Enhanced sensitivity of the LIGO gravitational wave detector by using squeezed states of light
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Citations
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References
Quantum Mechanical Noise in an Interferometer
LIGO: The Laser Interferometer Gravitational-Wave Observatory.
Introductory quantum optics
Observation of squeezed states generated by four-wave mixing in an optical cavity.
Advanced LIGO: the next generation of gravitational wave detectors
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Frequently Asked Questions (11)
Q2. What is the phase of the squeezed vacuum?
The beat between the 29 MHz frequency shifted coherent beam and the interferometer beam provides an error signal which is used to control the phase of the squeezed vacuum field relative to the interferometer field.
Q3. What is the recent research on the physics of aqueous quantum states?
Search for gravitational waves from low mass compact binary coalescence in LIGO’s sixth science run and Virgo’s science runs 2 and 3.
Q4. What is the optical loss in the vacuum?
The 1064 nm ‘control laser” is phase-locked to the “pump laser” to generate a 29 MHz frequency shifted coherent beam which co-propagates with the squeezed vacuum beam, entering the interferometer through the “output Faraday isolator”.
Q5. How much light is pumped to the vacuum source?
It is typically pumped with about 40 mW of 532 nm light, where the thresh-old for spontaneous sub-harmonic generation is near 95 mW.
Q6. Who was the lead scientist on the LIGO experiment?
N. SmithLefebvre, M. Evans, R. Schofield and C. Vorvick kept the LIGO interferometer at its peak sensitivity and supported the integration of the squeezed vacuum source, with contributions from G. Meadors and D. Gustafson.
Q7. What is the squeezing angle of the vacuum laser?
1. The 1064 nm “pump laser” is phase-locked to the “H1 laser” and it drives the second harmonic generator (SHG) to produce light at 532 nm.
Q8. What is the name of the paper?
New J. Phys. 11 073032 (2009)The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector.
Q9. What is the cause of the mode mismatch?
The mode mismatch between the squeezed beam and the output mode cleaner (OMC) is mainly caused by a complicated optical train in the vacuum envelope, which precluded improving the mode matching on a time scale compatible with this experiment.
Q10. what is the reason for the loss in the LIGO H1 detector?
Most of these losses are due to the fact that the LIGO H1 detector was not initially designed for injection of squeezed states, and the squeezing injection path was retrofitted within the original LIGO optical layout.
Q11. What is the reason for the large optical losses in the OMC?
The losses in the OMC itself are also larger than expected, and they are believed to be due to scatter and absorption inside the mode cleaner cavity.