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Quantum noise reduction using squeezed states in LIGO

Published byDwight Golden Modified over 6 years ago

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Presentation on theme: "Quantum noise reduction using squeezed states in LIGO"— Presentation transcript:

1 Quantum noise reduction using squeezed states in LIGO

2 LIGO interferometers, quantum light and quantum noise
Generation and detection of squeezing Squeezing in Enhanced LIGO Environmental noise couplings Limits to the level of squeezing Losses Squeezing angle fluctuations Potential benefit for Advanced LIGO and beyond

3 Michelson interferometer
Laser 10^-18m/rtHz

4 Michelson interferometer
Laser 10^-18m/rtHz

5 Michelson interferometer
Laser 10^-18m/rtHz

6 LIGO interferometers

7 Need to reduce quantum noise

8 Quantum noise in an interferometer
Radiation pressure noise: ΔFα|Ey|2 -|Ex|2 Radiation pressure noise: ΔFαIm[EL *δEd] Laser Ey=EL+δEL+iδEd Ey EL +δEL Ex Ex=iEL +iδEL+δEd δEd Shot noise: δI PD α Re[EL *δEd] Shot noise limited sensitivity α Re[δEd]/EL

9 Quantum Light X2 ∆X2 The uncertainty principle ∆X1 ∆X1 ∆X2 ≥1 A X1 θ 9

10 Quantum Light ∆X1 ∆X2 ≥1 X2 The uncertainty principle X1 θsqz
Squeezed vacuum Vacuum Fluctuations 10

11 Squeezing in an interferometer
Laser

12 LIGO interferometers, quantum light and quantum noise
Generation and detection of squeezing Squeezing in Enhanced LIGO Environmental noise couplings Limits to the level of squeezing Losses Squeezing angle fluctuations Potential benefit for Advanced LIGO and beyond

13 Vacuum and coherent states are sums of uncorrelated sidebands
This is a squeezer- Built at MIT using design elements from ANU, AEI Shipped piece by piece and reassembled here OPO creates squeezing Advanced LIGO electronics This is where I spend most of my time! 13 13

14 Squeezer: Optical parametric oscillator
Quantum OPO: Turns a vacuum state into squeezed vacuum Classical OPO: Phase sensitive amplifier

15 A squeezed state is a sum of correlated sidebands
This is a squeezer- Built at MIT using design elements from ANU, AEI Shipped piece by piece and reassembled here OPO creates squeezing Advanced LIGO electronics This is where I spend most of my time! 15 15

16 A squeezer table SHG OPO Laser Homodyne Detector Interferometer
Dark Port OPO Laser

17 Balanced Homodyne Detection
Noise of local oscillator is subtracted Local Oscillator

18 Balanced Homodyne Detection
Local Oscillator amplifies noise on the squeezed field Vacuum fluctuations Local Oscillator

19 Balanced Homodyne Detection
Local Oscillator amplifies noise on the squeezed field Local Oscillator noise is subtracted Squeezed State Local Oscillator

20 Unbalanced Homodyne Detection
High reflectivity beam splitter Requires low noise local oscillator Change this tomorrow!!!

21 Unbalanced Homodyne Detection
Laser High reflectivity beam splitter Requires low noise local oscillator Change this tomorrow!!!

22 LIGO interferometers, quantum light and quantum noise
Generation and detection of squeezing Squeezing in Enhanced LIGO Environmental noise couplings Limits to the level of squeezing Losses Squeezing angle fluctuations Potential benefit for Advanced LIGO and beyond

23 H1 squeezing experiment
Demonstrate that squeezing does not add noise in the LIGO band Study environmental noise couplings Understand limits to measured squeezing in order to plan for aLIGO+ squeezing

24 H1 Squeezer built at MIT (2009-2010)
H1 Squeezer shipped to LHO (Oct 2010) Bow-tie cavity OPO design from ANU (2008) Squeeze injection in H1 (Nov – Dec ) H1 Recovery (Sept 2011) H1 Squeezer Installation (Summer 2011)

25 Experiment Layout

26 Squeezing in Enhanced LIGO
2.1dB 20% improvement in SNR

27 Best broadband sensitivity to date

28 Squeezing in Enhanced LIGO
1Mpc range added to NS range 24% increase in volume

29 LIGO interferometers, quantum light and quantum noise
Generation and detection of squeezing Squeezing in Enhanced LIGO Environmental noise couplings Limits to the level of squeezing Losses Squeezing angle fluctuations Potential benefit for Advanced LIGO and beyond

30 Backscatter noise Light from interferometer is sent towards OPO
A second scattering event in OPO sends light back towards IFO Spurious interferometer adds noise LASER

31 Noise Coupling Around 100 fW of backscattered power at detector

32 Backscatter in Advanced LIGO
Better Acoustic enclosure (factor of 10 above 100 Hz) Lower OPO finesse (needed anyway) Good Faraday performance in vacuum Worse More power 6 dB of squeezing Better detection efficiency Possibly better matching of scattered beam into OPO Backscatter noise 40-80x below shot noise above 100 Hz. Out of vacuum OPO is compatible with Advanced LIGO sensitivity, in vacuum OPO probably needed for a third generation interferometer.

33 LIGO interferometers, quantum light and quantum noise
Generation and detection of squeezing Squeezing in Enhanced LIGO Environmental noise couplings Limits to the level of squeezing Losses Squeezing angle fluctuations Potential benefit for Advanced LIGO and beyond

34 Losses destroy squeezing
Every loss can be seen as a beamsplitter with power transmission ηloss

35 Losses destroy squeezing
Every loss can be seen as a beamsplitter with power transmission ηloss A loss allows vacuum state to “leak” into the beam

36 Losses destroy squeezing
Every loss can be seen as a beamsplitter with power transmission ηloss Beamsplitter mixes the squeezed state with vacuum state Resulting state has higher noise in squeezed quadrature

37 Losses limit squeezing

38 Loss budget and goals Based on a tally of 11 different loss sources
Enhanced LIGO squeezing Advanced LIGO assumptions 3 faraday passes 5% each 3% each Mode matching 30% 4% Output mode cleaner 19% 3% Total losses 55-60% 20-25% Based on a tally of 11 different loss sources

39 Losses degrade the purity of the squeezed state
∆X2=er =10dB ∆X2=7dB ∆X1=e-r =-10dB ∆X1=-2dB 55% loss

40 Squeezing with a radiation pressure limited interferometer

41 LIGO interferometers, quantum light and quantum noise
Generation and detection of squeezing Squeezing in Enhanced LIGO Environmental noise couplings Limits to the level of squeezing Losses Squeezing angle fluctuations Potential benefit for Advanced LIGO and beyond

42 Squeezing Angle Fluctuations
X1 X2

43 Squeezing Angle Fluctuations

44 Squeezing angle fluctuations

45 Measurement of squeezing angle fluctuations and losses

46 Squeezing angle fluctuations
Fit: 62% losses 81±13 mrad 109±9 mrad Log scale!! 37±6 mrad

47 LIGO interferometers, quantum light and quantum noise
Generation and detection of squeezing Squeezing in Enhanced LIGO Environmental noise couplings Limits to the level of squeezing Losses Squeezing angle fluctuations Potential benefit for Advanced LIGO and beyond

48 An alternative to high power operation in Advanced LIGO

49 Squeezing in Advanced LIGO

50 Squeezing with full power
28% increase in volume

51 Frequency Dependent Squeezing

52 Paths to better squeezing
Non linear gain optimized for shot noise limited interferometer, maximum pump power 80% of threshold

53 Summary 2dB of squeezing in Enhanced LIGO Squeezing compatible with low frequency sensitivity Backscatter should not be a problem for aLIGO To get higher levels of squeezing we will need to reduce interferometer losses and squeezing angle fluctuations Squeezing will soon be the simplest way to improve LIGO’s sensitivity

54 Thank you! My committee Mentors: Nergis Mavalvala, Lisa Barsotti, Daniel Sigg LIGO Lab at MIT, staff at Hanford, and all the squeezers

55 Coherent locking of squeezing angle inject frequency shifted sideband with coherent amplitude
IFO carrier SQZ sideband x

56 Squeezing angle error signal
IFO carrier SQZ sideband IFO carrier SQZ sideband x x

57 Squeezing angle error signal
IFO carrier SQZ sideband x + +

58 Squeezing angle error signal
SQZ sideband IFO carrier x + + Static misalignments will cause a change in the demodulation phase needed to detect the maximum squeezing Beam jitter will add phase noise, especially when beating against a static misalignment.

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