Laser Interferometer Gravitational-wave Observatory1 Characterization of LIGO Input Optics...

Laser Interferometer Gravitational-wave Observatory

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

Rana Adhikari

Peter Fritschel

Mike Zucker

Caltech

Jordan Camp

Bill Kells

Nergis Mavalvala

David Ottaway

Daniel Sigg

Stan Whitcomb

Presented by Haisheng Rong atLSC Meeting 7

Hanford, 15-17 August 2000

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

Input Optics Components

IO System Interfaces

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

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%

MC Output Beam Pointing Stability

» Long-term drift ~4rad/hr

» Beam jitter 10 -10 rad/rtHz at f >20Hz

MC cavity linewidth measurements

Ringdown Transfer function

MC linewidth measurement results

Internal Q’s of MC mirrors

MC - a sensitive analyzer cavity

Frequency noise of the PSL

Effect of the vertical mirror motion

PSD of MC length control signal

= 0.62 mrad

: Angle of MC plane wrt. horizontal

Frequency noise of MC output

Frequency noise measured with 2k FP arm cavity

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

Laser Interferometer Gravitational-wave Observatory1 Characterization of LIGO Input Optics...

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