Title: HiCIAO Instrument Status
1HiCIAO 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)
2Table of Contents
- Overall View
- Observation Modes
- Performance
- User Interface
- Future Upgrade
- Schedule
3Overall View
Cryogenic IR Camera Module
Warm Coronagraph Module
1830 mm
Instrument Support Frame
2060 mm
1530 mm
4Observation Modes
5Performance
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
6Performance
- 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
7User Interface
- Abstract commands
- GUIs
- QL, Data analysis package
8Future Upgrade
PIAA coronagraph (Olivier)
- proven to work in the laboratory
- will be implemented to HiCIAO as the first step
upgrade
9Future Upgrade
10Schedule
We are expecting that the instrument will be
ready for science observations by next winter
11Specification
12User 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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