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KEOPS: Scientific Challenges and Technical Steps

Published online by Cambridge University Press:  23 May 2007

B. Valat
Affiliation:
Laboratoire Universitaire d'Astrophysique de Nice UMR 6525, Université de Nice Sophia Antipolis, France AlcatelAleniaSpace, France
P.-M. Gori
Affiliation:
Laboratoire Universitaire d'Astrophysique de Nice UMR 6525, Université de Nice Sophia Antipolis, France
F.-X. Schmider
Affiliation:
Laboratoire Universitaire d'Astrophysique de Nice UMR 6525, Université de Nice Sophia Antipolis, France
B. Lopez
Affiliation:
Observatoire de la Côte d'Azur, Département GEMINI, Nice, France
F. Vakili
Affiliation:
Laboratoire Universitaire d'Astrophysique de Nice UMR 6525, Université de Nice Sophia Antipolis, France
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Abstract

The recent site testing pointed out the potential of Dome C for Next Generation Optical Interferometer. KEOPS (Kilo parsec Explorer Optical Planet Search) is proposed in a context which also considere the post VLTI perspectives. This interferometer will be composed of 36 telescopes with a maximal baseline of 1 km. This instrument will open new horizons: stellar imaging, circumstellar environment studies, extra solar planet detection, Earth like planet search. The possibility of observations in double field mode takes advantage of the large isopistonic angle to give acces to faint object (see Elhalkouj 2006). It allows active galactic nuclei and cosmological observations. The achievement of that project implies different steps. The first one could be MYKERINOS, proposed by LUAN. This prototype interferometer, composed to 3 telescopes of 40 cm, demonstrate technological feasibility, complete the specific site characterisation and contribute to validate the scientific program objectives.

Type
Research Article
Copyright
© EAS, EDP Sciences, 2007

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