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Infrared Wavefront Sensor (IR-WFS)

Infrared Wavefront Sensor (IR-WFS). Yutaka Hayano Internal Meeting on Future Instrument Projects at Subaru April 26, 2010. Why IR WFS. Highly obscured region. (No visible guide star.) Galactic center. Star forming region. Disks around massive YSOs

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Infrared Wavefront Sensor (IR-WFS)

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  1. Infrared Wavefront Sensor(IR-WFS) Yutaka Hayano Internal Meeting on Future Instrument Projects at Subaru April 26, 2010.

  2. 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.

  3. From Telescope HOWFS AO IMR AU1 DM ADC LOWFS BS2 AU2 BS1 To science instrument

  4. BS2 AU2 LOWFS 250mm 150mm

  5. Reserved location for IR-WFS

  6. Reserved location for IR-WFS 250mm 150mm

  7. 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)

  8. Conceptual optical design of IR pyramid WFS.

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