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)

Data archivehttp://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.

FeI 630.2nm

SMART Publications

• 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

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.

(Problem 1)

(Problem 2)

SMART Narrow band filtersタイプ 口径

(mm)波長 FWHM

(mA) 用途 現状Lyot 32 6563+/-2 250 SMART T1 休止中Lyot 40 6563+/-2 250 SMART T1 稼働中（調整中）Lyot 50 6563+/-2 250 SMART T3 休止中（改修中）Lyot 32 6302+/-2 125 SMART T2 稼働中FP(tandem) 60 6302 100 SMART T4 準備中FP 60 6302 100-125 SMART T4 休止中FP 60 6563 150-250 SMART T4 休止中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.

Lyot Filter

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Fabry-Perot filters

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TCE specificationTCE110Thickness: 0.427mmFSR: 0.19nmFWHM: 0.0133nmFiness: 14.3Tilt mechanism: noPre-filter: installedClear aperture: 60mm

TCE114Thickness: 0.303mmFSR: 0.27nmFWHM: 0.0172nmFiness: 15.5Tilt mechanism: installedPre-filter: noClear aperture: 60mm

1. Etalon cell2. Linear actuator for tilting3. Heater for temperature control4. Windows x 25. Window retaining rings x 26. Pre-filter mounting location7. Pre-filter retaining ring8. Manual screwdriver tilt adjust 9. High Voltage connectors x 210. Control cable connectors x 2

Lith ium n iobate s ubst rate

M ult ilaye r m irro r coat ings

C ond uct ingt rans pa re ntind ium t in ox ide laye rs

HV pow er s upp ly

Direct io n ofinc ide nt lig ht

d s

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bR

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630.0 630.2 630.40

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40

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80

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0.42mm Etalon

Full Width Half MaximumFWHM

Maximum TransmittanceTmax

Free Spectral RangeFSR

Minimum TransmittanceTmin

Tran

smitt

ance

(%)

Wavelength (nm)

Distance and optical index are changed by applying voltage

Multiple reflection between the two surfaces.

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Fabry-perot filters characterization

FWHM(nm) 0.017 0.013FSR 0.266 0.189Finnese 15.5 14.3

FWHM(nm) 0.019 0.017FSR 0.26 0.19Finnese 13.6 11.2

FWHM ~0.017nm

Calibrated at the Domeless Solar TelescopeHida Observatory

SMART T1Objective lens

collimator lens

Narrow band filter

Imaging lens

CCDCamera

SMART T2Objective lens

collimator lens

Narrow band filter

Imaging lens

CCDCamera

SMART T3Objective lens

collimator lens

Narrow band filter

Imaging lens

CCDCamera

SMART T4Objective lens

RelayLens

Narrow band filter

Relaylens

CCDCamera

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

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）

Transmittance degradation

T3 spatial resolution problem example (2007.12.06)

T1(32mm) T3(50mm)

SMART FP Filter issues

• 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 :1.Central wavelength: 630.2 nm2.FWHM: 0.01 nm 3.Overall Finesse of each etalon based on Reflectance of coatings: ~ 144.FWHM stability/variation over the aperture : target < 4.9 % of FWHM5.Central wavelength stability/variation over the aperture : target < 0.002 nm

Test configuration

He-Ne Laser

Spatial filter

Collimator lensimaging lensCCD camera (Prosilica GE1650)

FP filter

Test configuration

He-Ne 光 Φ0.48mm

BS05-STP-910Collimator lens Imaging lens

Fabry-Perot Filter PupilCamera(GE1650-100246)

Camera(GE1650-24004)

The light through filter

Calibration light path

Test 4mirror

Without FP filter With FP filter

“Transmittance” map

“transmittance” is observed to be larger tan 100%

Test configuration

He-Ne 光 Φ0.48mm

BS05-STP-910Collimator lens Imaging lens

Fabry-Perot Filter PupilCamera(GE1650-100246)

Camera(GE1650-24004)

The light through filter

Calibration light path

Test 4mirror

The FP filter works as lens?The FP filter work as wave-plae?

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?