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KEOPS: Scientific Challenges and Technical Steps

Published online by Cambridge University Press:  23 May 2007

N. Epchtein ,
M. Candidi ,
B. Valat ,
P.-M. Gori ,
F.-X. Schmider ,
B. Lopez  and
F. Vakili
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 NextGeneration Optical Interferometer. KEOPS (Kilo parsec ExplorerOptical Planet Search) is proposed in a context which alsoconsidere the post VLTI perspectives. Thisinterferometer will be composed of 36 telescopes with a maximalbaseline of 1 km. This instrument will open new horizons: stellarimaging, circumstellar environment studies, extra solar planet detection, Earthlike planet search. The possibility of observations in doublefield mode takes advantage of the large isopistonic angle to give acces tofaint object (see Elhalkouj 2006). It allows active galactic nuclei and cosmological observations.The achievement of that project implies different steps. The firstone could be MYKERINOS, proposed by LUAN. This prototypeinterferometer, composed to 3 telescopes of 40 cm, demonstrate technological feasibility, complete the specific sitecharacterisation and contribute to validate the scientific program objectives.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 25: 1st ARENA Conference on "Large Astronomical Infrastructures at CONCORDIA, prospects and constraints for Antarctic Optical/IR Astronomy" , 2007 , pp. 295 - 299
Copyright
© EAS, EDP Sciences, 2007

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