EAS Publications Series
Volume 22, 2006Astronomy with High Contrast Imaging III: Instrumental Techniques, Modeling and Data Processing
|Page(s)||379 - 388|
|Published online||13 October 2006|
M. Carbillet, A. Ferrari and C. Aime (eds)
EAS Publications Series, 22 (2006) 379-388
Differential Interferometry with the AMBER/VLTI instrument: Description, performances and illustration
d'Astrophysique de Nice, UMR 6525, Université de Nice-Sophia
Antipolis, Parc Valrose, 06108 Nice Cedex 02, France
2 Laboratoire d'Astrophysique de Grenoble, UMR 5571 Université Joseph Fourier/CNRS, BP. 53, 38041 Grenoble Cedex 9, France
3 European Southern Observatory, Casilla 19001, Santiago 19, Chile
4 Laboratoire Gemini, UMR 6203 Observatoire de la Côte d'Azur/CNRS, Avenue Copernic, 06130 Grasse, France
5 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA
AMBER is the near I.R. focal instrument of the VLTI. It recombines 3 beams simultaneously and has spectral resolution capability allowing simultaneous spectrum, visibilities, differential visibilities, closure phase and differential phases measurements on the observed sources. We present here the general formalism used on AMBER in order to compute differential phases and differential visibilities, in complement to the article of Tatulli et al. (2006). We show that these differential observables have precisions close to the fundamental noises and we present an illustration of model-fitting using them on the binary star γ2 Velorum where we made a precise measurment of the astrometry of the 2 components (3.65±0.1 mas).
© EAS, EDP Sciences, 2006
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