Optical interferometry in astronomy

@article{Monnier2003OpticalII,
  title={Optical interferometry in astronomy},
  author={John D. Monnier},
  journal={Reports on Progress in Physics},
  year={2003},
  volume={66},
  pages={789-857}
}
  • J. Monnier
  • Published 25 April 2003
  • Physics
  • Reports on Progress in Physics
Here I review the current state of the field of optical stellar interferometry, concentrating on ground-based work although a brief report of space interferometry missions is included. We pause both to reflect on decades of immense progress in the field as well as to prepare for a new generation of large interferometers just now being commissioned (most notably, the CHARA, Keck and VLT Interferometers). First, this review summarizes the basic principles behind stellar interferometry needed by… 

Imaging the heart of astrophysical objects with optical long-baseline interferometry

The number of publications of aperture-synthesis images based on optical long-baseline interferometry measurements has recently increased due to easier access to visible and infrared interferometers.

Imaging the heart of astrophysical objects with optical long-baseline interferometry

The number of publications of aperture-synthesis images based on optical long-baseline interferometry measurements has recently increased due to easier access to visible and infrared interferometers.

Beam characterization and guiding for optical/infrared interferometry

The GRAVITY instrument has been built with the goal of studying the Milky Way Galactic Center super-massive black hole. It is a powerful phase-referenced and closure phase interferometric imaging (4

Image reconstruction in optical interferometry

This article aims at reviewing image reconstruction algorithms in astronomical interferometry using a general framework to formally describe and compare the different methods and the challenging issues in image reconstruction from interferometric data are introduced.

Precision Stellar Astrophysics in the Kepler Era

The study of fundamental properties (such as temperatures, radii, masses, and ages) and interior processes (such as convection and angular momentum transport) of stars has implications on various

Optical Intensity Interferometry with Atmospheric Cerenkov Telescope Arrays

In the 1970s, the Narrabri intensity interferometer was used to measure 32 stellar diameters; some as small as 0.4 mas. The interferometer consisted of a pair of 6.5 m telescopes (30 m2) with

An x-ray interferometry concept for the ESA Voyage 2050 programme

The design of a single-spacecraft interferometer design is discussed and the process of fringe detection and image reconstruction from multiple baselines is discussed, showing simulated images of test cases from the Voyage 2050 White Paper.

Asteroseismology and interferometry

Current limitations to asteroseismic studies are discussed, including difficulties in mode identification and in the accurate determination of global parameters of pulsating stars, and how interferometric observations may contribute to overcome these limitations are discussed.

Interferometric studies of rapid rotators

Abstract Stellar rotation, like stellar mass and metallicity, is a fundamental property of stars. Rapid rotation distorts the stellar photosphere and affects a star's luminosity, abundances and

6 Optical and Infrared Interferometers

This chapter presents the basic theory and overall design considerations for an interferometer with an emphasis on the practical aspects of constructing a working instrument that overcomes obstacles imposed by the atmosphere, submicron path length matching requirements, limitations on number of telescopes and their layout, light losses throughmultiple reflections and transmissions necessary to superimpose telescope beams in the beam-combining laboratory, and other realities of the art of interferometry.
...

References

SHOWING 1-10 OF 416 REFERENCES

Optical Interferometry

■ Abstract The field of optical and infrared (IR) interferometry has seen rapid technical and scientific progress over the past few years. A number of instruments capable of precise visibility

Spectro-polarimetric interferometry (SPIN) of magnetic stars

Stellar magnetic fields are usually studied by spectropolarimetric analysis of the Zeeman effect across spectral lines. Such studies are often limited by the net detectable polarization after

Potential of long-baseline infrared interferometry for narrow-angle astrometry

Narrow-angle astrometry has many astrophysical applications, from the measurement of parallaxes to the search for planets around nearby stars. Ground-based long-focus telescopes with photoelectric

AMBER: the near-infrared focal instrument for the Very Large Telescope Interferometer

AMBER is a focal instrument for the Very Large Telescope Interferometer working in the near infrared from 1.1 to 2.4 micrometers . It has been designed having in mind the General User of

Michelson Interferometry with the Keck I Telescope

We report the first use of Michelson interferometry on the Keck I telescope for diffraction‐limited imaging in the near‐infrared JHKL bands. By using an aperture mask located close to the f/25

Scientific Drivers for a Future Polarimetric Mode for the VLTI: VISPER

The scientific drivers and the concept of a Polarimetric instrument for the VLTI, VISPER (Vlti Imaging Spectro-PolarimetER) will be presented. Many scientific programs in stellar physics as well as

The Mark III stellar interferometer

Abstract : The Mark III interferometer is an operational long baseline stellar interferometer on Mt. Wilson with four-possible baseline configurations from 9m NE-SW to 20m N-S. The interferometer was

Detection of Earth-like Planets Using Apodized Telescopes

The mission of NASA's Terrestrial Planet Finder (TPF) is to find Earth-like planets orbiting other stars and characterize the atmospheres of these planets using spectroscopy. Because of the enormous

Laboratory detection of X-ray fringes with a grazing-incidence interferometer

The prototype interferometer, having just under one millimetre of baseline, creates fringes at 1.25 keV with an angular resolution of 100 milliarcseconds, will be possible to resolve X-ray sources at 10-7 arcseconds with a larger version in orbit, three orders of magnitude better than the finest-resolution images ever achieved on the sky.

On the Interferometric Sizes of Young Stellar Objects

Long-baseline optical interferometers can now detect and resolve hot dust emission thought to arise at the inner edge of circumstellar disks around young stellar objects (YSOs). We argue that the
...