Aperture masking behind AO systems

Michael J. Ireland

doi:10.1117/12.926763

Aperture masking behind AO systems

Michael J. Ireland^*

^*Corresponding author for this work

Research output: Chapter in Book/Report/Conference proceeding › Conference proceeding contribution › peer-review

3 Citations (Scopus)

64 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 language	English
Title of host publication	Adaptive Optics Systems III
Subtitle of host publication	Proceedings of SPIE
Editors	Brent L. Ellerbroek, Enrico Marchetti, Jean-Pierre Véran
Place of Publication	Bellingham, WA
Publisher	SPIE
Pages	1-7
Number of pages	7
Volume	8447
ISBN (Print)	9780819491480
DOIs	https://doi.org/10.1117/12.926763
Publication status	Published - 2012
Event	Adaptive Optics Systems III - Amsterdam, Netherlands Duration: 1 Jul 2012 → 6 Jul 2012

Other

Other	Adaptive Optics Systems III
Country/Territory	Netherlands
City	Amsterdam
Period	1/07/12 → 6/07/12

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10.1117/12.926763

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Cite this

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title = "Aperture masking behind AO systems",

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.",

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AB - 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.

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Aperture masking behind AO systems

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