1 / 41

Basic Principles / State of the Art

Novel Microchannel Plate (MCP) X-ray Optics for Astronomy and Other Applications G.W. Fraser Space Research Centre, Michael Atiyah Building, Department of Physics and Astronomy, University of Leicester. Basic Principles / State of the Art

edena
Télécharger la présentation

Basic Principles / State of the Art

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Novel Microchannel Plate (MCP) X-ray Optics for Astronomy and Other ApplicationsG.W. FraserSpace Research Centre, Michael Atiyah Building, Department of Physics and Astronomy, University of Leicester • Basic Principles / State of the Art • Applications in X-ray Astronomy, Planetary Science and Auroral Imaging • Other Applications (neutron focusing, high intensity X-ray sources, X-ray lithography..) Third Symposium on Large TPCs, Paris, 11th December 2006

  2. J.Pearson, A.Martindale, C.Brown, H.Yates, and H.Su (University of Leicester, UK) E.Schyns and R. Fairbend (Photonis, France) M.Bavdaz and K.Wallace (ESA) M.Beiersbergen and M.Collon, (cosine Research, Netherlands) Acknowlegements Third Symposium on Large TPCs, Paris, 11th December 2006

  3. Conventional diamond-turned (Chandra) or replicated Nickel (XMM-Newton) mirrors are heavy – a big disadvantage in space applications - and have limited ( ~1 degree) fields-of-view (FOVs) MCP (micropore) optics can have a mass advantage of ~1000 times per unit effective area and FOVs of ~3000 square degrees. The need for novel X-ray mirror technologies Third Symposium on Large TPCs, Paris, 11th December 2006

  4. Principles of a Lobster EyeX-ray Lens Angel (1979) ; Wilkins et al. (1989) ; Fraser et al. (1993). X-rays Diffuse background Double reflection (2-axes, true focus) Single reflection (1 axis, line focus) Third Symposium on Large TPCs, Paris, 11th December 2006

  5. Technical Challenges • (from an MCP electron multiplier starting point) • MCP channel cross-section and figure • Surface roughness • Uniformity and straightness of fibre • Mechanical perfection of multifibres • Stacking of multifibres • Spherical slumping (0.1<R<10 m) • Channel coating (Ni, Ir..) • Aluminium filming of channels Third Symposium on Large TPCs, Paris, 11th December 2006

  6. Planar MCP size - 40 mm x 40 mm 20 μm pores, 26 μm pitch ; L/D = 50:1 (1 mm thick) ;59% open area Mechanical Regularity I Multifibre boundary Third Symposium on Large TPCs, Paris, 11th December 2006

  7. MCP regularity II – multifibre scales Manufacture of MCP optics industrialised by ESA TRP funding at Photonis SAS (Brive-la-Gaillarde) Third Symposium on Large TPCs, Paris, 11th December 2006

  8. Current MCP X-ray image quality Planar MCP Point-to-Point focusing, Cu L X-rays (0.93 keV) 2 arcminute FWHM Third Symposium on Large TPCs, Paris, 11th December 2006

  9. Uncoated Ir-coated Demonstration of enhanced X-ray reflectivity at 2.5 keV for CVD Iridium-coated MCP optic Third Symposium on Large TPCs, Paris, 11th December 2006

  10. Comparison of bare, Ni-coated and Ir-coated reflectivities at 3.1 keV. Daresbury SRS Beamline 3.4 Third Symposium on Large TPCs, Paris, 11th December 2006

  11. X-ray results with planar, square-pore, square-packed MCP optics 2 arcminute FWHM focusing at ~ 1 keV ; ESTEC (Bavdaz et al ) measure ~15 arcsec on single multifibres. Implied radius of curvature – 21.7m – mounting optics identified as critical Third Symposium on Large TPCs, Paris, 11th December 2006

  12. Spherical Figure measured by Contact Profilometer Nominal R = 75 cm Measured R = 69 cm (blue curve) Third Symposium on Large TPCs, Paris, 11th December 2006

  13. Missions Mission Instrument Partners Kuafu WFAI China Lobster ASM ESA/Russia BepiColombo IXS ESA XNAV Multifocus telescope LANL/DARPA Jupiter-Europa IXS/WFAI ESA LAD-C Capture Cell ESA Third Symposium on Large TPCs, Paris, 11th December 2006

  14. LobsterThe first imaging X-ray all-sky monitor • Fast X-ray transients • Gamma Ray Bursts & X-ray flashes • Cataclysmic Variables • Non-flaring coronal sources • X-ray bursts & superbursts • Supersoft sources • AGN time variability • Type II supernovae shock breakout • Novae • Flares from non-active galaxies • Black holes in X-ray binaries • Deep surveys • X-ray background mapping • X-ray emission in the solar system (cometary studies) Third Symposium on Large TPCs, Paris, 11th December 2006

  15. Variation of resolution with focal distance Third Symposium on Large TPCs, Paris, 11th December 2006

  16. Lobster-ISS (Phase A study 2000-4) Third Symposium on Large TPCs, Paris, 11th December 2006

  17. Zenith 30º Direction of Motion The ISS as a platform for All Sky Monitoring ISS Truss Length 178 m ; Module Length 74 m ; Mass400 tons Tilt: 30º forward of zenith Total field: 162° x 22.5° • Field sweeps sky every 90 minute orbit. Rotation Axis Third Symposium on Large TPCs, Paris, 11th December 2006

  18. Sun sensor Optic Module Star Tracker Front Back Lobster-ISS Baseline Configuration Third Symposium on Large TPCs, Paris, 11th December 2006

  19. eRosita ART Sun Lobster-SRG Accommodation of Lobster (5 x 30deg x 30deg scan modules, plus co-aligned eRosita module) on Navigator platform Third Symposium on Large TPCs, Paris, 11th December 2006

  20. View towards +Z Third Symposium on Large TPCs, Paris, 11th December 2006

  21. Lobster-ISS Effective Area versus X-ray Energy Third Symposium on Large TPCs, Paris, 11th December 2006

  22. Instrument Grasp (Aeff x field of view) Lobster-ISS XMM-Newton Aeff x FOV (cm2 deg2) Lobster and XMM-Newton Third Symposium on Large TPCs, Paris, 11th December 2006

  23. Planetary IXRF - X-ray Remote Sensing Fluorescent X-rays Solar X-rays Third Symposium on Large TPCs, Paris, 11th December 2006

  24. Al/Si ratio of the lunar equatorial region from Apollos 15 and 16 (C.G. Andre et al. (Science 197 (1977) 986) Surface resolution - 30 km Surface coverage - 10% Third Symposium on Large TPCs, Paris, 11th December 2006

  25. Mariner 10 image of south polar region (Typical crater size in Mercury highlands ~120 km) • Science with BepiColombo MIXS • We aim to : • Map the elemental composition of the planetary surface on global, regional • and local scales, to help elucidate the origin and evolution of Mercury, • its anomalously high density, its cratering and volcanism • Measure the line and continuum X-ray emissions from the dynamic • interaction of the solar wind with the surface, exosphere and magnetosphere Third Symposium on Large TPCs, Paris, 11th December 2006

  26. Square-pore, Radially-packed MCP Wolter I Optics (Willingale and Fraser, 1993) Third Symposium on Large TPCs, Paris, 11th December 2006

  27. Wolter Type 1 for BepiColombo MIXS-T Third Symposium on Large TPCs, Paris, 11th December 2006

  28. Status of MCP optics for MIXS-T Measured X-ray focusing with planar radially-packed optic LB001-R-2: “point to point” focusing mode at Leicester

  29. Space research centre (a) (b) (c) Idealised ray trace model: in focus along the optical axis. Ray trace model including the effects of out-of-focus shift along the optical axis. Measured X-ray image, linear intensity scale Third Symposium on Large TPCs, Paris, 11th December 2006

  30. Log intensity re-scaled X-ray image from the prototype radial optic. Note “double arc” indicative of out-of-focus. The axes are marked in pixels (1pixel = 76microns) Cut in Azimuth Radial Cut Third Symposium on Large TPCs, Paris, 11th December 2006

  31. IXRFS Laboratory System : BepiColombo MIXS-T in miniature Third Symposium on Large TPCs, Paris, 11th December 2006

  32. Fiducial Marks and Resolution Estimation using 0.25 mm diameter copper wire Minimal effect of PSF Third Symposium on Large TPCs, Paris, 11th December 2006

  33. Garnetiferous Anorthosite: CCD Spectrum Third Symposium on Large TPCs, Paris, 11th December 2006

  34. Overlaid Optical and X-ray Images Third Symposium on Large TPCs, Paris, 11th December 2006

  35. Mg/Si Na/Ca Al/Si Element ratios Third Symposium on Large TPCs, Paris, 11th December 2006

  36. KuaFu (2012-2015) KuaFu-A at L1 KuaFu-B1&2polar orbit SOHO image Third Symposium on Large TPCs, Paris, 11th December 2006

  37. UV Auroral Imagery Global imaging of magnetospheric dynamics from space DE IMAGE FUV Polar UVI Third Symposium on Large TPCs, Paris, 11th December 2006

  38. Ultraviolet/Optical Focusing with MCPs of ~7 cm Radius of Curvature Talysurf Profilometer measurements Third Symposium on Large TPCs, Paris, 11th December 2006

  39. Wide Field Auroral Imager for KuaFu B Third Symposium on Large TPCs, Paris, 11th December 2006

  40. Season’s Greetings/ Joyeux Noel Third Symposium on Large TPCs, Paris, 11th December 2006

  41. Dust detection using filmed MCPs Microchannel Plates bearing 60nm thick Al film thermal barriers were exposed on the Russian PIRS module to the external ISS environment for 734 days The impacts reveal the presence of a high density of previously unobservable nanoscale particles either debris or natural dust The films are ~ a factor of 10 more sensitive to impacts than previously flown foils Nanoparticle Impacts (J.Carpenter et al.) at J.Geophys.Res.(2005) Third Symposium on Large TPCs, Paris, 11th December 2006

More Related