LIGO Laboratory1 Thermal Compensation Experience in LIGO Phil Willems- Caltech Virgo/LSC Meeting,...
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Transcript of LIGO Laboratory1 Thermal Compensation Experience in LIGO Phil Willems- Caltech Virgo/LSC Meeting,...
![Page 1: LIGO Laboratory1 Thermal Compensation Experience in LIGO Phil Willems- Caltech Virgo/LSC Meeting, Cascina, May 2007 LIGO-G070339-00-Z.](https://reader030.fdocuments.us/reader030/viewer/2022032702/56649ca45503460f949641d2/html5/thumbnails/1.jpg)
LIGO Laboratory 1
Thermal Compensation Experience in LIGO
Phil Willems- Caltech
Virgo/LSC Meeting, Cascina, May 2007
LIGO-G070339-00-Z
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LIGO Laboratory 2
The Essence of the Problem, and of its Solution
Power recycling cavity Arm cavity
Optical power absorbed by the ITM creates a thermal lens in the (marginally stable) recycling cavity, distorting the RF sideband fields there.
ITM ETMPRM
Add optical power to the ITM to erase the thermal gradient, leaving a uniformly hot, flat-profile substrate.
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LIGO Laboratory 3
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LIGO Laboratory 4
LIGO CO2 Laser Projector Thermal Compensator
CO2 Laser
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Over-heat Correction
Inhomogeneous Correction
Under-heat Correction
ZnSe Viewport Over-heat pattern
Inner radius = 4cm Outer radius =11cm
•Imaging target onto the TM limits the effect of diffraction spreading
•Modeling suggests a centering tolerance of 10 mm is required
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LIGO Laboratory 5
CO2 Laser Projector Layout
Image planes here, here, and at ITM HR face
over-heat correction
under-heat correction
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LIGO Laboratory 6
Thermal Compensation as Installed
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TCS Servo Control
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LIGO Laboratory 8
Thermal Compensation Controls
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LIGO Laboratory 9
Heating Both ITMs in a Power-Recycled Michelson
No Heating 30 mW 60 mW 90 mW
120 mW 150 mW 180 mW Carrier
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LIGO Laboratory 10
RF Sideband Power Buildup
•Both ITMs heated equally
•Maximum power with 180 mW total heat
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LIGO Laboratory 11
RF Sideband Power Buildup
•Only ITMy heated
•Maximum power with 120 mW total heat
•Same maximum power as when both ITMs heated
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LIGO Laboratory 12
Common-mode Bulls-eye Sensor
Good mode overlap of RF sideband with carrier determines optimal thermal compensation- so we measure the RF mode size to servo TCS.
Sensor output is proportional to LG10 mode content of RF sidebands.
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LIGO Laboratory 13
Differential TCS- Control of AS_I
AS_Q: RF sidebands at dark port create swinging LO field- when arm imbalance detunes carrier from dark fringe signal appears at quadrature phase
AS_I: dark fringe means no carrier, RF sideband balance means no LO at this phase- there should be no signal.
Yet, this signal dominates the RF photodetection electronics!--there must be carrier contrast defect--there must be RF sideband imbalance--apparently, slightly imperfect ITM HR surfaces mismatch the arm modes, creating the contrast defect. TCS provides the cure.
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LIGO Laboratory 14
Thermal Time Scales
After locking at high power, the heat distribution in the ITM continues to evolve for hours. To maintain constant thermal focusing power requires varying TCS power.
In practice, constant TCS power is often enough.
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TCS Noise Issues
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LIGO Laboratory 16
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LIGO Laboratory 17
TCS Noise Coupling Mechanisms
Thermoelastic (TE)- fluctuations in locally deposited heat cause fluctuations in local thermal expansion
Thermorefractive (TR)- fluctuations in locally deposited heat cause fluctuations in local refractive index
Flexure (F)- fluctuations in locally deposited heat cause fluctuations in global shape of optic
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LIGO Laboratory 18
Flexure Noise- A Simple Model
probe beam
heating
heating
slat mirror
CM lineA very skinny mirror with ‘annular’ heating
The probe beam sees the mirror move at the center due to wiggling far from center
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LIGO Laboratory 19
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LIGO Laboratory 20
TCS Injected Noise Spectrum
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LIGO Laboratory 21
TCS-Induced Transients
Upgraded TCS controllers use rotating polarizers to adjust power.
Every 10 seconds, the polarizers reorient.
Every 10 seconds a glitch appears in TCS.
Most glitches are well below LIGO sensitivity.
After discovering this mechanism, polarizer stage motion was smoothed.
Impulses in TCS output can produce impulsive signals in the interferometer output: laser switching, mode transitions, and more obscure sources of noise…
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Quality of Compensation
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LIGO Laboratory 23
Projector Heating Patterns
Annulus Mask Central Heat Mask
•Intensity variations across the images due to small laser spot size
•Projection optics work well
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LIGO Laboratory 24
Expected Profile of Thermal Lens
Expected uncompensated phase profile. Expected compensated phase profile.
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LIGO Laboratory 25
Actual Profile of Thermal Lens
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LIGO Laboratory 26
‘Gold Star’ Mask Design
“star”- from hole pattern“gold”- gold coating to reduce power
absorptionHole pattern is clearly not ideal but
diffraction and heat diffusion smooth the phase profile
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LIGO Laboratory 27
Improved Carrier Power with Gold Star Mask
Why this helps the carrier is mysterious, but we’ll take it
optical gain up 5%
carrier recycling gain up 10%
Note: no similar improvement in the sideband power was observed
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Enhanced LIGO TCS
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LIGO Laboratory 29
Our Need for Power
Initial LIGO runs at ~7W input power Enhanced LIGO will run at ~30W input power
» 4-5x more absorbed power
» Naively, ~4-5x more TCS power needed
» Practically, more power even than this may be needed since LIGO point design is meant to make TCS unnecessary at 6W
» Or less power, if we can clean the mirrors
» Correction of static mirror curvature errors clouds this picture
Our current projectors are not adequate
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LIGO Laboratory 30
Test Mass Absorption Measurement Technique-Spot Size
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LIGO Laboratory 31
Enhanced LIGO TCS Projector
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LIGO Laboratory 32
Axicon design proposed by II-VI for Enhanced LIGO
The Axicon
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LIGO Laboratory 33
Conclusions
TCS becomes essential instantly after it is installed. TCS works even though thermal lens is poorly
known. TCS is flexible (all three IFOs have different
installations). The external projector design is flexible and easy to
maintain. Unexpected behaviors and uses (e.g. AS_I, carrier
arm coupling, static correction) appear during commissioning.
Noise couplings and injections can be rich but are predictable, measurable, not fatal.