Presentation is loading. Please wait.

Presentation is loading. Please wait.

Laser Interferometer Gravitational-wave Observatory1 Characterization of LIGO Input Optics University of Florida Thomas Delker Guido Mueller Malik Rakhmanov.

Published by Modified over 8 years ago

Similar presentations

Presentation on theme: "Laser Interferometer Gravitational-wave Observatory1 Characterization of LIGO Input Optics University of Florida Thomas Delker Guido Mueller Malik Rakhmanov."— Presentation transcript:

1 Laser Interferometer Gravitational-wave Observatory1 Characterization of LIGO Input Optics University of Florida Thomas Delker Guido Mueller Malik Rakhmanov David Reitze Haisheng Rong Qi-ze Shu David Tanner Sanichio Yoshida MIT Rana Adhikari Peter Fritschel Mike Zucker Caltech Jordan Camp Bill Kells Nergis Mavalvala David Ottaway Daniel Sigg Stan Whitcomb Presented by Haisheng Rong at LSC Meeting 7 Hanford, 15-17 August 2000

2 Laser Interferometer Gravitational-wave Observatory2 Input Optics System Primary Functions of the IO System  Conditioning of the PSL output  Frequency, Intensity and beam pointing stability  Filter high-order modes  Mode matching and beam delivery  Optical isolation  RF sidebands generation for IFO sensing

3 Laser Interferometer Gravitational-wave Observatory3 Input Optics Components IFO

4 Laser Interferometer Gravitational-wave Observatory4 IO System Interfaces

5 Laser Interferometer Gravitational-wave Observatory5 Status of the IO System LHO 2k »Operational since 08/99 »Major characterization measurements finished »Integration with 2k IFO arm cavity successful »Modification and realignment 04/00 – 05/00 LLO 4k »Mode cleaner locked in 03/00 »Characterization and improvement 03/00 – 06/00 »IO realignment 06/00 – 08/00 LHO 4k »Installation started 07/00

6 Laser Interferometer Gravitational-wave Observatory6 Characterization Measurements Mode Cleaner Length »Measured with RF resonant side band detuning method. »Uncertainty / Drift ~ 3ppm (50  m ) »Position Accuracy < 1mm MC Transmission »0.98  0.05 Mode Matching into the 2k Arm Cavity »Power Coupling: 95%-98%

7 Laser Interferometer Gravitational-wave Observatory7 Characterization Measurements MC Output Beam Pointing Stability »Long-term drift ~4  rad/hr »Beam jitter 10 -10 rad/rtHz at f >20Hz

8 Laser Interferometer Gravitational-wave Observatory8 Characterization Measurements MC cavity linewidth measurements RingdownTransfer function

9 Laser Interferometer Gravitational-wave Observatory9 Characterization Measurements MC linewidth measurement results

10 Laser Interferometer Gravitational-wave Observatory10 Characterization Measurements Internal Q’s of MC mirrors

11 Laser Interferometer Gravitational-wave Observatory11 MC - a sensitive analyzer cavity Frequency noise of the PSL

12 Laser Interferometer Gravitational-wave Observatory12 Effect of the vertical mirror motion PSD of MC length control signal  = 0.62 mrad  = 0  :Angle of MC plane wrt. horizontal

13 Laser Interferometer Gravitational-wave Observatory13 Frequency noise of MC output Frequency noise measured with 2k FP arm cavity

14 Laser Interferometer Gravitational-wave Observatory14 Coming up Lock MC at designed input power »Scattered laser light interacts with suspension local sensors, causing angular instability »Solution –Phase sensitive detection (coherent sensor) –New shadow sensors

Download ppt "Laser Interferometer Gravitational-wave Observatory1 Characterization of LIGO Input Optics University of Florida Thomas Delker Guido Mueller Malik Rakhmanov."

Similar presentations

19. October 2004 A. Freise Automatic Alignment using the Anderson Technique A. Freise European Gravitational Observatory Roma 21.10.2004.

19. October 2004 A. Freise Automatic Alignment using the Anderson Technique A. Freise European Gravitational Observatory Roma
8/13/2004 Stefan Ballmer, MIT / LIGO Hanford 1 Length and angular control loops in LIGO Stefan Ballmer Massachusetts Institute of Technology LIGO Hanford.

8/13/2004 Stefan Ballmer, MIT / LIGO Hanford 1 Length and angular control loops in LIGO Stefan Ballmer Massachusetts Institute of Technology LIGO Hanford.
LIGO - G060008-00-R 1 HAM SAS Test Plan at LASTI David Ottaway November 2005 LIGO-G060184-00-Z.

LIGO - G R 1 HAM SAS Test Plan at LASTI David Ottaway November 2005 LIGO-G Z.
G1200688-v1Squeezed Light Interferometry1 Squeezed Light Techniques for Gravitational Wave Detection July 6, 2012 Daniel Sigg LIGO Hanford Observatory.

G v1Squeezed Light Interferometry1 Squeezed Light Techniques for Gravitational Wave Detection July 6, 2012 Daniel Sigg LIGO Hanford Observatory.
Koji Arai – LIGO Laboratory / Caltech LIGO-G1401147-v2.

Koji Arai – LIGO Laboratory / Caltech LIGO-G v2.
LIGO-G000160-00-W Status of LIGO Installation and Commissioning Frederick J. Raab, LIGO Hanford Observatory.

LIGO-G W Status of LIGO Installation and Commissioning Frederick J. Raab, LIGO Hanford Observatory.
LIGO-G020223-01-W Proposed LHO Commissioning Activities in May 02 Fred Raab 29 Apr 02.

LIGO-G W Proposed LHO Commissioning Activities in May 02 Fred Raab 29 Apr 02.
Performance of the LIGO Pre-stabilized Laser System Rick Savage LIGO Hanford Observatory Ninth Marcel Grossmann Meeting on General Relativity Rome 2000.

Performance of the LIGO Pre-stabilized Laser System Rick Savage LIGO Hanford Observatory Ninth Marcel Grossmann Meeting on General Relativity Rome 2000.
Investigation of the influence of suspended optic’s motion on LIGO detector sensitivity Sanichiro Yoshida Southeastern Louisiana University.

Investigation of the influence of suspended optic’s motion on LIGO detector sensitivity Sanichiro Yoshida Southeastern Louisiana University.
Measurement of the laser beam profile at PSL to Mode Cleaner interface for the 40 Meter Prototype Interferometer A table of contents 1. Introduction 1.1.

Measurement of the laser beam profile at PSL to Mode Cleaner interface for the 40 Meter Prototype Interferometer A table of contents 1. Introduction 1.1.
TeV Particle Astrophysics August 2006 Caltech Australian National University Universitat Hannover/AEI LIGO Scientific Collaboration MIT Corbitt, Goda,

TeV Particle Astrophysics August 2006 Caltech Australian National University Universitat Hannover/AEI LIGO Scientific Collaboration MIT Corbitt, Goda,
Generation of squeezed states using radiation pressure effects David Ottaway – for Nergis Mavalvala Australia-Italy Workshop October 2005.

Generation of squeezed states using radiation pressure effects David Ottaway – for Nergis Mavalvala Australia-Italy Workshop October 2005.
Recent Developments toward Sub-Quantum-Noise-Limited Gravitational-wave Interferometers Nergis Mavalvala Aspen January 2005 LIGO-G050044-00-R.

Recent Developments toward Sub-Quantum-Noise-Limited Gravitational-wave Interferometers Nergis Mavalvala Aspen January 2005 LIGO-G R.
G030527-00-D Tasks After S3 Commissioning Meeting, Oct 6., 2003 Peter Fritschel, Daniel Sigg.

G D Tasks After S3 Commissioning Meeting, Oct 6., 2003 Peter Fritschel, Daniel Sigg.
G1100445-v3 Integration Planning April 25, 2011 Valera Frolov, Daniel Sigg, Peter Fritschel NSF Review, LLO.

G v3 Integration Planning April 25, 2011 Valera Frolov, Daniel Sigg, Peter Fritschel NSF Review, LLO.
LIGO-G010406-00-D Commissioning PAC11, 2001 Daniel Sigg, LIGO Hanford Observatory.

LIGO-G D Commissioning PAC11, 2001 Daniel Sigg, LIGO Hanford Observatory.
LIGO-G000159-00-W Status of LIGO Installation and Commissioning Frederick J. Raab, LIGO Hanford Observatory.

LIGO-G W Status of LIGO Installation and Commissioning Frederick J. Raab, LIGO Hanford Observatory.
G030460-00-R DC Readout for Advanced LIGO P Fritschel LSC meeting Hannover, 21 August 2003.

G R DC Readout for Advanced LIGO P Fritschel LSC meeting Hannover, 21 August 2003.
Design of Stable Power-Recycling Cavities University of Florida 10/05/2005 Volker Quetschke, Guido Mueller.

Design of Stable Power-Recycling Cavities University of Florida 10/05/2005 Volker Quetschke, Guido Mueller.
Test mass dynamics with optical springs proposed experiments at Gingin Chunnong Zhao (University of Western Australia) Thanks to ACIGA members Stefan Danilishin.

Test mass dynamics with optical springs proposed experiments at Gingin Chunnong Zhao (University of Western Australia) Thanks to ACIGA members Stefan Danilishin.

Similar presentations

Ads by Google