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Proceedings Article

Phase closure image reconstruction for future VLTI instrumentation

[+] Author Affiliations
Mercedes E. Filho

Ctr. de Astrofisica, Univ. do Porto (Portugal)

Stephanie Renard, Eric Thiebaut

Observatoire de Lyon (France)

Paulo Garcia

Ctr. de Astrofisica, Univ. do Porto (Portugal) and Univ. do Porto (Portugal)

Gilles Duvert

Lab. d'Astrophysique de Grenoble, Observatoire de Grenoble (France)

Gaspard Duchene

Univ. of California, Berkeley (United States)

John Young

Cavendish Lab. (United Kingdom)

Olivier Absil, Jean-Phillipe Berger

Univ. Joseph Fourier, CNRS, Lab. d'Astrophysique de Grenoble (France)

Thomas Beckert, Sebastian Hoenig, Dieter Schertl, Gerd Weigelt

Max-Planck Institute for Radioastronomy (Germany)

Leonardo Testi, Eric Tatuli

INAF, Osservatorio di Astrofisica di Arcetri (Italy)

Virginie Borkowski, Micha"l de Becker, Jean Surdej

Institute of Astrophysics and Geophysics (Belgium)

Bernard Aringer, Joseph Hron, Thomas Lebzelter

Institute of Astrophysics, Univ. of Wien (Austria)

Andrea Chiavassa, Romano Corradi

Groupe de Recherche en Astronomie et Astrophysique du Languedoc (France)

Tim Harries

Univ. of Exeter (United Kingdom)

Proc. SPIE 7013, Optical and Infrared Interferometry, 70133Z (July 14, 2008); doi:10.1117/12.787877
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From Conference Volume 7013

  • Optical and Infrared Interferometry
  • Marseille, France | June 23, 2008


Classically, optical and near-infrared interferometry have relied on closure phase techniques to produce images. Such techniques allow us to achieve modest dynamic ranges. In order to test the feasibility of next generation optical interferometers in the context of the VLTI-spectro-imager (VSI), we have embarked on a study of image reconstruction and analysis. Our main aim was to test the influence of the number of telescopes, observing nights and distribution of the visibility points on the quality of the reconstructed images. Our results show that observations using six Auxiliary Telescopes (ATs) during one complete night yield the best results in general and is critical in most science cases; the number of telescopes is the determining factor in the image reconstruction outcome. In terms of imaging capabilities, an optical, six telescope VLTI-type configuration and ~200 meter baseline will achieve 4 mas spatial resolution, which is comparable to ALMA and almost 50 times better than JWST will achieve at 2.2 microns. Our results show that such an instrument will be capable of imaging, with unprecedented detail, a plethora of sources, ranging from complex stellar surfaces to microlensing events.

© (2008) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.

Mercedes E. Filho ; Stephanie Renard ; Paulo Garcia ; Gilles Duvert ; Gaspard Duchene, et al.
"Phase closure image reconstruction for future VLTI instrumentation", Proc. SPIE 7013, Optical and Infrared Interferometry, 70133Z (July 14, 2008); doi:10.1117/12.787877; http://dx.doi.org/10.1117/12.787877

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