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MIGA AND ELGAR: NEW PERSPECTIVES FOR LOW FREQUENCY GRAVITATIONAL WAVE OBSERVATION USING ATOM INTERFEROMETRY MIGA, GDR Ondes Gravitationnelles, 20/06/2018 1 MIGA Project A new large instrument combining matter- wave and laser interferometry

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MIGA, GDR Ondes Gravitationnelles, 20/06/2018

MIGA AND ELGAR: NEW PERSPECTIVES FOR LOW FREQUENCY GRAVITATIONAL WAVE OBSERVATION USING ATOM INTERFEROMETRY

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MIGA, GDR Ondes Gravitationnelles, 20/06/2018

MIGA Project

A new large instrument combining matter- wave and laser interferometry

  • Gravitational wave physics
  • Demonstrator for future sub-Hz ground based GW detectors
  • Geoscience
  • Gravity sensitivity of 10-10 g/Sqrt(Hz) @ 2Hz
  • Gradient sensitivity of 10-13 s-2/Sqrt(Hz) @ 2Hz: geology, hydrogeology…

Nice Toulon

  • Two 200 m horizontal optical cavity coupled with 3 AI
  • Possible evolutions towards 2D or 3D instrument on

site

A Large research infrastructure hosted in a low noise laboratory

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Design of a large-scale instrument with interdisciplinary applications based on recent advances in atomic interferometry: MIGA is the first of a new generation of detectors both built underground and using quantum m a n i p u l a t i o n o f a t o m s f o r geosciences, seismology and fundamental physics. C o o r d i n a t i o n o f e x p e r t s i n fundamental physics, geosciences and astronomy. A first generation of research facility enabling high-precision tests to be carried out by different communities. An important step towards a low- frequency gravitational strain sensor with an interest in the detection of gravitational waves and also geophysics.

Interféromètres

Physics Geophys. Astrophys.

Paris : Metrology and atomic sensors Bordeaux :
 lasers, instrument development , prototype and maintenance Rustrel : Geophysic s and Instrument

  • peration
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State-of-the-art GW detectors sense the ultimate evolution phase of binary systems

  • A transient of a few hundreds of ms which corresponds to system coalescence

A new astronomy is possible with low frequency detectors With low frequency detectors (f<1Hz)

  • Observation of the same sources on quasi continuous timescales

Sesana, arxiv.org/1602.06951

Can we extend the frequency band of state-of-the-art GW detectors?

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Space Ground Underground

  • New observables
  • New sources

Can we extend the frequency band of state-of-the-art GW detectors?

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« Advanced LIGO » Sensitivity

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Limitations for f<10 Hz:

  • Radiation pressure noise
  • Imperfections of Mirror suspensions
  • « Gravity gradient » noise

Fluctuations of the Earth gravity field

How to extend the frequency band of state-of-the-art GW detectors?

« Gravity Gradient » noise

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L

δϕlas ∝khL

Cold atoms for GW detection ?

Enable to overcome:

  • Limitations related to suspension systems.
  • Radiation pressure noise.

Sensitivity to Gravity Gradient Noise is the same !

Suspended mirors Free falling atoms

Let’s use free falling atoms as “test masses” instead of mirrors

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Networks of AIs for Gravity Gradient Noise cancellation

Example of the MIGA Geometry

Δφati-Δφatj

∝kh(Xi − Xj )

  • Effet GW
  • Gravity gradient ∝2kT 2 a(Xi)− a(Xj )

⎡ ⎣ ⎤ ⎦

Discrimination between GW effects and gravity gradients using the spatial resolution of the antenna

  • Low frequency (10-2-10 Hz) GW detection limited by detection noise
  • Measures of the local gravity field = Geoscience

Xi Xj

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Use of AI offers possibility to spatially resolve gravity

➡GW have long wavelength while GG have short characteristic length of variation (1 m

– few km)

➡Correlations between distant sensors provide information on the GG noise and

allows to discriminate it from the GW signal

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GW signal Inertial signal X

correlations

Networks of AIs for Gravity Gradient Noise cancellation

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Networks of AIs for Gravity Gradient Noise cancellation

➡

Strain sensitivity

➡

Shot noise

➡

Seismic noise

  • W. Chaibi, et al. Phys. Rev. D 93, 021101(R), 2016
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Dense arrays of Atom Interferometers could be used as future GW detectors

  • Gravitational Wave signal can be extracted using a spatial averaging method
  • N Correlated gradiometers enable to average the GGN over several realizations

Ltot

  • Ltot=32 km
  • N=80 gradiometers
  • baseline L = 16 km

H N(t) = 1 N ψi(t)

i=1 N

∑

  • The geometry of the detector (δ,L) is chosen with respect to the spatial correlation

properties of the GGN.

Next generation Matter-wave antenna can reach sensitivity

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GGN reduction with an AI network

  • Gain of about factor 10 in the 100 mHz 1 Hz band
  • Space for improvement using all spatial information of the network (use

different baseline L in the numerical treatment)

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Measurement noise 100 times lower than the quantum- projection limit using entangled atoms Quantum superposition at the half-metre scale Phase Locking a Clock Oscillator to a Coherent Atomic Ensemble Stability enhancement by joint phase measurements in a single cold atomic fountain

  • Phys. Rev. A 90, 063633
  • Phys. Rev. X 5, 021011

Nature 529, 505–508 Nature 528, 530–533

Tools for next generation Matter-wave antenna

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Underground site (LSBB) for MIGA

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200 m

  • A dismissed military facility
  • Former command centre for nuclear force

MIGA at the LSBB site

  • Infrastructure works will start end 2017
  • MIGA installation: mid 2019
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Cavité ultra-stable 200 m couplée à 3 IA

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The MIGA Instrument

200 m

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LSBB, a site of geological interest

MIGA: Access to gravity gradient & higher orders, long term fluctuations

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LSBB, a low noise site for MIGA

Environmental noise may prevent to reach detection noise (quantum noise) easily. Usual suspects: seismic and magnetic noise

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−2

10

−1

10 10

1

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2

10

−10

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10

−4

Acceleration m.s−2.Hz−1/2 Frequency (Hz)

σφ=640 mrad σφ=60 mrad RMS noise on AI measurements induced by seismic noise:

Tipical lab conditions (filtered) LSBB

Underground operation enables AI to reach optimal performances

≈ 5 10-10 g = 0.5 µGal

See T. Farah, et al., Gyroscopy Navig. 5, 266 (2014).

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1% 2% 2% GW Core area 240 m - C1-C3 MIGA Tank exploration Geotechnical anticipation of drilling Nor d

Core analysis and wall imaging Geological modeling Carbonated reservoir prediction Environment hydro-geological analysis around MIGA Seismic models

Collaboration with TOTAL to predict escalated site

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Projection of GGN for MIGA

Sources Gravity Gradient noise on detector site (10-2-10 Hz)

  • Seismic GGN
  • Atmospheric GGN
  • Other : geophysical properties (hydrology), linked to human activity

Seismic GGN for MIGA at LSBB

  • STS-2 sensor
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Projection for seismic noise

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Projection for seismic noise

MIGA (current design) MIGA (improved design) S/N x 10, LMT 100 hk

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Projection for infrasound noise

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Projection for infrasound noise

MIGA (current design) MIGA (improved design) S/N x 10, LMT 100 hk

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MIGA status and perspectives

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π

π/2

30 cm

π

s

ϕ(X1)

s

ϕ(X 2)

s

ϕ(X 3)

≈100m ≈100m

The MIGA antenna

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Test and callibration set-ups

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Accelerometer set up

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Accelerometer set up

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Accelerometer set up

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2013 2014 2015 2016 2017 2018 2012

2013 - Project manager hired from VIRGO 2014 – First design of the instrument 2016 – Publication (PRD) of the 
 Newtonian Noise suppression 
 technique 2016 – GW discovery 2015 – First suspension and sensor prototype 2017 – Gallery
 preparations 2019
 Instrument online 2017 – 3 sensors ready 2018 - prototype


2019

2015 – Gravimeter

MIGA Status

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After MIGA : ELGAR

3D antenna configuration Arm Length (1 - 10 km) Number of AI nodes (10 - 100) Strain :10-20
 Frequency 0.1 - 10 Hz

Sync with other GW observation instruments “full band analysis”, gravitational noise analysis improvement, joint data management and analysis

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Conclusion

  • Arrays of AIs can be configured to reject GGN

GGN is a strong limit for earth based detectors

  • MIGA will be a new infrastructure for a large community
  • Study new measurements methods for geophysics
  • Opens perspectives for low frequency GW detection, future of GW astronomy