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SCIDAR: an optical turbulence profiler for Dome A

Published online by Cambridge University Press:  30 January 2013

Li-Yong Liu ,
Yong-Qiang Yao ,
Jean Vernin ,
Merieme Chadid ,
Hong-Shuai Wang  and
Yi-Ping Wang
Li-Yong Liu
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, China email: [email protected] Université de Nice-Sophia Antipolis, Observatoire de la Côte d'Azur, CNRS-UMR7293, Lab. Lagrange, Parc Valrose, 06108, Nice Cedex 2, France email: [email protected]
Yong-Qiang Yao
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, China email: [email protected]
Jean Vernin
Affiliation:
Université de Nice-Sophia Antipolis, Observatoire de la Côte d'Azur, CNRS-UMR7293, Lab. Lagrange, Parc Valrose, 06108, Nice Cedex 2, France email: [email protected]
Merieme Chadid
Affiliation:
Université de Nice-Sophia Antipolis, Observatoire de la Côte d'Azur, CNRS-UMR7293, Lab. Lagrange, Parc Valrose, 06108, Nice Cedex 2, France email: [email protected]
Hong-Shuai Wang
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, China email: [email protected]
Yi-Ping Wang
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, China email: [email protected]
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Abstract

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This paper introduces a plan to detect turbulence profiles at Dome A with a Single Star Scidar (SSS), to enhance our understanding of the characteristics of the site. The development of a portable monitor for profiling vertical atmospheric optical turbulence and wind speed is presented. By analyzing the spatial auto and cross-correlation functions of very short exposure images of single star scintillation patterns, the SSS can provide the vertical profiles of turbulence intensity C2n(h) and wind speed V(h). A SSS prototype is already operational at Ali in Tibet which will be improved in order to become fully robotic and adapted to extreme weather conditions that prevail at Dome A in Antarctica.

Keywords

ScidarOptical turbulenceDome A
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S288: Astrophysics from Antarctica , August 2012 , pp. 316 - 317
Copyright
Copyright © International Astronomical Union 2013

References

Yang, H., Allen, G., Ashley, et al., 2009, PASP, 121, 174–184.CrossRefGoogle Scholar
Lawrence, J. S., Allen, G. R., Ashley, M. C. B.et al., 2008, Proc. SPIE, 7012, 701227-701227–12.Google Scholar
Bonner, C. S., Ashley, M. C. B., Cui, X.et al., 2010, PASP, 122, 1122–1131.Google Scholar
Pei, C., Chen, H., Yuan, X.et al., 2010, Proc. SPIE, 7733, pp. 77334W-77334W–8.Google Scholar
Vernin, J., Chadid, M., Aristidi, E.et al., 2009, A&A, 1271, 1276Google Scholar
Giordano, C., Vernin, J., Chadid, M.et al., 2012, PASP, 494, 506Google Scholar
Liu, L., Yao, Y., Vernin, J.et al., 2012, Proc. SPIE, 8444, pp. 844464 (1–7)Google Scholar