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Introduction of SST

An EUV Imaging Detector of Space Solar Telescope Qian Song, Binxun Ye, Zhaowang Zhao National Astronomical Observatories, China Chinese Academy of Sciences. Introduction of SST. The Space Solar Telescope, the first space astronomy program in China. Satellite.

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Introduction of SST

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  1. An EUV Imaging Detector of Space Solar TelescopeQian Song, Binxun Ye, Zhaowang ZhaoNational Astronomical Observatories, ChinaChinese Academy of Sciences SWD 2005, Taormina, Jun,19-26

  2. Introduction of SST The Space Solar Telescope, the first space astronomy program in China SWD 2005, Taormina, Jun,19-26

  3. Satellite Solar synchronous circular orbit Orbit height: 735 km Inclination: 98.3° Period: 99.3 min Attitude: accuracy ±6", stability ±3"/s Weight: 2 ton Lifetime: 3 years Launch: LM-4B SWD 2005, Taormina, Jun,19-26

  4. Payloads • MOT • EUT • HWT • WBS • SIR SWD 2005, Taormina, Jun,19-26

  5. Main optical telescop, MOT with a 2-D polarizing spectrograph, working in 8 channels simultaneously Resolution 0.1‘ FOV 2.8'×1.5‘ Polarization Accu. 2×10 –4 SWD 2005, Taormina, Jun,19-26

  6. Payloads HWT: a Hα and white light telescope, whole sun viewing resolution 1 , FOV 0.7°×0.7° WBS: a wide band spectrometer, investigating high energy flare process on  -ray, hard & soft x-ray SIR: solar and interplanetary radiospectrometer, 1-60GHz nonthermal electron populations SWD 2005, Taormina, Jun,19-26

  7. EUT Based on the EUVSAT proposal. Consists of four normal incidence telescopes mounted in a vacuum vessel, which should overlap, be well aligned and synchronized with each other and with the images of the MOT. Field of view 7’×7’ Resolution 0.8” Wave length 12.8, 17.1, 19.5, 30.4 nm (subject to change) Focal length 7.04 m Distance between Mirrors 1.4 m Primary Mirror 120 mm Secondary mirror 48 mm SWD 2005, Taormina, Jun,19-26

  8. EUT structure SWD 2005, Taormina, Jun,19-26

  9. EUT Detector: requirements • To achieve highest sensitivity, a combination of a phosphor screen, an image intensifier and a CCD is proposed. This not only improves the sensitivity for low intensity scenes, but as a bonus it provides an electronic shutter as well, one with no moving part. • 2048×2048 format • At least 12 bit dynamic range between CCD readout noise and full well capacity • Spacial resolution should match the telescope’s, 0.8”, or 27.3μ, 36.6 lp/mm SWD 2005, Taormina, Jun,19-26

  10. EUT Detector: Structure In order to achieve high sensitivity, an image intensifier is used A phosphor screen is needed to converse EUV photons to visible. A CCD imager is to be used with format changing optics (fiber optic taper) SWD 2005, Taormina, Jun,19-26

  11. Phosphor’s response on EUV SWD 2005, Taormina, Jun,19-26

  12. Phosphor’s output against input SWD 2005, Taormina, Jun,19-26

  13. MCP image intensifier, resolution 57 Lp/mm, gain 8900 cd /m2 /Lx, equivalent background irradiance 0.16 µLx • Optic taper: resolution >102Lp/mm SWD 2005, Taormina, Jun,19-26

  14. The front end of the detector SWD 2005, Taormina, Jun,19-26

  15. The outlook and inside of the detector SWD 2005, Taormina, Jun,19-26

  16. 5s dark: MCP contribution 800DN SWD 2005, Taormina, Jun,19-26

  17. Test on BSRF SWD 2005, Taormina, Jun,19-26

  18. The image of the 17.1nm beam of BSRF SWD 2005, Taormina, Jun,19-26

  19. Resolution test on 17.1nm SWD 2005, Taormina, Jun,19-26

  20. The intensity distribution of the 19μ grid SWD 2005, Taormina, Jun,19-26

  21. Response of the detector on 17.1nm & 19.5nm 17.1nm, 18e/photon 19.5nm, 21e/photon SWD 2005, Taormina, Jun,19-26

  22. Possible Solution • Better phosphor screen, MCP, fiber optic taper • Open MCP with CrI or KBr-coated photon cathode+CCD • EUV L3 CCD Suggestions and comments are very precious for us SWD 2005, Taormina, Jun,19-26

  23. SWD 2005, Taormina, Jun,19-26

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