infrared wavefront sensor (ir-wfs) yutaka hayano internal meeting on future instrument projects at...
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![Page 1: Infrared Wavefront Sensor (IR-WFS) Yutaka Hayano Internal Meeting on Future Instrument Projects at Subaru April 26, 2010](https://reader036.vdocument.in/reader036/viewer/2022062518/56649e915503460f94b96e11/html5/thumbnails/1.jpg)
Infrared Wavefront Sensor(IR-WFS)
Yutaka Hayano
Internal Meeting on Future Instrument Projects at SubaruApril 26, 2010.
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Why IR WFS• Highly obscured region. (No visible guide star.)– Galactic center.– Star forming region.
• Disks around massive YSOs• Molecular Gas disks in planet forming disks• Companion search for Class I stars (low mass YSOs)• Jet/Outflow (Class I includes HH objects)
• Red objects. (Bright source in IR no in visible.)– M dwarf stars in local group.– Brown dwarf.
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From Telescope
AO IMR
DM
HOWFS
LOWFS
To science instrument
BS1
BS2
AU1
AU2
ADC
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150mm
250mm
AU2
LOWFS
BS2
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Reserved location for IR-WFS
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Reserved location for IR-WFS
150mm
250mm
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Letter of Understandingbetween Subaru and MPIA
• Contact person– Hayano (Subaru)– Markus Feldt (MPIA)
• Feasibility study.– S-H WFS.– IR Pyramid WFS.
• Science team.• Funding efforts.
– MPIA.– Wakate S. (Usuda)– Tokusui. (Tamura)
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Conceptual optical design of
IR pyramid WFS.