ESA technology development activities for fundamental
physics space missions
B. Leone, E. Murphy, E. Armandillo
Optoelectronics Section
ESA-ESTECEuropean Space Research and Technology Centre
European Space AgencyNoordwijk, The Netherlands
14 July 2006 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
14 July 2006 ASTROD 2006
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• Lidar• Distance metrology• Frequency standards• Laser-cooled atom interferometry• Laser damage (laboratory)
14 July 2006 ASTROD 2006
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
14 July 2006 ASTROD 2006
Our Role within ESA
• Directorate of Technical and Quality Management• Support Directorate within a matrix organisation• Customers:
– 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
14 July 2006 ASTROD 2006
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
14 July 2006 ASTROD 2006
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
14 July 2006 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
14 July 2006 ASTROD 2006
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
14 July 2006 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
14 July 2006 ASTROD 2006
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
[1]
14 July 2006 ASTROD 2006
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
14 July 2006 ASTROD 2006
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
14 July 2006 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
14 July 2006 ASTROD 2006
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
14 July 2006 ASTROD 2006
Ultra-High Accuracy Metrology
• Tests fundamental physics theories require ultra-high accuracy metrology of:– 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
14 July 2006 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
14 July 2006 ASTROD 2006
A Compelling Strategy
• Given:– 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
14 July 2006 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
14 July 2006 ASTROD 2006
Gravimetry
• Studies:– EO: “Enabling Observation Techniques for Future Solid
Earth Missions”– Optoelectronics Section: “Gravity Gradient Sensor
Technology for Planetary Missions”
• 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.
[1, 2]
[3]
14 July 2006 ASTROD 2006
Earth Gravity Missions
• 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
14 July 2006 ASTROD 2006
Applications
• Use satellite and ground data + modelling• Solid Earth• Geophysics• Geodesy• Hydrology• Oceanography• Ice sheets• Glaciers• Sea level• Atmosphere• Lumped sum• Aliasing
14 July 2006 ASTROD 2006
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
14 July 2006 ASTROD 2006
HEO mission
• Use high orbit as natural filter (low harmonics)• GPS tracking• Accelerometers• High precision clock (10-16)• Advantages:
– Innovative– Earth sciences– Time keeping– Fundamental physics– Telecommunications
• Drawbacks (as compared to LAGEOS):– Mission life time
14 July 2006 ASTROD 2006
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
14 July 2006 ASTROD 2006
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?
14 July 2006 ASTROD 2006
Planets and Moons
• ESA funded GSP study: “Gravity Gradient Sensor Technology for Future Planetary Missions” by University of Twente
14 July 2006 ASTROD 2006
Future Needs
• 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
14 July 2006 ASTROD 2006
Planetary Gradiometer
• Back of the envelope concept• Assuming laser and optics miniaturisation• Vacuum chamber size: ~10 cm• Atom cloud size: ~5 mm• Atomic species: Cs or Rb• Baseline 1 m• Weight: few kg?• Could achieve 1 mE/√Hz• 1 m baseline: 10-13g/√Hz• Interrogation time: 10 s
1m
Lasercontrol
electronics
g1
g2
Gravity gradient= (g1-g2)/L
Vacuum chamber with the atom cloud
Optical fibers
14 July 2006 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
14 July 2006 ASTROD 2006
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
14 July 2006 ASTROD 2006
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
14 July 2006 ASTROD 2006
Planned Activities
• Optical Frequency Synthesizer activities
• Optical Frequency Comb: Critical Elements Pre-Development
– 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
14 July 2006 ASTROD 2006
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
14 July 2006 ASTROD 2006
Possible Future Activities
• Laser frequencies for Optical Atomic Clocks – Some possibilities:– Single ion
• Hg+ 282 nm• In+ 237 nm• 171Yb+ (Octopole) 467 nm• 171Yb+ (Quadrupole) 435.5 nm• 88Sr+ 674 nm
– Cold atom• Strontium (Sr) 698 nm• Ytterbium (Yb) 578 nm• Calcium (Ca) 657 nm• Calcium (Ca) 457.5 nm• Silver (Ag) 661.2 nm
14 July 2006 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
14 July 2006 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:
– Time keeping
– Gravimetry for Earth and planets
– Navigation
– etc…
• Comments and suggestions from experts most welcome
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