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An Introduction to Optical Stellar Interferometry A ~ Book Description This book first published in 2006 was the first on optical stellar interferometry It covers the history theory and future uses of interferometeric techniques It discusses ideas and instruments used in interferometry for advanced students in physics optics and astronomy with an interest in astronomical interferometry
AN INTRODUCTION TO OPTICAL STELLAR INTERFEROMETRY ~ AN INTRODUCTION TO OPTICAL STELLAR INTERFEROMETRY During the last two decades optical stellar interferometry has become an important tool in astronomical investigations requiring spatial resolution well beyond that of traditional telescopes This is the first book to be written on the subject The authors
An Introduction to Optical Stellar Interferometry ~ Intensity interferometry was developed by Hanbury Brown and Twiss and originally used to measure the angular diameter of stars at both optical and radio frequencies Since then this method
AN INTRODUCTION TO OPTICAL STELLAR INTERFEROMETRY ~ 8 Amplitude interferometry techniques and instruments 158 81 Introduction 158 811 The Michelson stellar interferometer 159 812 The Narrabri Intensity Interferometer 160 813 Aperture masking 161 82 What do we demand of an interferometer 161 83 The components of modern amplitude interferometers 162 831 Subapertures and telescopes 163
AN INTRODUCTION TO OPTICAL STELLAR INTERFEROMETRY ~ University Printing House Cambridge cb2 8bs United Kingdom Published in the United States of America by Cambridge University Press New York Cambridge University Press is part of the University of Cambridge
An Introduction to Optical Stellar Interferometry ~ An Introduction to Optical Stellar Interferometry Volume 0 Part 0 Autor A Labeyrie S G Lipson P Nisenson Autor A Labeyrie S G Lipson P Nisenson
CHARA Basics of Interferometry ~ Basics of Interferometry The resolution of a telescope is set by the size of its primary mirror or lens The larger the diameter of the telescope the higher the spatial resolution improving its ability to see finer details However there are physical limitations to how large we can build a single telescope At a certain point
VLTI Tutorial ESO ~ 2 α dα F1Gν This is the measured quantity in a stellar interferometer – γ is the degree of spatial and temporal coherence also called the visibility – γ is a function of u 1 u 2 the difference vector –for a point source the spatial coherence is 1 and the contrast is determined by the temporal coherence
Astronomical optical interferometry Wikipedia ~ In optical astronomy interferometry is used to combine signals from two or more telescopes to obtain measurements with higher resolution than could be obtained with either telescopes individually This technique is the basis for astronomical interferometer arrays which can make measurements of very small astronomical objects if the telescopes are spread out over a wide area
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