Space Research Centre Silicon Carbide X-Ray detectors for Planetary Exploration Dr. John E. Lees University of Leicester 8 th International Conference.

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Presentation transcript:

Space Research Centre Silicon Carbide X-Ray detectors for Planetary Exploration Dr. John E. Lees University of Leicester 8 th International Conference on Position Sensitive Detectors September 2008

Space Research Centre Introduction Limitations of silicon based detectors for planetary exploration cooling radiation damage Search for other materials – wide band gap GaAs Diamond Silicon Carbide SiC imaging arrays Collaboration with University of Newcastle

Space Research Centre Ideal requirements for X-ray detectors Photon counting Imaging Good timing resolution High spatial resolution Solar blind – not sensitive to visible light High quantum efficiency High dynamic range Low background Radiation hard Energy resolution XX SiC

Space Research Centre Semi-Transparent SiC Schottky Diode LHS: A 280  m 2 Schottky contact and gold bond pad RHS: Die layout with a range of diode sizes 1.0x10 -3 cm x10 -3 cm x10 -4 cm  m

Space Research Centre STSSD structure 20  m epitaxial layer on a 370  m substrate Semi-transparent Schottky contact. 3 nm Ti / 12 nm Ni 25 nm thermally grown SiO 2 4nm Cr / 200nm Au 5 nm Cr / 250nm Au4nmCr/100nmNi Ohmic Contact n 4H-SiC n + 4H-SiC Lees et al., Nucl. Inst. Meth A 578 (2007)

Space Research Centre Improving the Low Energy Response K-shell emission lines of elements: Na (Z=11, E=1.04 keV) to Zn (Z=30, E=8.64 keV) STSSD has an 18nm thick electrode

Space Research Centre Planetary Exploration GeneralMulti-spectral: X-rays/UV/Optical/Infra-red Imaging pixel arrays EnvironmentRadiation environment Shielding Radiation hard electronics Operating temperatures SpacecraftMass Power Cost

Space Research Centre Some current and planned planetary missions MercuryMessenger and BepiColombo VenusVenus Express and Venus Climate Orbiter MarsMars Reconnaissance Orbiter, Mars Express, ExoMars SaturnCassini-Huygens and Tandem JupiterJUNO and Laplace

Space Research Centre Jupiter X-rays (Chandra) FUV (HST)

Space Research Centre Auroral Processes Precipitation of energetic ions and electrons along field lines from the planetary magnetosphere into the atmosphere produces emissions in IR, visible, UV, and X-ray wavelengths Table shows typical values for the magnetised planets PlanetEarthJupiterSaturnUranusNeptune Electron input power (GW) UV output (GW) X-ray brem output (MW)

Space Research Centre Radiation environment Alessandro Atzei and Peter Falkner, ESA technical note, SCI-AP/2004/TN-085/AA

Space Research Centre Radiation environment Comparison between ONERA-full (D&G + GIRE + Salammbô) and ESA ref. D&G at an equatorial distance of 3 Rj from Jupiter centre

Space Research Centre Irradiation of STSSDs Phase 1 - irradiation at Paul Scherrer Institut 63 MeV protons Total fluence 1x10 11 cm -2 Phase 2 - irradiation at Theodor Svedberg Laboratory 50 MeV. Total fluence ~1 x protons cm-2.

Space Research Centre STSSD Radiation Tolerance I-V measurements

Space Research Centre STSSD Radiation Tolerance 55 Fe X-ray spectra

Space Research Centre STSSD Radiation Tolerance 109 Cd X-ray spectra

Space Research Centre Next Steps Material characterisation Improve electronics  better energy resolution Extend radiation fluences Protons, neutrons, electrons and X-ray/gamma-ray Modelling New device structures

Space Research Centre Acknowledgements Nigel BannisterUniversity of Leicester David Bassford Emma Bunce Stan Cowley George Fraser Mark Sims Dean Talboys Chris Whitford Alton HorsfallUniversity of Newcastle