NASA ADS Astronomy Abstract Service


Title:
Aperture synthesis using multiple facilities: Keck aperture masking and the IOTA interferometer
Authors:
Monnier, John D.; Millan-Gabet, Rafael; Tuthill, Peter G.; Traub, Wesley A.; Carleton, Nathaniel P.; Coude du Foresto, Vincent; Danchi, William C.; Lacasse, Marc G.; Morel, Sebastien; Perrin, Guy S.; Porro, Irene L.
Affiliation:
AA(Harvard-Smithsonian Ctr. for Astrophysics (USA) and Univ. of Michigan (USA)), AB(Harvard-Smithsonian Ctr. for Astrophysics (USA) and California Institute of Technology (USA)), AC(Univ. of Sydney (Australia)), AD(Harvard-Smithsonian Ctr. for Astrophysics (USA)), AE(Harvard-Smithsonian Ctr. for Astrophysics (USA)), AF(Observatoire de Paris-Meudon (France)), AG(NASA Goddard Space Flight Ctr. (USA)), AH(Harvard-Smithsonian Ctr. for Astrophysics (USA)), AI(European Southern Observatory (Germany)), AJ(Observatoire de Paris-Meudon (France)), AK(Massachusetts Institute of Technology (USA))
Journal:
Interferometry for Optical Astronomy II. Edited by Wesley A. Traub. Proceedings of the SPIE, Volume 4838, pp. 379-386 (2003). (SPIE Homepage)
Publication Date:
02/2003
Origin:
SPIE
Abstract Copyright:
(c) 2003: SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.
Bibliographic Code:
2003SPIE.4838..379M

Abstract

As the number of optical interferometers increase, multi-facility observations become both feasible and scientifically interesting. For imaging of complex sources, the capability of increasing (u,v) coverage by using multiple arrays may be necessary for accurately interpreting the fringe visibility and closure phase data. Toward this end, coordinated observations with the IOTA interferometer and Keck aperture masking have been carried out to test techniques for synthesizing images using data from heterogeneous arrays with sparse (u,v) coverage. In particular, we will focus on how the image prior in the Maximum Entropy Method can be used to efficiently incorporate very high spatial frequency information with "low-resolution" data for imaging the generic prototype "Star + Dust Shell" image morphology. Preliminary results using real data for a few dusty evolved stars are presented.