geo 600 status
DESCRIPTION
GEO 600 STATUS. Andreas Freise on behalf of Hartmut Grote for the LSC. Gravitational Waves: New Frontier Seoul, 16.01.2013 LIGO-G1300030. Ground based detector network. GWIC ‚The future of gravitation wave astronomy‘. GEO 600 optical design. GEO 600: detector and technology development. - PowerPoint PPT PresentationTRANSCRIPT
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GEO 600 STATUS
Andreas Freise on Andreas Freise on behalf of Hartmut behalf of Hartmut Grote for the LSCGrote for the LSCGravitational Waves: New FrontierSeoul, 16.01.2013 LIGO-G1300030
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Ground based detector network
GWIC ‚The future of gravitation wave astronomy‘
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GEO 600 optical design
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GEO 600: detector and technology development
• Unique position as detector and technology test bed• GEO 600 more freely examines new techniques• GEO pioneers techniques– Signal-recycling– Monolithic fused silica suspensions– Electrostatic actuators– Squeezing & its control
• GEO techniques have propagatedto LIGO / VIRGO detectors
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GEO High Frequency (HF)Interesting high frequencyregion limited by shot noise
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GEO-HF upgrade program• Implementation started in 2009• Seismic, thermal, and unexplained noise below 500 Hz• Goal: Improve sensitivity at frequencies > 500 Hz
→ Improve shot noise limited sensitivity
Frequency [Hz]
Str
ain
[1
/sq
rt(H
z)]
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GEO-HF program components
• Output Mode Cleaner (OMC)• Switch to Homodyne / DC readout• Signal-recycling configuration change• Squeezed vacuum injection• Light power increase• `Astrowatch’ whenever possible!
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Output Mode Cleaner (OMC)
Dark fringe contrast defect, due to mode mismatch and misalignment of the interferometer arms
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• OMC housed in vacuum tank• Multi-stage seismic isolation
starting at 1 Hz
Output Mode Cleaner (OMC)
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• Design: (optimised for DC readout)– Quasi-monolithic– Four mirror cavity– Length actuation via PZT
After OMC (≈6 mW):
Before OMC (≈60 mW):
Output Mode Cleaner (OMC)
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Heterodyne vs DC readout
• Heterodyne readout– GW information in beat
of GW-SBs ↔ RF-SBs– (Almost) no carrier
at IFO output
• DC readout– GW information in beat
of GW-SBs ↔ carrier– Some carrier light at the
output required– GW signal directly in detected
power
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Signal Recycling
Signal Recycling: •makes GEO resonant to GWs•Allows shaping of the shot noise•Influences higher-order modes in the dark fringe
QuickTime™ and aPNG decompressor
are needed to see this picture.
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Signal Recycling Change (2010)
Increase transmission of Signal Recycling mirror to reduce shot noise at high frequencies
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Changed signal-recycling
• More HOMs withreduced signal-recycling mirror reflectivity
R=98 % R=90 %
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Changed signal-recycling
• Analyze interferometer output beam using the OMC
Mode order
Power [mW]
0 6.3
1 7.7
2 10.6
3 1.2
4 0.6
5 1.7
6 3.6
7 3.7
8 3.6
9 1.1
10 0.8
11 0.5
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Thank you
Signal Recycling: Sensitivity Comparison
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Squeezed vacuum injection
• Directly reduces shot noise• (Frequency independent) squeezing is similar to an
increase in laser power• 10 dB squeezing source developed at the AEI
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GEO 600 and Squeezed Light
Mode Matching
T=10%
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Squeezing Phase Lock
Start with SQZ master to IFO main laser (fiber/PLL)
Error signal in refl. of IFO(Coherent Control signal)
different ports / possibilities
Feedback to SQZ master frequency (DC-2kHz)
Low-freq. Error signal (<0.01Hz) from noise dither
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Optical Loss
(Faraday Rotators: 0.65% loss)
Detection
Efficiency:
0.626
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Stable operation of squeezing!
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Spectrum (August 2012)
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Next steps on Squeezing (GEO)
Need Automatic Alignment (started) Need OPA temp set-point control Lower OMC loss (->2%), high-QE PD (->1%) New Phase noise budget after OMC change Lower det. Noise (main IFO) ->6dB look realistic, perhaps little more...
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Percent of time operated in Astrowatch (Science) mode: 70%Percent of Science mode, operated with squeezed light: 90%
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Burst DetectionHubble image of Betelgeuse (@200 pc)
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Detector Status from Nov 17, 2011 to Oct 15, 2012
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... endStar trails over GEO 600, by Jerome Degallaix
Thank you!
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... end
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• Squeezing–Try new control schemes–Try new optical / low loss components–Automatic alignment
• OMC–Try alternative alignment control techniques
• Thermal compensation–Test mass side heaters (recently installed)
–Compensation of beamsplitter lens with thermal radiation
• Astrowatch!
Next Steps
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Timeline
• 07-2009: Tuned signal-recycling• 09-2009: DC-readout• 12-2009: OMC installation• 04-2010: Squeezing installation• 05-2011: Output optic suspension• 06-2011: Use 5W input power, Routine Squeezing• 06-2011 to 09-2011: Joint GEO - VIRGO run• 09-2011: Laser upgrade• 11-2012: IMC upgrade, baffle installation, side
heater • 2013: Input mode cleaner change, TCS, power
increase, mid freq. Noise hunting, baffle installation