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Quantum Optomechanics Experiments at MIT: Radiative Pressure Rules

Dive into the cutting-edge field of optomechanics at MIT where quantum states of mirrors are manipulated using radiation pressure forces and advanced techniques for improving gravitational wave detector sensitivity. Explore the generation of squeezed light states, entanglement of mirror and light quantum states, and the observation of quantum radiation pressure effects.

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Quantum Optomechanics Experiments at MIT: Radiative Pressure Rules

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  1. Radiation Pressure Rules Optomechanics Experiments MIT Quantum Measurement Group

  2. Quantum optomechanics • Techniques for improving gravitational wave detector sensitivity • Tools for quantum information science • Opportunities to study quantum effects in macroscopic systems • Observation of quantum radiation pressure • Generation of squeezed states of light • Entanglement of mirror and light quantum states • Quantum states of mirrors

  3. Optomechanical coupling • The radiation pressure force couples the optical field to mirror motion • Alters the dynamics of the mirror • Spring-like forces  optical trapping • Viscous forces  optical damping • Tune the frequency response of the GW detector • Manipulate the quantum noise • Quantum radiation pressure noise and the standard quantum limit • Produce quantum states of the mirrors and light Classical Quantum

  4. Optomechanical coupling:Radiation pressure forces • Detune optical field from cavity resonance • Change in mirror position changes intracavity power  radiation pressure exerts force on mirror • Time delay in cavity results in cavity response doing work on mechanics

  5. Gram-scale mirrors

  6. Experimental cavity setup 1 m 10% 90% 5 W Optical fibers 1 grammirror Coil/magnet pairs for actuation (x5)‏

  7. Trapping and cooling • Stable optical trap with bichromatic light • Dynamic backaction cooling Stiff! Stable! T. Corbitt et al., Phys. Rev. Lett 98, 150802 (2007)

  8. Squeezed Vacuumfluctuations The experiment grows T. Corbitt et al., Phys. Rev. A 73, 023801 (2006) • Two identical cavities with 1 gram mirrors at the ends • Common-mode rejection cancels out laser noise

  9. The experiment grows

  10. Optically trapped and cooled mirror Optical fibers Teff = 0.8 mKN = 35000 1 grammirror C. Wipf, T. Bodiya, et al. (March 2010)

  11. That elusive quantum regime Thermal noise Radiation pressure noise goal (5 W input) C. Wipf, T. Bodiya, et al. (Feb. 2011)

  12. 7 dB or 2.25x Ponderomotive Squeezing Squeezing T. Corbitt, Y. Chen, F. Khalili, D.Ottaway, S.Vyatchanin, S. Whitcomb, and N. Mavalvala, Phys. Rev A 73, 023801 (2006)

  13. Cryogenic microgram-scale mirrors Thomas Corbitt @ MIT (but soon LSU)

  14. Micromirror oscillators • AlGaAs layers forming a Bragg mirror • ~ 1 to 5 mm long, ~10 μm supports, 50 to 100 μm mirror pads • Fundamentalfrequency ~ 200 Hz • Q factor ~ 2x105 at 5 K • Mass ~ 250 nanograms • Reflectivity ~ 99.982% • Very fragile • Power handling:breaks at >100 mW of incident power Fabricated by Garrett Cole at Univ. of Vienna

  15. Experimental layout

  16. Noise budget

  17. What can we learn? • Verify models of radiation pressure noise, squeezed radiation pressure noise, sub-SQL topologies • Verify models of thermal noise (ability to measure thermal noise as function of both frequency and temperature across broad bandwidth in monolithic structure) • Characterize materials and understand dissipation mechanisms • Gain experience in low vibration cryogenics

  18. Amazing cast of characters MIT • Thomas Corbitt • Christopher Wipf • Timothy Bodiya • Sheila Dwyer • Lisa Barsotti • Nicolas Smith-Lefevbre • Eric Oelker • Rich Mittleman • MIT LIGO Laboratory Collaborators • Yanbei Chen & group • David McClelland & group • Roman Schnabel & group • Stan Whitcomb • Daniel Sigg • Caltech 40m Lab team • Caltech LIGO Lab • Garrett Cole of Aspelmeyer group (Vienna) • LIGO Scientific Collaboration

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