Conceptual Design for Advanced LIGO Suspensions Norna A Robertson University of Glasgow and Stanford University for the GEO suspension team +contribution.

Slides:



Advertisements
Similar presentations
2 mm diameter region 300 micron thermoelastic noise cancellation section Neck region, for transition from 2 mm stock to 300  m fibre 150  m section for.
Advertisements

Laser Interferometer Gravitational-wave Detectors: Advancing toward a Global Network Stan Whitcomb LIGO/Caltech ICGC, Goa, 18 December 2011 LIGO-G v1.
T1 task- update Mike Plissi. 2 Collaboration Groups actively involved INFN-VIRGO MAT IGR-Glasgow Groups that have expressed interest INFN-AURIGA CNRS-LKB.
LIGO - G R 1 HAM SAS Test Plan at LASTI David Ottaway November 2005 LIGO-G Z.
LIGO-G D Comments: Staged implementation of Advanced LIGO Adv LIGO Systems 17 may02 dhs Nifty idea: a way to soften the shock, spread cost, allow.
Aspects of Fused Silica Suspensions in Advanced Detectors Geppo Cagnoli University of Texas at Brownsville and TSC LIGO, Hanford.
LIGO-G PLIGO Laboratory 1 Advanced LIGO The Next Generation Philip Lindquist, Caltech XXXVIII Moriond Conference Gravitational Waves and Experimental.
Global longitudinal quad damping vs. local damping Brett Shapiro Stanford University 1/32G v13 LIGO.
G R LIGO Laboratory1 Advanced LIGO Research and Development David Shoemaker LHO LSC 11 November 2003.
LIGO-G D Suspensions Update: the View from Caltech Phil Willems LIGO/Caltech Livingston LSC Meeting March 17-20, 2003.
Silica Research in Glasgow Gianpietro Cagnoli – IGR - University of Glasgow GEO Collaboration Ginzton Lab, Stanford Caltech.
Review of HAM Suspension Designs for Advanced LIGO Norna A Robertson HAM Isolation Requirements Review Caltech, July 11th 2005.
LIGO-G D Suspensions Design for Advanced LIGO Phil Willems NSF Review, Oct , 2002 MIT.
Active Seismic Isolation Systems for Enhanced and Advanced LIGO Jeffrey S. Kissel 1 for the LSC 1 Louisiana State University The mechanical system for.
Development of a CO 2 laser machine for pulling and welding of silica fibres and ribbons D. Crooks for the GEO 600 collaboration Aspen January 2005 LIGO-G Z.
LIGO-G D 1 25-May-02 Advanced LIGO Suspension Model in Mathematica Gravitational Wave Advanced Detector Workshop Elba - May 2002 Mark Barton.
September 8, 2015 THE MONOLITHIC SUSPENSION STATUS FOR THE VIRGO INTERFEROMETER THE MONOLITHIC SUSPENSION STATUS FOR THE VIRGO INTERFEROMETER Helios Vocca.
Substrate mechanical loss studies Sheila Rowan (Stanford University) for: LIGO Laboratory (Caltech, MIT, LLO, LHO) LSC Partners (University of Glasgow,
GWADW 2010 in Kyoto, May 19, Development for Observation and Reduction of Radiation Pressure Noise T. Mori, S. Ballmer, K. Agatsuma, S. Sakata,
Advanced LIGO: our future in gravitational astronomy K.A. Strain for the LIGO Science Collaboration NAM 2008 LIGO-G K.
STREGA WP1/M1 mirror substrates GEO LIGO ISA Scientific motivation: Mechanical dissipation from dielectric mirror coatings is predicted to be a significant.
SUSPENSION DESIGN FOR ADVANCED LIGO: Update on GEO Activities Norna A Robertson University of Glasgow for the GEO 600 suspension team LSC Meeting, Louisiana,
G M 1 Advanced LIGO Update David Shoemaker LSC/Virgo MIT July 2007.
Update on Advanced LIGO suspension design and technology development towards the quad noise prototype Caroline A. Cantley for Advanced LIGO Suspension.
Thermal noise from optical coatings Gregory Harry Massachusetts Institute of Technology - on behalf of the LIGO Science Collaboration - 25 July
T1 task- update Mike Plissi. 2 Motivation  Thermo-elastic noise is higher than the ‘intrinsic’ noise in crystalline materials  There are several sources.
LIGO- G D The LIGO Instruments Stan Whitcomb NSB Meeting LIGO Livingston Observatory 4 February 2004.
Advanced LIGO Suspension Status Caroline A. Cantley Advanced LIGO Suspension Team / University of Glasgow for the GEO600 Group LSC Meeting, LLO March 2004.
Advanced interferometers for astronomical observations Lee Samuel Finn Center for Gravitational Wave Physics, Penn State.
SUSPENSION DESIGN FOR ADVANCED LIGO: Update on GEO Activities Norna A Robertson University of Glasgow for the GEO 600 suspension team LSC Meeting, Hanford.
Simulation for KAGRA cryogenic payload: vibration via heat links and thermal noise Univ. Tokyo, D1 Takanori Sekiguchi.
David Shoemaker Aspen 3 February 03
Global longitudinal quad damping vs. local damping Brett Shapiro Stanford University 1/36 LIGO G v15.
18 th - 22 nd May 2015 LIGO-G GWADW Alaska Suspension Upgrades: Discussion Points + Questions Giles Hammond (Institute for Gravitational Research,
LSC August G Z Gingin High Optical Power Test Facility (AIGO) 1 High Optical Power Test Facility - Status First lock, auto-alignment and.
Update on Suspension Activities for Advanced LIGO Caroline A. Cantley University of Glasgow for the GEO600 Group LSC Meeting, Livingston, March 2003 (Technical.
18 th - 22 nd May 2015 LIGO-G GWADW Alaska Suspension Upgrades for Enhanced Interferometers Giles Hammond (Institute for Gravitational Research,
LIGO-G Z Thermal noise in sapphire - summary and plans Work carried out at: Stanford University University of Glasgow Caltech MIT.
External forces from heat links in cryogenic suspensions D1, ICRR, Univ. Tokyo Takanori Sekiguchi GWADW in Hawaii.
Abstract The Hannover Thermal Noise Experiment V. Leonhardt, L. Ribichini, H. Lück and K. Danzmann Max-Planck- Institut für Gravitationsphysik We measure.
Prototype Quadruple Pendulum Update – Part 1 Norna Robertson and Calum Torrie University of Glasgow for the GEO 600 suspension team LSC Meeting, Hanford,
Update on Activities in Suspensions for Advanced LIGO Norna A Robertson University of Glasgow and Stanford University LSC meeting, Hanford, Aug 20 th 2002.
Thermal Noise performance of advanced gravitational wave detector suspensions Alan Cumming, on behalf of the University of Glasgow Suspension Team 5 th.
Thermoelastic dissipation in inhomogeneous media: loss measurements and thermal noise in coated test masses Sheila Rowan, Marty Fejer and LSC Coating collaboration.
Suspension Thermal Noise Giles Hammond (University of Glasgow) on behalf of the Strawman Red Team GWADW 2012, 18 th May 2012 LIGO-G
Advanced LIGO Status Report
LIGO-G M LIGO Status Gary Sanders GWIC Meeting Perth July 2001.
Mechanical Mode Damping for Parametric Instability Control
Advanced LIGO UK 1 LIGO-G Z Development issues for the UK Advanced LIGO project Caroline Cantley Glasgow University for the UK Advanced LIGO Team.
LSC Meeting March ‘07 1 LIGO ADVANCED SYSTEMS TEST INTERFEROMETER (LASTI) LASTI Progress and Plans LSC Meeting, LLO Dave Ottaway/Richard Mittleman March.
C1) K. Tokmakov on behalf of the Advanced LIGO Suspensions Team Monolithic suspensions of the mirrors of the Advanced LIGO gravitational-wave detector.
Optical Spring Experiments With The Glasgow 10m Prototype Interferometer Matt Edgar.
Proposal for baseline change from ribbons to fibres in monolithic stage Mark Barton for the IGR Monolithic Team Systems Meeting 16 April 2008 G
LIGO-G Z Silicon as a low thermal noise test mass material S. Rowan, R. Route, M.M. Fejer, R.L. Byer Stanford University P. Sneddon, D. Crooks,
Advanced LIGO UK 1 LIGO-G K OSEM Development UK Advanced LIGO project Stuart Aston University of Birmingham for the UK Advanced LIGO Team LSC.
LIGO-G R 1 Gregory Harry and COC Working Group Massachusetts Institute of Technology - Technical Plenary Session - March 17-20, 2003 LSC Meeting.
LIGO-G Z LIGO’s Thermal Noise Interferometer Progress and Status Eric D. Black, Kenneth G. Libbrecht, and Shanti Rao (Caltech) Seiji Kawamura.
ALIGO 0.45 Gpc 2014 iLIGO 35 Mpc 2007 Future Range to Neutron Star Coalescence Better Seismic Isolation Increased Laser Power and Signal Recycling Reduced.
Modelling and Testing of Cryogenic Suspensions Giles Hammond Institute for Gravitational Research SUPA University of Glasgow on behalf of the KAGRA suspensions.
ALIGO Monolithic stage Giles Hammond, University of Glasgow for the Advanced LIGO Suspensions Team aLIGO/aVirgo Workshop Pisa, Italy 23 rd -24 th February.
LIGO-G D Advanced LIGO Systems & Interferometer Sensing & Control (ISC) Peter Fritschel, LIGO MIT PAC 12 Meeting, 27 June 2002.
Overview of monolithic suspension work for Advanced LIGO Mariëlle van Veggel, Mark Barton, Tim Bodiya, Alan Cumming, Liam Cunningham, Giles Hammond, Gregg.
Paola Puppo INFN – Rome Thermal Noise Meeting – “Sapienza”-Rome - February 26 th 2008.
Advanced LIGO Quad Prototype Janeen Romie LSC, March 2004
Nergis Mavalvala MIT IAU214, August 2002
S. Rowan, M. Fejer, E. Gustafson, R. Route, G. Zeltzer
External forces from heat links in cryogenic suspensions
HAM SAS Test Plan at LASTI
Characterisation of the aLIGO monolithic suspensions
R&D in Glasgow MATERIALS ACTIVITY AIM Silica
Presentation transcript:

Conceptual Design for Advanced LIGO Suspensions Norna A Robertson University of Glasgow and Stanford University for the GEO suspension team +contribution from Mark Barton (Caltech) LSC meeting, Livingston, March 22 nd 2002 (Suspensions and Isolation Session) DCC Number: LIGO-G Z

Conceptual Design Conceptual design presented at Design Requirements Review, Sept 20 th, 2001 presentation DCC number: G D document DCC number:T D Design requirements document also presented (ref. Willems) Target sensitivity 10^-19 m/rtHz at 10 Hz at each of the main mirrors, and falling above this frequency (ref. discussion of low frequency cut-off, Fritschel, to follow). First prototype quad. pendulum suspension under test at MIT (ref. Mittleman, to follow)

Baseline Design for Adv. LIGO suspensions Fused silica ribbons suspending 40 kg sapphire mirror – lowest mass in quadruple pendulum Quadruple pendulum incorporating 3 stages of enhanced vertical isolation using blades Local control sensors/actuators or eddy current damping on top mass Overall length ~ 2 m All locally controlled freqs. in range ~ Hz Global control: hierarchical feedback, acting against quad. reaction pendulum

Schematic Diagram of Quadruple Pendulum

Current Baseline Design Final mass: 40 kg sapphire, 31.4 cm x 13 cm Penultimate mass: 72 kg (heavy glass) Upper masses: 36 kg, 36 kg Overall length: 1.7 m (from top blade to centre of mirror) Ribbon parameters: length 60 cm cross-section 113  m x 1.13 mm stress in ribbon 770 MPa

Quadruple Pendulum: Thermal Noise light solid curve – baseline, heavy solid curve – light penultimate mass, dotted line – sapphire internal thermal noise

Open Issues/Areas of Research: Overall Design and Thermal Noise Aspects Use of sapphire or silica (and size): downselect Nov 02 Choice of lower frequency cut-off: for low frequency require Long fibre length in final stage (~60 cm) Use of heavy penultimate mass Fibres/ribbons of low x-section Ribbons or fibres (constant or varying x-section) Research on manufacture, strength, reliability, loss, possible use of twists recent result – strength of ribbons >1.8GPa Bonding of silica to sapphire and heavy glass Losses Strength Final design of silica ears Plan to test assembly and suspension of sapphire ( 25 cm diam x 12cm thick) from heavy glass penultimate mass at Glasgow Materials issues (coating losses etc – as discussed in joint morning session) Engineering issues Research on above at Caltech, Glasgow, MIT, Stanford, Syracuse

Example of engineering issue: blade adjustment Experience with MIT quad prototype: position of blade tip in vertical direction more critical than in GEO design for mode frequencies and coupling. Prototype adjuster being developed in Glasgow pre adjustment post adjustment

Open Issues/Areas of Research: Local Control Use of active control - require isolation of sensor noise. Key factors: Sensor noise level Isolation of sensor noise by multiple pendulum Allowable level of residual motion (residual Qs) Possibility for global actuation to take over (certain degrees of freedom) Possible alternative – eddy current damping. Thermal noise level OK: for Q~10 (lowest mode) ~4 ×10^-20 m/rt Hz at 10 Hz Fixed Qs OK? Require diagnostic sensors and actuators as well? Plan to test eddy current damping of multiple pendulum at Glasgow

Longitudinal Transfer Function: Damping of Modes Active ControlEddy Current Damping Q=10.0 Q=7.2 Q=2.7 Q=2.8Q=10.0 Q=7.3 Q=1.9 Q=4.2

Sensor Noise – Transfer Functions (TF) Longitudinal (left) and vertical transfer function (TF) from sensor to mirror for quadruple pendulum with sensor at the top mass. Gain is such that lowest frequency peak has Q ~10 If gain decreased by factor f, Q increases by factor f. Let gain fraction = 1/f TF at 10 Hz: ~2x10^-7/rt Hz (long.) ~2x10^-4/rt Hz (vert.)

Residual Sensor Noise at Mirror at 10 Hz sensor noise × TF (× x-coupling) × gain fraction < 10^-19 m/rt Hz 10^-10 × 2 ×10^-7 × 5 ×10^-3 = 10^-19 m/rt Hz 10^-11 × 2 ×10^-7 × 5 ×10^-2 = 10^-19 m/rt Hz 5 × 10^-13 × 2 ×10^-7 × 1 = 10^-19 m/rt Hz Above figures hold for both longitudinal and vertical directions, where x-coupling factor for the latter taken as 1 ×10^-3. Current GEO sensors: 10^-10 m/rt Hz, with range ~ 1 mm

Open Issues/Areas of Research: Global Control Global control – issues Required bandwidth, magnitude of drive for different mirrors Details of hierarchical feedback Final stage – electrostatic or photon pressure? Violin mode damping – passive as in GEO? (small regions of PTFE coating used to reduce Q’s to ~10^6) Quad. prototype and subsequently LASTI controls prototypes will be used for investigations

Some Current Activities Controls prototypes for LASTI: Modecleaner (triple) detailed design underway at Caltech, based on GEO signal recycling mirror suspension Recycling mirror (triple) detailed design to follow, then test mass (quad) Electronics for controls p’types: design underway (Glasgow/Caltech) The triple prototypes will be tested on LIGO 1-type isolation stage Prototype quad currently at MIT to move to Caltech for further tests Modelling: Extended quad model developed by M Barton, compared to existing MATLAB model - see next slides.