Scattering loss (Hiro CIT on April 11, 2007 G0702401 Extra loss ~ 40ppm / mirror microroughness = 4~5 ppm? Visibility, recycling gain, large.

Slides:



Advertisements
Similar presentations
G v1 1 The reality of Mirrors? GWADW May 15, 2012 GariLynn Billingsley Liyuan Zhang Zygo… CSIRO…
Advertisements

Hiro Yamamoto LLO April 3, 2014 LIGO-G Core Optics related loss hierarchy of aLIGO Hiro Yamamoto LIGO/Caltech Introduction Loss related to geometry.
Laser Interferometer Gravitational-wave Detectors: Advancing toward a Global Network Stan Whitcomb LIGO/Caltech ICGC, Goa, 18 December 2011 LIGO-G v1.
Spring LSC 2001 LIGO-G W E2 Amplitude Calibration of the Hanford Recombined 2km IFO Michael Landry, LIGO Hanford Observatory Luca Matone, Benoit.
Atmospheric Dispersion Correctors. ZnSe linear ADC Plots are for 60° zenith angle < 10 mas residual dispersion for λ= μ ZnSe transmission starts.
LSC-Virgo Hannover on October 24, 2007 G E1 Scattering Loss Hiro Yamamoto - Caltech LIGO LIGO I mirror loss estimation surface figure,
Stefan Hild and Andreas Freise University of Birmingham Advanced Virgo telecon, June 2008 Beam sizes and mirror curvatures for Advanced Virgo.
LIGO-G W LIGO Scientific Collaboration Meeting – LLO March Summary of recent measurements of g factor changes induced by thermal loading.
Progress on Laser Induced Damage Studies of Grazing Incidence Metal Mirrors Mark S. Tillack T. K. Mau Mofreh Zaghloul Laser-IFE Program Workshop May 31-June.
FFT study of the realistic Optics of LIGO I July 12th, 2004 Commissioning meeting Hiro Yamamoto, Biplab Bhawal, Xiao Xu (CIT-SURF)  LIGO I mirror phase.
Laser &Optics of LCGT 2011/10/5(Wed) Norikatsu Mio Photon Science Center University of Tokyo EGO-ICRR Meeting 2011/10/4-5.
BS and Mirrors for the LCGT Norikatsu Mio, PSC Univ. of Tokyo Eiichi Hirose, ICRR Univ. of Tokyo December 13, 2011 CSIRO, Lindfield Australia.
Stefan Hild, Andreas Freise, Simon Chelkowski University of Birmingham Roland Schilling, Jerome Degallaix AEI Hannover Maddalena Mantovani EGO, Cascina.
Modeling beam and mirror distortions using modal models: FINESSE V.1 Charlotte Bond, Daniel Brown and Andreas Freise Tokyo Institute of Technology 21/06/2013.
1 G Mike Smith Gravitational Waves & Precision Measurements.
Overview of Research in the Optics Working Group Gregory Harry, on behalf of the OWG Massachusetts Institute of Technology July 25, 2007 LSC Meeting –
Status of LCGT and CLIO Masatake Ohashi (ICRR, The University of TOKYO) and LCGT, CLIO collaborators TAUP2007 Sendai, Japan 2007/9/12.
Optical Configuration Advanced Virgo Review Andreas Freise for the OSD subsystem.
LIGO-G Black holes, Einstein, and space-time ripples Peter R. Saulson Syracuse University.
G M 1 Advanced LIGO Update David Shoemaker LSC/Virgo MIT July 2007.
G v5 1 Core Optics Components Technical Status NSF Review of Advanced LIGO Project April 2011 GariLynn Billingsley.
Design of a Lightweight Mounted Tip/Tilt Mirror
LIGO- G D The LIGO Instruments Stan Whitcomb NSB Meeting LIGO Livingston Observatory 4 February 2004.
Gravitational Wave Detection Using Precision Interferometry Gregory Harry Massachusetts Institute of Technology - On Behalf of the LIGO Science Collaboration.
DFG-NSF Astrophysics Workshop Jun 2007 G Z 1 Optics for Interferometers for Ground-based Detectors David Reitze Physics Department University.
Koji Arai – LIGO Laboratory / Caltech LIGO-G v2.
Status of Beams L. Page & C. Barnes et al.. Why do we need to model the beams? Computing solid angles (T_jup) & windows from the raw maps depends on the.
Aerosol Limits for Target Tracking Ronald Petzoldt ARIES IFE Meeting, Madison, WI April 22-23, 2002.
Haifeng Huang and Kevin K. Lehmann
40m AOS DRD, G R1 40m Auxiliary Optics Support Design Requirements Document & Conceptual Design Michael Smith 10/18/01 Stray Light Control Initial.
1st Advanced Virgo Review – November 3-4, 2008 – L. Pinard 1 Mirrors Sub-System Overview  Introduction  Scope of the subsystem, main tasks  Substrates.
LIGO LaboratoryLIGO-G R Coatings and Their Influence on Thermal Lensing and Compensation in LIGO Phil Willems Coating Workshop, March 21, 2008,
Advanced LIGO Simulation, 6/1/06 Elba G E 1 ✦ LIGO I experience ✦ FP cavity : LIGO I vs AdvLIGO ✦ Simulation tools ✦ Time domain model Advanced.
Coating Program Update Gregory Harry LIGO/MIT on behalf of the Coating Working Group March 22, 2006 LSC Meeting – LHO G R.
Hiro Yamamoto GWADW Girdwood, Alaska LIGO-G Beam Splitter in aLIGO Hiro Yamamoto LIGO/Caltech BS02 to BS05? larger BS? BS in aLIGO IFO for.
G Z Test Mass Butterfly Modes and Alignment Amber Bullington, Stanford University Warren Johnson, Louisiana State University LIGO Livingston Detector.
First DR FFT Results on Advanced LIGO Using Perfect and Imperfect Optics By Ken Ganezer, George Jennings, and Sam Wiley CSUDH LIGO-G Z by Ken.
LSC-Virgo Caltech on March 20, 2008 G E1 AdvLIGO Static Interferometer Simulation AdvLIGO simulation tools  Stationary, frequency domain.
Status of Modeling of Damage Effects on Final Optics Mirror Performance T.K. Mau, M.S. Tillack Center for Energy Research Fusion Energy Division University.
TCS and IFO Properties Dave Ottaway For a lot of people !!!!!! LIGO Lab Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of.
Elba 2006 Suppressing Parametric Instabilities Li Ju, Slawek Gras, Pablo Barriga, Chonnong Zhao, Jerome Degallaix, David Blair, Yaohui Fan, Zewu Yan University.
A bin-free Extended Maximum Likelihood Fit + Feldman-Cousins error analysis Peter Litchfield  A bin free Extended Maximum Likelihood method of fitting.
Equivalence relation between non spherical optical cavities and application to advanced G.W. interferometers. Juri Agresti and Erika D’Ambrosio Aims of.
The Effect of Transverse Shifts on the LIGO Interferometer Doug Fettig - Oregon State University Mentor: Biplab Bhawal.
Effects of as-built Mirrors - analysis using FFT - Hiro Yamamoto, Biplab Bhawal, Xiao Xu, Raghu Dodda (SLU)  LIGO I mirror phase map  FFT tools  Thermal.
1 DC readout for Virgo+? E. Tournefier WG1 meeting, Hannover January 23 rd,2007 DC vs AC readout: technical noises Output mode cleaner for DC readout.
06/2006I.Larin PrimEx Collaboration meeting  0 analysis.
LIGO-G D1 Losses in LHO HR Surfaces W. Kells LIGO Laboratory, Caltech With assistance from: H. Radkins, V. Parameshwaraiah, D. Cook, L. Zhang,
G D Workshop on Optical Coating, March 20-21, The Coating Scattering and Absorption Measurements of LIGO I mirrors at Caltech Liyuan Zhang,
LIGO Scientific Collaboration
LIGO-G D 1 R&D Technical Review LIGO Lab October 8, 2002 Core Optics.
Optical Coatings for Gravitational Wave Detection Gregory Harry Massachusetts Institute of Technology - On Behalf of the LIGO Science Collaboration - August.
Hiro Yamamoto LIGO seminar on Dec. 1st, 2015 LIGO-G aLIGO test masses, revisited  Scattering and loss by test mass  Discrepancy between the measured.
LIGO-G D Core Optics Components (COC) Polishing Pathfinder Kickoff Advanced LIGO Project GariLynn Billingsley Caltech.
The Proposed Holographic Noise Experiment Rainer Weiss, MIT On behalf of the proposing group Fermi Lab Proposal Review November 3, 2009.
1 Cascina – October 19, 2011 ASPERA Forum Laurent Pinard Substrates, Polishing, Coatings and Metrology for the 2 nd generation of GW detector Laurent PINARD.
Light In this presentation: 1)What is light? 2)Electromagnetic Spectrum 3)Interactions of Light 4)Color.
Hiro Yamamoto LVC March 15 th, 2016, Pasadena CA LIGO-G Mirror scattering loss analysis by integrating sphere measurement  Scattering and loss.
LIGO-G v1 Inside LIGO LIGO1 Betsy Weaver, GariLynn Billingsely and Travis Sadecki 2016 – 02 – 23 at CSIRO, Lindfield.
LIGO-G Z Bilenko I.A. Gromova E.S. 1 Recent Results on the Measurement of Transmission and Scattering Structure on Doped and Non-doped Mirrors.
Characterization of Advanced LIGO Core Optics
Advanced LIGO status Hiro Yamamoto LIGO lab/Caltech
LIGO Core Optics: a decade of development and experience
W. Kells LIGO Laboratory, Caltech C. Vorvick LIGO Laboratory, Hanford
Mark S. Tillack T. K. Mau Mofreh Zaghloul
LIGO Core Optics: a decade of development and experience
Modeling of Advanced LIGO with Melody
Scattering Loss Hiro Yamamoto - Caltech LIGO
W. Kells LIGO Laboratory, Caltech C. Vorvick LIGO Laboratory, Hanford
LIGO Scientific Collaboration
Presentation transcript:

Scattering loss (Hiro CIT on April 11, 2007 G Extra loss ~ 40ppm / mirror microroughness = 4~5 ppm? Visibility, recycling gain, large angle scatterometer, etc are consistent with 150 ppm loss per arm known loss per arm  surface figure (  ppm / mirror x 2  ETM transmission : 7 ppm  absorption : 4ppm / mirror x 2  diffractive loss : 2ppm known = 80 ppm / arm or 40 ppm / mirror FFT calculation with phasemaps(  extra loss as a free parameter

Scattering loss (Hiro CIT on April 11, 2007 G Advanced LIGO total arm loss budget = 70ppm known loss : ~ 50 ppm / arm  diffraction : 0.4 ppm  absorption : 0.5 ppm x 2  surface figure : 20ppm x 2  ETM transmission : 7 ppm 11 ppm / mirror for microroughness and all other losses LIGO I mirror : 40 ppm

Scattering loss (Hiro CIT on April 11, 2007 G Summary rms = 0.17 nm loss = 5.5ppm 3.8cm -1 CSIRO rms FFT 20-30ppm + 10 ppm non smooth scattering (C 1D->2D =1.2) Bill’s scatterometer H1 ETMy ? ? Liyuan’s integrating sphere 20ppm? CSIRO polished surface Mike ITMy [1] fit = 7e -19 f rms = 0.33 nm loss = 21ppm [2] [3] [4] [5]

Scattering loss (Hiro CIT on April 11, 2007 G CSIRO RMS = 0.5 x true RMS 1d topo data - tilt - curvature using 1024 data points  rms = 0.17nm generate data using spectrum f -2  rms = 0.12 using raw data  rms = using data with  tilt and curvature subtracted loss ~ rms 2

Scattering loss (Hiro CIT on April 11, 2007 G Integrating sphere data Liyuan ? 1cm x 1cm 0.2mm beam size 0.1mm step mean

Scattering loss (Hiro CIT on April 11, 2007 G Point scattering loss ~ 10ppm      »  cut ppm bad points 1.5 ° point scattering : uniform ~10 ppm smooth roughness : BRDF(θ)~θ loss(>3.8cm -1 ) = (1.5 ° /380    x 15ppm = 100 ppm

Scattering loss (Hiro CIT on April 11, 2007 G Fine structure in mm region

Scattering loss (Hiro CIT on April 11, 2007 G loss per mirror with different FFT bin size or loss from different frequency Loss calculated using a bin size : assume no loss with spatial frequency longer than 1/bin size loss(1/bin2) - loss(1/bin1) = loss coming spatial freq between 1/bin2 - 1/bin1 should analyze with proper 2D down sampling ?