Science programs for a 2-m class telescope at Dome C, Antarctica: PILOT, the Pathfinder for an International Large Optical Telescope
Burton, M.G., Lawrence, J.S., Ashley, M.C.B., Bailey, J.A., Blake, C., Bedding, T.R., Bland-Hawthorn, J., Bond, I. A., Glazebrook, K., Hidas, M.G., Lewis, G., Longmore, S.N., Maddison, S.T., Mattila, S., Minier, V., Ryder, S.D., Sharp, R., Smith, C.H., Storey, J.W. V., Tinney, C.G., Tuthill, P., Walsh, A.J., Walsh, W., Whiting, M., Wong, T., Woods, D., and Yock, P.C.M. (2005) Science programs for a 2-m class telescope at Dome C, Antarctica: PILOT, the Pathfinder for an International Large Optical Telescope. Publications of the Astronomical Society of Australia, 22 (3). pp. 199-235.
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The cold, dry, and stable air above the summits of the Antarctic plateau provides the best ground-based observing conditions from optical to sub-millimetre wavelengths to be found on the Earth. Pathfinder for an International Large Optical Telescope (PILOT) is a proposed 2 m telescope, to be built at Dome C in Antarctica, able to exploit these conditions for conducting astronomy at optical and infrared wavelengths. While PILOT is intended as a pathfinder towards the construction of future grand-design facilities, it will also be able to undertake a range of fundamental science investigations in its own right. This paper provides the performance specifications for PILOT, including its instrumentation. It then describes the kinds of projects that it could best conduct. These range from planetary science to the search for other solar systems, from star formation within the Galaxy to the star formation history of the Universe, and from gravitational lensing caused by exo-planets to that produced by the cosmic web of dark matter. PILOT would be particularly powerful for wide-field imaging at infrared wavelengths, achieving near diffraction-limited performance with simple tip–tilt wavefront correction. PILOT would also be capable of near diffraction-limited performance in the optical wavebands, as well be able to open new wavebands for regular ground-based observation, in the mid-IR from 17 to 40 μm and in the sub-millimetre at 200 μm.
|Item Type:||Article (Refereed Research - C1)|
|Keywords:||telescopes; site testing; atmospheric effects; techniques; high angular resolution; stars; formation; cosmology; observations|
|Date Deposited:||16 Mar 2010 04:43|
|FoR Codes:||02 PHYSICAL SCIENCES > 0201 Astronomical and Space Sciences > 020102 Astronomical and Space Instrumentation @ 100%|
|SEO Codes:||97 EXPANDING KNOWLEDGE > 970102 Expanding Knowledge in the Physical Sciences @ 100%|
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