SAGE : Can we detect gravitational waves with CubeSats? S . Lacour, - - PowerPoint PPT Presentation

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SAGE : Can we detect gravitational waves with CubeSats? S . Lacour, - - PowerPoint PPT Presentation

Jun 29, 2023 278 likes •563 views

SAGE : Can we detect gravitational waves with CubeSats? S . Lacour, P . Bourget, M. Nowak, F . Vincent, V . Lapeyrere, L. David, A. Le Tiec, A. Kellerer, O. S traub, J. Woillez PICSAT Photometer 100ppm Technology demonstrator for

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S . Lacour, P . Bourget, M. Nowak, F . Vincent, V . Lapeyrere,

  • L. David, A. Le Tiec, A. Kellerer, O. S

traub, J. Woillez

SAGE : Can we detect gravitational waves with CubeSats?

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  • Photometer 100ppm
  • Technology demonstrator for single mode

fibre

  • Development started Mach 2015
  • Launched January 2018 on PS

L V C-40

  • Lost contact in Mars 2018

GDR Ondes Gravitationnelles 2

PICSAT

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GDR Ondes Gravitationnelles 3

Pricing

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  • Michelson interferometer in space
  • 2.5 millions kilometers arm length

GDR Ondes Gravitationnelles 4

LISA

A B C

Proof masses Laser

From LISA White Book 2017

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GDR Ondes Gravitationnelles 5

LISA

  • 2 off axis telescopes 30cm
  • 2 optical bench with bulk interferometers
  • 2 accelerometer (5 centimeters cubes)
  • 1 Disturbance R

eduction S ystem (thrusters)

  • Thermal stability !
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GDR Ondes Gravitationnelles 6

LISA = > SAGE

  • 2 off axis telescopes 30cm => 10cm mirrors
  • 2 optical bench with bulk interferometers => Fibered interferometry
  • 2 accelerometer (5 centimeters cubes)
  • 1 Disturbance R

eduction S ystem (thrusters)

  • Thermal stability ! => 100mW laser beam only
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  • 60°intertwined telescopes:

GDR Ondes Gravitationnelles 7

SAGE

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Phase Modulator f2 Phase Modulator f1

S pacecraft A

L a s e r D2 D1 D3 99.99% 0.01% 99% 1% 1e‐8 50% 50% 99.99% 0.01% 99% 1% 1e‐8 12 12 11 13 12 Spacecraft B Spacecraft C

GDR Ondes Gravitationnelles 8

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GEO 42000km 72 000 km => 0.25s Satellite A Satellite C a) t=0s Satellite B

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b) t=0.25s

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c) t=0.5s

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d) t=0.75s 220 000 km interferometer 1 s light travel time Measurement at zero OPD Satellites on ballistic trajectory

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TDI

φ12(t) = 21(t + ∆ 21) − 12(t) + L 21(t) φ21(t) = 12(t + ∆ 12) − 21(t) + L 12(t) φ11(t) = 1/ 2( 12(t) − 13(t)) φ13(t) = 31(t + ∆ 31) − 13(t) + L 21(t) φ31(t) = 13(t + ∆ 13) − 31(t) + L 12(t) h(t) = φ12(t) + φ21(t − ∆ 12) + 2φ11(t − ∆ 12 − ∆ 21) + φ13(t − ∆ 12 − ∆ 21) + φ31(t − ∆ 31 − ∆ 12 − ∆ 21) − φ13(t) − φ31(t − ∆ 13) − φ11(t − ∆ 13 − ∆ 31) − φ12(t − ∆ 13 − ∆ 31) − φ21(t − ∆ 21 − ∆ 13 − ∆ 31) + 2φ11(t) − 2φ11(t − ∆ 21 − ∆ 12 − ∆ 13 − ∆ 31) h(t) = L 12(t) + L 21(t − ∆ 12) + L 13(t − ∆ 12 − ∆ 21) + L 31(t − ∆ 12 − ∆ 21 − ∆ 13)) − L 13(t) − L 31(t − ∆ 13) − L 21(t − ∆ 13 − ∆ 31) − L 12(t − ∆ 13 − ∆ 31 − ∆ 12)

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SAGE ?

Graph From ESA Gravitation Observatory Advisory team, final report 2016

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1 pm (73 000 km arm length)

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Sensitivity of SAGE

Solar Wind Solar Wind 9 µN/m2 1‐6 µN/m2

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GDR Ondes Gravitationnelles 17

Sensitivity of SAGE

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GDR Ondes Gravitationnelles 18

Sensitivity of SAGE

Radiation Pressure

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GDR Ondes Gravitationnelles 19

Sensitivity of SAGE

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Sensitivity of SAGE

Radiation Pressure Solar Wind

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Diffraction analysis

  • Diffraction + fiber inj ection coupling cause an energy loss of 1.5 10-10

between the two satellites: 100mW=>15pW

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72 000 km 1km 250mW 2.5nW s hcλ 2Pphot ons = 23pm/ p H z

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Sensitivity of SAGE

Photon Noise Radiation Pressure Solar Wind

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Sensitivity of SAGE

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But…

  • No 104 IMBH?

GDR Ondes Gravitationnelles 24

  • A. Sesana, M. Volonteri, and F. Haardt, 2007
  • M. Colpi, A. Sesana, 2018
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But…

  • No 104 IMBH?

GDR Ondes Gravitationnelles 25

  • A. Sesana, M. Volonteri, and F. Haardt, 2007
  • M. Colpi, A. Sesana, 2018
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But…

  • Technical challenges:

– Orbitography – Thermal expansion (20pm/ sqrt(Hz)

GDR Ondes Gravitationnelles 26

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To conclude

LIGO timeline