Seismic Noise & Vibration Isolation Systems. AIGO Summer Workshop School of Physics, UWA Feb Mar. 2, 2010

Similar documents
The VIRGO suspensions

GAS (Geometric Anti Spring) filter and LVDT (Linear Variable Differential Transformer) Enzo Tapia Lecture 2. KAGRA Lecture 2 for students

Control Servo Design for Inverted Pendulum

Improving seismic isolation in Advanced LIGO using a ground rotation sensor

High performance vibration isolation techniques for the AIGO gravitational wave detector

Tilt sensor and servo control system for gravitational wave detection.

Superattenuator seismic isolation measurements by Virgo interferometer: a comparison with the future generation antenna requirements

Angular control of Advanced Virgo suspended benches

The VIRGO injection system

DRAFT Expected performance of type-bp SAS in bkagra

PUSHING THE ADVANCED VIRGO INTERFEROMETER TO THE LIMIT

How to Build a Gravitational Wave Detector. Sean Leavey

PRM SRM. Grav. Wave ReadOut

7th Edoardo Amaldi Conference on Gravitational Waves (Amaldi7)

Mechanical modeling of the Seismic Attenuation System for AdLIGO

The AEI 10 m Prototype. June Sina Köhlenbeck for the 10m Prototype Team

Model Independent Numerical Procedure for the Diagonalization of a Multiple Input Multiple Output Dynamic System

Using a Negative Impedance Converter to Dampen Motion in Test Masses

Noise Budget Development for the LIGO 40 Meter Prototype

Development of Optical lever system of the 40 meter interferometer

Barrier. (a) State the conditions which must be met for an object to move with simple harmonic motion. (2)

Virgo and the quest for low frequency sensitivity in GW detectors. Adalberto Giazotto INFN Pisa

Dynamic Modeling of Air Cushion Vehicles

Quantum States of Light and Giants

On the axes of Fig. 4.1, sketch the variation with displacement x of the acceleration a of a particle undergoing simple harmonic motion.

The VIRGO Environmental Monitoring System

Virgo status and commissioning results

A gravitational wave is a differential strain in spacetime. Equivalently, it is a differential tidal force that can be sensed by multiple test masses.

(1.3.1) (1.3.2) It is the harmonic oscillator equation of motion, whose general solution is: (1.3.3)

VIRGO. The status of VIRGO. & INFN - Sezione di Roma 1. 1 / 6/ 2004 Fulvio Ricci

LIGO PROJECT. Piezo-Electric Actuator Initial Performance Tests. Eric Ponslet April 13, Abstract

Passive, Nonlinear, Mechanical Structures for Seismic Attenuation

The Virgo detector. L. Rolland LAPP-Annecy GraSPA summer school L. Rolland GraSPA2013 Annecy le Vieux

External seismic pre-isolation retrofit design

Constructing response curves: Introduction to the BODE-diagram

Commissioning of Advanced Virgo

Inverted pendulum as low frequency pre-isolation for advanced gravitational wave detectors

Vibration measurement in the cryogenic interferometric gravitational wave detector (CLIO interferometer)

Enhanced LIGO HAM ISI Prototype Preliminary Performance Review T

Part 2: Second order systems: cantilever response

Recent Work at the Stanford Engineering Test Facility

Squeezed light and radiation pressure effects in suspended interferometers. Thomas Corbitt

Advanced Virgo commissioning challenges. Julia Casanueva on behalf of the Virgo collaboration

LIQUID SLOSHING IN FLEXIBLE CONTAINERS, PART 1: TUNING CONTAINER FLEXIBILITY FOR SLOSHING CONTROL

TNI mode cleaner/ laser frequency stabilization system

CHAPTER 11 TEST REVIEW -- MARKSCHEME

Vibration studies of a superconducting accelerating

The X-arm interferometer test of HEPI at LIGO Livingston

Koji Arai / Stan Whitcomb LIGO Laboratory / Caltech. LIGO-G v1

Name: Date: Period: Physics: Study guide concepts for waves and sound

Optical bench Seismic Isolation System (SAS) Prototyped for the HAM chambers of the Advanced LIGO Interferometers

Electronics and Instrumentation Name ENGR-4220 Fall 1999 Section Modeling the Cantilever Beam Supplemental Info for Project 1.

Diffractive gratings. in high-precision interferometry. for gravitational wave detection

high, thin-walled buildings in glass and steel

Outline: Introduction: What is SPM, history STM AFM Image treatment Advanced SPM techniques Applications in semiconductor research and industry

Multiply Resonant EOM for the LIGO 40-meter Interferometer

Texas Components - Data Sheet. The TX53G1 is an extremely rugged, low distortion, wide dynamic range sensor. suspending Fluid.

Development of the accelerometer for cryogenic experiments II

LIGO. LIGO Output Mode Cleaner HAM Seismic Attenuation System.

Auto-levelling geophone development and testing

Vertical-Vibration Suppressing Design of Accumulator with New Vibration-Measuring Method

Arm Cavity Finesse for Advanced LIGO

New Long Stroke Vibration Shaker Design using Linear Motor Technology

Load application in load cells - Tips for users

ACOUSTIC MITIGATION STATUS FOR S3

Elastic Support of Machinery and Equipment

ELECTROMAGNETIC MULTIFUNCTIONAL STAND FOR MEMS APPLICATIONS

Aspects of the GEO 600 Style Triple and Quadruple Pendulum Suspension Systems. 4 October 2002

ENHANCEMENT OF THE TRANSMISSION LOSS OF DOUBLE PANELS BY MEANS OF ACTIVELY CONTROLLING THE CAVITY SOUND FIELD

1. Introduction. 2. Concept. reflector. transduce r. node. Kraftmessung an verschiedenen Fluiden in akustischen Feldern

Introduction to laser interferometric gravitational wave telescope

Results from the Stanford 10 m Sagnac interferometer

the pilot valve effect of

Interferometer signal detection system for the VIRGO experiment. VIRGO collaboration

Direct Measurement of the Spectral Distribution of Thermal Noise

10W Injection-Locked CW Nd:YAG laser

Introduction of Receivers

The Principle and Simulation of Moving-coil Velocity Detector. Yong-hui ZHAO, Li-ming WANG and Xiao-ling YAN

CHAPTER 3. Multi-stage seismic attenuation system

Designing Optical Layouts for AEI s 10 meter Prototype. Stephanie Wiele August 5, 2008

Resonance and resonators

Dynamic Vibration Absorber

Optical Encoder Applications for Vibration Analysis

Rotordynamics Analysis Overview

In this chapter we describe the history of GW detectors and the design of the LIGO GW detectors,

PHY1 Review for Exam 9. Equations. V = 2πr / T a c = V 2 /r. W = Fdcosθ PE = mgh KE = ½ mv 2 E = PE + KE

Natural Frequencies and Resonance

Set Up and Test Results for a Vibrating Wire System for Quadrupole Fiducialization

GENERAL GUIDELINES FOR APPLICATION OF THE EXTENDED SUBTRACTION METHOD IN SASSI SOIL-STRUCTURE INTERACTION ANALYSIS

Application Note L26ROY

SAT pickup arms - discussions on some design aspects

DEMONSTRATIONS Spring 2008 WEEK# MON FRI WED FRI FEB 6 FEB 1 C35 C2 C5 C2 C5 L1 C12 FRI. Registration Day FEB 4 FEB 1

Active Stabilization of a Mechanical Structure

Module 4 TEST SYSTEM Part 2. SHAKING TABLE CONTROLLER ASSOCIATED SOFTWARES Dr. J.C. QUEVAL, CEA/Saclay

Material Parameter Measurement (MPM)

Vertical-Vibration Suppressing Design of Accumulator with New Vibration-Measuring Method

Modeling and Commisioning of the 10m Prototype Autoalignment System

9) Describe the down select process that led to the laser selection in more detail

Vibration Fundamentals Training System

Parametric signal amplification

Transcription:

Seismic Noise & Vibration Isolation Systems AIGO Summer Workshop School of Physics, UWA Feb. 28 - Mar. 2, 2010

Seismic noise Ground noise: X =α/f 2 ( m/ Hz) α: 10-6 ~ 10-9 @ f = 10 Hz, x = 1 0-11 m GW detector requirement: 10-18 m @ 10 Hz Vibration isolation essential Ground displacement noise m/sqrt(hz) 10-10 10-12 10-14 10-16 10-18 Quiet site 10-9 /f 2 10-1 10 0 10 1 10 2 10 3 10 4 Frequency Hz

Vibration isolation basic ideas Mechanical low pass filter Below resonant f << f 0 x = x 0 follow excitation At resonant f = f 0 x > x 0 motion amplified Above resonant f >> f 0 x > x 0, vibration isolation

Vibration Isolators horizontal and vertical components Vertical Spring/Mass system y0 + y Horizontal Pendulum x0 x * Transfer function Input output TF output TF = = input x x 0

Transfer Function single stage 10 4 10 2 10 0 X/X 0 TF= 10-2 10-4 (f 0 /f) 2 10-6 10-8 10-1 10 0 10 1 10 2 10 3 10 4 Frequency Hz

Some numbers 1 Hz isolator, TF@10Hz~(1/10) 2 =0.01 @10 Hz, seismic x 0 =10-11 m x=x 0 TF=10-14 m Not good enough Multiple stages: TF=TF1 TF2 TF3 TF N @ high frequency Input TF1 TF2 TF3 output

Multi-stage isolator k 1 l 1 m 1 Vertical isolator spr ing/mass system k 2 m 2 k i m i x i + m i m 2 l i m 1 Integrated 3-D isolator l 2 θ i Horizontal isolator pe ndulums k n l n x i m n m n Roll off slope (f 0 /f )2( f 1 /f) 2( f 2 /f) 2.(f n /f )2 If f 0 =f 1 =f 2 =.., then slope (f 0 /f )2n

Transfer function multi-stage 5 stage 1 Hz pendulum 10 2 10 0 Single 1Hz pendulum slope 10-2 10-4 x/x 0 10-6 10-8 10-10 10-12 10-14 10-16 Now @10Hz TF=(1/10) 2 5 X=x0 TF=10-21 m Wonderful 10-18 0.1 0.2 0.5 1 2 5 10. 20. 50. 100. Frequency Hz

Some facts Coupled system: the total transfer function is not simply multiplication At high frequency, TF=TF1xTF2xTF3 Near resonant frequencies, the peaks spilt Corner frequency highest resonant peak Spring mass system with identical stages: fc~2f 0 Pendulum system with identical stages: fc~2f 0 N

At low frequencies. Vibration isolation mechanical low pass filter High resonant peaks at low frequency amplitude Q-factor of the isolation components Hard for interferometer cavity locking control Needs damping to reduce the peaks height Or.

Pre-isolation stages Have an Ultra-low frequency (ULF) pre-isolation stage in front of the isolation chain with f 0 ~0.1 Hz. Then the peaks of the chain will fall on the slope of the this preisolator. Trnasfer function 50 0-50 -100-150 -200 0.01 0.1 1 10 frequency

A single ultra ultra low f stage? 50 0 Trnasfer function -50-100 Not as simple as that! -150-200 0.01 0.1 1 10 frequency

Internal frequencies Any structure will have internal resonances. Chladni figures are the results of the internal resonates of the plate

Example: cantilever Mode 1 Mode f 1. 163.26 2. 1016.7 3. 1030.7 4. 1498.1 5. 2835.7 6. 3215.2 7. 5521.9 8. 5743.3 Mode 2 Mode 5

Pre-isolation stage working range Low frequency pre-isolation is usually large structures with low internal f Usually the first internal frequency is roughly 10~100 times of f 0. It roll off does not goes on forever Needs to combined with low f isolation chain. 0.001 0.01 0.1 1

Remarks Due to the cross coupling between the vertical and horizontal direction ~10-3 (nothing is perfect), it is important to have good vertical isolation system. It is relatively easy to create horizontal low frequency isolation system pendulums Vertical low frequency isolation system is not so straight forward (coil spring, cantilever ) Needs to support heavy load spring creeping Low frequency larger structure lower internal modes

Pre- isolation First stage of seismic noise reduction Very low frequency Two approaches Active, stiff system Passive, soft system

Stiff system Basic Idea: Sensing the seismic motion, then move the stiff system accordingly to hold it still seismometer Stiff system Require very sensitive commercial seismometer Large forces on rigid system LIGO system is stiff system

Requirements for Active systems Complicated servo control Needs very good seismometer to sense the motion of m. Noise in seismometer would be taken as displacement signal and fedback Remark: the passive isolation chain is actually a very good seismometer Usually the a isolation system is a combination of both but more active-like or more passive-like

LIGO isolation system Active isolation platform + quadruple pendulum hydraulic external pre-isolator (HEPI) active isolation platform quadruple pendulum

Basic idea: Soft system Spring-mass system (or equivalent) Transfer function falls as (f 0 /f) 2 at f 0 >>f i, seismic will be reduced Soft system is a very good seismometer itself Small control force mainly for alignment and damping VIRGO, TAMA, ACIGA adopted the soft system

Pre-isolation Linkages Anti-springs Example: Inverted pendulum (wobbly table) Gravity acted as anti-spring

Inverse Pendulum 1 st horizontal ULF Pre-isolation ~100mHz

Lacoste Linkage Vertical ULF preisolation stage ~100mHz

Zero length spring ka 2 =bw f=0

Robert linkage 2 nd ULF horizontal Pre-isolation stage ~100mHz Key feature Two stages allow super-spring implementation

Robert s Linkage Suspension point P moving in a shallow potential well

Key feature Passive critical damping Self-Damped pendulums (3 Stages) ~

Self Damped Pendulum thin fibre pendulum link simple wire pivot 2-d gimbal pivot Eddy current viscous coupling magnets copper to next stage Eddy current damped rocker vertical Euler springs Couple pendulum motion with very low frequency rocking motion use eddy current damping between these two motions

Vertical Euler Springs (3 Stages) Euler spring with anti-spring is near critically damped Tuned near pendulum frequency

Euler Spring mass load motion l clamped end Low stored energy means low mass high internal mode frequency superior to blade springs

UWA Vibration Isolation and Suspension System Inverse Pendulum (Horizontal) 0.05 Hz Roberts Linkage (Horizontal) 0.05 Hz LaCoste (Vertical) 0.5Hz 4 horizontal Self-damped pendulum stages (~0.6Hz) 4 Vertical Euler Springs stage (~0.6Hz) Test mass

Newtonian Noise fundamental limit Gravity Gradient Noise Local gravitational field fluctuation: masses (people, vehicles, kangaroos) moving ground density change due to land wave.. (go underground) Environment is coupled to test masses by a equivalent spring with typical frequency G f 7 10 5 grav 2 π ρ Hz