Astronomy at High Angular Resolution: A Compendium of by Henri M. J. Boffin, Gaitee Hussain, Jean-Philippe Berger,

By Henri M. J. Boffin, Gaitee Hussain, Jean-Philippe Berger, Linda Schmidtobreick

This ebook deals a vital compendium of astronomical high-resolution options. contemporary years have noticeable substantial advancements in such innovations, that are severe to advances in lots of parts of astronomy. As mirrored within the ebook, those ideas may be divided into direct tools, interferometry, and reconstruction tools, and will be utilized to an enormous number of astrophysical structures, starting from planets, unmarried stars and binaries to energetic galactic nuclei, delivering angular solution within the micro- to tens of milliarcsecond scales. Written through specialists of their fields, the chapters conceal adaptive optics, aperture overlaying imaging, spectra disentangling, interferometry, fortunate imaging, Roche tomography, imaging with interferometry, interferometry of AGN, AGN reverberation mapping, Doppler- and magnetic imaging of stellar surfaces, Doppler tomography, eclipse mapping, Stokes imaging, and stellar tomography.

This ebook is meant to allow a subsequent iteration of astronomers to use high-resolution innovations. It informs readers on find out how to in attaining the simplest angular solution within the seen and near-infrared regimes from diffraction-limited to micro-arcsecond scales.

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Additional info for Astronomy at High Angular Resolution: A Compendium of Techniques in the Visible and Near-Infrared

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4 Overview of the most common differential imaging techniques Name ADI RDI SDI PDI Diversity parameter Strengths pupil/field rel- easy implementation ative rotation science/ref. no self-subraction star Drawbacks PSF decorrelation over time, self-subtraction rapid switching required or large library, subject to change in the PSF shape/AO correction, overheads due to the calibrator wavelength simultaneous difference relies on spectral features, chromaticity linear polarisa- simultaneous difference, relies on linear polarisation feature, calibration achromatic tion of instrumental polarisation.

The prism can be fixed or oscillating. The measured flux in each quadrant can be related to the slope of the wavefront. The PWFS is more sensitive to low-order modes than the SHWFS [54]. This drawback of the SHWFS is of critical importance because many high-rejection coronagraphs require an excellent correction of low-order aberrations to provide a high contrast. The PWFS is also less prone to aliasing effects than the SHWFS, although this can be mitigated by the use of an adjustable spatial filter, as in Gemini/GPI and VLT/SPHERE.

The pyramid wavefront sensor (PWFS) is a more recent development proposed in 1995 [53]. A pyramidal prism is inserted in a focal plane. Each face of the prism deflects the light in a different direction and a lens relay conjugates the four apparent exit pupils onto four pupil images on the detector (Fig. 5 right). The prism can be fixed or oscillating. The measured flux in each quadrant can be related to the slope of the wavefront. The PWFS is more sensitive to low-order modes than the SHWFS [54].

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