VEGA: Visible spEctroGraph and polArimeter for the CHARA array: principle and performance

@article{Mourard2009VEGAVS,
  title={VEGA: Visible spEctroGraph and polArimeter for the CHARA array: principle and performance},
  author={Denis Mourard and J. M. Clausse and Aur{\'e}lie Marcotto and K. Perraut and I. Tallon-Bosc and Philippe B{\'e}rio and Alain Blazit and Daniel Bonneau and Sandra Bosio and Yves Bresson and Olivier Chesneau and Omar Delaa and François H{\'e}nault and Y. Hughes and St'ephane Lagarde and Guy Merlin and Alain Roussel and Alain Spang and P. Stee and Michel Tallon and Pierre Antonelli and Renaud Foy and Pierre Kervella and Romain G. Petrov and {\'E}ric Thi{\'e}baut and Farrokh Vakili and Harold A. Mcalister and Theo A. ten Brummelaar and Judit Sturmann and Laszlo Sturmann and Nils H. Turner and Christopher D. Farrington and P. J. Goldfinger},
  journal={Astronomy and Astrophysics},
  year={2009},
  volume={508},
  pages={1073-1083}
}
Context. Among optical stellar interferometers, the CHARA Array located at Mt Wilson in California offers the potential of very long baselines (up to 330 m) and the prospect of coupling multiple beam combiners. This paper presents the principle and the measured performance of VEGA, Visible spEctroGraph and polArimeter installed in September 2007 at the coherent focus of the array. Aims. With 0.3 ms of arc of spatial resolution and up to $30 000$ of spectral resolution, VEGA intends to measure… 
Performances and first science results with the VEGA/CHARA visible instrument
This paper presents the current status of the VEGA (Visible spEctroGraph and polArimeter) instrument installed at the coherent focus of the CHARA Array, Mount Wilson CA. Installed in september 2007,
SPICA, Stellar Parameters and Images with a Cophased Array: a 6T visible combiner for the CHARA array.
TLDR
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VEGA/CHARA interferometric observations of Cepheids - I. A resolved structure around the prototype classical Cepheid δ Cep in the visible spectral range
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The enigmatic binary, e Aur, is yielding its parameters as a result of new methods applied to the recent eclipse, including optical spectro-interferometry with the VEGA beam combiner at the CHARA
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