1. The Proposed Holographic Noise Experiment Rainer Weiss, MIT On behalf of the proposing group Fermi Lab Proposal Review November 3, 2009

2. Strategy for the Experiment Direct test for the holographic noise –Positive signal if it exists Sufficient sensitivity –Provide margin for prediction –Probe systematics of perturbing noise Measure properties of the holographic noise –Frequency spectrum –Spatial correlation function

3. Experiment Concept Measurement of the correlated optical phase fluctuations in a pair of isolated but collocated power recycled Michelson interferometers –exploit the spatial correlation of the holographic noise –use the broad band nature of the noise to measure at high frequencies where other correlated noise is expected to be small

4. Pedagogic Michelson Interferometer

5. Schematic of Power Recycled Michelson S. Waldman P0P0 P BS ~ P 0 / ifo loss

6. Experiment parameters Input laser power @ 1.06 m0.75 watt Arm length BS - EM40 meters Free spectral range recycling cavity3.5 MHz Min. beam waist diameter7.4 mm Power recycling arm length0.5 meter End mirror transmission10ppm Beam splitter transmission0.5 Anti reflection coating reflectivity10 ppm Mirror loss (PRM,BS,TM)50 ppm Substrate loss10 ppm Differential arm loss25 ppm Power on BS2 kW Differential length offset4 x 10 -10 meters = 4 x 10 -4 l Output power at antisym10 mW 5mW / detector Recycling mirror transmission1.0x10 -3 Recycling cavity frequency pole365 Hz Transimpedance of preamp100 ohms Preamp voltage noise3nV/sqrt(Hz) Quantum phase noise9 x 10 -12 radians/sqrt(Hz)

7. Basic experiment relations signal quantum phase fluctuations: expected dominant noise

8. Basic experiment relations Interferometer correlation

9. S. Waldman Transfer functions for differential and common mode loops

10. S. Waldman

14. Noise sources Preamplifier voltage and Johnson Noise Poisson noise due to reduced contrast Unbalance end mirror reflectivities Overlap of beams at BS rms longitudinal motion G diff ~ 10 5 B ~ 10kHz

15. Noise sources Phase noise from amplitude fluctuations Phase noise from frequency noise Not serious Phase noise from scattering paths

16. Noise sources Phase noise from forward scattering by the residual gas P < 10 -4 lower pressure to avoid mirror contamination

17. Comparison of phase noise InterferometerPower on beam splitter watts Phase noise rad/sqrt(Hz) LIGO Phase noise interferometer (1998) 703 x 10 -10 LIGO H1,L1 (2009)2502 x 10 -11 GEO 600 (2009)27008 x 10 -12 /SRGain Proposed instrument20009 x 10 -12 @ f > 10kHz

18. LIGO Phase Noise Test Interferometer

19. About the optics All optics requirements can be met by (now) standard superpolish surfaces coated by plasma thin film deposition. To avoid thermal lensing in the beam splitter will need to use low loss Heraeus fused silica such as Supersil 3001/3002/300. Purchase dedicated coating runs with commercial vendor for initial components and spares. Use vacuum compatible PZT controlled 2” optics mounts being developed in industry by the Advanced LIGO project.

20. Uncertainties and decisions to be made In vacuum or outside detectors – begin with outside detectors, decide from initial noise performance PZT hard optics mounts or suspensions –begin with PZT, decide from required locking dynamic range Alignment servos –begin with simple adjustment, add dither servo alignment if needed Laser frequency stabilization and filtering –begin with only interferometer common mode feedback to laser, add in-line filter cavity and active frequency stabilization to reference cavity if needed