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Abstract Review
| Corresponding Author |
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| Authors |
| Name | | Affiliation |
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Jose M. Delgado |
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Instituto de Astrofísica de Canarias |
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Jesús J. Fuensalida |
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Instituto de Astrofísica de Canarias |
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Begoña García-Lorenzo |
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Instituto de Astrofísica de Canarias |
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Elvio Hernández |
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Instituto de Astrofísica de Canarias |
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M. Ángeles C. Rodríguez-Hernández |
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Instituto de Astrofísica de Canarias |
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Marcos Reyes |
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Instituto de Astrofísica de Canarias |
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| Abstract |
| Session | | 1 (Instrumentation and observations to quantify the magnitude and distribution of atmospheric optical turbulence.) |
| Title | | 'A G-SCIDAR instrument for the inter-calibration of the atmospheric turbulence between the Roque de los Muchachos and Paranal observatories' |
| Abstract | | The most reliable and confirmed technique for measuring atmospheric turbulence profiles with height Cn2(h), is the well known G-Scidar method [Fuchs, Tallon & Vernin (1994)]. During the last 3 years, this technique has been implemented and developed with two automated instruments installed in the Roque de los Muchachos and in the Teide observatories. Periodic and continued measurements have been carried out for several years.
The installation and operation in Paranal Observatory (ESO, Chile) of a replica of these instruments has been included within the European Framework Program FP6 ELT Design Study, concretely into the WP12000 Site Characterization and WP 12200 Instrumentation, measurements and modelling work packages. This instrument has been adapted to the site infrastructure.
This G-Scidar instrumentation has been developed under the standard requirements of measurement techniques, acquisition procedures and methods of analysis established into the WP12000. It will permit the suitable automatic control and position of the devices, with near performances of real-time measurements. In addition, it should allow reliable inter-calibration of data obtained at the different sites.
The basic concept of the instruments and their features are described, detailing the adaptability peculiarities of each one to the different telescopes which support them. Furthermore, the specific characteristics of automatic reduction procedures are shown as well.
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