1 Fumiko 2006 Elba Meeting Current status of the 4m RSE.

Slides:



Advertisements
Similar presentations
Gravitational Wave Astronomy Dr. Giles Hammond Institute for Gravitational Research SUPA, University of Glasgow Universität Jena, August 2010.
Advertisements

19. October 2004 A. Freise Automatic Alignment using the Anderson Technique A. Freise European Gravitational Observatory Roma
Cascina, January 25th, Coupling of the IMC length noise into the recombined ITF output Raffaele Flaminio EGO and CNRS/IN2P3 Summary - Recombined.
Polarization Techniques for Interferometer Control Peter Beyersdorf National Astronomical Observatory of Japan LSC March 2002 Advanced Configurations LIGO-G Z.
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.
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.
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.
Koji Arai – LIGO Laboratory / Caltech LIGO-G v1.
Virgo Control Noise Reduction
GWADW 2010 in Kyoto, May 19, Development for Observation and Reduction of Radiation Pressure Noise T. Mori, S. Ballmer, K. Agatsuma, S. Sakata,
40m Laboratory Progress Report LSC meeting at LIGO Hanford Observatory
Several Fun Research Projects at NAOJ for the Future GW Detectors
LIGO-G R Aspen Current Status of the 40m Detuned RSE Prototype Seiji Kawamura 2004 Aspen Winter Conference on Gravitational Waves Gravitational.
Interferometer Control Matt Evans …talk mostly taken from…
Stefan Hild October 2007 LSC-Virgo meeting Hannover Interferometers with detuned arm cavaties.
1 1.ISC scope and activities 2.Initial Virgo status 3.Design requirements 4.Reference solution and design status 5.Plans toward completion 6.Technical.
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.
LIGO-G Z 2) Accomplishment of Japan RSE '98-'01 -- Result of Osamu’s RSE Experiments -- LSC Livingston 2002 Kentaro Somiya University.
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.
LIGO- G R Sensing and control, SPIE conference, June Sensing and control of the Advanced LIGO optical configuration SPIE conference at.
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.
Isola d’Elba, Italy 2006GWADW-VESF meeting Diagonalizing sensing matrix of RSE interferometer Shuichi Sato TAMA project National Astronomical Observatory.
LIGO- G R LIGO seminar, November Optical spring and optical resonance in the 40m Detuned RSE interferometer LIGO seminar November 1, 2005.
AIGO 2K Australia - Italy Workshop th October th October 2005 Pablo Barriga for AIGO group.
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.
Institute for Cosmic Ray Research Univ. of Tokyo Development of an RSE Interferometer Using the Third Harmonic Demodulation LIGO-G Z Osamu Miyakawa,
LIGO- G R 40m weekly meeting, Jan 05, Explore demodulation phase for DDM on 40m RSE prototype Osamu Miyakawa, Caltech LIGO-G R.
1 Development schedule of Static IFO Simulation (SIS) Basic building blocks »Framework »mirror, cavity or propagator, detector FP cavity »Simple locking,
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.
LIGO-G Z March 2007, LSC meeting, Osamu Miyakawa 1 Osamu Miyakawa Hiroaki Yamamoto March 21, 2006 LSC meeting Modeling of AdLIGO arm lock acquisition.
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 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.
Yoichi Aso Columbia University, New York, NY, USA University of Tokyo, Tokyo, Japan July 14th th Edoardo Amaldi Conference on Gravitational Waves.
Testing Advanced LIGO length sensing and control scheme at the Caltech 40m interferometer. at the Caltech 40m interferometer. Yoichi Aso*, Rana Adhikari,
Current Status of Main Interferometer Design Yoichi Aso 2011/2/4, LCGT f2f Meeting.
Main Interferometer Subsystem
H1 Squeezing Experiment: the path to an Advanced Squeezer
Interferometer configurations for Gravitational Wave Detectors
Main Interferometer Subsystem
Demonstration of lock acquisition and optical response on
GEO600 Control aspects where do the error signal come from?
A study of Arm Length Stabilization in KAGRA
Status report of Polarization RSE
Yoichi Aso on behalf of the LCGT ISC Group
The Advanced LIGO Angular Control System (ASC) (Hanford edition)
Heterodyne Readout for Advanced LIGO
Homodyne or heterodyne Readout for Advanced LIGO?
Current Status of the 40m Detuned RSE Prototype
Workshop on Gravitational Wave Detectors, IEEE, Rome, October 21, 2004
Heterodyne Readout for Advanced LIGO
40m Laboratory Upgrade Progress Report
Effect of sideband of sideband on 40m and Advanced LIGO
Advanced LIGO optical configuration investigated in 40meter prototype
Estimation of each loop shot noise limit for AdLIGO
Progress report from 40m team for the Advanced LIGO
Homodyne detection: understanding the laser noise amplitude transfer function Jérôme Degallaix Ilias meeting – June 2007.
Presentation transcript:

1 Fumiko 2006 Elba Meeting Current status of the 4m RSE

2 Introduction Control Scheme Experimental Parameters Experimental Setup Current Status Schedule In This Talk

3 To demonstrate LCGT’s control scheme to lock the RSE The Goal What Is 4mRSE A broadband (tuned) power-recycled RSE interferometer, prototype of LCGT interferometer, built inside NAOJ’s campus Introduction

4 L+ = (Lx + Ly) / 2 L- = (Lx – Ly) / 2 lp = (lx + ly) / 2 l- = (lx – ly) / 2 ls = (lsx + lsy)/2 Degrees of Freedom lsy PRM SEM LASER lsx ly lx Ly Lx BS ITMxETMx ITMy

5 Control Scheme PM(f1) AM(f1) l- LASER Diff.(f2-f1) ls lp SEM PRM BS L- L+

6 Michelson Asymmetry Recycling Cavity Lengths Sideband Frequencies Other Parameters Experimental Parameters

7 Michelson Asymmetry dl AM reflect from Michelson PM transmit through Michelson dl = (ly – lx)= 3.5m dl /λ f PM (17.25MHz) f AM (103.5MHz) 1/2 3 lx PM AM SEM PRM ly PM AM SEM PRM ly lx

8 Recycling Cavity Lengths Length P ower R ecycling C avity 4.34 m S ignal E xtraction C avity 4.34 m f2 Carrier Transmission curves of PRC and SEC Carrier PRC SEC f1 (17.25MHz)(103.5MHz) f1 (17.25MHz)

9 Sideband Frequencies f2= n × f1 n = 6 f1f2Ca. Beat between carrier and f1 Beat between f1 and f2 Mix if n= 2 f2 When n = 6 4 th order of the f1 sidebands…small enough Clear beat signal between f1&f2 f2 f1Ca.

10 Other Parameters Arm finesse122 Power recycling gain15 Arm length4.05m

11 Mach-Zehnder To avoid SBs of SBs f2 Ca. f2 Ca. f1 f2 f1 EOM f1f2 Ca. Sidebands of sidebands f1f2 Ca.

12 Current Status FPMI Locked(single demodulation) Redesign of a Suspension System MZ Lock (w/o AM EOM in) Ready for Double Demodulation

13 FPMI Locked PM(f1) L+ l- LASER L- Time(sec ) Power Inline FP Arm Perpendicular FP Arm Michelson

14 Redesign of a Suspension System Q of Picth 15 Q of Yaw 7 l d = l m Damping magnets glued ldld lmlm Actuator magnets close to damping magnets Glue free Far from damping magnets Coupling between Pitch and Yaw fixed Uses Eddy Current Damping Cu mdmd m m d = m m

15 Schedule Lock Michelson on double demodulationJuly August September October November December 2007 Lock Arms with L- from Dark Port Put in Power Recycling Mirror Lock PRFPMI Put in Signal Extraction Mirror Lock full RSE Noise characterization, Test Delocation Scheme

16 Have locked FPMI on single demodulation Redesigned the suspension system Mach-Zehnder locked Double Demodulation getting ready What Has Been Done Control Scheme Single modulation and demodulation for FP arms Double modulation and demodulation for the central part of the IFO Summary