling Cavities University of Florida 10/05/2005 Volker Quetschke, Guido Mueller.
The GEO 600 Detector Andreas Freise for the GEO 600 Team Max-Planck-Institute for Gravitational Physics University of Hannover May 20, 2002.
Interferometer Control Matt Evans …talk mostly taken from…
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.
Modulation techniques for length sensing and control of advanced optical topologies B.W. Barr, S.H. Huttner, J.R. Taylor, B. Sorazu, M.V. Plissi and K.A.
04. November 2004 A. Freise A. Freise, M. Loupias Collaboration Meeting November 04, 2004 Alignment Status.
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.
LIGO- G R Sensing and control, SPIE conference, June Sensing and control of the Advanced LIGO optical configuration SPIE conference at.
Modulators & SHG (a) Longitudinal field; (b) Transverse field; (c) Travelling-wave field.
G Z AJW for Marcus Benna, Cambridge Wavefront Sensing for Advanced LIGO Model of wavefront sensing in a dual- recycled interferometer Consequences.
Advanced Virgo Optical Configuration ILIAS-GW, Tübingen Andreas Freise - Conceptual Design -
LSC-VIRGO joint meeting - Pisa1 Input mirrors thermal lensing effect Frequency modulation PRCL length in Virgo Some results from a Finesse simulation.
Koji Arai – LIGO Laboratory / Caltech LIGO-G v2.
Conversion of the Glasgow 10m Prototype for Detuned Operation Bryan Barr Institute for Gravitational Research University of Glasgow LSC - AIC August 13.
RSE Experiment in Japan Feb. 20 th, 2004 Aspen Meeting LIGO-G Z K.Somiya, O.Miyakawa, P.Beyersdorf, and S.Kawamura.
LIGO- G R Aspen winter conference, January Toward the Advanced LIGO optical configuration investigated in 40meter prototype Aspen winter.
Basic electromagnetics and interference Optics, Eugene Hecht, Chpt 3.
Isola d’Elba, Italy 2006GWADW-VESF meeting Diagonalizing sensing matrix of RSE interferometer Shuichi Sato TAMA project National Astronomical Observatory.
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,
Nov 3, 2008 Detection System for AdV 1/8 Detection (DET) Subsystem for AdV  Main tasks and requirements for the subsystem  DC readout  Design for: the.
LIGO-G D 1 Status of Detector Commissioning LSC Meeting, March 2001 Nergis Mavalvala California Institute of Technology.
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.
First DR FFT Results on Advanced LIGO Using Perfect and Imperfect Optics By Ken Ganezer, George Jennings, and Sam Wiley CSUDH LIGO-G Z by Ken.
Institute for Cosmic Ray Research Univ. of Tokyo Development of an RSE Interferometer Using the Third Harmonic Demodulation LIGO-G Z Osamu Miyakawa,
MOTIVATION OF THIS PROJECT Testing the control scheme with a prototype interferometer to demonstrate the control of the tuned RSE for LCGT is necessary.
Concept and Current Status of Japan 4m RSE March Kentaro Somiya LIGO-G Z.
1 Locking in Virgo Matteo Barsuglia ILIAS, Cascina, July 7 th 2004.
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.
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.
LIGO-G Z 3) Current Status & Plan for Japan RSE -- Stabilization and Installation of PRC & Detuning -- LSC Livingston 2002 Kentaro Somiya.
Stefan Hild 1GWADW, Elba, May 2006 Experience with Signal- Recycling in GEO 600 Stefan Hild, AEI Hannover for the GEO-team.
1 ILIAS WG1 meeting, Hannover The 2 nd modulation frequency project.
1 Fumiko 2006 Elba Meeting Current status of the 4m RSE.
Testing Advanced LIGO length sensing and control scheme at the Caltech 40m interferometer. at the Caltech 40m interferometer. Yoichi Aso*, Rana Adhikari,
Interferometer configurations for Gravitational Wave Detectors
Peter Beyersdorf TAMA300 Results from the Stanford 10m all-reflective polarization Sagnac interferometer Peter Beyersdorf TAMA300.
A look at interferometer topologies that use reflection gratings
Status report of Polarization RSE
Design of Stable Power-Recycling Cavities
Homodyne readout of an interferometer with Signal Recycling
Heterodyne Readout for Advanced LIGO
Homodyne or heterodyne Readout for Advanced LIGO?
Workshop on Gravitational Wave Detectors, IEEE, Rome, October 21, 2004
Heterodyne Readout for Advanced LIGO
Modeling of Advanced LIGO with Melody
Effect of sideband of sideband on 40m and Advanced LIGO
Advanced LIGO optical configuration investigated in 40meter prototype
Elliptical polarization
Advanced Virgo ISC subsystem
Presentation transcript:

Polarization Techniques for Interferometer Control Peter Beyersdorf National Astronomical Observatory of Japan LSC March 2002 Advanced Configurations LIGO-G Z

Outline Motivation Introduction to basic polarization techniques Some uses of these techniques Examples –Locking of a Ring Mode Cleaner –Generating multiple sidebands –Creating a “single sideband” My plans to use these techniques with RSE –Getting a LO for SEC past the power recycling mirror –An RSE interferometer with only 4 degrees of freedom Conclusion

Motivation for this talk Since the interferometers we work with have many constraints, having an extra degree of freedom (polarization) can greatly simplify the design. Despite this I’ve found that many gravity wave interferometer experts are not familiar with polarization techniques.

Motivation for this talk Since the interferometers we work with have many constraints, having an extra degree of freedom (polarization) can greatly simplify the design. Despite this I’ve found that many gravity wave interferometer experts are not familiar with polarization techniques.

Motivation for this talk Since the interferometers we work with have many constraints, having an extra degree of freedom (polarization) can greatly simplify the design. Despite this I’ve found that many gravity wave interferometer experts are not familiar with polarization techniques. frequency Pound-Drever-Hall locking frontal modulation

Motivation for this talk Since the interferometers we work with have many constraints, having an extra degree of freedom (polarization) can greatly simplify the design. Despite this I’ve found that many gravity wave interferometer experts are not familiar with polarization techniques. phase Pound-Drever-Hall locking frontal modulation

Motivation for this talk Since the interferometers we work with have many constraints, having an extra degree of freedom (polarization) can greatly simplify the design. Despite this I’ve found that many gravity wave interferometer experts are not familiar with polarization techniques. spatial profile

Motivation for this talk Since the interferometers we work with have many constraints, having an extra degree of freedom (polarization) can greatly simplify the design. Despite this I’ve found that many gravity wave interferometer experts are not familiar with polarization techniques. polarization

Motivation for this talk Since the interferometers we work with have many constraints, having an extra degree of freedom (polarization) can greatly simplify the design. Despite this I’ve found that many gravity wave interferometer experts are not familiar with polarization techniques. frequency phase spatial profile polarization

Basic polarization techniques  p-polarization s-polarization ApAsApAs EOM 1 EOM 2  PBS 1. Detection of phase difference between cross-polarized beams 2. Make interferometers with fewer degrees of freedom (only 1 beam path!) 3. Shift the transmission spectrum of a cavity to get an arbitrary sideband through 4. Switch between different values of cavity finesse  +-+-

Uses of polarization techniques Lock a cavity without modulation sidebands Transmit arbitrary frequency components through cavities Eliminate degrees of freedom of interferometer by overlaying multiple cavities Simplify lock acquisition by lowering the finesse of cavities

Locking a RMC Transmission of cavity  X frequency Transmission p-polarization s-polarization  PBS Polarization of input light +I P.D.H. input spectrum Pound-Drever-Hall method polarization method

Multiple Sideband Generation frequency Mach-Zender configuration EOM 1 EOM 2 EOM 1 EOM 2  polarization configuration PBS Multiple, non-cascaded sideband pairs are useful for IFO control. How can this frequency spectrum be created?

Passing arbitrary frequency sidebands through cavities p-polarization s-polarization A birefringent element inside of an interferometer (i.e. a cavity) will shift the transmission spectrum of one polarization state relative to the other. The amount of the shift is set by the round-trip birefringence . Examples of suitable birefringent elements include: For Cavities Waveplates Sapphire substrates Mirrors at non-normal incidence For a Michelson Unbalanced beamsplitters + asymmetric arm lengths  =0   cavity transmission spectrum

Single Sideband Generation EOM 1 EOM 2  1. Take linear p-polarization and rotate it a few degrees 2. Add sidebands to the p-carrier at f p = m x FSR 3. Convert the s-carrier to sidebands at f s = (n+  ) x FSR 4. Lock RMC to carrier (can use reflected s-sideband as LO!) 

My plans for polarization RSE For current research: Improve control signals of power recycled RSE interferometer at NAOJ by using an orthogonally polarized pair of 2 nd order sidebands. For fun: Remove SEC degree of freedom by folding SEC onto power recycling cavity.

Third-Harmonic Demodulation for RSE control Control of the RSE cavity using THD - 2 nd order sidebands reflect from the RSE cavity - 1 st order sidebands resonate in the RSE cavity frequency Input spectrum Signal Extraction Cavity

Third-Harmonic Demodulation for Power-recycled RSE control Control of the RSE cavity using THD is problematic 2 nd order sidebands are suppressed by P.R. cavity - 1 st order sidebands resonate in the RSE cavity frequency Input spectrum

Third-Harmonic Demodulation with polarization control for P.R. RSE Control of the RSE cavity using THD & polarization control is possible - 2 nd order s-polarized sidebands resonate in P.R. cavity, but not RSE cavity - 1 st order sidebands resonate in P.R. cavity and the RSE cavity  p-polarization s-polarization quarter-waveplate shifts the P.R. cavity spectrum by 180º P.R. cavity transmission spectrum and input spectrum Control of the Power Recycling cavity using THD is unchanged - 2 nd order p-polarized sidebands reflects from P.R. cavity - 1 st order sidebands resonates in P.R. cavity Signal Extraction Cavity

A polarization RSE interferometer   PBS By using a polarizing beamsplitter for the Michelson the dark port and bright port can be made to overlap – distinguishable by their polarization. This allows the SEC and the PR cavity to share the same path and eliminates 1 degree of freedom of the interferometer. (my plans for a fun table-top experiment)

A polarization RSE interferometer   PBS a)Linear polarized light couples into the interferometer through a low reflectivity window. (my plans for a fun table-top experiment)

A polarization RSE interferometer   PBS b) The polarization is rotated 45 degrees by a half wave plate and separated into two arms based on polairzation (my plans for a fun table-top experiment)

A polarization RSE interferometer   PBS b) The returning light is recombined and rotated -45 degrees by the half wave plate. Differential phase from the michelson makes the returning polarization elliptical. (my plans for a fun table-top experiment)

A polarization RSE interferometer   PBS c) The light is recycled by a recycling mirror. A small amount is coupled out by the window. The power and signal are recycled in the same cavity, so there is one less degree of freedom to control (my plans for a fun table-top experiment)

A polarization RSE interferometer  PBS e) The finesse of the power recycling cavity and the signal extraction cavity can be set independantly because the IO coupling efficiency depends on the angle of incidence and the polarization. The SEC can be tuned by adjusting the birefringence in the cavity (  ).  (my plans for a fun table-top experiment)

A polarization RSE interferometer   PBS e) Control of the interferometer is identical to that of a P.R. F.P. Michelson interferometer with 3 signal extraction ports 1. “reflected” 2. “intra-cavity pickoff” 3. “transmitted” (1) (2) (3) This should be a good demonstration of many of these polarization techniques. Some of them may be applied to the 3m suspended optic interferometer. (my plans for a fun table-top experiment)

Conclusion Polarization control is 1 more degree of freedom for generating interferometer control signals. There are useful applications for polarization control in GW interferometry. –Locking cavities –Tuning cavity transmission spectrum –Overlaying beam paths to simplify alignment and control We plan to use an orthogonally polarized L.O. for the 3m power recycled RSE interferometer.