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Published byPresley Dungey Modified about 1 year ago

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LIGO-G v2 Form F v1 Advanced LIGO1 SCATTERED LIGHT CONTROL in ADVANCED LIGO Michael Smith LIGO Laboratory Caltech, Pasadena, CA

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LIGO-G v2 Form F v1 LIGO II2 Scattered Light Displacement Noise Theory Min Gravity Wave Signal Scattered Light Requirement: »Phase Shift due to motion of surface »Noise

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LIGO-G v2 Form F v1 LIGO II3 Stray Light Design Requirement <1/10 of the thermal noise limit strain

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LIGO-G v2 Form F v1 LIGO II4 Total Scattered Light Displacement Noise from Multiple Sources, m/rtHz Sources Are Random, Add in Quadrature Scattered Light Transfer functions

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LIGO-G v2 Form F v1 LIGO II5 Scattered Light Transfer Functions from FFT simulation LIGO T Hiro Yamamoto Worse scatter paths

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LIGO-G v2 Form F v1 LIGO II6 Scattered Injection Points

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LIGO-G v2 Form F v1 LIGO II7 Scattered Power into IFO Scattered power depends upon: »Incident power hitting scattering surface, W »Bidirectional Scatter Distribution Function of scattering surface, BRDF, sr^-1 »Solid angle subtended by the mode inside IFO arm, sr »Relative area ratio of IFO mode area to the area of incident beam waist »Transmissivity of optical path from scatter surface to the injection point

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LIGO-G v2 Form F v1 LIGO II8 Measuring BRDF

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LIGO-G v2 Form F v1 LIGO II9 Cleanliness Is Next To Godliness Dust particles scattering light on the sample surface!

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LIGO-G v2 Form F v1 LIGO II10 Example Of BRDF Data

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LIGO-G v2 Form F v1 LIGO II11 Motion Of Scattering Surface, m/rtHz

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LIGO-G v2 Form F v1 LIGO II12 Scattered Light Control Suspended Output Faraday Isolator from Dark-port Signal to Gravity Wave Detector Eddy current damping magnets BS for squeezed light injection

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LIGO-G v2 Form F v1 LIGO II13 Output Faraday Isolator Scatter Displacement Noise Damping to frame Self damping

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LIGO-G v2 Form F v1 LIGO II14 Other Examples Arm Cavity Baffle Wide-angle Baffle Cavity Beam Dump Damped suspension Test mass

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LIGO-G v2 Form F v1 LIGO II15 Modeling Of Ghost Beams Modeling with ZEMAX: beam splitter chamber—ghost beams from internal reflections in the wedged compensation plate next to Input Test Mass (ITM) BS elliptical baffle from ITMX

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LIGO-G v2 Form F v1 LIGO II16 Putting It All Together Scattered Light Meets Requirement!! Total Scatter Requirement Thermal noise

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