HiCIAO Instrument Status

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HiCIAO Instrument Status
Ryuji Suzuki
Subaru Telescope
Motohide Tamura, Lyu Abe, Hiroshi Suto, Jun-ichi
Morino, Ryo Kandori, Hideki Takami, Olivier
Guyon, Alexander Tavrov, Naoshi Murakami, Jun
Nishikawa, Nobuharu Ukita, Hideyuki Izumiura,
Tetsuo Nishimura, Masahiko Hayashi (NAOJ), Jun
Hashimoto (GUAS), Shane Jacobson, Vern
Stahlberger, Hubert Yamada, Richard Shelton,
Klaus Hodapp (University of Hawaii)
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Table of Contents

• Overall View
• Observation Modes
• Performance
• User Interface
• Future Upgrade
• Schedule

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Overall View
Cryogenic IR Camera Module
Warm Coronagraph Module
1830 mm
Instrument Support Frame
2060 mm
1530 mm
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Observation Modes
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Performance
Laboratory tests

• Image quality
• Pupil viewer mode
• Detector characterization

First engineering observation in 12/3/2007

• Test all observation modes
• Alignment with the telescope
• Find out any kinds of bugs

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Performance

• Optics A pinhole image was obtained as
  simulated.
• Detector still high readout noise (30 e-) ?
  Use cold ASIC?
• Coronagraph laboratory tests are planned.
• DI/PDI/SDI modes worked

SDI image of Saturn
Obtained PSF
Simulated PSF
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User Interface

• Abstract commands
• GUIs
• QL, Data analysis package

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Future Upgrade
PIAA coronagraph (Olivier)

• proven to work in the laboratory
• will be implemented to HiCIAO as the first step
  upgrade

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Future Upgrade
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Schedule
We are expecting that the instrument will be
ready for science observations by next winter
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Specification
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User Interface

• IRAF based QL using external FFT libraries
• Create semi-publishable level images on the site

Image analysis simulation in the SDI mode
Reduction work flow

• Sky/Dark subtraction. Flat-fielding, Bad pixel
  removal, Distortion correction (if necessary)
• Correction for each sub-frame (PDI SDI)
• translate (sub-pixel accuracy FFT shift)
• relative field position (optional)
• compensate effect of atmospheric dispersion (if
  necessary)
• scale (very high precision iterative FFT
  scaling)
• rotate (very high precision iterative FFT
  rotation) (if necessary)
• Sub-field intensity scaling (depending on
  filter/spectrum)
• Sub-field pairs subtraction

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