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SMART, Hida and next

SMART, Hida and next. NAGATA, SHIN’ICHI. Solar Magnetic Activity Research Telescope (SMART). The telescope was built at the Hida Observatory Kyoto University 2003 (Ueno et al. 2004) Bundle of Four telescopes T1:full disk H-alpha imaging ( f 20cm)

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SMART, Hida and next

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  1. SMART, Hida and next NAGATA, SHIN’ICHI

  2. Solar Magnetic Activity Research Telescope (SMART) The telescope was built at the Hida Observatory Kyoto University 2003 (Ueno et al. 2004) Bundle of Four telescopes T1:full disk H-alpha imaging (f20cm) T2:full disk magnetograph (f20cm) T3:partial disk H-alpha (f25cm)‏ T4:partial disk magnetograph(f25cm) FeI 630.2nm Data archive http://www.hida.kyoto-u.ac.jp/SMART/ Project status: H-alpha observations keeps going well. On the other hand, precise vector magnetic field measurements are not realised yet.

  3. SMART Publications (Problem 1) • Refereed • Nagashima et al. ApJ (2007) • Narukage et al. ApJL (2008) • Asai et al. JGR (2009) • Proceedings • UeNo et al. SPIE (2003) • Ishii et al. ASPC (2004) • Nagata et al. ASCP (2004) • Ueno et al. ASPC (2004) • Nagata et al. SPIE (2009) The list is incomplete but the products of 7 years operations is not so large ~0.4 refreed papers /year ~0.7 proceedings papers /year (Problem 2) Scientific contribution from core team members is not enough (Nagata, Ueno, PDs). What is the matter? We still have to spend most of our time for instrumentation: (a) Magnetic field measurement system improvement for T4. (b) Automated operations to save our time for science.

  4. SMART Narrow band filters We have a lot of narrow band filters, and the experience, including human resources, with those filters are precious heritage of us for the future missions.

  5. Lyot Filter

  6. Fabry-Perot filters

  7. 10 1 2 3 3 4 4 6 8 7 5 9 5 TCE specification TCE110 Thickness: 0.427mm FSR: 0.19nm FWHM: 0.0133nm Finess: 14.3 Tilt mechanism: no Pre-filter: installed Clear aperture: 60mm TCE114 Thickness: 0.303mm FSR: 0.27nm FWHM: 0.0172nm Finess: 15.5 Tilt mechanism: installed Pre-filter: no Clear aperture: 60mm • Etalon cell • Linear actuator for tilting • Heater for temperature control • Windows x 2 • Window retaining rings x 2 • Pre-filter mounting location • Pre-filter retaining ring • Manual screwdriver tilt adjust • High Voltage connectors x 2 • Control cable connectors x 2

  8. Distance and optical index are changed by applying voltage Multiple reflection between the two surfaces.

  9. Fabry-perot filters characterization FWHM ~0.017nm • FWHM(nm) 0.017 0.013 • FSR 0.266 0.189 • Finnese 15.5 14.3 • FWHM(nm) 0.019 0.017 • FSR 0.26 0.19 • Finnese 13.6 11.2 Calibrated at the Domeless Solar Telescope Hida Observatory

  10. SMART T1 Objective lens collimator lens Narrow band filter Imaging lens CCD Camera

  11. SMART T2 Objective lens collimator lens Narrow band filter Imaging lens CCD Camera

  12. SMART T3 Objective lens collimator lens Narrow band filter Imaging lens CCD Camera

  13. SMART T4 Objective lens Relay Lens Narrow band filter Relay lens CCD Camera

  14. SMART Lyot Filter problems • Damesage on optical element • Some of calcites were broken into pieces due to mechanical stress? • Degradation of transmittance • Transmittance degrades along with time mechanical • Supperior spatial resolution • Due to wave front errors, spatial resolution is significantly degraged? • Observation system • Operation is affected by electro-magnetic noise from other instrument

  15. The dark features on 50mm H-alpha filter(2009.02.28) ８Ａブロックを構成する４枚の方解石のうち３枚が割れているのを 確認。 この４枚を交換した（２０１０．０３）

  16. Transmittance degradation

  17. T3spatial resolution problem example (2007.12.06) T1(32mm) T3(50mm)

  18. SMART FP Filterissues • The filter has not been mounted on the telescope • Optical performance verification • Transmittance map across the clear aparture Some of the key parameters to be confirmed: • Central wavelength: 630.2 nm • FWHM: 0.01 nm • Overall Finesse of each etalon based on Reflectance of coatings: ~ 14 • FWHM stability/variation over the aperture : target < 4.9 % of FWHM • Central wavelength stability/variation over the aperture : target < 0.002 nm

  19. Test configuration CCD camera (Prosilica GE1650) imaging lens FP filter Collimator lens Spatial filter He-Ne Laser

  20. Test configuration Camera(GE1650-24004) Calibration light path Test 4 mirror Camera (GE1650-100246) Fabry-Perot Filter Pupil He-Ne 光Φ0.48mm 05-STP-910 BS Collimator lens Imaging lens The light through filter

  21. Without FP filter With FP filter

  22. “Transmittance” map “transmittance” is observed to be larger tan 100%

  23. Test configuration Camera(GE1650-24004) Calibration light path Test 4 mirror Camera (GE1650-100246) Fabry-Perot Filter Pupil He-Ne 光Φ0.48mm 05-STP-910 BS Collimator lens Imaging lens The light through filter The FP filter works as lens? The FP filter work as wave-plae?

  24. What is next? • Classical three problems in the solar physics. What is the break through for the next? • Solar Flares (Non-thermal particle acceleration) • Solar Coronal heating • Chromospheric fields • Solar Dynamo • Precise surface velocity field measurement • Projects (globalization should be taken into account) • SOLAR-C project with ISAS/JAXA • Ground-based telescopes • Hida heritage • Narrow band filters development?

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