Progress report from 40m team for the Advanced LIGO

Slides:



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

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.
1 Virgo commissioning status M.Barsuglia LAL Orsay.
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 Springs at the 40m 1 QND Workshop, Hannover Dec 14, 2005 Robert Ward for the 40m Team Osamu Miyakawa, Rana Adhikari, Matthew Evans, Benjamin Abbott,
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.
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.
40m Modeling and Experiment 1 Modeling the 40m QND Workshop, Hannover Dec 15, 2005 Robert Ward Seiji Kawamura, Osamu Miyakawa, Hiro Yamamoto, Matthew Evans,
40m TAC, 10/13/05 1 Report to the 40m Technical Advisory Committee October 13, 2005 The 40m Team Ben Abbott, Rana Adhikari, Dan Busby, Jay Heefner, Osamu.
Koji Arai – LIGO Laboratory / Caltech LIGO-G v1.
GWADW 2010 in Kyoto, May 19, Development for Observation and Reduction of Radiation Pressure Noise T. Mori, S. Ballmer, K. Agatsuma, S. Sakata,
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.
LIGO- G R 40m Progress, LSC meeting, Aug m Laboratory Upgrade Progress Report Osamu Miyakawa, Caltech 40m Technical Advisory Committee.
LIGO-G R Aspen Current Status of the 40m Detuned RSE Prototype Seiji Kawamura 2004 Aspen Winter Conference on Gravitational Waves Gravitational.
Stefan Hild October 2007 LSC-Virgo meeting Hannover Interferometers with detuned arm cavaties.
LIGO- G R 40m Progress, LSC meeting, 3/031 40m Laboratory Upgrade Progress Report Osamu Miyakawa, Caltech 40m Technical Advisory Committee LIGO-G R.
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 Virgo commissioning: Next steps December 12 st 2005 Hannover, ILIAS-GWA WG1 Matteo Barsuglia, LAL/CNRS.
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.
1 Virgo Commissioning progress ILIAS, Nov 13 th 2006 Matteo Barsuglia on behalf of the Commissioning Team.
Advanced Virgo Optical Configuration ILIAS-GW, Tübingen Andreas Freise - Conceptual Design -
G D Commissioning Progress and Plans Hanford Observatory LSC Meeting, March 21, 2005 Stefan Ballmer.
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:
LIGO- G R Aspen winter conference, January Toward the Advanced LIGO optical configuration investigated in 40meter prototype Aspen winter.
Robert Ward NAOJ seminar, March 1, The Caltech 40m Prototype Detuned RSE Interferometer Robert Ward NAOJ seminar March 1, 2006 Osamu Miyakawa, Rana.
LIGO- G R LIGO seminar, November Optical spring and optical resonance in the 40m Detuned RSE interferometer LIGO seminar November 1, 2005.
LIGO- G R 40m Progress, LSC meeting, 8/021 40m Laboratory Upgrade Progress Report Dennis Ugolini, Caltech 40m Technical Advisory Committee LIGO-G R.
LIGO-G R DC Detection at the 40m Lab Plans for DC Readout Experiment at the 40m Lab Alan Weinstein for the 40m Lab July 19, 2005 Ben Abbott, Rana.
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.
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.
LIGO- G R LSC meeting at LSU, August Caltech 40m Lab Update LSC meeting at LSU Aug 16, 2006 Robert Ward, Caltech and the 40m team: Rana.
Aligning Advanced Detectors L. Barsotti, M. Evans, P. Fritschel LIGO/MIT Understanding Detector Performance and Ground-Based Detector Designs LIGO-G
LIGO- G R 40m weekly meeting, Jan 05, Explore demodulation phase for DDM on 40m RSE prototype Osamu Miyakawa, Caltech LIGO-G R.
Jan 17th 2006Ward Candicacy1 Length Sensing and Control for an Advanced Gravitational Wave Detector Robert Ward PhD Candidacy Caltech, 17 Jan 2006.
1 Locking in Virgo Matteo Barsuglia ILIAS, Cascina, July 7 th 2004.
LIGO- G Z LSC meeting at Baton Rouge, March Caltech 40m Lab Update LSC Meeting Baton Rouge Mar 21, 2007 Robert Ward, Caltech and the 40m.
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 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.
GEO Status and Prospects Harald Lück ILIAS / ETmeeting Cascina November 2008.
The Proposed Holographic Noise Experiment Rainer Weiss, MIT On behalf of the proposing group Fermi Lab Proposal Review November 3, 2009.
LIGO- G R Amaldi7 July 14 th, 2007 R. Ward, Caltech 1 Prototyping for eLIGO: Power Recycled Fabry Perot Michelson DARM RF ITMy ITMx BS PRM SRM.
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
Time domain simulation for a FP cavity with AdLIGO parameters on E2E
Main Interferometer Subsystem
The Proposed Holographic Noise Experiment
Demonstration of lock acquisition and optical response on
Time domain simulation for a FP cavity with AdLIGO parameters on E2E
A study of Arm Length Stabilization in KAGRA
Design of Stable Power-Recycling Cavities
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
40m Laboratory Upgrade Progress Report
Effect of sideband of sideband on 40m and Advanced LIGO
Summary of iKAGRA Test Run Mar 25-31, 2016
Advanced LIGO optical configuration investigated in 40meter prototype
Estimation of each loop shot noise limit for AdLIGO
40m TAC Update October 2006 The 40m Team 11 April 2019 G I.
Homodyne detection: understanding the laser noise amplitude transfer function Jérôme Degallaix Ilias meeting – June 2007.
Presentation transcript:

Progress report from 40m team for the Advanced LIGO optical configuration LSC meeting August 15, 2005 O. Miyakawa, Caltech and the 40m collaboration LSC meeting, August 2005

Caltech 40 meter prototype interferometer Objectives Develop lock acquisition procedure of detuned Resonant Sideband Extraction (RSE) interferometer, as close as possible to AdLIGO optical design Characterize noise mechanisms Verify optical spring and optical resonance Develop DC readout scheme Extrapolate to AdLIGO via simulation BS SRM PRM Bright port Dark port X arm Y arm LSC meeting, August 2005

Differences between AdvLIGO and 40m prototype 100 times shorter cavity length Arm cavity finesse at 40m chosen to be = to AdvLIGO ( = 1235 ) Storage time is x100 shorter. Control RF sidebands are 33/166 MHz instead of 9/180 MHz Due to shorter PRC length, less signal separation. LIGO-I 10-watt laser, negligible thermal effects 180W laser will be used in AdvLIGO. Noisier seismic environment in town, smaller stack ~1x10-6m at 1Hz. LIGO-I single pendulum suspensions are used AdvLIGO will use triple (MC, BS, PRM, SRM) and quad (ITMs, ETMs) suspensions. LSC meeting, August 2005

AdLIGO signal extraction scheme ETMy Mach-Zehnder will be installed to eliminate sidebands of sidebands. Only + f2 is resonant on SRC. Unbalanced sidebands of +/-f2 due to detuned SRC produce good error signal for Central part. 4km f2 ITMy PRM ITMx ETMx BS 4km f1 f1 -f1 f2 -f2 Carrier (Resonant on arms) SRM Single demodulation Arm information Double demodulation Central part information Arm cavity signals are extracted from beat between carrier and f1 or f2. Central part (Michelson, PRC, SRC) signals are extracted from beat between f1 and f2, not including arm cavity information. LSC meeting, August 2005

DRMI lock using double demodulation with unbalanced sideband by detuned cavity August 2004 DRMI locked with carrier resonance (like GEO configuration) November 2004 DRMI locked with sideband resonance (Carrier is anti resonant preparing for RSE.) Carrier 33MHz Unbalanced 166MHz Belongs to next carrier Carrier 33MHz 166MHz ITMy ITMx BS PRM SRM OSA DDM PD Typical lock acquisition time : ~10sec Longest lock : 2.5hour LSC meeting, August 2005

All 5 degrees of freedom under controlled with DC offset on L+ loop Both arms locked with DRMI Lock acquisition time ~1 min Lasts ~ 20 min Can be switched to common/differential control L- : AP166 with no offset L+ : Trx+Try with DC offset Yarm lock Xarm lock Arm power Error signal Ideal lock point Offset lock Have started trying to reduce offset from L+ loop But… LSC meeting, August 2005

Progress in last 6 months For the last 6 months , we have been able to control all 5DOF, but with CARM offset. Reducing the CARM offset has been made difficult by technical noise sources. We have spent last 6months reducing them; suspension noise, vented to reduce couplings in ITMX improved diagonalization of all suspensions improved frequency noise with common mode servo automation of alignment and lock acquisition procedures improved DC signals and improved RF signals for lock acquisition. We can now routinely lock all 5 DOFs in a few minutes at night. LSC meeting, August 2005

Lock acquisition procedure towards detuned RSE Low gain High gain Start TrY PDs ITMy 166MHz ITMx 13m MC High gain BS 33MHz PRM TrX PDs Low gain SP33 PO DDM SP166 SRM SP DDM AP166 AP DDM LSC meeting, August 2005

Lock acquisition procedure towards detuned RSE Low gain High gain DRMI TrY PDs done every 10sec Lx =38.55m T =7% Ly=38.55m ITMy 166MHz ITMx 13m MC High gain BS 33MHz PRM TrX PDs Low gain SP33 PO DDM SP166 SRM I SP DDM Q AP166 AP DDM LSC meeting, August 2005

Lock acquisition procedure towards detuned RSE Low gain High gain DRMI + single arm with offset TrY PDs done every 30 seconds Lx =38.55m Finesse=1235 T =7% Ly=38.55m ITMy 166MHz ITMx 13m MC 1/sqrt(TrX) BS High gain 33MHz PRM TrX PDs Low gain PO DDM SP33 SP166 SRM I SP DDM Q AP166 AP DDM LSC meeting, August 2005

Lock acquisition procedure towards detuned RSE 1/sqrt(TrY) Low gain High gain DRMI + 2arms with offset TrY PDs done every 1 minute Lx =38.55m Finesse=1235 T =7% Ly=38.55m ITMy 166MHz ITMx 13m MC 1/sqrt(TrX) BS High gain 33MHz PRM TrX PDs Low gain PO DDM SP33 SP166 SRM I SP DDM Q AP166 AP DDM LSC meeting, August 2005

Lock acquisition procedure towards detuned RSE To CARM Low gain High gain Switching to CARM and DARM control TrY PDs 1/sqrt(TrX)+ 1/sqrt( TrY) (1/sqrt(TrX)- 1/sqrt( TrY)) (1/sqrt(TrX)+ 1/sqrt( TrY)) done every several minutes Lx =38.55m Finesse=1235 T =7% Ly=38.55m To DARM CARM + + ITMy -1 DARM 166MHz ITMx 13m MC High gain BS 33MHz PRM TrX PDs Low gain PO DDM SP33 SP166 SRM I SP DDM Q AP166 AP DDM LSC meeting, August 2005

Lock acquisition procedure towards detuned RSE To CARM Low gain High gain Switching DRMI to DDM TrY PDs 1/sqrt(TrX)+ 1/sqrt( TrY) (1/sqrt(TrX)- 1/sqrt( TrY)) (1/sqrt(TrX)+ 1/sqrt( TrY)) done every several minutes Lx =38.55m Finesse=1235 T =7% Ly=38.55m To DARM CARM + + ITMy -1 DARM 166MHz ITMx 13m MC High gain BS 33MHz PRM TrX PDs Low gain PO DDM SP33 SRM SP166 SP DDM AP166 AP DDM LSC meeting, August 2005

Lock acquisition procedure towards detuned RSE Low gain High gain Switching DARM to RF TrY PDs 1/sqrt(TrX)+ 1/sqrt( TrY) done every 5 minutes Lx =38.55m Finesse=1235 T =7% Ly=38.55m CARM + + ITMy -1 DARM 166MHz ITMx 13m MC High gain BS 33MHz PRM TrX PDs Low gain PO DDM SP33 SRM SP166 SP DDM To DARM AP166 AP DDM AP166/(TrX+TrY) LSC meeting, August 2005

Lock acquisition procedure towards detuned RSE Low gain High gain Switching CARM feedback to MC length TrY PDs 1/sqrt(TrX)+ 1/sqrt( TrY) Done every 10 minutes Lx =38.55m Finesse=1235 T =7% Ly=38.55m To CARM -1 DARM ITMy 166MHz ITMx 13m MC High gain BS 33MHz PRM TrX PDs Low gain PO DDM SP33 SRM SP166 SP DDM To DARM AP166 CARM AP DDM AP166/(TrX+TrY) LSC meeting, August 2005

Lock acquisition procedure towards detuned RSE Low gain High gain Switching CARM to RF signal TrY PDs In progress Lx =38.55m Finesse=1235 T =7% Ly=38.55m -1 DARM ITMy 166MHz ITMx 13m MC High gain BS SP166 33MHz PRM TrX PDs Low gain PO DDM SP33 SRM SP DDM To DARM SP166/(TrX+TrY) AP166 AP DDM AP166/(TrX+TrY) LSC meeting, August 2005

Lock acquisition procedure towards detuned RSE Ly=38.55m Finesse=1235 Low gain High gain Reduce CARM offset to Full RSE TrY PDs In Progress Lx =38.55m Finesse=1235 T =7% GPR=14.5 Ly=38.55m -1 DARM ITMy 166MHz ITMx 13m MC High gain BS SP166 33MHz PRM TrX PDs Low gain PO DDM SP33 SRM SP DDM To DARM SP166/(TrX+TrY) AP166 AP DDM AP166/(TrX+TrY) LSC meeting, August 2005

Differential mode of Arm : RSE peak! Common mode of Arm : small offset exists Effectively the same as low power recycling (G=1.4) RSE LSC meeting, August 2005

RSE peak! Optical gain of L- loop No offset on L- loop DARM_IN1/DARM_OUT divided by pendulum transfer function No offset on L- loop ~60pm offset on L+ loop Phase includes time delay of the digital system. Optical resonance of detuned RSE can be seen around the design RSE peak of 4kHz. Q of this peak is about 7. Effectively the same as Full RSE with GPR=1.4 with 1W input laser. Model was calculated by Thomas’s tool. We will be looking for optical spring peak. Design RSE peak ~ 4kHz LSC meeting, August 2005

Peak in CARM loop CARM loop has small offset. Peak started from 1.6kHz and reached to ~450H, then lock was lost. This peak introduces phase delay around unity gain frequency. LSC meeting, August 2005

CARM at 218 pm offset (~locking point) Unity Gain Frequency LSC meeting, August 2005

CARM at 118 pm offset Unity Gain Frequency LSC meeting, August 2005

CARM offset at 59 pm (losing lock) Unity Gain Frequency LSC meeting, August 2005

Dynamic compensative filter for CARM servo by Rob Ward Optical gain of CARM Open loop TF of CARM Optical gain (normalized by transmitted power) shows moving peaks due to reducing CARM offset. We have a dynamic compensative filter having an exactly the same shape as optical gain except for upside down. Open loop transfer function has no phase delay in all CARM offset. LSC meeting, August 2005

How large is the CARM offset? Evaluation of power recycling gain Design Measured(calculated) Cavity reflectivity 93% 85%(X arm 84%, Yarm 86%) PRM reflectivity 93% 92.2% Loss in PRC 0% 2.3% Achievable PRG 14.5 5.0 Coupling Over coupled Under coupled Estimated actual power in arms with 1W input and smallest CARM offset achieved is 0.5kW of ~2kW(25% of the way to full resonance). LSC meeting, August 2005

CARM switching from DC to RF signal E2E simulation by Matthew Evans in June 2005 Simulation verifies that controlled reduction of CARM offset should work. LSC meeting, August 2005

CARM switching from DC to RF signal 1 2 3 4 5 CARM is locked by DC signal with offset Let’s hold CARM feedback signal and mirror speed is zero. Mirror start moving Linear response of DC can bee seen. Linear response of RF can be seen. Power is stored. Error signal RF(SP166) Linear range of DC Linear range of RF DC(1/sqrt(TrX)+1/sqrt( TrY)) 6 Transmitted power GPR=2 This result shows RF(SP166) should work well, but still we have not yet done. GPR=1 Holding CARM signal LSC meeting, August 2005

DC Readout at the 40m DC Readout eliminates several sources of technical noise (mainly due to the RF sidebands): Oscillator phase noise Effects of unstable recycling cavity. The arm-filtered carrier light will serve as a heavily stabilized local oscillator. Perfect spatial overlap of LO and GW signal at PD. DC Readout has the potential for QND measurements, without major modifications to the IFO. We may not be able to see shot noise at low frequency, given our noise environment. We may not even see any noise improvements, but we might! The most important thing we will learn is : How to do it How to lock it? How best to control the DARM offset? What are the unforeseen noise sources associated with an in-vacuum OMC? How do we make a good in-vac photodiode? What unforeseen noise sources are associated with it? LSC meeting, August 2005

Output Optical Train SRM BSC OOC IOC Mike Smith 1st PZT steering mirror gets a little tight around IMMT SRM 2nd PZT steering mirror BSC OOC IOC Mike Smith LSC meeting, August 2005

Output Optic Chamber to OMCR beamline from SRM to OMCT beamline 2nd PZT steering mirror PZT steering mirrors and their controls are duplicates of a pair that we have already installed and commissioned for steering from IMC to main IFO (in-vac); controls are fully implemented in the ASC system (by Rolf). Similar systems can be used for “LIGO I.V”. Piezosystem Jena PSH 5/2 SG-V, PZT tilting mirror mount with strain gauge, and associated drivers and power supplies to OMCT beamline IMCR, IMCT, and SP beamlines to ASRF beamline (roughly 1/3 of AS power) also a convenient path for autocollimator beam, for initial alignment in air from PSL to IMC LSC meeting, August 2005 Mike Smith

OMMT layout Primary radius of curvature, mm 618.4 Secondary radius of curvature, mm 150 Defocus, mm 6.3 Input beam waist, mm 3.03 Output beam waist, mm 0.38 Make mirror(s) by coating a cc lens to get larger selection of ROC Mike Smith LSC meeting, August 2005

Two in-vac DC PDs OMCT two DC PDs beamsplitter lens beam dump to OMCT beamline Ben Abbott has designed an aluminum stand to hold a bare photodiode, and verified that the block can radiate 100 mW safely. A small amplifier circuit will be encased in the stand, and vacuum-sealed with an inert, RGA detectable gas. Two such assemblies will be mounted together with a 50:50 beamsplitter to provide in-loop and out-of-loop sensors. LSC meeting, August 2005

OMC, four mirror design Mike Smith From MMT reflected beam SS fixed spacer ~ 20 cm PZT mirror mechanical clamps (no glue) Mike Smith to DCPD Mirrors mounted mechanically, on 3 points (no glue) curved mirror: off-the-shelf CVI laser mirror with ROC = 1 m ± 0.5% Fixed spacer should be rigid, vented, offset from table OMC length signal: Dither-lock? >> Should be simple; we’ll try this first. PDH reflection? >> There’s only one sideband, but it will still work. Servo: Will proceed with a simple servo, using a signal generator and a lock-in amp. Feedback filters can easily be analog or digital. Can use a modified PMC servo board for analog. Can use spare ADC/DAC channels in our front end IO processor for digital. PZT actuation LSC meeting, August 2005