Abstract
Aperture-mask interferometry has a long history in the speckle regime – in principle equalling the performance of speckle interferometry in the low-flux, 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 speckles. I will describe the principles of quasi-static speckle limited imaging in the Fourier plane, where bispectral phase (or Kernel-phase ) and Fourier power are the primary observables, and will show that where Strehl ratios are low or moderate, a non-redundant aperture can offer superior imaging performance. Finally, I will demonstrate the applicability of aperture-masking imaging both to laser-guide star imaging of faint (K ∼ 14) star systems and bright transition disc stars (e.g. LkCa 15) surrounded by faint (1000:1 dynamic range) structures.
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Ireland, M.J. (2016). Aperture Masking Imaging. In: Boffin, H., Hussain, G., Berger, JP., Schmidtobreick, L. (eds) Astronomy at High Angular Resolution. Astrophysics and Space Science Library, vol 439. Springer, Cham. https://doi.org/10.1007/978-3-319-39739-9_3
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DOI: https://doi.org/10.1007/978-3-319-39739-9_3
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