Titlebook: Astronomy at High Angular Resolution; A Compendium of Tech Henri M. J. Boffin,Gaitee Hussain,Linda Schmidtobr Book 2016 Springer Internatio

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Book 2016ues, which are critical to advances in many areas of astronomy. As reflected in the book, these techniques can be divided into direct methods, interferometry, and reconstruction methods, and can be applied to a huge variety of astrophysical systems, ranging from planets, single stars and binaries to

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Lucky Imaging in Astronomy,y Imaging is a passive observing technique with individual integration times comparable to the atmospheric coherence time. Thanks to the advent of essentially noise free “Electron multiplying CCD” detectors, Lucky Imaging saw a renewed interest in the past decade. It is now routinely used at a numbe

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Adaptive Optics in High-Contrast Imaging,ging is a very rich and complementary method that can reveal the orbital motion of the planet, the spectrophotometry of its atmosphere but also the architecture and properties of its circumstellar environment. It can unveil possible interactions with a disc, whether a proto-planetary disc in case of

AORTA

Aperture Masking Imaging,ux, zero read-noise regime and offering superior calibration in the bright regime. Since adaptive optics has become commonplace on large telescopes, the key advantage of aperture-mask interferometry is in calibration, particularly of low spatial-frequency phase aberrations that cause quasi-static sp

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Optical Long Baseline Interferometry,les (interferometric phase and contrast) and the image of the source is a Fourier transform expressed first by van Cittert and Zernike. Depending on the source size and the amount of information collected, the analysis of these Fourier components allows a measurement of the typical source size, a pa

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Velocity Fields in Stellar Atmospheres Probed by Tomography,ing at given, pre-specified ranges of optical depths. Different masks thus probe different line-formation depths in the stellar atmosphere. The masks are cross-correlated with the observed spectrum to yield cross-correlation functions (CCFs). The cross-correlation has two advantages: (i) to overcome