The Hinode Solar Optical Telescope

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The Hinode Solar Optical Telescope Instrument
Performance Dr. Thomas Berger Lockheed Martin
Advanced Technology Center Palo Alto, CA and the
SOT TEAM
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What is Hinode?
SOT Solar Optical Telescope
EIS Extreme-ultraviolet Imaging Spectrometer
XRT X-ray Telescope
Hinode is a Japanese/US/UK mission designed to
investigate the Suns generation of magnetic
field, heating of the outer atmosphere, and
initiation of flares and mass ejections.
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Hinode is in a Sun Synchronous Orbit
Launch vehicle ISAS MV Launch date
23-September-2006 Orbit polar Sun synchronous,
altitude 600 km
inclination 97.9 Eclipse season mid-May -
August Nominal mission lifetime 3 years
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Hinode Launch, 23-Sept-2006
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SOT Optical Telescope Assembly
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SOT OTA FPP
OTA Optical Telescope Assembly
FPP Focal Plane Package
Secondary mirror
Heat dump mirror
Optical Telescope Assembly (OTA), is a Gregorian
telescope with 50 cm aperture, built by
NAOJ/ISAS. Focal Plane Package (FPP), includes
observation filters, spectrometer, and cameras ,
built by LMSAL/HAO/NASA.
50 cm F/2 primary mirror
Collimating Lens Unit
Polarization Modulator
Tip/Tilt Active Mirror
FPP Reimaging/Focus Lens
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SOT Optical Schematic
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FG CCD
FPP NFI BFI SP
Spectropolarimeter (SP) Littrow spectrograph
Broadband Filter Imager (NFI) Interference
filters 388 - 680 nm
SP CCD 112 x 1024 split-frame readout
FG CCD 4096 x 2048 split-frame readout
Narrowband Filter Imager (NFI) Tunable Lyot
Filter 500 - 700 nm
Correlation Tracker 64 x 64 800 MHz
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BFI Characteristics
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NFI Characteristics
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SP Characteristics
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The SP takes spectra of the two Fe I lines near
630 nm Fe I 630.15 and 630.25 nm. Spectra are
taken in synchronous patterns with the
Polarization Modulator in the OTA and
added/subtracted in on-board memories.
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Hinode Fields of View
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SOT Field of View and Resolution
Solar Diameter 1,400,000 km
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SOT Spatial Resolution
4000 km
16,000 km
G-band 430.5 nm
150 km
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Courtesy of J. Okamoto, NAOJ
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SOT Spatial Stability
0.01 RMS
Servo Off!
Correlation Tracker Image
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SOT Focus Stability
Gradual shift of focus is due to shrinkage of
CFRP structure of OTA. This is expected behavior.
Limb measurements Offset between center and limb
5 steps
FPP reimaging lens steps
Date
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SOT Focus stability during eclispe season
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BFI Chromatic Aberration
FPP Reimaging Lens
9 steps of reimaging lens 1.36 mm 4 steps ? WFE
of 21 nm lt ?/20 at 430 nm
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SOT SP Performance
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SOT SP Performance
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sp_prep
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SOT BFI throughput decrease
FG CCD Bakeout
Eclipse
Cause is still under investigation. No science
impact since we can increase exposures to
compensate.
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SOT NFI throughput decrease
Fe I 630.25 nm continuum 60 in throughput since
launch. Cause is UV exposure on the blocking
filter. The trend is now suppressed by stowing
the blocking filter when not in use. Science
impact Fe I 630 nm spectral region is not
recommended for magnetograms anymore.
Does not effect SP 630 nm performance
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SOT NFI bubbles
The NFI has air bubbles in the index-matching oil
of the filter. These cause loss of throughput in
localized regions of the FOV. The bubbles move
when the filter is tuned. We are learning how to
tune to put the bubbles out of the FOV. Science
impact NFI cannot rapidly tune between
wavelengths. You must know where the bubbles
are when analyzing NFI data.
Lyot Elements
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SOT NFI bubble appearance
Current situation
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Possible tunings without bubble movement
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Fe I 557.6 nm dopplergram 2007-07-14 5576 136
mÅ
Continuum
dopplergram
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Seasonal orbital doppler velocity variation
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Mg Ib 517.3 nm Shutterless Stokes IQUV images
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