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Fizeau interferometric cophasing of segmented mirrors.

Anthony C Cheetham¹, Peter G Tuthill, Anand Sivaramakrishnan

¹Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia. a.cheetham@physics.usyd.edu.au

|February 8, 2013

Summary

A new Fizeau Interferometric Cophasing of Segmented Mirrors (FICSM) method precisely aligns telescope segments. This technique simplifies cophasing, reducing errors for clearer astronomical observations.

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Area of Science:

Optical engineering
Astronomy
Telescope design

Background:

Segmented mirror telescopes offer mechanical advantages but require precise segment alignment (cophasing).
Existing cophasing methods face challenges like non-common path errors and complex hardware setups.
Addressing these limitations is crucial for optimal telescope performance.

Purpose of the Study:

To introduce a novel method, Fizeau Interferometric Cophasing of Segmented Mirrors (FICSM), for precise alignment of segmented mirrors.
To demonstrate the efficacy of FICSM in simplifying cophasing and reducing associated errors.
To validate the method's performance using simulations based on the James Webb Space Telescope (JWST).

Main Methods:

Utilizing non-redundant sparse aperture interferometry for segment phasing.
Employing Fizeau interferometry for high-precision alignment.
Simulating FICSM performance under realistic conditions, including large initial segment misalignments.

Main Results:

FICSM successfully phased simulated JWST primary mirror segments from large initial errors (150 microns piston, 0.5 arcseconds tilt).
Achieved final segment precision of 0.75 nm rms piston and 3.7 mas rms tilt.
Resulted in a root-mean-square (rms) wavefront error of 3.65 nm, significantly below JWST's coarse phasing requirement.

Conclusions:

FICSM offers a robust and efficient solution for cophasing segmented mirrors.
The method simplifies the cophasing process by using standard science hardware and avoiding separate coarse/fine regimes.
FICSM shows significant potential for improving the performance of large segmented telescopes like JWST.