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Jason Hogan May 22, 2014

Single-arm gravitational wave detectors based on atom interferometry. LISA Symposium X. Jason Hogan May 22, 2014. Single Baseline Gravitational Wave Detection. frequency. L (1 + h sin( ω t )). strain. Are multiple baselines required?. Motivation Formation flying: 2 vs. 3 spacecraft

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Jason Hogan May 22, 2014

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  1. Single-arm gravitational wave detectors based on atom interferometry LISA Symposium X Jason Hogan May 22, 2014

  2. Single Baseline Gravitational Wave Detection frequency L (1 + h sin(ωt)) strain Are multiple baselines required? Motivation Formation flying: 2 vs. 3 spacecraft Reduce complexity, potentially cost Laser interferometer GW detector

  3. Atom interference Light interferometer Light fringes Beamsplitter Atom fringes Atom interferometer Beamsplitter Mirror Atom http://scienceblogs.com/principles/2013/10/22/quantum-erasure/ http://www.cobolt.se/interferometry.html

  4. Measurement Concept Essential Features Atoms are good clocks Light propagates across the baseline at a constant speed Atom Clock Atom Clock L (1 + h sin(ωt))

  5. Simple Example: Two Atomic Clocks Time Phase evolved by atom after time T

  6. Simple Example: Two Atomic Clocks Time GW changes light travel time Phase difference

  7. Phase Noise from the Laser The phase of the laser is imprinted onto the atom. Laser phase noise, mechanical platform noise, etc. Laser phase is common to both atoms – rejected in a differential measurement.

  8. Single Photon Accelerometer Three pulse accelerometer Long-lived single photon transition (e.g. clock transition in Sr, Yb, Ca, Hg, etc.) Graham, et al., PRD 78, 042003, (2008). Yu, et al., GRG 43, 1943, (2011).

  9. Two-photon vs. single photon configurations 1 photon transitions 2 photon transitions Sr Rb How to incorporate LMT enhancement? Graham, et al., PRD 78, 042003, (2008). Yu, et al., GRG 43, 1943, (2011).

  10. Laser frequency noise insensitive detector Excited state Pulses from alternating sides allow for sensitivity enhancement (LMT atom optics) Laser noise is common Graham, et al., arXiv:1206.0818, PRL (2013)

  11. LMT enhancement with single photon transition Example LMT beamsplitter (N = 3) Each pair of pulses measures the light travel time across the baseline. Excited state Graham, et al., arXiv:1206.0818, PRL (2013)

  12. Reduced Noise Sensitivity Leading order kinematic noise sources: 1. Platform acceleration noise da 2. Pulse timing jitter dT 3. Finite duration Dt of laser pulses 4. Laser frequency jitter dk Differential phase shifts (kinematic noise) suppressed by Dv/c < 3×10-11

  13. Satellite GW Antenna Common interferometer laser Atoms Atoms L ~ 100 - 1000 km JMAPS bus/ESPA deployed

  14. Potential Strain Sensitivity J. Hogan, et al., GRG 43, 7 (2011).

  15. Technology development for GW detectors • Laser frequency noise mitigation strategies • Large wavepacket separation (meter scale) • Ultra-cold atom temperatures (picokelvin) • Very long time interferometry (> 10 seconds)

  16. Ground-based GW technology development Long duration Large wavepacket separation 4 cm

  17. 10 m Drop Tower Apparatus

  18. Interference at long interrogation time Wavepacket separation at apex (this data 50 nK) 2T = 2.3 sec Near full contrast 6.7×10-12 g/shot (inferred) Demonstrated statistical resolution: ~5 ×10-13g in 1 hr (87Rb) Interference (3 nK cloud) Dickerson, et al., PRL 111, 083001 (2013).

  19. Preliminary LMT in 10 m apparatus LMT using sequential Raman transitions with long interrogation time. 6 ħk 4 cm wavepacket separation 10 ħk 7 cm wavepacket separation LMT demonstration at 2T = 2.3 s (unpublished)

  20. Atom Lens Geometric Optics: position time Atom Lens:

  21. Atom Lens Cooling Optical Collimation: position time Atom Cooling:

  22. AC Stark Lens Apply transient optical potential (“Lens beam”) to collimate atom cloud in 2D “point source” Radial Lens Beam Time

  23. 2D Atom Refocusing Lens Without Lens With Lens

  24. Record Low Temperature Vary Focal Length North West

  25. Extended free-fall on Earth Launch  Lens  Relaunch  Detect Lens Image of cloud after 5 seconds total free-fall time Launched to 9.375 meters Relaunched to 6 meters Towards T > 10 s interferometry (?)

  26. Future GW work Single photon AI gradiometer proof of concept Ground based detector prototype work 10 m tower studies MIGA; ~1 km baseline (Bouyer, France)

  27. Sr compact optical clock 6 liter physics package As built view with front panel removed in order to view interior. 408-735-9500 AOSense.com Sunnyvale, CA AOSense

  28. Collaborators Stanford Mark Kasevich (PI) Susannah Dickerson Alex Sugarbaker Tim Kovachy Christine Donnelly Chris Overstreet Theory: Peter Graham SavasDimopoulos SurjeetRajendran Former members: David Johnson Sheng-weyChiow Visitors: Philippe Bouyer (CNRS) Jan Rudolph (Hannover) NASA GSFC BabakSaif Bernard D. Seery Lee Feinberg RitvaKeski-Kuha AOSense Brent Young (CEO)

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