Flat-Top Beam Profile Cavity Prototype

Slides:



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

Task M2 – Advanced Materials and Techniques for Resonant Detectors Motivation : Reduce thermal noise contribution to the acoustic detector noise budget.
Aspects of Fused Silica Suspensions in Advanced Detectors Geppo Cagnoli University of Texas at Brownsville and TSC LIGO, Hanford.
LIGO Laboratory1 Thermal Compensation Experience in LIGO Phil Willems- Caltech Virgo/LSC Meeting, Cascina, May 2007 LIGO-G Z.
COMPUTER MODELING OF LASER SYSTEMS
Thermally Deformable Mirrors: a new Adaptive Optics scheme for Advanced Gravitational Wave Interferometers Marie Kasprzack Laboratoire de l’Accélérateur.
Stefan Hild, Andreas Freise, Simon Chelkowski University of Birmingham Roland Schilling, Jerome Degallaix AEI Hannover Maddalena Mantovani EGO, Cascina.
Stefan Hild, Andreas Freise, Simon Chelkowski University of Birmingham Roland Schilling, Jerome Degallaix AEI Hannover Maddalena Mantovani EGO, Cascina.
Installation of a Four-mirror Fabry-Perot cavity at ATF 1.Our setup/goal 2.Why 4 mirrors ? 3.The ATF 4-mirror cavity 4.The optical scheme 5.The laser/cavity.
GWADW, May 2012, Hawaii D. Friedrich ICRR, The University of Tokyo K. Agatsuma, S. Sakata, T. Mori, S. Kawamura QRPN Experiment with Suspended 20mg Mirrors.
GWADW 2010 in Kyoto, May 19, Development for Observation and Reduction of Radiation Pressure Noise T. Mori, S. Ballmer, K. Agatsuma, S. Sakata,
Joshua Smith December 2003 Detector Characterization of Dual-Recycled GEO600 Joshua Smith for the GEO600 team.
Status of LCGT and CLIO Masatake Ohashi (ICRR, The University of TOKYO) and LCGT, CLIO collaborators TAUP2007 Sendai, Japan 2007/9/12.
Alban REMILLIEUX3 rd ILIAS-GW Annual General Meeting. London, October 26 th -27 th, New coatings on new substrates for low mechanical loss mirrors.
Optical Configuration Advanced Virgo Review Andreas Freise for the OSD subsystem.
Composite mirror suspensions development status Riccardo DeSalvo For the ELiTES R&D group WP1 & 2 JGW-xxxxxx.
Australia-Italy Australia 6, October 2005 LCGT project Kazuaki Kuroda LCGT Collaboration Cryogenics for LCGT.
T1 task- update Mike Plissi. 2 Motivation  Thermo-elastic noise is higher than the ‘intrinsic’ noise in crystalline materials  There are several sources.
LISA October 3, 2005 LISA Laser Interferometer Space Antenna Gravitational Physics Program Technical implications Jo van.
Gravitational Wave Detection Using Precision Interferometry Gregory Harry Massachusetts Institute of Technology - On Behalf of the LIGO Science Collaboration.
ICRR Seminar 2009/07/24 Cryogenics in CLIO Masatake Ohashi and the LCGT collaboration.
T Akutsu 1, S Telada 2, T Uchiyama 1, S Miyoki 1, K Yamamoto 1, M Ohashi 1, K Kuroda 1, N Kanda 3 and CLIO Collaboration. 1 ICRR, Univ. of Tokyo, 2 AIST,
R&D activities in Florence Geppo Cagnoli INFN and U. of Glasgow WG2 & WG3 Meeting – 27 th Apr Firenze.
LIGO Laboratory1 Enhanced and Advanced LIGO TCS Aidan Brooks - Caltech Hannover LSC-VIRGO Meeting, October 2007 LIGO-G Z.
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.
Advanced Virgo Optical Configuration ILIAS-GW, Tübingen Andreas Freise - Conceptual Design -
LIGO-G0200XX-00-M GWADW Isola d'Elba (Italy), May 281 Generation of flat-top beam in a “Mexican hat” Fabry-Perot cavity prototype for advanced GW.
Minimizing the Resonant Frequency of MGAS Springs for Seismic Attenuation System in Low Frequency Gravitational Waves Interferometers Maddalena Mantovani,
LIGO-G0200XX-00-M LIGO Scientific Collaboration1 First Results from the Mesa Beam Profile Cavity Prototype Marco Tarallo 26 July 2005 Caltech – LIGO Laboratory.
1 Mexican-Hat (Flat-Topped) Beams for Advanced LIGO LIGO-G Z Research by Sergey Strigin & Sergey Vyatchanin [MSU] (with advice from Vladimir Braginsky)
Flat top beam profile cavity prototype J. Agresti, E. D’Ambrosio, R. DeSalvo, J.M. Mackowski, A. Remillieux, B. Simoni, M. G. Tarallo, P. Willems CNRS.
1 Thermal noise and high order Laguerre-Gauss modes J-Y. Vinet, B. Mours, E. Tournefier GWADW meeting, Isola d’Elba May 27 th – Jun 2 nd, 2006.
Beams of the Future Mihai Bondarescu, Oleg Kogan, Yanbei Chen, Andrew Lundgreen, Ruxandra Bondarescu, David Tsang A Caltech - AEI - Cornell Collaboration.
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.
Virgo-Material “macro” group M.Punturo. VIRGO-MAT2 VIRGO-MAT components Virgo-MAT is composed by three INFN groups –Firenze/Urbino M.Lorenzini, G.Losurdo,
LIGO LaboratoryLIGO-G R Coatings and Their Influence on Thermal Lensing and Compensation in LIGO Phil Willems Coating Workshop, March 21, 2008,
1 Reducing Thermoelastic Noise by Reshaping the Light Beams and Test Masses Research by Vladimir Braginsky, Sergey Strigin & Sergey Vyatchanin [MSU] Erika.
LIGO-G050XXX-00-R Gingin’s Australia-Italia workshop on GW Detection The Mesa Beam Juri Agresti 1,2, Erika D’Ambrosio 1, Riccardo DeSalvo 1, Danièle Forest.
S. ChelkowskiSlide 1LSC Meeting, Amsterdam 09/2008.
AdV Thermal Compensation System Viviana Fafone AdV/aLIGO joint technical meeting, February 4, 2004.
Thermoelastic dissipation in inhomogeneous media: loss measurements and thermal noise in coated test masses Sheila Rowan, Marty Fejer and LSC Coating collaboration.
Studies of Thermal Loading in Pre-Modecleaners for Advanced LIGO Amber Bullington Stanford University LSC/Virgo March 2007 Meeting Optics Working Group.
LIGO Laboratory1 Thermal Compensation in LIGO Phil Willems- Caltech Baton Rouge LSC Meeting, March 2007 LIGO-G Z.
ACIGA High Optical Power Test Facility
Equivalence relation between non spherical optical cavities and application to advanced G.W. interferometers. Juri Agresti and Erika D’Ambrosio Aims of.
17/05/2010A. Rocchi - GWADW Kyoto2 Thermal effects: a brief introduction  In TM, optical power predominantly absorbed by the HR coating and converted.
LIGO-G R 1 Mexican Hat developments LMA cantilever measurements Riccardo DeSalvo LIGO Gravitational Wave Observatories California Institute of.
Aspen Flat Beam Profile to Depress Thermal Noise J.Agresti, R. DeSalvo LIGO-G Z.
C1) K. Tokmakov on behalf of the Advanced LIGO Suspensions Team Monolithic suspensions of the mirrors of the Advanced LIGO gravitational-wave detector.
Beams of the Future Mihai Bondarescu, Oleg Kogan, Yanbei Chen, Andrew Lundgreen, Ruxandra Bondarescu, David Tsang A Caltech - AEI - Cornell Collaboration.
Some considerations on radiative cooling V. Fafone, Y. Minenkov, I. Modena, A. Rocchi INFN Roma Tor Vergata.
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,
Thermal Compensation System TCS V. Fafone for the TCS Subsystem.
The VIRGO detection system
LIGO-G Z 1 Report of the Optics Working Group to the LSC David Reitze University of Florida March 20, 2003.
Active Vibration Isolation using a Suspension Point Interferometer Youichi Aso Dept. Physics, University of Tokyo ASPEN Winter Conference on Gravitational.
The Proposed Holographic Noise Experiment Rainer Weiss, MIT On behalf of the proposing group Fermi Lab Proposal Review November 3, 2009.
LIGO-G D Advanced LIGO Systems & Interferometer Sensing & Control (ISC) Peter Fritschel, LIGO MIT PAC 12 Meeting, 27 June 2002.
Lessons from CLIO Masatake Ohashi (ICRR, The University of TOKYO) and CLIO collaborators GWADW2012 Hawaii 2012/5/16.
Talk by Thorne, O’Shaughnessy, d’Ambrosio
External forces from heat links in cryogenic suspensions
The Mesa Beam Update Juri Agresti1, Erika D’Ambrosio1, Riccardo DeSalvo1, Danièle Forest2, Patrick Ganau2, Bernard Lagrange2, Jean-Marie Mackowski2, Christophe.
Ponderomotive Squeezing Quantum Measurement Group
Flat-Top Beam Profile Cavity Prototype: design and preliminary tests
First Results from the Mesa Beam Profile Cavity Prototype
Thermal noise and high order Laguerre-Gauss modes J-Y. Vinet, B
Flat-Top Beam Profile Cavity Prototype
Considerations about triangular and L-shaped detectors
Presentation transcript:

Flat-Top Beam Profile Cavity Prototype J.Agresti, E.D’Ambrosio, R. DeSalvo, J.M. Mackowsky, M. Mantovani, A. Remillieux, B. Simoni, P. Willems LIGO-G040412-00-D Hanford August 2004

Motivations for a flat-top beam: Advanced-Ligo sensitivity (Sapphire Mirror Substrates) Dominated by test-masses thermoelastic and coating thermal noises. Can we reduce the influence of thermal noise on the sensitivity of the interferometer? Hanford August 2004

Thermoelastic Noise: Mirror surface Created by stochastic flow of heat within the test mass Fluctuating hot spots and cold spots inside the mirror Fluctuating bumps Expansion in the hot spots and contraction in the cold spots creating fluctuating bumps and valleys on the mirror’s surface Interferometer output: proportional to the test mass average surface position, sampled according to the beam’s intensity profile. Hanford August 2004

Gaussian beam Mirror surface As large as possible (within diffraction loss constraint). The sampling distribution changes rapidly following the beam power profile Larger-radius, flat-top beam will better average over the mirror surface. Hanford August 2004

The mirror shapes match the phase front of the beams. Diffraction prevents the creation of a beam with a rectangular power profile…but we can build a nearly optimal flat-top beam: Flat-top beam Gaussian beam The mirror shapes match the phase front of the beams. Hanford August 2004

Comparison between the two beams ( Same diffraction losses ) Hanford August 2004

Indicative thermal noise suppression trends Substrate thermoelastic noise Coating thermal noise Substrate thermal noise Exact results require accurate information on material properties (Q-factors) Expected gain in sensitivity ~ 3 Hanford August 2004

Goals of our project: Build a small optical cavity to verify the behaviour of the flat top beams and gain experience in their generation and control. Hanford August 2004

Misalignment produces coupling between modes We will investigate the modes structure and characterize the sensitivity to perturbations when non Gaussian beams are supported inside the cavity. Misalignment produces coupling between modes Hanford August 2004

Design of the test cavity : Rigid cavity suspended under vacuum Flat folding mirror Thermal shield Spacer plate INVAR rod Vacuum pipe Flat input mirror folded cavity length MH mirror Hanford August 2004

Optical and mechanical design: Injection Gaussian beam designed to optimally couple to the cavity. Required finesse F = 100 to suppress Gaussian remnants in the cavity. Length stability: ~ 5 nm INVAR rods (low thermal expansion coefficient). Stabilized temperature. Vacuum eliminates atmospheric fluctuations of optical length. Ground vibrations can excite resonance in our interferometer structure: suspension from wires and Geometrical-Anti-Spring blades. Mirror’s size constrained by beam shape and diffraction losses Hanford August 2004

Diffraction losses of ~ 1ppm requires mirror’s radius >1 cm. Our Mexican Hat mirror: Diameter set by diffraction losses and technical difficulties… Diffraction losses of ~ 1ppm requires mirror’s radius >1 cm. Hanford August 2004

LMA’s Technique to build Mexican Hat mirrors Rough Shape Deposition: Coating the desired Mexican Hat profile using a pre-shaped mask Achievable precision ~60nm Peak to Valley Corrective coating: Measurement of the achieved shape Coating thickness controlled with a precision <10 nm. Maximum slope ~ 500nm/mm Hanford August 2004

Cavity Suspensions Suspension System: V~ 0.6 Hz H ~ 1 Hz GAS spring wires Hanford August 2004

Cavity Vacuum & Thermal Shield Suspension view Suspension wires Vacuum pipe Thermal shield Spacer plate INVAR rod Hanford August 2004

Suspension at work! Hanford August 2004

Schedule for the future Complete building the cavity including the optics and the electronics Lock the cavity with spherical mirror (test the apparatus) Switch to Mexican-Hat mirror as soon as available Characterization of Flat-top beam modes and misalignment effects Flat topped beam inside a nearly-concentric cavity: same power distribution over the mirrors but less sensitive to misalignment. Overcome the technical limitation on the slope of the coating…not impossible. Next possible developments Hanford August 2004