Differential interferometry with the AMBER/VLTI instrument: Description, performances and illustration

被引：17
|
作者：
Millour, F. [1 ,2 ]
Vannier, M. [3 ]
Petrov, R. G. [1 ]
Chesneau, O. [4 ]
Dessart, L. [5 ]
Stee, P. [4 ]
机构：
[1] Univ Nice, UMR 6525, Lab Univ Astrophys, Parc Valrose, F-06108 Nice 02, France
[2] Univ Grenoble 1, CNRS, UMR 5571 Lab Astrophys Grenoble, F-38041 Grenoble 9, France
[3] European So Observ, Santiago 19001, Chile
[4] Observ Cote Azur, CNRS, UMR 6203 Lab Gemini, F-06130 Grasse, France
[5] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA
来源：
ASTRONOMY WITH HIGH CONTRAST IMAGING III: INSTRUMENTAL TECHNIQUES, MODELING AND DATA PROCESSING | 2006年 / 22卷
关键词：
D O I：
10.1051/eas:2006143
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
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 gamma(2) Velorum where we made a precise measurment of the astrometry of the 2 components (3.65 +/- 0.1 mas).
引用
收藏
页码：379 / +
页数：2
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