Aperture masking behind AO systems

Michael J. Ireland*

*Corresponding author for this work

Research output: Chapter in Book/Report/Conference proceedingConference proceeding contributionpeer-review

3 Citations (Scopus)
20 Downloads (Pure)

Abstract

Sparse Aperture-Mask Interferometry (SAM or NRM) behind Adaptive Optics (AO) has now come of age, with more than a dozen astronomy papers published from several 5-10m class telescopes around the world. I will describe the reasons behind its success in achieving relatively high contrasts (1000:1 at lambda/D) and repeatable binary astronomy at the diffraction limit, even when used behind laser-guide star adaptive optics. Placed within the context of AO calibration, the information in an image can be split into pupil-plane phase, Fourier amplitude and closure-phase. It is the closure-phase observable, or its generalisation to Kernel phase, that is immune to pupil-plane phase errors at first and second-order and has been the reason for the technique's success. I will outline the limitations of the technique and the prospects for aperture-masking and related techniques in the future.

Original languageEnglish
Title of host publicationAdaptive Optics Systems III
Subtitle of host publicationProceedings of SPIE
EditorsBrent L. Ellerbroek, Enrico Marchetti, Jean-Pierre Véran
Place of PublicationBellingham, WA
PublisherSPIE
Pages1-7
Number of pages7
Volume8447
ISBN (Print)9780819491480
DOIs
Publication statusPublished - 2012
EventAdaptive Optics Systems III - Amsterdam, Netherlands
Duration: 1 Jul 20126 Jul 2012

Other

OtherAdaptive Optics Systems III
CountryNetherlands
CityAmsterdam
Period1/07/126/07/12

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