Interferometer for LCGT 1st Korea Japan Workshop on Korea University Jan. 13, 2012 Seiji Kawamura (ICRR, Univ. of Tokyo)
|
|
- Virginia Sutton
- 6 years ago
- Views:
Transcription
1 Interferometer for LCGT 1st Korea Japan Workshop on Korea University Jan. 13, 2012 Seiji Kawamura (ICRR, Univ. of Tokyo) JGW G v01
2 Outline Resonant Sideband Extraction interferometer Length sensing and control system Alignment sensing and control system Detuning optimization Curvature of the mirrors Lock acquisition Noise coupling reduction Quantum noise optimization Summary
3 Outline Resonant Sideband Extraction interferometer Length sensing and control system Alignment sensing and control system Detuning optimization Curvature of the mirrors Lock acquisition Noise coupling reduction Quantum noise optimization Summary
4 Interferometer for LCGT Main interferometer Laser Mode cleaner
5 Resonant Sideband Extraction (RSE) interferometer Power recycling Mirror (PRM) Fabry Perot arm cavity Signal Extraction Mirror (SEM) Beam splitter Photodetector
6 Michelson interferometer (MI) The maximum arm length on earth is only a few km. Beam splitter Photodetector
7 Shot noise of MI Strain MI White noise: Statistical fluctuation of photon counting Frequency
8 Fabry Perot Michelson interferometer (FPMI) The effective arm length is increased GW signal is increased Optical configuration for ilcgt Fabry Perot arm cavity resonant High reflectivity low transmissivity
9 Shot noise of FPMI MI Strain FPMI Frequency f 1 frequency dependence Cavity pole: GW signal cancels above this frequency
10 Power recycled Fabry Perot Michelson interferometer (PRFPMI) Power Recycling Mirror (PRM) The effective light power is increased The shot noise is reduced Bright fringe Dark fringe Optical configuration for iligo, Virgo, and TAMA300
11 Shot noise of PRFPMI Strain FPMI PRFPMI Cavity pole frequency does not change Frequency
12 PRFPMI C LSB USB GW sidebands are differentially produced Only the carrier is recycled C LSB LSB C USB USB
13 RSE interferometer The GW signal is frequencydependently extracted before it is cancelled The shot noise is optimized Signal Extraction Mirror (SEM)
14 RSE C LSB USB Only the GW sidebands are affected C SEM LSB C USB LSB USB
15 RSE GW signal sees SEM If the SEC is resonant, the reflectivity of the SEC can be lower than that of input mirror C Signal extraction cavity (SEC) LSB USB
16 RSE Make the finesse of the arm cavity very high to increase the carrier power and extract the GW signal before cancellation by SEM
17 Shot noise of RSE Strain PRFPMI (Low finesse) RSE RSE has more carrier power than PRFPMI (Low finesse) PRFPMI (High finesse) Frequency RSE increases the cavity pole frequency
18 Shot noise of PRFPMI (High recycling gain) PRFPMI (Low finesse, Low recycling gain) Strain PRFPMI (Low finesse, High recycling gain) RSE and PRFPMI (Low finesse High recycling gain) give the same sensitivity Frequency
19 RSE and PRFPMI (Low finesse, High recycling gain) RSE High finesse PRFPMI Low Recycling gain High recycling gain Low finesse Combination of finesse and recycling gain is limited by the loss of the optics the same sensitivity
20 Advantage of RSE (1) RSE PRFPMI Low Recycling gain High finesse High recycling gain Low finesse Lower Power at BS and Input Mirrors Less Thermal Problem
21 Advantage of RSE (2) RSE Low Recycling gain High finesse Strain Shot noise Detuning RSE Detuned RSE Shot noise can be optimized Frequency
22 Optical parameters Arm cavity finesse: 1500 Power recycling gain: 10 Signal band gain (no detuned case): 24
23 Important subsystems/functions Length sensing and control system Alignment sensing and control system Detuning optimization Curvature of the mirrors Lock acquisition Noise coupling reduction Quantum noise optimization Etc.
24 Summary We use RSE interferometer for LCGT RSE has advantages over PFPMI Many subsystems/functions have been already developed
Koji Arai / Stan Whitcomb LIGO Laboratory / Caltech. LIGO-G v1
Koji Arai / Stan Whitcomb LIGO Laboratory / Caltech LIGO-G1401144-v1 General Relativity Gravity = Spacetime curvature Gravitational wave = Wave of spacetime curvature Gravitational waves Generated by motion
More informationAlignment signal extraction of the optically degenerate RSE interferometer using the wave front sensing technique
Alignment signal extraction of the optically degenerate RSE interferometer using the wave front sensing technique Shuichi Sato and Seiji Kawamura TAMA project, National Astronomical Observatory of Japan
More informationExperience with Signal- Recycling in GEO600
Experience with Signal- Recycling in GEO600 Stefan Hild, AEI Hannover for the GEO-team Stefan Hild 1 GWADW, Elba, May 2006 Stefan Hild 2 GWADW, Elba, May 2006 Motivation GEO600 is the 1st large scale GW
More informationAdvanced Virgo commissioning challenges. Julia Casanueva on behalf of the Virgo collaboration
Advanced Virgo commissioning challenges Julia Casanueva on behalf of the Virgo collaboration GW detectors network Effect on Earth of the passage of a GW change on the distance between test masses Differential
More informationThe Virgo detector. L. Rolland LAPP-Annecy GraSPA summer school L. Rolland GraSPA2013 Annecy le Vieux
The Virgo detector The Virgo detector L. Rolland LAPP-Annecy GraSPA summer school 2013 1 Table of contents Principles Effect of GW on free fall masses Basic detection principle overview Are the Virgo mirrors
More informationarxiv: v1 [gr-qc] 10 Sep 2007
LIGO P070067 A Z A novel concept for increasing the peak sensitivity of LIGO by detuning the arm cavities arxiv:0709.1488v1 [gr-qc] 10 Sep 2007 1. Introduction S. Hild 1 and A. Freise 2 1 Max-Planck-Institut
More informationThe Florida control scheme. Guido Mueller, Tom Delker, David Reitze, D. B. Tanner
The Florida control scheme Guido Mueller, Tom Delker, David Reitze, D. B. Tanner Department of Physics, University of Florida, Gainesville 32611-8440, Florida, USA The most likely conguration for the second
More informationReceived 14 May 2008, in final form 14 July 2008 Published 11 September 2008 Online at stacks.iop.org/cqg/25/195008
IOP PUBLISHING (12pp) CLASSICAL AND QUANTUM GRAVITY doi:10.1088/0264-9381/25/19/195008 Experimental investigation of a control scheme for a zero-detuning resonant sideband extraction interferometer for
More informationAdvanced LIGO optical configuration investigated in 40meter prototype
Advanced LIGO optical configuration investigated in 4meter prototype LSC meeting at LLO Mar. 22, 25 O. Miyakawa, Caltech and the 4m collaboration LIGO- G5195--R LSC meeting at LLO, March 25 1 Caltech 4
More informationIntroduction to laser interferometric gravitational wave telescope
Introduction to laser interferometric gravitational wave telescope KAGRA summer school 013 July 31, 013 Tokyo Inst of Technology Kentaro Somiya Interferometric GW detector Far Galaxy Supernova explosion,
More informationToward the Advanced LIGO optical configuration investigated in 40meter prototype
Toward the Advanced LIGO optical configuration investigated in 4meter prototype Aspen winter conference Jan. 19, 25 O. Miyakawa, Caltech and the 4m collaboration LIGO- G547--R Aspen winter conference,
More information5 Advanced Virgo: interferometer configuration
5 Advanced Virgo: interferometer configuration 5.1 Introduction This section describes the optical parameters and configuration of the AdV interferometer. The optical layout and the main parameters of
More informationThis is a brief report of the measurements I have done in these 2 months.
40m Report Kentaro Somiya This is a brief report of the measurements I have done in these 2 months. Mach-Zehnder MZ noise spectrum is measured in various conditions. HEPA filter enhances the noise level
More informationInterferometer signal detection system for the VIRGO experiment. VIRGO collaboration
Interferometer signal detection system for the VIRGO experiment VIRGO collaboration presented by Raffaele Flaminio L.A.P.P., Chemin de Bellevue, Annecy-le-Vieux F-74941, France Abstract VIRGO is a laser
More informationVibration measurement in the cryogenic interferometric gravitational wave detector (CLIO interferometer)
Vibration measurement in the cryogenic interferometric gravitational wave detector (CLIO interferometer) ICRR Univ. of Tokyo, Dept. of geophysics Kyoto University A, KEK B, Dept. of advanced materials
More informationVIRGO. The status of VIRGO. & INFN - Sezione di Roma 1. 1 / 6/ 2004 Fulvio Ricci
The status of VIRGO Fulvio Ricci Dipartimento di Fisica - Università di Roma La Sapienza & INFN - Sezione di Roma 1 The geometrical effect of Gravitational Waves The signal the metric tensor perturbation
More informationMeasurement of optical response of a detuned resonant sideband extraction gravitational wave detector
PHYSICAL REVIEW D 74, 221 (26) Measurement of optical response of a detuned resonant sideband extraction gravitational wave detector Osamu Miyakawa, Robert Ward, Rana Adhikari, Matthew Evans, Benjamin
More informationPossibility of Upgrading KAGRA
The 3 rd KAGRA International Workshop @ Academia Sinica May 22, 2017 Possibility of Upgrading KAGRA Yuta Michimura Department of Physics, University of Tokyo with much help from Kentaro Komori, Yutaro
More informationParametric signal amplification
Parametric signal amplification ET meeting @ Birmingham Mar 27, 2017 K.Somiya Observation of high freq GW sources [Kiuchi, 2010] BNS merger with different models D=100Mpc BNS merger appears above the cavity
More informationHow to Build a Gravitational Wave Detector. Sean Leavey
How to Build a Gravitational Wave Detector Sean Leavey Supervisors: Dr Stefan Hild and Prof Ken Strain Institute for Gravitational Research, University of Glasgow 6th May 2015 Gravitational Wave Interferometry
More informationArm Cavity Finesse for Advanced LIGO
LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY - LIGO - CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Technical Note LIGO-T070303-01-D Date: 2007/12/20 Arm Cavity Finesse
More informationMultiply Resonant EOM for the LIGO 40-meter Interferometer
LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY - LIGO - CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY LIGO-XXXXXXX-XX-X Date: 2009/09/25 Multiply Resonant EOM for the LIGO
More informationA gravitational wave is a differential strain in spacetime. Equivalently, it is a differential tidal force that can be sensed by multiple test masses.
A gravitational wave is a differential strain in spacetime. Equivalently, it is a differential tidal force that can be sensed by multiple test masses. Plus-polarization Cross-polarization 2 Any system
More informationDevelopment of the accelerometer for cryogenic experiments II
Development of the accelerometer for cryogenic experiments II ICRR Univ. of Tokyo, KEK A, Dept. of advanced materials science Univ. of Tokyo B K. Yamamoto, H. Hayakawa, T. Uchiyama, S. Miyoki, H. Ishitsuka,
More informationExperimental Test of an Alignment Sensing Scheme for a Gravitational-wave Interferometer
Experimental Test of an Alignment Sensing Scheme for a Gravitational-wave Interferometer Nergis Mavalvala *, Daniel Sigg and David Shoemaker LIGO Project Department of Physics and Center for Space Research,
More informationStatus and Future of the Caltech 40m Lab
Status and Future of the Caltech 40m Lab Jan 29, 2007 the 40m team: Rana Adhikari, Ben Abbott, Rich Abbott, Rolf Bork, Tobin Fricke, Keisuke Goda, Jay Heefner, Alexander Ivanov, Kirk McKenzie, Osamu Miyakawa,
More informationCommissioning of Advanced Virgo
Commissioning of Advanced Virgo VSR1 VSR4 VSR5/6/7? Bas Swinkels, European Gravitational Observatory on behalf of the Virgo Collaboration GWADW Takayama, 26/05/2014 B. Swinkels Adv. Virgo Commissioning
More informationThe VIRGO detection system
LIGO-G050017-00-R Paolo La Penna European Gravitational Observatory INPUT R =35 R=0.9 curv =35 0m 95 MOD CLEAN ER (14m )) WI N d:yag plar=0 ne.8 =1λ 064nm 3km 20W 6m 66.4m M odulat or PR BS N I sing lefrequ
More informationDownselection of observation bandwidth for KAGRA
Downselection of observation bandwidth for KAGRA MG13, Stockholm Jul. 2012 K.Somiya, K.Agatsuma, M.Ando, Y.Aso, K.Hayama, N.Kanda, K.Kuroda, H.Tagoshi, R.Takahashi, K.Yamamoto, and the KAGRA collaboration
More informationThe VIRGO injection system
INSTITUTE OF PHYSICSPUBLISHING Class. Quantum Grav. 19 (2002) 1829 1833 CLASSICAL ANDQUANTUM GRAVITY PII: S0264-9381(02)29349-1 The VIRGO injection system F Bondu, A Brillet, F Cleva, H Heitmann, M Loupias,
More informationComparison of tuned and detuned Signal-Recycling. Stefan Hild for the GEO-team
Comparison of tuned and detuned Signal-Recycling Stefan Hild for the GEO-team Stefan Hild 1 ILIAS WG1 meeting, Cascina, November 2006 Stefan Hild 2 ILIAS WG1 meeting, Cascina, November 2006 Signal-Recycling
More informationLength sensing and control of a Michelson interferometer with power recycling and twin signal recycling cavities
Length sensing and control of a Michelson interferometer with power recycling and twin signal recycling cavities Christian Gräf, André Thüring, Henning Vahlbruch, Karsten Danzmann, and Roman Schnabel Institut
More informationIn this chapter we describe the history of GW detectors and the design of the LIGO GW detectors,
19 Chapter 3 Introduction to LIGO In this chapter we describe the history of GW detectors and the design of the LIGO GW detectors, which have been built for the detection of GWs. This description is broken
More informationThermal correction of the radii of curvature of mirrors for GEO 600
INSTITUTE OF PHYSICS PUBLISHING Class. Quantum Grav. 21 (2004) S985 S989 CLASSICAL AND QUANTUM GRAVITY PII: S0264-9381(04)68250-5 Thermal correction of the radii of curvature of mirrors for GEO 600 HLück
More information7th Edoardo Amaldi Conference on Gravitational Waves (Amaldi7)
Journal of Physics: Conference Series (8) 4 doi:.88/74-6596///4 Lock Acquisition Studies for Advanced Interferometers O Miyakawa, H Yamamoto LIGO Laboratory 8-34, California Institute of Technology, Pasadena,
More informationExperiment begins this autumn. This Talk: Motivation for TAMA300 recycling Length sensing/control system Lock acquisition
Experiment begins this autumn. This Talk: Motivation for TAMA300 recycling Length sensing/control system Lock acquisition Earlier operation as a gravitational wave detector ~ We could start the operation
More informationAdvanced Virgo Technical Design Report
Advanced Virgo Technical Design Report VIR xxxa 12 Issue 1 The Virgo Collaboration March 21, 2012 Contents 1 ISC 1 1.1 General description of the sub-system........................ 1 1.2 Input from other
More informationLength Sensing and Control for AdLIGO
LIGO LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY LIGO Laboratory / LIGO Scientific Collaboration LIGO T060272 00 I ADVANCED LIGO 06/11/19 Length Sensing and Control for AdLIGO Kentaro Somiya, Osamu
More informationVirgo status and commissioning results
Virgo status and commissioning results L. Di Fiore for the Virgo Collaboration 5th LISA Symposium 13 july 2004 VIRGO is an French-Italian collaboration for Gravitational Wave research with a 3 km long
More informationInstallation and Characterization of the Advanced LIGO 200 Watt PSL
Installation and Characterization of the Advanced LIGO 200 Watt PSL Nicholas Langellier Mentor: Benno Willke Background and Motivation Albert Einstein's published his General Theory of Relativity in 1916,
More informationStable recycling cavities for Advanced LIGO
Stable recycling cavities for Advanced LIGO Guido Mueller LIGO-G070691-00-D with input/material from Hiro Yamamoto, Bill Kells, David Ottaway, Muzammil Arain, Yi Pan, Peter Fritschel, and many others Stable
More informationPolarization Sagnac interferometer with a common-path local oscillator for heterodyne detection
1354 J. Opt. Soc. Am. B/Vol. 16, No. 9/September 1999 Beyersdorf et al. Polarization Sagnac interferometer with a common-path local oscillator for heterodyne detection Peter T. Beyersdorf, Martin M. Fejer,
More informationMichelson interferometer with diffractively-coupled arm resonators in second-order Littrow configuration
Michelson interferometer with diffractively-coupled arm resonators in second-order Littrow configuration Michael Britzger, 1 Maximilian H. Wimmer, 1 Alexander Khalaidovski, 1 Daniel Friedrich, 2 Stefanie
More informationExperimental Demonstration of a Gravitational Wave Detector Configuration Below the Shot Noise Limit
Experimental Demonstration of a Gravitational Wave Detector Configuration Below the Shot Noise Limit Kirk McKenzie 20 June 2002 Supervisors Prof. David McClelland Dr Daniel Shaddock Dr Ping Koy Lam Dr
More informationResults from the Stanford 10 m Sagnac interferometer
INSTITUTE OF PHYSICSPUBLISHING Class. Quantum Grav. 19 (2002) 1585 1589 CLASSICAL ANDQUANTUM GRAVITY PII: S0264-9381(02)30157-6 Results from the Stanford 10 m Sagnac interferometer Peter T Beyersdorf,
More informationOptical Recombination of the LIGO 40-m Gravitational Wave Interferometer
Optical Recombination of the LIGO 40-m Gravitational Wave Interferometer T.T. Lyons, * A. Kuhnert, F.J. Raab, J.E. Logan, D. Durance, R.E. Spero, S. Whitcomb, B. Kells LIGO Project, California Institute
More informationMASSACHUSETTS INSTITUTE OF TECHNOLOGY Department of Electrical Engineering and Computer Science
Student Name Date MASSACHUSETTS INSTITUTE OF TECHNOLOGY Department of Electrical Engineering and Computer Science 6.161 Modern Optics Project Laboratory Laboratory Exercise No. 6 Fall 2010 Solid-State
More informationOptical lever for KAGRA
Optical lever for KAGRA Kazuhiro Agatsuma 2014/May/16 2014/May/16 GW monthly seminar at Tokyo 1 Contents Optical lever (OpLev) development for KAGRA What is the optical lever? Review of OpLev in TAMA-SAS
More informationGingin High Optical Power Test Facility
Institute of Physics Publishing Journal of Physics: Conference Series 32 (2006) 368 373 doi:10.1088/1742-6596/32/1/056 Sixth Edoardo Amaldi Conference on Gravitational Waves Gingin High Optical Power Test
More informationPhysics of interferometric gravitational wave detectors
PRAMANA c Indian Academy of Sciences Vol. 63, No. 4 journal of October 2004 physics pp. 645 662 Physics of interferometric gravitational wave detectors BIPLAB BHAWAL LIGO Laboratory, California Institute
More informationPlans for DC Readout Experiment 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 Adhikari, Dan Busby, Jay Heefner, Keita Kawabe, Osamu Miyakawa, Virginio Sannibale, Mike Smith,
More informationvisibility values: 1) V1=0.5 2) V2=0.9 3) V3=0.99 b) In the three cases considered, what are the values of FSR (Free Spectral Range) and
EXERCISES OF OPTICAL MEASUREMENTS BY ENRICO RANDONE AND CESARE SVELTO EXERCISE 1 A CW laser radiation (λ=2.1 µm) is delivered to a Fabry-Pérot interferometer made of 2 identical plane and parallel mirrors
More informationOptical Vernier Technique for Measuring the Lengths of LIGO Fabry-Perot Resonators
LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY -LIGO- CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Technical Note LIGO-T97074-0- R 0/5/97 Optical Vernier Technique for
More informationThe generation and application of squeezed light in gravitational wave detectors and status of the POLIS project
The generation and application of squeezed light in gravitational wave detectors and status of the POLIS project De Laurentis* on behalf of POLIS collaboration *Università degli studi di Napoli 'Federico
More informationReadout and control of a power-recycled interferometric gravitational wave antenna
LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY - LIGO - CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Publication LIGO-P000008-A - D 10/2/00 Readout and control of a power-recycled
More informationDevelopment of Optical lever system of the 40 meter interferometer
LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY -LIGO- CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Technical Note x/xx/99 LIGO-T99xx- - D Development of Optical lever system
More informationUltra stable high power laser for the VIRGO project
Ultra stable high power laser for the VIRGO project C.N. Man To cite this version: C.N. Man. Ultra stable high power laser for the VIRGO project. International Conference: Laser M2P 3, 1993, Lyon, France.
More informationEE119 Introduction to Optical Engineering Fall 2009 Final Exam. Name:
EE119 Introduction to Optical Engineering Fall 2009 Final Exam Name: SID: CLOSED BOOK. THREE 8 1/2 X 11 SHEETS OF NOTES, AND SCIENTIFIC POCKET CALCULATOR PERMITTED. TIME ALLOTTED: 180 MINUTES Fundamental
More informationNoise Budget Development for the LIGO 40 Meter Prototype
Noise Budget Development for the LIGO 40 Meter Prototype Ryan Kinney University of Missouri-Rolla, Department of Physics, 1870 Miner Circle, Rolla, MO 65409, USA Introduction LIGO 40 meter prototype What
More informationCompensating thermal lensing in Faraday rotators.
Compensating thermal lensing in Faraday rotators. Donovan McFeron University of Florida. New Physics Building Corner of Museum and North South Drive Gainesville, FL 36 ( August 3, 000) ABSTRACT An analyzer
More informationOPSENS WHITE-LIGHT POLARIZATION INTERFEROMETRY TECHNOLOGY
OPSENS WHITE-LIGHT POLARIZATION INTERFEROMETRY TECHNOLOGY 1. Introduction Fiber optic sensors are made up of two main parts: the fiber optic transducer (also called the fiber optic gauge or the fiber optic
More informationCalibration of the LIGO displacement actuators via laser frequency modulation
IOP PUBLISHING Class. Quantum Grav. 27 (21) 2151 (1pp) CLASSICAL AND QUANTUM GRAVITY doi:1.188/264-9381/27/21/2151 Calibration of the LIGO displacement actuators via laser frequency modulation E Goetz
More informationNotes on the Pound-Drever-Hall technique
LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY -LIGO- CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Technical Note LIGO-T980045-00- D 4/16/98 Notes on the Pound-Drever-Hall
More informationMode mismatch and sideband imbalance in LIGO I PRM
LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY -LIGO- CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Technical Note LIGO-T04077-00- E Sep/0/04 Mode mismatch and sideband
More informationReview of 40m upgrade goals ffl The primary goal of the 40 m upgrade is to demonstrate a scheme for using resonant sideband extraction (RSE), in eithe
40m Upgrade Plans ffl Review of 40m upgrade goals ffl 40m infrastructure upgrade ffl RSE configuration - design considerations ffl IFO optical configuration ffl RSE control scheme ffl people, money, schedule
More informationOPSENS WHITE-LIGHT POLARIZATION INTERFEROMETRY TECHNOLOGY
OPSENS WHITE-LIGHT POLARIZATION INTERFEROMETRY TECHNOLOGY 1. Introduction Fiber optic sensors are made up of two main parts: the fiber optic transducer (also called the fiber optic gauge or the fiber optic
More informationSingle Photon Interference Katelynn Sharma and Garrett West University of Rochester, Institute of Optics, 275 Hutchison Rd. Rochester, NY 14627
Single Photon Interference Katelynn Sharma and Garrett West University of Rochester, Institute of Optics, 275 Hutchison Rd. Rochester, NY 14627 Abstract: In studying the Mach-Zender interferometer and
More informationStabilized lasers for advanced gravitational wave detectors
Early View publication on www.interscience.wiley.com (issue and page numbers not yet assigned; citable using Digital Object Identifier DOI) Laser & Photon. Rev., 1 15 (2010) / DOI 10.1002/lpor.200900036
More informationThe Core Optics. Input Mirror T ~ 3% T ~ 3% Signal Recycling Photodetector
The Core Optics End Mirror Power Recycling Mirror Input Mirror T ~ 3% T ~ 3% End Mirror T ~ 10 ppm Laser Nd:Yag 6 W 100 W 12 kw 20 m 4000 m Signal Recycling Photodetector Mirror (dark fringe) Fold mirrors
More informationOptical design of shining light through wall experiments
Optical design of shining light through wall experiments Benno Willke Leibniz Universität Hannover (member of the ALPS collaboration) Vistas in Axion Physics: A Roadmap for Theoretical and Experimental
More informationshould be easy to arrange in the 40m vacuum envelope. Of course, some of the f 1 sidebands will also go out the asymmetric port of the BS. Because f 1
21 RF sidebands, cavity lengths and control scheme. There will be two pairs of phase-modulated sidebands, placed on the main beam just downstream of the PSL, in air, using two fast- and high-powered Pockels
More informationWavelength Control and Locking with Sub-MHz Precision
Wavelength Control and Locking with Sub-MHz Precision A PZT actuator on one of the resonator mirrors enables the Verdi output wavelength to be rapidly tuned over a range of several GHz or tightly locked
More informationWave Front Detection for Virgo
Wave Front Detection for Virgo L.L.Richardson University of Arizona, Steward Observatory, 933 N. Cherry ave, Tucson Arizona 8575, USA E-mail: zimlance@email.arizona.edu Abstract. The use of phase cameras
More informationOutput Mode Cleaner Design
LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY LIGO LIGO Laboratory / LIGO Scientific Collaboration LIGO-T04xxxx 9 February 2004 Output Mode Cleaner Design P Fritschel Distribution of this draft:
More informationReadout and control of a power-recycled interferometric gravitational-wave antenna
Readout and control of a power-recycled interferometric gravitational-wave antenna Peter Fritschel, Rolf Bork, Gabriela González, Nergis Mavalvala, Dale Ouimette, Haisheng Rong, Daniel Sigg, and Michael
More informationMechanical Characterization of a LISA Telescope Test Structure
UNIVERSITY OF TRENTO Faculty of Mathematical, Physical and Natural Sciences Undergraduate school in Physics Mechanical Characterization of a LISA Telescope Test Structure Candidate Ilaria Pucher Advisors
More informationQuantum States of Light and Giants
Quantum States of Light and Giants MIT Corbitt, Bodiya, Innerhofer, Ottaway, Smith, Wipf Caltech Bork, Heefner, Sigg, Whitcomb AEI Chen, Ebhardt-Mueller, Rehbein QEM-2, December 2006 Ponderomotive predominance
More informationStable Recycling Cavities for Advanced LIGO
Stable Recycling Cavities for Advanced LIGO Guido Mueller University of Florida 08/16/2005 Table of Contents Stable vs. unstable recycling cavities Design of stable recycling cavity Design drivers Spot
More informationParallel phase modulation scheme for interferometric gravitational-wave detectors
Parallel phase modulation scheme for interferometric gravitational-wave detectors M. T. Hartman, 1, V. Quetschke, D. B. Tanner, 1 D. H. Reitze, 1,3 and G. Mueller 1 1 Department of Physics, University
More informationAdvanced Virgo phase cameras
Journal of Physics: Conference Series PAPER OPEN ACCESS Advanced Virgo phase cameras To cite this article: L van der Schaaf et al 2016 J. Phys.: Conf. Ser. 718 072008 View the article online for updates
More informationWhen Light Gets Pushy: Radiation Pressure Effects in Interferometric Gravitational Wave Detectors
When Light Gets Pushy: Radiation Pressure Effects in Interferometric Gravitational Wave Detectors Anna Catriona Green A thesis submitted to the University of Birmingham for the degree of DOCTOR OF PHILOSOPHY
More informationFabry Perot Resonator (CA-1140)
Fabry Perot Resonator (CA-1140) The open frame Fabry Perot kit CA-1140 was designed for demonstration and investigation of characteristics like resonance, free spectral range and finesse of a resonator.
More informationSimulations of Advanced LIGO: Comparisons between Twiddle and E2E
LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY LIGO CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Document Type LIGO-T010160-00-R 10/15/01 Simulations of Advanced LIGO:
More informationUnit-23 Michelson Interferometer I
Unit-23 Michelson Interferometer I Objective: Study the theory and the design of Michelson Interferometer. And use it to measure the wavelength of a light source. Apparatus: Michelson interferometer (include
More informationCurrent Status of LCGT
Current Status of LCGT Masaki Ando (Department of Physics, Kyoto University) On behalf of the LCGT Collaboration There was a huge earthquake (M9.0) 130km east of Sanriku, Japan. Several cities along eastern
More information10W Injection-Locked CW Nd:YAG laser
10W Injection-Locked CW Nd:YAG laser David Hosken, Damien Mudge, Peter Veitch, Jesper Munch Department of Physics The University of Adelaide Adelaide SA 5005 Australia Talk Outline Overall motivation ACIGA
More informationLIGO-P R Detector Description and Performance for the First Coincidence Observations between LIGO and GEO
LIGO-P030024-00-R Detector Description and Performance for the First Coincidence Observations between LIGO and GEO α??,1, a INFN, Sezione di Pisa, I-56100 Pisa, Italy Abstract For 17 days in August and
More informationLateral input-optic displacement in a diffractive Fabry-Perot cavity
Journal of Physics: Conference Series Lateral input-optic displacement in a diffractive Fabry-Perot cavity To cite this article: J Hallam et al 2010 J. Phys.: Conf. Ser. 228 012022 View the article online
More informationLinewidth-broadened Fabry Perot cavities within future gravitational wave detectors
INSTITUTE OF PHYSICS PUBLISHING Class. Quantum Grav. 21 (2004) S1031 S1036 CLASSICAL AND QUANTUM GRAVITY PII: S0264-9381(04)68746-6 Linewidth-broadened Fabry Perot cavities within future gravitational
More informationarxiv: v1 [astro-ph.im] 19 Dec 2011
arxiv:1112.4388v1 [astro-ph.im] 19 Dec 2011 Review of the Laguerre-Gauss mode technology research program at Birmingham P. Fulda, C. Bond, D. Brown, F. Brückner L. Carbone, S. Chelkowski 1, S. Hild 2,
More informationThe Pre Stabilized Laser for the LIGO Caltech 40m Interferometer: Stability Controls and Characterization.
LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY LIGO CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Document Type LIGO-T010159-00-R 10/15/01 The Pre Stabilized Laser for the
More informationElectronically tunable fabry-perot interferometers with double liquid crystal layers
Electronically tunable fabry-perot interferometers with double liquid crystal layers Kuen-Cherng Lin *a, Kun-Yi Lee b, Cheng-Chih Lai c, Chin-Yu Chang c, and Sheng-Hsien Wong c a Dept. of Computer and
More informationThe AEI 10 m Prototype. June Sina Köhlenbeck for the 10m Prototype Team
The AEI 10 m Prototype June 2014 - Sina Köhlenbeck for the 10m Prototype Team The 10m Prototype Seismic attenuation system Suspension Platform Inteferometer SQL Interferometer Suspensions 2 The AEI 10
More informationOur 10m Interferometer Prototype
Our 10m Interferometer Prototype KAGRA f2f, February 14, 2014 Fumiko Kawaoze AEI 10 m Prototype 1 10m Prototype Interferometer Standard Quantum Limit experiment Macroscopic Quantum mechanics Thermal Noise
More informationOptical Cavity Designs for Interferometric Gravitational Wave Detectors. Pablo Barriga 17 August 2009
Optical Cavity Designs for Interferoetric Gravitational Wave Detectors Pablo Barriga 7 August 9 Assignents.- Assuing a cavity of 4k with an ITM of 934 radius of curvature and an ETM of 45 radius of curvature.
More informationSqueezing with long (100 m scale) filter cavities
23-28 May 2016, Isola d Elba Squeezing with long (100 m scale) filter cavities Eleonora Capocasa, Matteo Barsuglia, Raffaele Flaminio APC - Université Paris Diderot Why using long filter cavities in enhanced
More informationFirst, the definition of finesse. From Encyclopedia of Laser Physics and Technology,
Finesse Enhancement Factors Steve Adler, IAS, 2/29/06; expanded /4/08 First, the definition of finesse. From Encyclopedia of Laser Physics and Technology, article on Finesse, htp://www.rp-photonics.com/finesse.html,
More informationTheoretical Approach. Why do we need ultra short technology?? INTRODUCTION:
Theoretical Approach Why do we need ultra short technology?? INTRODUCTION: Generating ultrashort laser pulses that last a few femtoseconds is a highly active area of research that is finding applications
More informationFilter Cavity Experiment and Frequency Dependent Squeezing. MIT Tomoki Isogai
Filter Cavity Experiment and Frequency Dependent Squeezing MIT Tomoki Isogai Outline What is squeezing? Squeezing so far Why do we need frequency dependent squeezing? Filter Cavity Experiment at MIT Frequency
More informationTNI mode cleaner/ laser frequency stabilization system
LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY -LIGO- CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Technical Note LIGO-T000077-00- R 8/10/00 TNI mode cleaner/ laser frequency
More information