Low probability, large fluctuations of the noise in detectors of gravitational waves
|
|
- Bruce Warren
- 5 years ago
- Views:
Transcription
1 European Research Council Low probability, large fluctuations of the noise in detectors of gravitational waves Nickname oftheproject: RareNoise Project Number: Principal Investigator: Livia Conti INFN Team Members: Michele Bonaldi CNR Lamberto Rondoni Politecnico di Torino infn it
2 The team Livia Conti, PI experimentalist INFN Padova 1FTE Stefano Longo technologist (DAQ & computing) INFN Padova 1FTE Mario Saraceni Matteo Pegoraro technologist (mechanics) technologist (electronics) Rosella Battistella INFN Padova INFN Padova financial officer 1FTE 0.1FTE INFN LNL Michele Bonaldi experimentalist CNR IFN Trento Lamberto Rondoni theoretician Politecnico di Torino 0.7FTE Paolo De Gregorio theoretician Politecnico di Torino 1FTE
3 Driving question: What are the spontaneous vibration fluctuations of an elastic body non at the thermodynamic equilibrium? eg subject to a steady state thermal gradient Answer: small fluctuations: similar to those at the equilibrium large fluctuations: we don t know. Indications suggest they are more frequent than at the equilibrium. Moreover there is not a general rule to predict departure point from gaussian distribution At the thermodynamic equilibrium: the spontaneous vibration fluctuations have normal distribution and are quantified by the Fluctuation Dissipation Theorem
4 Why this question? Non equilibrium systems are ubiquitous in nature: eg Universe, Earth, atmosphere, oceans. Interest in NonEquilibrium fluctuations so far limited to experimental investigations of behaviour of nanodevices and theoretical studies for motivating the 2 law of thermodynamics. So far only a few, ad hoc applications of theoretical results to macroscopic systems Novel application: Gravitational Wave detectors 1e-15 LIGO They are macroscopic instruments but with displacement sensitivity approaching the quantum limit. Theirnoise budget iscalculated very accurately; any subtle noise contribution must be taken into account: as both rms and statistics Dis placement [m m/ Hz] 1e-20 1e1 Frequency [Hz] 1e3 With their high h sensitivityand long acquisition iiti times GW dt detectorst might ihtprove the natural application of NonEquilibrium Theories to macroscopic systems
5 Non equilibrium in GW interferometers Thermal gradient due to laser power dissipated in the mirror How to compute the spontaneous vibration fluctuations ( thermalnoise ) in non equilibrium instruments? Future Japanese cryogenic interferometer For small fluctuations one could apply the Fluctuation Dissipation theorem using position dependent temperature: T=T(x) (local equilibrium). But: what is the probability of the large fluctuations? Indications suggest that they are more frequent than if gaussian Moreover: what hthappens to the acoustic modes??the modes cannot be defined locally! The concept of local equilibrium does not apply to the acoustic modes. So far the problem is addressed as if thermal equilibrium and normal mode expansion hold. Nota Bene: Cryogenics is being considered for 3 rd generation EU Interferometer (design study supported by FP7) similar NonEquilibrium issue
6 Intricating the thermal budget: thermal compensation Absorbed light power causes mirror thermal deformation need of compensation for recovering optimal mirror geometry Surface towards heater Mirror surface Operating detector GEO600 What is the distribution of the spontaneous vibration fluctuations of such a non equilibrium body?
7 This project: mutually reinforcing experimental + theoretical work YEAR 1 YEAR 2 YEAR 3 YEAR 4 YEAR 5 Exp. Setup & calibrations Model of rod vibrating under thermal gradient Measurements at 300K Measurements at 77K Measurements at 4.2K Production of Si oscillators Exp. Setup & calibrations Measurements at 300K and 77K Specialization of rod model to experim materials Molecular dynamics tests of Fluctuation Theorems Refinement of the theory Application of theory of Fluctuations to GW detectors Experimental work : Phase 1 Experimental work: Phase 2 Experimental work : Phase 3 Theoretical work
8 Experimental work Goal: Observe spontaneous vibration fluctuations of elastic bodies, ie mechanical resonators, subject to steady state thermal gradient Nota Bene: At the equilibrium thermal fluctuations are due to dissipations (Fluctuation Dissipation Theorem). Control of dissipations is mandatory if fluctuations are to be studied. focus on material low intrinsic dissipations, as in high precision experiments investigation of 2 kinds of low mechanical loss materials: a metal tl(aluminum) and a semiconductor (Silicon) repeated measurements at different temperatures: 300K, 77K, 4K, ie at different materialparameters material equilibrium T [K] Expected losses Phase 1 Al5056, Si 300, Phase 2 Al5056, Si Phase 3 Si 300,
9 Theoretical work Modelof of rods used in the experiments and subject to steady state state thermalgradients: numerical studies of the NonEquilibrium fluctuations. mathematical and numerical investigations of 1-dimensional chains of oscillators subject to thermal gradient Specialization of the particle interaction ti potentials ti to the experimental materials Coupling of several 1dim chains to go beyond 1dim: nonequilibrium molecular dynamics simulations Computation of observables not sensed experimentally: characterization of the nonequilibrium state of the system and of its noise. refinements of the nonequilibrium theory assessment of validity of the normal mode expansion formalism m application to interferometric L. Conti - RareNoise - Amaldi 09 GW detectors
10 Potential impact Impact on GW detectors: if NonEquilibrium effects are important need to reconsider design of future detector and/or adapt data analyses Also impact on experiments with low signal to noise ratios Impact on NonEquilibrium theories: new theoretical results availability of large amount of data with different material conditions and regimes, with focus on very low losses and intrinsic loss mechanisms from toy models to realistic models simulations NonEquilibrium theories have impact on micro nano motors. Assessment of validity of the normal mode expansion in non equilibrium systems Impact also in many fields
11 A case study: AURIGA AURIGA is gravitational wave bar detector located at INFN Legnaro (Padova, Italy) bar: material Al5056 mass 2300kg length 3m 1 st longitud. ~900Hz resonance diameter 600mm thermodynamic temperature 4.2K readout: capacitive transucer (bias 8MV/m) low loss matching transformer (5H/4μH) double stage SQUID amplifier (500hbar) the displacement sensitivity is of order several m/ Hz over a ~100Hz bandwidth overall, a system of 3 coupled ldresonators: 2 mechanical + 1 electrical
12 Cooling of AURIGA 2 types of cooling employed in AURIGA, with different effects: Thermodynamic cooling to 4.2K Feedback cooling to T eff ~ 0.01K of bar+transducer+electronics, of only the 3 electromechanical modes via thermal contact with LHe bath. via electronic feedback It reduces the thermal noise of mechanics and electronics by lowering both the temperature and (for the bar in Al5056) the losses. It improves the electronic stability and eases the data analysis; it does not improve the sensitivity to an external force such as an impinging gravitational wave. The losses of the electromechanical The effective losses of the electromechanical oscillators drop to oscillators raise to
13 Feedback cooling cold damping AURIGA modeled as the system of 3 coupled resonators (2 mechanical, 1 electrical): 3 normal modes Model each mode as RLC series electrical mode: T 0 = 4.6K We measure the noisy position of the 3 oscillators and feed back a force proportional to their velocity, equivalent to an additional damping. For each oscillator the resulting Langevin equation does not satisfy the Einstein relation: the additional damping R d calms down the oscillator (cooling to T eff) ) BUT the thermal driving force remains the same (due to bath at T 0 >T eff )
14 Active cooling: spectrum AURIGA runs continuously with fixed feedback settings. However, we investigated the effect of changing feedback settings. these numbers indicate the equivalent temperature of the mode, in mk units non equilibrium steady states caused by stochastic driving PRL 101, (2008)
15 Application of 1 st law of Thermodynamics With feedback off, the thermal driving forces the motion of the oscillator. This energy is given back to the bath by the intrinsic damping R. With feedback on, part the energy is extracted as work done on the feedback (additional damping R d ): this results in cooling. τ = integration ti time time averaged oscillator s energy difference symmetric as for an equilibrium oscillator time averaged work done by oscillator positive by definition positive mean, independent of τ time averaged heat absorbed by oscillator positive mean, independent of τ net heat transfer from the bath to the oscillator: the reverse (ie Q τ <0) is very rare PRL in press, arxiv: v1 RareNoise & Auriga collaborations
16 Power injected by the thermal bath (ε τ : normalized power) it maintains the dissipative system in a nonequilibrium steady state 3 years Auriga data compared with theoretical model for stochastically driven Langevin system singularity in the 2 nd derivative of the (large deviation function of the) injected power = predictions for τ/τ/ eff testing Fluctuation Relations is a standard tool to characterize nonequilibrium systems: here we test the FR for the power injected by the thermal bath PRL in press, arxiv: v1 RareNoise & Auriga collaborations
RareNoise. Livia Conti INFN Padova RareNoisePrincipal Investigator.
RareNoise Livia Conti INFN Padova RareNoisePrincipal Investigator RareNoise is funded by a Starting Independent Researcher Grant of ERC (IDEAS/FP7). Start in: July 2008 Duration: 5 years www.rarenoise.lnl.infn.it
More informationNonequilibrium issues in macroscopic experiments
Nonequilibrium issues in macroscopic experiments L. Conti, M. Bonaldi, L. Rondoni www.rarenoise.lnl.infn.it European Research Council Gravitational Wave detector Motivation: GWs will provide new and unique
More informationModelling nonequilibrium macroscopic oscillators. oscillators of interest to experimentalists.
Modelling nonequilibrium macroscopic oscillators of interest to experimentalists. P. De Gregorio RareNoise : L. Conti, M. Bonaldi, L. Rondoni ERC-IDEAS: www.rarenoise.lnl.infn.it Nonequilibrium Processes:
More informationA wideband and sensitive GW detector for khz frequencies: the dual sphere
INSTITUTE OF PHYSICSPUBLISHING Class. Quantum Grav. 19 (2002) 2013 2019 CLASSICAL ANDQUANTUM GRAVITY PII: S0264-9381(02)29134-0 A wideband and sensitive GW detector for khz frequencies: the dual sphere
More informationA broad band detector of Gravitational Waves: The dual torus
A broad band detector of Gravitational Waves: The dual torus M.BONALDI 1, M.CERDONIO 2, L.CONTI 2, M.PINARD 3, G.A.PRODI 4, L.TAFFARELLO 5, J.P.ZENDRI 5 1 Istituto di Fotonica e Nanotecnologie, ITC-CNR,
More information1 Elenco delle pubblicazioni su riviste internazionali con peer review e indicizzate da Thomson ISI
1 Elenco delle pubblicazioni su riviste internazionali con peer review e indicizzate da Thomson ISI [1] Serra E, Bonaldi M, Borrielli A, Conti L, Pandraud G, and Sarro P, Low loss single-crystal silicon
More informationThermal Noise in Non-Equilibrium Steady State Hannah Marie Fair Department of Physics, University of Tokyo, Tokyo, Japan (August 2014)
Thermal Noise in Non-Equilibrium Steady State Hannah Marie Fair Department of Physics, University of Tokyo, Tokyo, Japan (August 2014) Abstract Gravitational wave detectors are working to increase their
More informationStatus and Plans for Future Generations of Ground-based Interferometric Gravitational-Wave Antennas
Status and Plans for Future Generations of Ground-based Interferometric Gravitational-Wave Antennas 4 th international LISA Symposium July 22, 2002 @ Penn State University Seiji Kawamura National Astronomical
More informationInnovative Technologies for the Gravitational-Wave Detectors LIGO and Virgo
Innovative Technologies for the Gravitational-Wave Detectors LIGO and Virgo Jan Harms INFN, Sezione di Firenze On behalf of LIGO and Virgo 1 Global Network of Detectors LIGO GEO VIRGO KAGRA LIGO 2 Commissioning
More informationLow temperature mechanical dissipation measurements of silicon and silicon carbide as candidate material for DUAL detector
Journal of Physics: Conference Series Low temperature mechanical dissipation measurements of silicon and silicon carbide as candidate material for DUAL detector To cite this article: M Bignotto et al 2008
More informationThe Quantum Limit and Beyond in Gravitational Wave Detectors
The Quantum Limit and Beyond in Gravitational Wave Detectors Gravitational wave detectors Quantum nature of light Quantum states of mirrors Nergis Mavalvala GW2010, UMinn, October 2010 Outline Quantum
More informationInterferometric. Gravitational Wav. Detectors. \p World Scientific. Fundamentals of. Peter R. Sawlson. Syracuse University, USA.
SINGAPORE HONGKONG Fundamentals of Interferometric Gravitational Wav Detectors Second Edition Peter R. Sawlson Martin A. Pomerantz '37 Professor of Physics Syracuse University, USA \p World Scientific
More informationC.W. Gardiner. P. Zoller. Quantum Nois e. A Handbook of Markovian and Non-Markovia n Quantum Stochastic Method s with Applications to Quantum Optics
C.W. Gardiner P. Zoller Quantum Nois e A Handbook of Markovian and Non-Markovia n Quantum Stochastic Method s with Applications to Quantum Optics 1. A Historical Introduction 1 1.1 Heisenberg's Uncertainty
More informationDisplacement Noises in Laser Interferometric Gravitational Wave Detectors
Gravitational Wave Physics @ University of Tokyo Dec 12, 2017 Displacement Noises in Laser Interferometric Gravitational Wave Detectors Yuta Michimura Department of Physics, University of Tokyo Slides
More informationDay 3: Ultracold atoms from a qubit perspective
Cindy Regal Condensed Matter Summer School, 2018 Day 1: Quantum optomechanics Day 2: Quantum transduction Day 3: Ultracold atoms from a qubit perspective Day 1: Quantum optomechanics Day 2: Quantum transduction
More informationAdvanced Workshop on Nanomechanics September Quantum Measurement in an Optomechanical System
2445-03 Advanced Workshop on Nanomechanics 9-13 September 2013 Quantum Measurement in an Optomechanical System Tom Purdy JILA - NIST & University of Colorado U.S.A. Tom Purdy, JILA NIST & University it
More informationRadiation pressure effects in interferometric measurements
Laboratoire Kastler Brossel, Paris Radiation pressure effects in interferometric measurements A. Heidmann M. Pinard J.-M. Courty P.-F. Cohadon T. Briant O. Arcizet T. Caniard C. Molinelli P. Verlot Quantum
More informationNew directions for terrestrial detectors
New directions for terrestrial detectors The next ten years Nergis Mavalvala (just a middle child) Rai s party, October 2007 Rai-isms Zacharias s picture This isn t half stupid = brilliant! What do you
More informationGravitational Wave Detection from the Ground Up
Gravitational Wave Detection from the Ground Up Peter Shawhan (University of Maryland) for the LIGO Scientific Collaboration LIGO-G080393-00-Z From Simple Beginnings Joe Weber circa 1969 AIP Emilio Segre
More informationarxiv: v1 [physics.ins-det] 16 Nov 2015
Newtorites in bar detectors of gravitational wave arxiv:1511.04882v1 [physics.ins-det] 16 Nov 2015 Francesco Ronga (ROG collaboration) 1 INFN Laboratori Nazionali di Frascati via Fermi, Frascati I 00044,
More informationOptical Techniques for Gravitational-Wave Detection
Optical Techniques for Gravitational-Wave Detection M. Tacca Nikhef - Amsterdam Nikhef- 2017 July 14th Born in Novara (Italy) Introducing Myself PostDoc Fellow @ Nikhef (since July 2017) Laurea & PhD @
More informationGravitational wave cosmology Lecture 2. Daniel Holz The University of Chicago
Gravitational wave cosmology Lecture 2 Daniel Holz The University of Chicago Thunder and lightning Thus far we ve only seen the Universe (and 95% of it is dark: dark matter and dark energy). In the the
More informationDevelopment of ground based laser interferometers for the detection of gravitational waves
Development of ground based laser interferometers for the detection of gravitational waves Rahul Kumar ICRR, The University of Tokyo, 7 th March 2014 1 Outline 1. Gravitational waves, nature & their sources
More informationLIGOʼs first detection of gravitational waves and the development of KAGRA
LIGOʼs first detection of gravitational waves and the development of KAGRA KMI2017 Jan. 2017 Tokyo Institute of Technology Kentaro Somiya Self Introduction Applied Physics (U Tokyo) NAOJ 2000-04 Albert-Einstein
More informationQuantum Noise and Quantum Measurement
Quantum Noise and Quantum Measurement (APS Tutorial on Quantum Measurement)!F(t) Aashish Clerk McGill University (With thanks to S. Girvin, F. Marquardt, M. Devoret) t Use quantum noise to understand quantum
More informationDocument Number: SPIRE-UCF-DOC Issue 1.0. November Matt Griffin
Sensitivity of the SPIRE Detectors to Operating Parameters Document Number: SPIRE-UCF-DOC-9 Issue. November 4 7 Matt Griffin Contents. Introduction.... List of symbols... 3. Principles of semiconductor
More informationTemperature coefficient of refractive index of sapphire substrate at cryogenic temperature for interferometric gravitational wave detectors
Temperature coefficient of refractive index of sapphire substrate at cryogenic temperature for interferometric gravitational wave detectors T. Tomaru, T. Uchiyama, C. T. Taylor, S. Miyoki, M. Ohashi, K.
More informationTHE NEW RUN OF EXPLORER AND NAUTILUS
5th EDOARDO AMALDI CONFERENCE ON GRAVITATIONAL WAVES July 6-11, 2003 Green Park Resort Tirrenia (Pisa) - Italy THE NEW RUN OF EXPLORER AND NAUTILUS P.Astone, A.Fauth, D.Babusci, M.Bassan, P.Carelli, G.Cavallari,
More informationOverview of future interferometric GW detectors
Overview of future interferometric GW detectors Giovanni Andrea Prodi, University of Trento and INFN, many credits to Michele Punturo, INFN Perugia New perspectives on Neutron Star Interiors Oct.9-13 2017,
More informationValidation Of Data In Operating Resonant Detectors
Validation Of Data In Operating Resonant Detectors G.A.Prodi, L.Baggio 2, M.Cerdonio 2, V.Crivelli Visconti 2, V.Martinucci, A.Ortolan 3, L.Taffarello 4, G.Vedovato 3, S.Vitale, J.P.Zendri 4 Dipartimento
More informationGravitational Wave Astronomy the sound of spacetime. Marc Favata Kavli Institute for Theoretical Physics
Gravitational Wave Astronomy the sound of spacetime Marc Favata Kavli Institute for Theoretical Physics What are gravitational waves? Oscillations in the gravitational field ripples in the curvature of
More informationFirst Virgo Science Run. Press Conference - May 22, 2007 Cascina, Pisa, Italy PRESS INFORMATION
First Virgo Science Run Press Conference - May 22, 2007 Cascina, Pisa, Italy PRESS INFORMATION Introduction On May 18 th, the Virgo interferometer started its first science run. This is a major milestone
More informationFuture underground gravitational wave observatories. Michele Punturo INFN Perugia
Future underground gravitational wave observatories Michele Punturo INFN Perugia Terrestrial Detectors Advanced detectors 2015-2025 GEO, Hannover, 600 m aligo Hanford, 4 km 2015 2016 AdV, Cascina, 3 km
More informationET: Einstein Telescope
ET: Einstein Telescope Michele Punturo INFN Perugia On behalf of the ET design study team ILIAS General meeting, Jaca Feb 2008 1 Evolution of the current GW detectors Current Gravitational Wave interferometric
More informationMD Thermodynamics. Lecture 12 3/26/18. Harvard SEAS AP 275 Atomistic Modeling of Materials Boris Kozinsky
MD Thermodynamics Lecture 1 3/6/18 1 Molecular dynamics The force depends on positions only (not velocities) Total energy is conserved (micro canonical evolution) Newton s equations of motion (second order
More informationShot Noise and the Non-Equilibrium FDT
Shot Noise and the Non-Equilibrium FDT Rob Schoelkopf Applied Physics Yale University Gurus: Michel Devoret, Steve Girvin, Aash Clerk And many discussions with D. Prober, K. Lehnert, D. Esteve, L. Kouwenhoven,
More informationDetermining thermal noise limiting properties of thin films
Determining thermal noise limiting properties of thin films Courtney Linn Institute for Gravitational Research University of Glasgow Summer 2011 Abstract In order to make thermally stable mirrors to be
More informationIGEC toolbox for coincidence search
IGEC toolbox for coincidence search L. Baggio, M. Cerdonio, I.S. Heng, A. Ortolan, G.A. Prodi, E. Rocco, G. Vedovato and S. Vitale Univ. of Trento and INFN, via Sommarive, 14, 38050, Povo, TN, Italy Univ.
More informationAyaka Shoda University of Tokyo. M. Ando A, K. Okada, K. Ishidoshiro B, Y. Aso, K. Tsubono Kyoto University A, KEK B
Ayaka Shoda University of Tokyo M. Ando A, K. Okada, K. Ishidoshiro B, Y. Aso, K. Tsubono Kyoto University A, KEK B Table of contents 1. Introduction 2. Torsion-bar Antenna 3. Simultaneous observational
More informationHow to measure a distance of one thousandth of the proton diameter? The detection of gravitational waves
How to measure a distance of one thousandth of the proton diameter? The detection of gravitational waves M. Tacca Laboratoire AstroParticule et Cosmologie (APC) - Paris Journée GPhys - 2016 July 6th General
More informationReview of LIGO Upgrade Plans
Ando Lab Seminar April 13, 2017 Review of LIGO Upgrade Plans Yuta Michimura Department of Physics, University of Tokyo Contents Introduction A+ Voyager Cosmic Explorer Other issues on ISC Summary KAGRA+
More informationFirst Results from the Mesa Beam Profile Cavity Prototype
First Results from the Mesa Beam Profile Cavity Prototype Marco Tarallo 26 July 2005 Caltech LIGO Laboratory LIGO-G050348-00-D LIGO Scientific Collaboration 1 Contents Environment setup: description and
More informationFirst results of the RAP experiment (acoustic detection of particles) in the low temperature regime
Institute of Physics Publishing Journal of Physics: Conference Series 32 (2006) 393 397 doi:10.1088/1742-6596/32/1/060 Sixth Edoardo Amaldi Conference on Gravitational Waves First results of the RAP experiment
More informationINO-CNR BEC Center
Experiments @ INO-CNR BEC Center The INO-CNR team: CNR Researchers: PostDocs: Tom Bienaimé Giacomo Lamporesi, Gabriele Ferrari PhD students: Simone Serafini (INO), Eleonora Fava, Giacomo Colzi, Carmelo
More informationStatus of LIGO. David Shoemaker LISA Symposium 13 July 2004 LIGO-G M
Status of LIGO David Shoemaker LISA Symposium 13 July 2004 Ground-based interferometric gravitational-wave detectors Search for GWs above lower frequency limit imposed by gravity gradients» Might go as
More informationLast Name Minotti Given Name Paolo ID Number
Last Name Minotti Given Name Paolo ID Number 20180131 Question n. 1 Draw and describe the simplest electrical equivalent model of a 3-port MEMS resonator, and its frequency behavior. Introduce possible
More informationMetastable states in an RF driven Josephson oscillator
Metastable states in an RF driven Josephson oscillator R. VIJAYARAGHAVAN Daniel Prober Robert Schoelkopf Steve Girvin Department of Applied Physics Yale University 3-16-2006 APS March Meeting I. Siddiqi
More informationarxiv:gr-qc/ v1 29 Apr 2006
Principles of wide bandwidth acoustic detectors and the single-mass DUAL detector Michele Bonaldi, 1, Massimo Cerdonio, 2 Livia Conti, 2 Paolo Falferi, 1 Paola Leaci, 3 Stefano Odorizzi, 4 Giovanni A.
More informationAdvanced Virgo and LIGO: today and tomorrow
Advanced Virgo and LIGO: today and tomorrow Michał Was for the LIGO and Virgo collaborations Michał Was (SFP Gravitation) 2017 Nov 22 1 / 21 d Basics of interferometric gravitational wave detections Need
More informationThe technology behind LIGO: how to measure displacements of meters
The technology behind LIGO: how to measure displacements of 10-19 meters The LIGO interferometers Interferometry: displacement sensing Noise limits Advanced LIGO 4pm today, 1 West: Results from science
More informationNanometrology and its role in the development of nanotechnology
Nanometrology and its role in the development of nanotechnology Rob Bergmans Nederlands Meetinstituut Van Swinden Laboratorium 1 NMi Van Swinden Laboratorium The Art of Measurement Dutch national metrology
More informationThe status of VIRGO. To cite this version: HAL Id: in2p
The status of VIRGO E. Tournefier, F. Acernese, P. Amico, M. Al-Shourbagy, S. Aoudia, S. Avino, D. Babusci, G. Ballardin, R. Barillé, F. Barone, et al. To cite this version: E. Tournefier, F. Acernese,
More informationES 272 Assignment #2. in,3
ES 272 Assignment #2 Due: March 14th, 2014; 5pm sharp, in the dropbox outside MD 131 (Donhee Ham office) Instructor: Donhee Ham (copyright c 2014 by D. Ham) (Problem 1) The kt/c Noise (50pt) Imagine an
More informationQuantum optics. Marian O. Scully Texas A&M University and Max-Planck-Institut für Quantenoptik. M. Suhail Zubairy Quaid-i-Azam University
Quantum optics Marian O. Scully Texas A&M University and Max-Planck-Institut für Quantenoptik M. Suhail Zubairy Quaid-i-Azam University 1 CAMBRIDGE UNIVERSITY PRESS Preface xix 1 Quantum theory of radiation
More informationPaper Review. Special Topics in Optical Engineering II (15/1) Minkyu Kim. IEEE Journal of Quantum Electronics, Feb 1985
Paper Review IEEE Journal of Quantum Electronics, Feb 1985 Contents Semiconductor laser review High speed semiconductor laser Parasitic elements limitations Intermodulation products Intensity noise Large
More informationQuantum-noise reduction techniques in a gravitational-wave detector
Quantum-noise reduction techniques in a gravitational-wave detector AQIS11 satellite session@kias Aug. 2011 Tokyo Inst of Technology Kentaro Somiya Contents Gravitational-wave detector Quantum non-demolition
More informationMODERN OPTICS. P47 Optics: Unit 9
MODERN OPTICS P47 Optics: Unit 9 Course Outline Unit 1: Electromagnetic Waves Unit 2: Interaction with Matter Unit 3: Geometric Optics Unit 4: Superposition of Waves Unit 5: Polarization Unit 6: Interference
More informationGravitational Waves & Precision Measurements
Gravitational Waves & Precision Measurements Mike Smith 1 -20 2 HOW SMALL IS THAT? Einstein 1 meter 1/1,000,000 3 1,000,000 smaller Wavelength of light 10-6 meters 1/10,000 4 10,000 smaller Atom 10-10
More informationPresent and Future. Nergis Mavalvala October 09, 2002
Gravitational-wave Detection with Interferometers Present and Future Nergis Mavalvala October 09, 2002 1 Interferometric Detectors Worldwide LIGO TAMA LISA LIGO VIRGO GEO 2 Global network of detectors
More informationNon-Equilibrium Fluctuations in Expansion/Compression Processes of a Single-Particle Gas
Non-Equilibrium Fluctuations in Expansion/Compression Processes o a Single-Particle Gas Hyu Kyu Pa Department o Physics, UNIST IBS Center or Sot and Living Matter Page 1 November 8, 015, Busan Nonequilibrium
More informationNext Generation Interferometers
Next Generation Interferometers TeV 06 Madison Rana Adhikari Caltech 1 Advanced LIGO LIGO mission: detect gravitational waves and initiate GW astronomy Next detector» Should have assured detectability
More informationpickup from external sources unwanted feedback RF interference from system or elsewhere, power supply fluctuations ground currents
Noise What is NOISE? A definition: Any unwanted signal obscuring signal to be observed two main origins EXTRINSIC NOISE examples... pickup from external sources unwanted feedback RF interference from system
More informationTheory of bifurcation amplifiers utilizing the nonlinear dynamical response of an optically damped mechanical oscillator
Theory of bifurcation amplifiers utilizing the nonlinear dynamical response of an optically damped mechanical oscillator Research on optomechanical systems is of relevance to gravitational wave detection
More informationPiezoelectric Actuators and Future Motors for Cryogenic Applications in Space
Piezoelectric Actuators and Future Motors for Cryogenic Applications in Space Christian Belly*, Francois Barillot* and Fabien Dubois * Abstract The purpose of this paper is to present the current investigation
More informationQuantum Reservoir Engineering
Departments of Physics and Applied Physics, Yale University Quantum Reservoir Engineering Towards Quantum Simulators with Superconducting Qubits SMG Claudia De Grandi (Yale University) Siddiqi Group (Berkeley)
More informationGEO 600: Advanced Techniques in Operation
GEO 600: Advanced Techniques in Operation Katherine Dooley for the GEO team DCC# G1400554-v1 LISA Symposium X Gainesville, FL May 21, 2014 GEO600 Electronics shop Corner building Operator's station Offices
More information2 Each satellite will have two test masses, each being the end mirror for an interferometer.
Ground Testing for LISA Test Masses with a Torsion Pendulum Matthew Schmidt Valdosta State University International REU: University of Trento, Italy Advisor: Dr. Bill Weber Abstract: One of the most important
More informationGravitational Waves and LIGO: A Technical History
Gravitational Waves and LIGO: A Technical History Stan Whitcomb IEEE SV Tech History Committee Event 11 October 2018 LIGO-G180195-v3 Goal of Talk Review a few of the technical developments that enabled
More informationThe gravitational wave detector VIRGO
The gravitational wave detector VIRGO for the VIRGO collaboration Raffaele Flaminio Laboratoire d Annecy-le-Vieux de Physique des Particules (LAPP) IN2P3 - CNRS Summary I. A bit of gravitational wave physics
More information1990. Temperature dependence of soft-doped / hard-doped PZT material properties under large signal excitation and impact on the design choice
1990. Temperature dependence of soft-doped / hard-doped PZT material properties under large signal excitation and impact on the design choice Charles Mangeot Noliac A/S, Kvistgaard, Denmark E-mail: cm@noliac.com
More informationAdvanced Virgo: Status and Perspectives. A.Chiummo on behalf of the VIRGO collaboration
Advanced Virgo: Status and Perspectives A.Chiummo on behalf of the VIRGO collaboration Advanced Virgo 2 Advanced Virgo What s that? 3 Advanced Virgo Advanced Virgo (AdV): upgrade of the Virgo interferometric
More informationExperience with matlab, python, and signal processing would be useful.
LIGO Livingston (Louisiana) Real-time Simulated LIGO The limit to detection of high mass binary black holes is the technical noise in the LIGO interferometers below 30 Hz. To better understand this, we
More informationMaximum heat transfer along a sapphire suspension fiber for a cryogenic interferometric gravitational wave detector
Maximum heat transfer along a sapphire suspension fiber for a cryogenic interferometric gravitational wave detector T. Tomaru 1, T. Suzuki, T. Uchiyama, A. Yamamoto, T. Shintomi High Energy Accelerator
More informationNon-equilibrium phenomena and fluctuation relations
Non-equilibrium phenomena and fluctuation relations Lamberto Rondoni Politecnico di Torino Beijing 16 March 2012 http://www.rarenoise.lnl.infn.it/ Outline 1 Background: Local Thermodyamic Equilibrium 2
More informationLarge-scale Cryogenic Gravitational wave Telescope (LCGT) TAMA/CLIO/LCGT Collaboration Kazuaki KURODA
29-March, 2009 JPS Meeting@Rikkyo Univ Large-scale Cryogenic Gravitational wave Telescope (LCGT) TAMA/CLIO/LCGT Collaboration Kazuaki KURODA Overview of This talk Science goal of LCGT First detection of
More informationGravitational Wave Astronomy Suggested readings: Camp and Cornish, Ann Rev Nucl Part Sci 2004 Schutz, gr-qc/ Kip Thorne WEB course
Gravitational Wave Astronomy Suggested readings: Camp and Cornish, Ann Rev Nucl Part Sci 2004 Schutz, gr-qc/0003069 Kip Thorne WEB course http://elmer.caltech.edu/ph237/week1/week1.html L. Bergstrom and
More informationSqueezed Light for Gravitational Wave Interferometers
Squeezed Light for Gravitational Wave Interferometers R. Schnabel, S. Chelkowski, H. Vahlbruch, B. Hage, A. Franzen, and K. Danzmann. Institut für Atom- und Molekülphysik, Universität Hannover Max-Planck-Institut
More informationDynamics of star clusters containing stellar mass black holes: 1. Introduction to Gravitational Waves
Dynamics of star clusters containing stellar mass black holes: 1. Introduction to Gravitational Waves July 25, 2017 Bonn Seoul National University Outline What are the gravitational waves? Generation of
More informationSUPPLEMENTARY FIGURES
1 SUPPLEMENTARY FIGURES Supplementary Figure 1: Schematic representation of the experimental set up. The PC of the hot line being biased, the temperature raises. The temperature is extracted from noise
More informationQuality Factor Thickness (nm) Quality Factor Thickness (nm) Quality Factor 10
Oxygen-Terminated Fluorine-Terminated Length = 24 mm Length = 2 mm Length = 1 mm Length = 12 mm Length = 8 mm 8 mm Width, K 12 mm Width, K 1 mm Width, K 8 mm Width, K 12 mm Width, K 1 mm Width, K Supplementary
More informationQuantum Mechanical Noises in Gravitational Wave Detectors
Quantum Mechanical Noises in Gravitational Wave Detectors Max Planck Institute for Gravitational Physics (Albert Einstein Institute) Germany Introduction Test masses in GW interferometers are Macroscopic
More informationLong-base Hydrostatic Incline Meter. gravitational antenna
Long-base Hydrostatic Incline Meter. gravitational antenna There are many reasons resulting in relative vertical displacements of end-capping and central mirrors of gravitational antenna. Firstly is passing
More informationPoint mass approximation. Rigid beam mechanics. spring constant k N effective mass m e. Simple Harmonic Motion.. m e z = - k N z
Free end Rigid beam mechanics Fixed end think of cantilever as a mass on a spring Point mass approximation z F Hooke s law k N = F / z This is beam mechanics, standard in engineering textbooks. For a rectangular
More informationNoise, AFMs, and Nanomechanical Biosensors
Noise, AFMs, and Nanomechanical Biosensors: Lancaster University, November, 2005 1 Noise, AFMs, and Nanomechanical Biosensors with Mark Paul (Virginia Tech), and the Caltech BioNEMS Collaboration Support:
More informationSearching for non-newtonian forces with optically levitated microspheres!
Searching for non-newtonian forces with optically levitated microspheres!! David Moore, Alexander Rider, Marie Lu, Giorgio Gratta! Stanford University! Testing Gravity 2015! Introduction! Searches for
More informationThe Status of KAGRA Underground Cryogenic Gravitational Wave Telescope
TAUP2017 @ Laurentian University Jul 26, 2017 The Status of KAGRA Underground Cryogenic Gravitational Wave Telescope Yuta Michimura Department of Physics, University of Tokyo on behalf of the KAGRA Collaboration
More informationSearching for gravitational waves
Searching for gravitational waves Matteo Barsuglia (barsuglia@apc.univ-paris7.fr) CNRS - Laboratoire Astroparticule et Cosmologie 1 The gravitational waves (GW) Perturbations of the space-time metrics
More informationNoise in voltage-biased scaled semiconductor laser diodes
Noise in voltage-biased scaled semiconductor laser diodes S. M. K. Thiyagarajan and A. F. J. Levi Department of Electrical Engineering University of Southern California Los Angeles, California 90089-1111
More informationA Guide to Experiments in Quantum Optics
Hans-A. Bachor and Timothy C. Ralph A Guide to Experiments in Quantum Optics Second, Revised and Enlarged Edition WILEY- VCH WILEY-VCH Verlag CmbH Co. KGaA Contents Preface 1 Introduction 1.1 Historical
More informationThe MID instrument.
The MID instrument International Workshop on the Materials Imaging and Dynamics Instrument at the European XFEL Grenoble, Oct 28/29, 2009 Thomas Tschentscher thomas.tschentscher@xfel.eu Outline 2 History
More informationVibration-Free Pulse Tube Cryocooler System for Gravitational Wave Detectors I
1 Vibration-Free Pulse Tube Cryocooler System for Gravitational Wave Detectors I - Vibration-Reduction Method and Measurement - T. Tomaru A, T. Suzuki A, T. Haruyama A, T. Shintomi A, N. Sato A, A. Yamamoto
More informationGravitational Wave Astronomy
Gravitational Wave Astronomy Giles Hammond SUPA, University of Glasgow, UK on behalf of the LIGO Scientific Collaboration and the Virgo Collaboration 14 th Lomonosov conference on Elementary Particle Physics
More informationScattering theory of current-induced forces. Reinhold Egger Institut für Theoretische Physik, Univ. Düsseldorf
Scattering theory of current-induced forces Reinhold Egger Institut für Theoretische Physik, Univ. Düsseldorf Overview Current-induced forces in mesoscopic systems: In molecule/dot with slow mechanical
More informationMEASUREMENT THEORY QUANTUM AND ITS APPLICATIONS KURT JACOBS. University of Massachusetts at Boston. fg Cambridge WW UNIVERSITY PRESS
QUANTUM MEASUREMENT THEORY AND ITS APPLICATIONS KURT JACOBS University of Massachusetts at Boston fg Cambridge WW UNIVERSITY PRESS Contents Preface page xi 1 Quantum measurement theory 1 1.1 Introduction
More informationTOBA: Torsion-Bar Antenna
TOBA: Torsion-Bar Antenna Small-scale TOBA at Tokyo Small-scale TOBA at Kyoto SWIM on SDS-1 satellite Masaki Ando (National Astronomical Observatory) K.Ishidoshiro, A.Shoda, K.Okada, W.Kokuyama, K.Yagi,
More informationStatus Report: Charge Cloud Explosion
Status Report: Charge Cloud Explosion J. Becker, D. Eckstein, R. Klanner, G. Steinbrück University of Hamburg Detector laboratory 1. Introduction and Motivation. Set-up available for measurement 3. Measurements
More informationPreferred spatio-temporal patterns as non-equilibrium currents
Preferred spatio-temporal patterns as non-equilibrium currents Escher Jeffrey B. Weiss Atmospheric and Oceanic Sciences University of Colorado, Boulder Arin Nelson, CU Baylor Fox-Kemper, Brown U Royce
More informationThermal Corrective Devices for Advanced Gravitational Wave Interferometers
Thermal Corrective Devices for Advanced Gravitational Wave Interferometers Marie Kasprzack, Louisiana State University 6 th October 2016 COMSOL Conference 2016 Boston 1 1. Advanced Gravitational Wave Detectors
More informationHarmonic Oscillator. Mass-Spring Oscillator Resonance The Pendulum. Physics 109 Experiment Number 12
Harmonic Oscillator Mass-Spring Oscillator Resonance The Pendulum Physics 109 Experiment Number 12 Outline Simple harmonic motion The vertical mass-spring system Driven oscillations and resonance The pendulum
More informationSummer Research Projects for 2018
Summer Research Projects for 2018 LIGO Livingston (Louisiana) Scattered Light Investigations Light scattered from the main beam path in the Advanced LIGO interferometer can re-enter the beam path after
More information