Science with the VLT Interferometer Proceedings of the ESO Workshop Held at Garching, Germany, 18–21 June 1996

The next major step for the highest possible angular resolution in astronomy will be taken with the construction of large interferometric arrays. ESO's VLT Interferometer will employ an array of four 8 m and three 1.8 m diameter telescopes coherently combined to reach an unprecedented resolutio...

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Corporate Author: SpringerLink (Online service)
Other Authors: Paresce, Francesco (Editor)
Format: eBook
Language:English
Published: Berlin, Heidelberg Springer Berlin Heidelberg 1997, 1997
Edition:1st ed. 1997
Series:ESO Astrophysics Symposia, European Southern Observatory
Subjects:
Online Access:
Collection: Springer Book Archives -2004 - Collection details see MPG.ReNa
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100 1 |a Paresce, Francesco  |e [editor] 
245 0 0 |a Science with the VLT Interferometer  |h Elektronische Ressource  |b Proceedings of the ESO Workshop Held at Garching, Germany, 18–21 June 1996  |c edited by Francesco Paresce 
250 |a 1st ed. 1997 
260 |a Berlin, Heidelberg  |b Springer Berlin Heidelberg  |c 1997, 1997 
300 |a XXII, 409 p. 264 illus  |b online resource 
505 0 |a Using a Space-Based Astrometric Reference Frame -- 4. The Potential of VLTI and the Connection with Related Techniques -- Tailoring an Interferometer to Its Science and Vice Versa -- Some Aspects of the VLTI’s Potential for Binary Star Research -- Combining Mid-Infrared Lunar Occultations and VLTI Measurements -- 5. Hot Stars -- Interferometric Observations of Be Stars -- Spectroscopic and Photometric Support for Interferometric Observations of Be Stars -- Imaging of Wolf-Rayet Stars with the VLTI -- 6. Circumstellar Environments and Mass Loss -- AGB and Post-AGB Stars: An Overview -- Winds of Red Giants and Supergiants: Basic Physical Processes, Structure and Appearance -- Study of Late-Type Stars with the Infrared Spatial Interferometer of the University of California at Berkeley -- Interferometric Studies of Late Phases of Stellar Evolution --  
505 0 |a Observations and Modelling -- Interferometric Observations of Mira Stars -- Results of Studies on the Environmental Factors Affecting the VLTI Performance -- Internal Optical Path Calibration System for VLTI -- Pupil Mask Interferometry of M8E-IR -- Observations of the Close Binary System ? Lyrae with the GI2T Interferometer -- Stellar Winds of T Tauri Stars -- Operating the VLTI in the Thermal Infrared --  
505 0 |a Pushing the Limit of Single-Dish Ground-Based Observations -- Differential Interferometry and the Non-axisymmetric Envelope of ? Cas -- HST Imaging of GM Aurigae: A Circumstellar Disk Seen in Scattered Light -- Software Concept for Four-Dimensional Bispectral Analysis of Stellar Interferograms -- Real-Time Image Compression Method for Astronomical Interferograms -- Synthetic Images from Dynamic Model Atmospheres of C-Rich Long-Period Variables -- Brightness Profiles and Spatial Spectra of Dynamical Models for C-Rich Circumstellar Dust Shells Around Long-Period Variables -- Author Index 
505 0 |a Conference Summary -- Poster Papers - 
505 0 |a Astrometric Variability as the Result of Supernova Explosions in Nuclear Starbursts --  
653 |a Geophysics 
653 |a Astronomy, Observations and Techniques 
653 |a Observations, Astronomical 
653 |a Astronomy—Observations 
653 |a Astrophysics and Astroparticles 
653 |a Astrophysics 
653 |a Geophysics/Geodesy 
710 2 |a SpringerLink (Online service) 
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989 |b SBA  |a Springer Book Archives -2004 
490 0 |a ESO Astrophysics Symposia, European Southern Observatory 
856 |u https://doi.org/10.1007/978-3-540-69398-7?nosfx=y  |x Verlag  |3 Volltext 
082 0 |a 520 
520 |a The next major step for the highest possible angular resolution in astronomy will be taken with the construction of large interferometric arrays. ESO's VLT Interferometer will employ an array of four 8 m and three 1.8 m diameter telescopes coherently combined to reach an unprecedented resolution of a millisecond of arc in the visible/IR for objects as faint as 24th visual magnitude. Thus it will open up vast new frontiers in modern astronomy. This book is in preparation for the first observations expected at the beginning of the next century. All areas to be seriously mined with this new facility are presented in a clear and brief exposition with an emphasis on what the VLTI can actually accomplish. Since optical interferometry is still a rather unfamiliar technique for many astronomers, the book contains four short but thorough tutorials that can be used as basic references to the art of interferometry. It will, therefore, also be useful for graduate students