Transcript ASTROD2006-Leone

ESA technology development activities for fundamental
physics space missions
B. Leone, E. Murphy, E. Armandillo
Optoelectronics Section
ESA-ESTEC
European Space Research and Technology Centre
European Space Agency
Noordwijk, The Netherlands
Outline
• Presentation of the Optoelectronics Section
• Fundamental Physics Missions at ESA
• Cosmic Vision
• Technology Needs for Future Fundamental
Physics Missions
• Technology Development Strategy
• Earth Observation and Planetology
• Current and Planned Activities
• Conclusions
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Optoelectronics Section
• Head: Errico Armandillo
• Team of experts:
– Detectors
• X-rays
• UV, VIS, IR
• FIR, THz, (sub)mm-wave
– Photonic devices
• Fibres and sensors
• Optical telecommunication
– Lasers
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Lidar
Distance metrology
Frequency standards
Laser-cooled atom interferometry
Laser damage (laboratory)
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Terms of Reference
• Optoelectronic device technologies and
applications
• Laser technology and components
• Photonic integrated optics
• Non-linear optics
• Superconductor technology
• Far-IR heterodyne instrument design and
verification > 1 THz
• Detector technology and radiometry for the X-ray,
UV, IR and Far-IR (incoherent and heterodyne) > 1
THz
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Our Role within ESA
• Directorate of Technical and Quality Management
• Support Directorate within a matrix organisation
• Customers:
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Science
Human Spaceflight, Microgravity and Exploration
Earth Observation
Applications
• Telecommunications
• Navigation
• Initiate technology development activities in
support of programmes and to enable future
missions
• Provide technical expertise to projects
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Technology R&D
• Initiate and follow up technology development activities up
to Technology Readiness Level 5/6
– TRL1 - Basic principles observed and reported
– TRL2 - Technology concept and/or application formulated
– TRL3 - Analytical and experimental critical function and/or
characteristic proof-of-concept
– TRL4 - Component and/or breadboard validation in laboratory
environment
– TRL5 - Component and/or breadboard validation in relevant
environment
– TRL6 - System/subsystem model or prototype demonstration in a
relevant environment (ground or space)
– TRL7 - System prototype demonstration in a space environment
– TRL8 - Actual system completed and "flight qualified" through test
and demonstration
– (ground or space)
– TRL9 - Actual system "flight proven" through successful mission
operations
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ESA Technology Landscape
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Qualification and Reliability
• Laser laboratory facility
• Laser diode reliability test envisaged
• Low to high power laser diode multimode
emitter/bars/stacks
– CW pumping (1-30 Watts) at 808, 9xx nm
– QCW pumping (≥ 100 Watts peak power)
• Qualification and reliability aspects
– Optical components
– Laser diodes
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Outline
• Presentation of the Optoelectronics Section
• Fundamental Physics Missions at ESA
• Cosmic Vision
• Technology Needs for Future Fundamental
Physics Missions
• Technology Development Strategy
• Earth Observation and Planetology
• Current and Planned Activities
• Conclusions
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Fundamental Physics Missions at ESA
• Science:
– LISA (Laser Interferometer Space Antenna)
• Search for gravitational waves
• 50% NASA
• Technology R&D not shared
– LISA Pathfinder (LTP)
• Technology demonstrator mission
• LISA precursor mission
– Cosmic Vision
• Human Spaceflight, Microgravity and Exploration
– ACES (Atomic Clock Ensemble in Space) onboard the ISS
• Main goal: technology demonstrator
– Test a cold atom clock in space
– Test a hydrogen maser in space
– Time and frequency comparison with ground clocks
• Three fundamental physics tests:
– Gravitational red shift increased accuracy
– Search for fine structure constant drift
– Search for Lorentz transformation violations
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Outline
• Presentation of the Optoelectronics Section
• Fundamental Physics Missions at ESA
• Cosmic Vision
• Technology Needs for Future Fundamental
Physics Missions
• Technology Development Strategy
• Earth Observation and Planetology
• Current and Planned Activities
• Conclusions
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Cosmic Vision 2015-2025
1. What are the Conditions for Planet Formation
and the Emergence of Life?
2. How does the Solar System Work?
3. What are the Fundamental Physical Laws of the
Universe?
4. How did the Universe Originate and what is it
Made of?
[1] Cosmic Vision Brochure – BR247: http://www.esa.int/esapub/br/br247/br247.pdf
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[1]
Cosmic Vision 2015-2025
• Explore the limits of contemporary physics
– Use stable and weightless environment of space to search
for tiny deviations from the standard model of fundamental
interactions
• The gravitational wave Universe
– Make a key step toward detecting the gravitational radiation
background generated at the Big Bang
– LISA follow-up mission
• Matter under extreme conditions
– Probe gravity theory in the very strong field environment of
black holes and other compact objects, and the state of
matter at supra-nuclear energies in neutron stars
– X-ray and gamma ray astronomy
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Fundamental Physics Explorer Programme
• Do all things fall at the same rate?
– Cold-Atom interferometer
• Do all clocks tick at the same rate?
– Optical clocks
• Does Newton’s law of gravity hold at very small distances?
– Take advantage of the drag-free environment
• Does Einstein’s theory of gravity hold at very large
distances?
– Pioneer anomaly: potential for optical clocks
• Do space and time have structure?
– Fundamental constants
– Cold-atom technology and/or ultra-stable clocks
• Does God play dice?
– BEC, atom laser, atom interferometer
• Can we find new fundamental particles from space?
– Cosmic-ray particle detection
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Outline
• Presentation of the Optoelectronics Section
• Fundamental Physics Missions at ESA
• Cosmic Vision
• Technology Needs for Future Fundamental
Physics Missions
• Technology Development Strategy
• Earth Observation and Planetology
• Current and Planned Activities
• Conclusions
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Technology Needs for FPEP
Technology
Comment
Cryogenic accelerometers
Superconducting test masses and readout (SQUIDs)
Magnetic shielding
Extremely low stray fields
Cold-atom source
Robustness and reliability, low power, lightweight; atom chips
Low-noise cold-atom source
Various elements, e.g. Cs, Rb, H, Mg, Ca, Sr, Ag, Xe, I
Bose-Einstein condensate
High level of integration and nanotechnology
Atom traps
Tight traps, smaller than the de Broglie wavelength; box-shaped
potential wells where atoms can be free-floating
Atom laser
Independent cooling and trapping, chip-based atom source, for
high brightness
Ultra-stable lasers
Low-amplitude and frequency noise, accurate beam-shaping
Ultra-stable microwave source
For laser control and frequency combs
Ultra-stable Raman lasers
High-frequency stabilisation for narrow atomic transitions
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Ultra-High Accuracy Metrology
• Tests fundamental physics theories require ultrahigh accuracy metrology of:
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Distance
Accelerations
Rotations
Time
• Focus on cold-atom technology:
– stabilized lasers: to cool and manipulate atoms
– atom interferometry: to measure accelerations, rotations …
– (optical) atomic clocks: to measure time and distance
• Miniaturization and space qualification
– Micro optics, atom chips
– Reliability
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Outline
• Presentation of the Optoelectronics Section
• Fundamental Physics Missions at ESA
• Cosmic Vision
• Technology Needs for Future Fundamental
Physics Missions
• Technology Development Strategy
• Earth Observation and Planetology
• Current and Planned Activities
• Conclusions
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A Compelling Strategy
• Given:
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One potential fundamental physics mission
Highly competitive, low funding environment
Cold-atom technology will benefit from space environment
Cold-atom technology will benefit fundamental physics
Large effort needed to bring cold-atom technology in space
• Need to propose cold-atom technology as generic not
limited to fundamental physics (navigation, gravimetry)
• Alternatively, find more applications to fundamental
physics measurements
• Seek objective commonalities with other customers
• For example: Gravimetry
– Earth Observation
– Planetology
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Outline
• Presentation of the Optoelectronics Section
• Fundamental Physics Missions at ESA
• Cosmic Vision
• Technology Needs for Future Fundamental
Physics Missions
• Technology Development Strategy
• Earth Observation and Planetology
• Current and Planned Activities
• Conclusions
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Gravimetry
• Studies:
– EO: “Enabling Observation Techniques for Future Solid
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Earth Missions”
– Optoelectronics Section: “Gravity Gradient Sensor
Technology for Planetary Missions” [3]
• Results:
– Sensitive gravimeters using very precise atomic clock
– Atom Interferometry; gravity gradiometry
– Development of Optical Clocks to measure variations of
fundamental constants
[1] “Enabling Observation Techniques for Future Solid Earth Missions”, Science Objectives for Future Geopotential Field Mission,
SOLIDEARTH-TN-TUM-001, Issue 6, 1 Nov. 2003.
[2] “Enabling Observation Techniques for Future Solid Earth Missions”, Final Report, SolidEarth-TN-ASG-009, Issue 1, 6 May 2004.
[3] “Gravity Gradient Senser Technology for future planetary missions”, Final Report, ESA ITT A0/1-3829/01/NL/ND, 13 July 2005.
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Earth Gravity Missions
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Using satellites to map global gravity field
Measure geopotential second order derivatives
Spherical harmonic expansion
Geoid (equipotential)
Gravity field
Anomalies
Precision (mm, mGal)
Spatial resolution
Temporal resolution
Time span
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Applications
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Use satellite and ground data + modelling
Solid Earth
Geophysics
Geodesy
Hydrology
Oceanography
Ice sheets
Glaciers
Sea level
Atmosphere
Lumped sum
Aliasing
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Types of Missions
• High Earth orbit (HEO) satellite
– Passive laser reflector (LAGEOS)
– Laser tracking from reference ground stations
– Non-gravitational forces removed by design + modelling
• High-Low Satellite-to-satellite tracking (SST)
– LEO satellite tracked by GPS type constellation (CHAMP)
– Non-gravitational forces measured by accelerometers
• Low-Low SST
– Inter-satellite ranging (GRACE)
– Combined with GPS tracking
– Non-gravitational forces measured by accelerometers
• Satellite gravity gradiometry (SGG)
– Gravity field accelerations measured by accelerometers (GOCE)
– Non-gravitational forces measured by (same) accelerometers
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HEO mission
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Use high orbit as natural filter (low harmonics)
GPS tracking
Accelerometers
High precision clock (10-16)
Advantages:
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Innovative
Earth sciences
Time keeping
Fundamental physics
Telecommunications
• Drawbacks (as compared to LAGEOS):
– Mission life time
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GOCE
• GOCE: Gravity field and steady state Ocean
Circulation Explorer
• Launch date: 2006
• Altitude: 250 km
• Orbit: sun synchronous
• Main payload: three-axis gradiometers
• Observables: diagonal gravity gradient tensor
components, Txx, Tyy, Tzz
• Predicted accuracy: 100 to 6 mE/√Hz
• Measurement band: 100 to 5 mHz
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Future Needs
• ESA funded Earth Sciences study: “Enabling
Observation Techniques for Future Solid Earth
Missions” by EADS Astrium
• Low-low SST
• Satellite Gravity Gradiometry (SGG)
• Observables: diagonal gravity gradient tensor
components, Txx, Tyy, Tzz
• Required accuracy: down to 0.1 mE/√Hz
• Measurement band: 100 to 0.1 mHz
• (Pointing rate knowledge: 4·10-11 rad s-1/√Hz)
• Will current three-axis gradiometer technology be
able to meet these requirements?
• Can atom interferometry do it better?
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Planets and Moons
• ESA funded GSP study: “Gravity Gradient Sensor
Technology for Future Planetary Missions” by
University of Twente
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Future Needs
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Volume and mass constraints
Size: TBD (assumed 10 cm)
Weight: ~3 kg
Available data: line of sight
Required accuracy: 1 mE/√Hz
Airplane gradiometers
(Earth, Mars, Titan)
Technology review:
Superconducting devices
MEMS
Atom interferometry
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AI Gradiometer
• Gravity gradiometer Proof-of-Concept (Kasevich et al.)
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Planetary Gradiometer
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Back of the envelope concept
Assuming laser and optics miniaturisation
Vacuum chamber size: ~10 cm
Vacuum chamber
g
with the atom cloud
Atom cloud size: ~5 mm
Atomic species: Cs or Rb
Gravity gradient= (g1-g2)/L
Baseline 1 m
1m
Weight: few kg?
Could achieve 1 mE/√Hz
1 m baseline: 10-13g/√Hz
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control
Laser
electronics
Interrogation time: 10 s
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Optical fibers
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ASTROD 2006
Outline
• Presentation of the Optoelectronics Section
• Fundamental Physics Missions at ESA
• Cosmic Vision
• Technology Needs for Future Fundamental
Physics Missions
• Technology Development Strategy
• Earth Observation and Planetology
• Current and Planned Activities
• Conclusions
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What is needed
• Atom Optics
– Space qualified stable Source of Cold Atoms
• Compact laser sources for cold atom production
– To cool down atoms and control atomic beams
• Ultra-stable Raman Lasers
– For coherent matter wave splitting
• Optical frequency synthesizer
– Space qualifiable femtosecond comb
• Realisation of a feasible Optical Frequency standard/s for
space
– Select most suitable option from the choices available
• Realise a completely optical atomic clock
– Design and verification
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Ongoing Activities
• Atom Optics
– Laser-cooled Atom Sensor for Ultra-High-Accuracy
Gravitational Acceleration and Rotation Measurements
• Optical Atomic Clocks
– Required linewidth narrower than for optically pumped
microwave atomic clocks
– Ultra-narrow linewidth probe lasers: ≤ 1 Hz
– Laser-pumped Rubidium gas cell clock (780nm/795nm)
• Solutions implemented @ 780nm:
» External cavity diode laser (ECDL): 100s kHz
» Fabry-Perot (FP): 4-6 MHz
– Laser-pumped Caesium bean clock (852nm/894nm)
• New activity (894nm) in support of navigation/GALILEO
• New activity (894nm) ultra-narrow linewidth for a more generic
application
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Planned Activities
• Optical Frequency Synthesizer activities
• Optical Frequency Comb: Critical Elements PreDevelopment
– Synthesis of optical frequencies and identification of critical
issues for space qualification
– Use for future fundamental physics experiments in space
• Space Compatibility Aspects of a Fibre-Based
Frequency Comb
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Needed Measurement and Verification
• Narrow band diode laser measurements
– To support the ongoing DFB/FP activities
– To initiate new activities aimed at ultra-narrow linewidth
development
– Establish consistent traceable standards in Europe
– Sources of error in linewidth determination
• Heterodyne vs homodyne
• Noise sources
• Line shape dependencies
• Diode laser measurement laboratory
• Comparison with other laboratory
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Possible Future Activities
• Laser frequencies for Optical Atomic Clocks –
Some possibilities:
– Single ion
• Hg+
• In+
• 171Yb+ (Octopole)
• 171Yb+ (Quadrupole)
• 88Sr+
282 nm
237 nm
467 nm
435.5 nm
674 nm
– Cold atom
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Strontium (Sr)
Ytterbium (Yb)
Calcium (Ca)
Calcium (Ca)
Silver (Ag)
698 nm
578 nm
657 nm
457.5 nm
661.2 nm
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Outline
• Presentation of the Optoelectronics Section
• Fundamental Physics Missions at ESA
• Cosmic Vision
• Technology Needs for Future Fundamental
Physics Missions
• Technology Development Strategy
• Earth Observation and Planetology
• Current and Planned Activities
• Conclusions
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ASTROD 2006
Conclusions
• Ongoing/planned work:
– Optical Atomic Clocks
– Cold atom source for atom interferometry in space
• Still a lot to be done
• Difficult to secure funding when no clear mission is on the
horizon
• Adopt strategy of developing generic technologies:
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Time keeping
Gravimetry for Earth and planets
Navigation
etc…
• Comments and suggestions from experts most welcome
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谢谢你
Thank you
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