Synthetic images from simulations of long-baseline 2D optical interferometers

1994 ◽  
Author(s):  
Robert W. Conley ◽  
Don M. Payne ◽  
Sergio R. Restaino ◽  
Gary C. Loos
Keyword(s):  
Long Baseline ◽  
Optical Interferometers ◽  
Synthetic Images

scholarly journals Long Baseline Optical Interferometry

1989 ◽  
Vol 8 ◽  
pp. 559-560
Author(s):  
S.T. Ridgway
Keyword(s):  
Emission Line ◽  
Spatial Resolution ◽  
Optical Interferometry ◽  
Hydrogen Emission ◽  
Long Baseline ◽  
Optical Interferometers ◽  
Imaging Science ◽  
Be Star ◽  
Hydrogen Emission Line ◽  
To Come

During the last three years significant results have been obtained from several operational, long baseline optical interferometers. Precision stellar angular diameters (accuracy of order 2% and better) have been reported in the infrared (DiBenedetto and Rabbia, 1987) and in the visible (Davis and Tango, 1986). Astrometric precision of order 20 milliarcsec has been demonstrated over large angles (Shao et al, in press). Spectro-spatial resolution of the disk of a Be star in the hydrogen emission line (Thom et al., 1986) suggests spectacular imaging science to come with many-telescope coherent and phased optical arrays.

scholarly journals Active Control and Adaptive Optics for Optical Interferometers

1989 ◽  
Vol 8 ◽  
pp. 565-566
Author(s):  
Fritz Merkle
Keyword(s):  
Control Systems ◽  
Real Time ◽  
Active Control ◽  
Adaptive Optics ◽  
Field Of View ◽  
Telescope Array ◽  
Large Unit ◽  
Long Baseline ◽  
Optical Interferometers ◽  
The Individual

Long baseline interferometry requires the full phasing of a telescope array. Especially for future arrays with large unit telescopes active control systems are mandatory. Adaptive optics can be applied for real-time phase compensation of the individual pupils due to atmospheric distortions. Additional to phasing of the individual pupils of independently mounted telescopes, the whole array has to be phased, including pupil position corrections due to pupil foreshortening and shift effects in order to reach a reasonable phased field-of-view.

scholarly journals O and B-star surface mapping

1996 ◽  
Vol 176 ◽  
pp. 121-128 ◽  
Author(s):  
D. R. Gies
Keyword(s):  
Binary Stars ◽  
Circumstellar Disks ◽  
Be Stars ◽  
Surface Mapping ◽  
Spectroscopic Observations ◽  
Long Baseline ◽  
Optical Interferometers ◽  
Distributed Array ◽  
New Generation ◽  
Star Surface

The massive O and B-type stars will be among the first targets of the new generation of long baseline optical interferometers (such as the CHARA Array, a 400-m diameter distributed array of five 1-m telescopes). Many of these objects are binary stars for which joint astrometric and spectroscopic observations will provide masses and distances (e.g., 15 Mon; Gies et al. 1993), but there is also great interest in resolving disks of single stars. Early interferometric observations have already resolved the flattened circumstellar disks around some Be stars (Quirrenbach et al. 1994).

Optimization of long-baseline optical interferometers for gravitational-wave detection

1988 ◽  
Vol 38 (2) ◽  
pp. 433-447 ◽  
Author(s):  
Jean-Yves Vinet ◽  
Brian Meers ◽  
Catherine Nary Man ◽  
Alain Brillet
Keyword(s):  
Gravitational Wave ◽  
Gravitational Wave Detection ◽  
Wave Detection ◽  
Long Baseline ◽  
Optical Interferometers

Optical interferometers in astrometry

1978 ◽  
Vol 48 ◽  
pp. 313-324 ◽  
Author(s):  
M. Shao
Keyword(s):  
Power Spectrum ◽  
Image Plane ◽  
The Other ◽  
Measurement Time ◽  
Square Root ◽  
Single Measure ◽  
Photon Noise ◽  
Long Baseline ◽  
Optical Interferometers ◽  
Pupil Plane

AbstractLong baseline stellar interferometers, for astrometry are potentially capable of extremely high accuracies, 10-4to 10-5arc sec for a single measure ment. There are three categories of errors that apply to an astrometric interferometer, instrumental, atmospheric and photon noise. Of these, only photon noise has a flat power spectrum. All of the other sources of error are systematic in the sense that the accuracy does not increase as the square root of the measurement time. The elimination of atmospheric error is the major difference between interferometers and other photoelectric astrometric instruments. Two types of interferometers, image plane and pupil plane, are described. The advantages and limitations of these two approaches are discussed.

scholarly journals Closure phase studies toward direct detection of light from hot Jupiters

2007 ◽  
Vol 3 (S249) ◽  
pp. 71-77
Author(s):  
Ming Zhao ◽  
John D. Monnier ◽  
Theo ten Brummelaar ◽  
Ettore Pedretti ◽  
Nathalie Thureau
Keyword(s):  
High Precision ◽  
Test Object ◽  
Direct Detection ◽  
Phase Measurements ◽  
Hot Jupiters ◽  
Long Baseline ◽  
Optical Interferometers ◽  
Phase Study ◽  
Chara Array ◽  
Very High

AbstractPrecision closure phase measurements obtained with ground-based long baseline optical interferometers is a promising way to directly detect light from nearby hot Jupiters. Here we present our closure phase simulations for the CHARA array for several bright hot Jupiters, υ And b, 51 Peg b, and τ Boo b. The maximum possible closure phase signals from these hot Jupiters are very small, for example, only ∼0.17 degrees for υ And b, requiring very high precision and stable closure phase measurements. We present preliminary results of a closure phase study on test object β Tau and hot Jupiter system υ And, both obtained with the MIRC instrument at the CHARA array. We demonstrate that directly detecting the light from hot Jupiters is feasible using high precision closure phase measurements obtained by CHARA-MIRC along with its sub-milli-arcsecond resolution, although challenges remain.

scholarly journals An Introduction to the Nomenclature Problem

2005 ◽  
Vol 13 ◽  
pp. 977-980
Author(s):  
Brian D. Mason ◽  
William I. Hartkopf
Keyword(s):  
Brown Dwarfs ◽  
Special Session ◽  
The Past ◽  
Reduction Techniques ◽  
Long Baseline ◽  
Optical Interferometers ◽  
Multiple Stars ◽  
Double And Multiple Stars ◽  
The Many

AbstractThe new observing and reduction techniques available to astronomers have led to remarkable changes in the field of double and multiple stars. New classes of companions, such as brown dwarfs and exoplanets, have been discovered. Binaries which previously constituted distinct classes are now observable by multiple techniques. With many long-baseline optical interferometers operational or planned, with improvements in other techniques, and with astrometric space-based missions in various states of planning and funding, the situation is likely to become more complicated. The result is greater understanding for the scientist, but greater challenges for the cataloger!The “problem” is that purveyors of different techniques use different nomenclature, both in terms of root designation and component identifier. It is this latter inconsistency which causes the most confusion and is the topic of this Special Session.This talk will illustrate some of the many designation ambiguities and summarize efforts made during the past few years to address this problem.

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