Design consideration of Chinese long-baseline stellar interferometer

1990 ◽  
Author(s):  
Zhao Peiqian ◽  
Bifang Zhou
Keyword(s):  
Design Consideration ◽  
Long Baseline ◽  
Stellar Interferometer

scholarly journals Long Baseline Interferometry and Binary Stars

1983 ◽  
Vol 62 ◽  
pp. 191-201
Author(s):  
John Davis
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Current Status ◽  
Fundamental Properties ◽  
Long Baseline ◽  
Stellar Interferometer ◽  
Spectroscopic Binary ◽  
Future Plans ◽  
Intensity Interferometer

AbstractThe observations of α Vir with the Narrabri Stellar Intensity Interferometer demonstrated the potential of long baseline interferometry for the determination of fundamental properties of double-lined spectroscopic binary systems. Since the completion of the programme with the Narrabri instrument the Chatterton Astronomy Department has been conducting a study aimed at developing a stellar interferometer with limiting magnitude V ≳ +8 and maximum baseline ≳ 1 km (resolution at 500 nm ≲ 7 × 10−5 seconds of arc). The way in which a long baseline interferometer may be used in the study of binary stars is outlined, the requirements for this work are discussed, and the current status and future plans of the Chatterton Astronomy Department’s programme to develop a new long baseline interferometer are summarised.

scholarly journals Present Status and Future Plans for the Two Color Astrometric Interferometer Project

1986 ◽  
Vol 109 ◽  
pp. 331-340 ◽  
Author(s):  
M. Shao ◽  
M. Colavita ◽  
D. Staelin ◽  
R. Simon ◽  
K. Johnston
Keyword(s):  
Atmospheric Turbulence ◽  
Present Status ◽  
Laser System ◽  
Slight Modification ◽  
The Past ◽  
Sources Of Error ◽  
Long Baseline ◽  
Stellar Interferometer ◽  
Color Fringe ◽  
Future Plans

A 3-meter two telescope stellar interferometer has been used to observe fringes for the past year in order to study the feasibility of using long baseline interferometers for astrometry. We have demonstrated that two color fringe measurements are capable of significantly reducing the astrometric error due to atmospheric turbulence. Currently, we are investigating the thermal and mechanical sources of error in the instrument. The results of our study will be incorporated into the design of the 20 meter astrometric interferometer which will be built in the next 1–2 years. The key to the 20-meter interferometer is the laser system which we expect to monitor all the mechanical and thermal imperfections relevant to astrometry at the 10−3 to 10−4 arc sec level. A slight modification of this system could be used in a space based interferometer for 1 to 10 microarcsecond astrometry of faint objects.

scholarly journals The Sydney University Stellar Interferometer (SUSI)

1994 ◽  
Vol 158 ◽  
pp. 135-142 ◽  
Author(s):  
J. Davis
Keyword(s):  
Path Length ◽  
Spectral Band ◽  
Optical Path Length ◽  
Optical Path ◽  
Current Status ◽  
Optical Interferometer ◽  
Beam Combining ◽  
Long Baseline ◽  
Stellar Interferometer

The Sydney University Stellar Interferometer has been designed and constructed as a two aperture, single ro, long baseline, optical interferometer with wavefront-tilt compensation and dynamic optical path length compensation. Initially it will operate in the blue part of the visual spectrum but provision has been made for the addition of an additional beam-combining system for a second spectral band. The rationale behind the choice of instrumental parameters, the potential developments which have been taken into account in its construction, and the current status of SUSI are outlined.

scholarly journals Measuring Stars with High Angular Resolution: Current Status and Future Prospects

1985 ◽  
Vol 111 ◽  
pp. 193-208
Author(s):  
John Davis
Keyword(s):  
Angular Resolution ◽  
Modern Technology ◽  
Surface Fluxes ◽  
Current Status ◽  
High Angular Resolution ◽  
Long Baseline ◽  
Stellar Interferometer ◽  
Current State ◽  
The University

The current state of knowledge of angular diameters of stars is reviewed and, based on this review and the requirements for the determination of surface fluxes, effective temperatures, radii and masses, targets of sensitivity, angular resolution and accuracy for future programs of stellar angular diameter measurements are established. Long baseline interferometry is the only technique with the potential to meet all the targets. The necessary improvements in sensitivity, angular resolution and accuracy are promised by the approach adopted in the modern Michelson stellar interferometer under development at the University of Sydney and the prototype instrument, which is currently nearing completion, is briefly described to illustrate how the atmospheric and mechanical problems which have inhibited the development of amplitude interferometry may be overcome using modern technology. This program together with the developments taking place at CERGA lead to the conclusion that the prospects for contributions by high angular resolution measurements to the determination of fundamental stellar quantities during the next decade are excellent.

scholarly journals The Potential of Long–Baseline Optical Interferometry of Binary Stars

1992 ◽  
Vol 135 ◽  
pp. 527-535 ◽  
Author(s):  
H.A. McAlister
Keyword(s):  
Binary Stars ◽  
Speckle Interferometry ◽  
Stellar Mass ◽  
Optical Interferometry ◽  
Spectroscopic Binaries ◽  
Direct Imaging ◽  
Multiple Star ◽  
Long Baseline ◽  
Stellar Interferometer

AbstractInterferometric arrays possessing sub-milliarcsecond resolution are either about to be fully scientifically productive, as in the case of the Sydney University Stellar Interferometer, or are under various stages of planning and development. The 1990’s will thus witness a hundred–fold gain in resolution over speckle interferometry at the largest telescopes and 5,000 times the resolution of classical direct imaging. Where speckle interferometry can now resolve binary stars with periods of 1 to 2 years, interferometric arrays with baselines of hundreds of meters will resolve binaries with periods of a few hours. Arrays will resolve the majority of the known spectroscopic binaries, providing a substantial increase in the quantity and quality of stellar mass determinations. Surveys for new binaries among the field stars and other restricted samples will be accomplished with unprecedented completeness. The remarkable enhancement in resolution we are about to witness from facilities like SUSI and our own proposed CHARA Array will quite literally revolutionize the field of double and multiple star research.

scholarly journals Astrometry with SIM PlanetQuest

2007 ◽  
Vol 3 (S248) ◽  
pp. 231-237
Author(s):  
M. Shao
Keyword(s):  
Local Group ◽  
Galactic Halo ◽  
Galactic Disk ◽  
Technology Program ◽  
Narrow Angle ◽  
Long Baseline ◽  
Stellar Interferometer ◽  
Nearby Stars ◽  
Global Accuracy ◽  
Very High

AbstractSIM PlanetQuest is a very high accuracy space astrometric instrument based on a long baseline stellar interferometer. For global astrometry SIM was designed to be accurate to ≈ 4μas(microarcsec) after a 5 year mission. For narrow angle astrometry (≈ 1000 s integration over a 1° radius field) SIM is designed for 1μas precision. The technology program was completed in 2005 and based on laboratory results, the current best estimate of SIM's performance would be 0.6 μas for narrow angle precision and 2.4 μas for global accuracy. This paper describes a variety of science programs that the SIM science team have proposed to conduct from a search for one Earth mass planets in the habitable zone of (≈130) nearby stars to the study of dark matter in the galactic disk, the galactic halo and the local group.

scholarly journals Forty Years of Progress in Long-Baseline Optical Interferometry: 2005 Robert Ellery Lecture

2006 ◽  
Vol 23 (2) ◽  
pp. 94-104 ◽  
Author(s):  
John Davis
Keyword(s):  
Optical Interferometry ◽  
Black Belt ◽  
Single Star ◽  
Leading Role ◽  
Long Baseline ◽  
Stellar Interferometer ◽  
Observational Technique ◽  
Made In ◽  
Scientific Achievements ◽  
Personal Viewpoint

AbstractThe development of long-baseline optical interferometry in Australia from the Narrabri Stellar Intensity Interferometer (NSII) to the Sydney University Stellar Interferometer (SUSI) and the resulting technical and scientific achievements are described. Three examples of results from the SUSI programme, for a single star, a double-lined spectroscopic binary, and a Cepheid variable, are presented to illustrate the advances made in the past four decades. The leading role that Australia has played in the development of the field worldwide is discussed from a personal viewpoint. Long-baseline optical interferometry has promised much, has been slow to deliver, and has been restricted to black-belt interferometrists, but it has now matured to the point where it is becoming an observational technique for astronomers in general.

scholarly journals Using SIM for Double Star Astronomy

2006 ◽  
Vol 2 (S240) ◽  
pp. 54-58
Author(s):  
Michael Shao
Keyword(s):  
Binary Stars ◽  
Double Star ◽  
Measurement Bias ◽  
Single Object ◽  
Composite Object ◽  
Double Stars ◽  
Long Baseline ◽  
Stellar Interferometer

AbstractThe SIM (Planet Quest) mission is a space-based long-baseline stellar interferometer designed for ultra-precise astrometry. This paper describes how SIM can be used for double star research. There are several regimes of operation. For binary stars separated by more than 1″.5, SIM treats these as distinct objects. Double stars less than ∼10 milliarcsec in separation are seen as a single object and SIM measures the photocenter of the composite object. Between 10 mas and 1″.15, SIM is able to see the double star as two distinct objects, but because photons from both stars are detected there is the possibility of increased noise and measurement bias. This paper describes how double stars are observed with SIM and what information can be derived.

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