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Extinction and Sky Brightness at Dome C

Published online by Cambridge University Press:  27 June 2012

M. Faurobert ,
C. Fang ,
T. Corbard ,
M. Faurobert ,
J. Arnaud  and
Y. Vernisse
M. Faurobert
Affiliation:
UMR 7293 Laboratoire Lagrange, Université de Nice Sophia Antipolis, CNRS, Observatoire de la Côte d’Azur, Campus Valrose, 06108 Nice, France
J. Arnaud
Affiliation:
UMR 7293 Laboratoire Lagrange, Université de Nice Sophia Antipolis, CNRS, Observatoire de la Côte d’Azur, Campus Valrose, 06108 Nice, France
Y. Vernisse
Affiliation:
UMR 7293 Laboratoire Lagrange, Université de Nice Sophia Antipolis, CNRS, Observatoire de la Côte d’Azur, Campus Valrose, 06108 Nice, France
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Abstract

We have installed a small telescope to monitor the sky brightness around the sun at the French-Italian station Concordia at Dome C in Antarctica. Previous campaigns have been performed with the same instrument at Haleakala in Hawai and Sunspot in New Mexico. We compare here the results of the first year of the campaign at Dome C (2008) to the purest sky observed at Haleakala. We show that Dome C is an outstanding site for coronal observations. Compared to Haleaka, it appears to be more transparent, and to contain less aerosols. Its water vapour content is also significantly smaller. These results still have to be confirmed by the analysis of the 2009 and 2010 data.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 55: 4th French-Chinese Meeting on Solar Physics - Understanding Solar Activity: Advances and Challenges , 2012 , pp. 365 - 367
Copyright
© EAS, EDP Sciences 2012

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References

Lin, H., & Penn, M., 2004, PASP, 116, 652 CrossRef
Penn, M., Lin, H., Schmidt, A.M., Gerke, J., & Hill, F., 2004, Solar Phys., 220, 107CrossRef