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

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Presentation transcript:

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 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.

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

150mm 250mm AU2 LOWFS BS2

Reserved location for IR-WFS

150mm 250mm

Letter of Understanding between 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)

Conceptual optical design of IR pyramid WFS.