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Published byFrederick Dorsey Modified over 9 years ago
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Status of GEO600 Benno Willke for the GEO600 team Aspen Meeting Aspen CO, January 2005 LIGO-G050030-00-Z
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Aspen05, B. Willke Sensitivity Improvements
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Aspen05, B. Willke Transition Commissioning - Observing overnight runs Aug04 – Jan05: 1405h (duty cycle: 93.7%)
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Aspen05, B. Willke
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Central Building
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Aspen05, B. Willke Tube / Trench
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Aspen05, B. Willke Clean Room / Control Room
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Aspen05, B. Willke Reaction Pendulum
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Aspen05, B. Willke GEO600 optical layout 12W laser mode cleaner interferometer with dual recycling detector Attenuated to 6W 1% Transmission 600m
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Aspen05, B. Willke Sensitivity progress (highlights) Typical S3 HPD lock + New MI+SR servo SR bench scattering
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Aspen05, B. Willke Sensitivity – Jan 2005 h(f) [ 1/sqrt(Hz )] Frequency [Hz]
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Aspen05, B. Willke
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Sensitivity Change with Heater Power
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Aspen05, B. Willke Amplitude Noise Coupling
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Aspen05, B. Willke Unbalanced Sidebands
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Aspen05, B. Willke Optical Gain
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Aspen05, B. Willke Calibration
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Aspen05, B. Willke On-line optical TF measurements actuator optical CAL P and Q
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Aspen05, B. Willke Calibration progress On-line calibration of both output quadratures HP and HQ Work on optimal combination is underway Estimation of optical parameters in real-time in control room On-line calibration leads to overnight runs
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Aspen05, B. Willke Combining HP and HQ - result HQ’ contains almost no signal compared to HP’ Where noise behaves like cal lines, we have apparent displacement Useful diagnostic for noise hunting (?)
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Aspen05, B. Willke Overnight Runs – Jan 14th
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Aspen05, B. Willke Noise Projections
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Aspen05, B. Willke Summary & Outlock GEO600 runs with dual-recycling on large baseline detector including calibration sensitivity improved by two orders of magnitude since S3-I data taking over night and on weekends with high duty cycle next steps: –LSC–S4 science run –increase injected power –increase power recycling gain –improve noise models and increase sensitivity –convert GEO into observatory GEO-HF
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Aspen05, B. Willke
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