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Suzanne L. Kenyon , Michael C. B. Ashley, Jon Everett, Jon S. Lawrence and
 

Summary: 
Suzanne L. Kenyon
, Michael C. B. Ashley, Jon Everett, Jon S. Lawrence and
John W. V. Storey
School of Physics, University of New South Wales, Sydney 2052, Australia
ABSTRACT
The brightness of the night sky at an astronomical site is one of the principal factors that determine the quality
of available optical observing time. At any site the optical night sky is always brightened with airglow, zodiacal
light, integrated starlight, diffuse Galactic light and extra-galactic light. Further brightening can be caused
by scattered sunlight, aurorae, moonlight and artificial sources. Dome C exhibits many characteristics that
are extremely favourable to optical and IR astronomy; however, at this stage few measurements have been
made of the brightness of the optical night sky. Nigel is a fibre-fed UV/visible grating spectrograph with a
thermoelectrically cooled 256 1024 pixel CCD camera, and is designed to measure the twilight and night sky
brightness at Dome C from 250 nm to 900 nm. We present details of the design, calibration and installation of
Nigel in the AASTINO laboratory at Dome C, together with a summary of the known properties of the Dome C
sky.
Keywords: Site testing, Antarctica, sky brightness
1. INTRODUCTION
Dome C, Antarctica (75
6 south, 123

  

Source: Ashley, Michael C. B. - School of Physics, University of New South Wales

 

Collections: Physics