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Issue A&A
Volume 451, Number 3, June I 2006
Page(s) 1133 - 1137
Section Instruments, observational techniques, and data processing
DOI http://dx.doi.org/10.1051/0004-6361:20054296



A&A 451, 1133-1137 (2006)
DOI: 10.1051/0004-6361:20054296

First sky validation of an optical polarimetric interferometer

K. Rousselet-Perraut1, J. B. Le Bouquin1, D. Mourard2, F. Vakili3, O. Chesneau2, D. Bonneau2, J. L. Chevassut2, A. Crocherie2, A. Glentzlin2, S. Jankov3, S. Ménardi4, R. Petrov3 and C. Stehlé5

1  Laboratoire d'Astrophysique de l'Observatoire de Grenoble, BP 53, 38041 Grenoble Cedex 9, France
    e-mail: Karine.Perraut@obs.ujf-grenoble.fr
2  Observatoire de la Côte d'Azur, Département Gemini, Avenue Copernic, 06130 Grasse, France
3  Laboratoire Universitaire d'Astrophysique de Nice, UNSA, Faculté des Sciences, 06108 Nice Cedex 02, France
4  ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
5  Laboratoire de l'Univers et de ses THéories, UMR 8102, Observatoire de Paris, 5 place Jules Janssen, 92195 Meudon, France

(Received 3 October 2005 / Accepted 10 January 2006 )

Abstract
Aims.We present the first lab and sky validation of spectro-polarimetric equipment put at the combined focus of an optical long-baseline interferometer. We tested the polarimetric mode designed for the visible GI2T Interferometer to offer spectropolarimetric diagnosis at the milliarcsecond scale.
Methods.We first checked the whole instrumental polarization in the lab with a fringe simulator, and then we observed $\alpha$ Cep and $\alpha$ Lyr as stellar calibrators of different declinations to tabulate the polarization effects throughout the GI2T declination range.
Results.The difference between both linear polarizations is within the error bars and the visibilities recorded in natural light (i.e. without the polarimeter) for calibration purposes are the same order of magnitude as the polarized ones. We followed the $\alpha$ Cep visibility for 2 h after the transit and $\alpha$ Lyr for 1.5 h and detected no decrease with hour angle due to the fringe pattern smearing by instrumental polarization.
Conclusions.Differential celestial rotation due to the dissymetric Coudé trains of the GI2T is well-compensated by the field rotators, so the instrumental polarization is controlled over a relatively wide hour angle range ($\pm$2 h around the transit at least). Such a polarimetric mode opens new opportunities especially for studies of circumstellar environments and significantly enhances both the potential of an optical array and its ability for accurate calibration.


Key words: technique: interferometric -- instrumentation: interferometers -- techniques: polarimetric

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