Vision and Revision
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Transcript of Vision and Revision
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Vision and RevisionWavefront Sensing from the Image Domain
Benjamin Pope@fringetracker
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Our Group
Peter Tuthill Ben Pope (me!)
Frantz Martinache Nick Cvetojevic
Anthony Cheetham
Niranjan Thatte
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James Webb Space Telescope
› The James Webb Space Telescope is the next-generation NASA major space observatory
› A 6.5 m diameter segmented primary mirror will make it the largest civilian space telescope
› Left: a full scale mockup of the telescope in Munich
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Phasing the JWST
› A major issue with JWST will be in using a segmented mirror in space
› No current robust, cheap approach to making sure the mirrors are aligned with required ~ nm accuracy
› This is where we come in!
› Mirror segments have actuators in tip, tilt, piston and curvature
› We can use these to correct the phasing
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Fourier Amplitudes and Phases
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V
Amplitudes
Phases
V
Amplitudes
Phases
Albert Michelson
Pablo Picasso
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Interferometry: Phase
› The phase delay between two receivers relates to the position of the astrophysical object
Δ𝜑=𝑑 /𝜆
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Interferometry: Phase
› The phase delay between two receivers relates to the position of the astrophysical object
› If the atmosphere disrupts the wavefront, this information is corrupted by errors!
Δ𝜑=? ??
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Closure Phase
› True phases are encoded on baselines, , but errors are on the wavefront and hit each detector separately
› If we add up measured phases around a loop, errors cancel out:
- If , then the closure phase
is immune to error: !
Δ𝜙1
Δ𝜙3
Δ𝜙2
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Redundant Baselines
› Multiple pairs of points sample each baseline.
› Random walk in the phasor space corrupts image
› Closure phase no longer works!
(𝑢 ,𝑣 )(𝑢 ,𝑣 )
Duplicate baselines!
ℑ𝔪
ℜ𝔢
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Non-Redundant Masking
› If we put a mask on the telescope aperture and let through only one copy of each baseline, we overcome this problem
› Non-redundant masking gives us good amplitude measurements – and also lets us recover some phase information
Aperture masks used on NIRC2 (image courtesy of Peter Tuthill).
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Kernel Phase Interferometry
› Kernel phase is a method of image deconvolution for high resolution astronomy
› Works on Nyquist-sampled, space-based or well-corrected (extreme) AO images
› A software-only idea similar to the aperture masking approach› Delivers contrast ~ hundreds within λ/D› Can also be used as a wavefront sensor (Martinache sensor)› Only five papers so far!› A solution looking for a problem!
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Linear Phase Transfer
› Martinache (2010) considered a generalisation of closure phase when phase errors are small enough to be linear
› For measured phases are , ‘true’ baseline phases and errors in the pupil plane are
› In this case, the phases on each baseline will be
where is a transfer matrix relating pupil and image plane phases and the redundancy of each baseline.
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Kernel Phase Interferometry
› Use singular value decomposition: express › Find an operator K such that
› This kernel operator maps measured phases to kernel phases which are immune to small errors:
› Can recover a large fraction of phase information › Even for a redundant aperture, we still have robust
observables – with no need of a mask!
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Phase Reconstruction
› What about the other way – get phases from their autocorrelation?
› The singular value decomposition also lets us create a pseudoinverse, such that
› This allows for an approximate reconstruction of pupil phases:
› This maps modes in the Fourier plane onto modes in the pupil, i.e. inverting the autocorrelation
› Reconstruct wavefronts using only an image!
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The Asymmetric Pupil
› The Fourier plane (FT of the image) is the autocorrelation of the pupil- Not sensitive to all symmetries! A
symmetric pupil can sense only even modes
› A Fourier wavefront sensor needs to have pupil asymmetry to sense asymmetric modes- This could be achieved with thick
spider(s), e.g. right.
- Alternatively, could mask out subapertures
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Martinache Wavefront Sensor Simulations
› Uses row phases (complement of kernel space)
› Wavefront sensor is your science camera!
› Initial Strehl > 35% required – can iterate to as high as 97% in simulations
› Sensitivity near-optimal for a given flux and wavefront error
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Experimental Setup I
› The microelectromechanical (MEMS) segmented mirror from Dragonfly was used as a JWST analogue
› This has piston, tip and tilt on each segment with ~ few nm precision
› Phasing JWST is hard – no apparatus in space!
› Ideal test case for the new wavefront sensor
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Experimental Setup II
› Laser introduced from single mode fibre
› Passed to MEMS array and through mask
› Imaged onto Xenics IR camera
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First Step - FICSM
› The first step in phasing a segmented mirror like this is the FICSM approach – ‘Fizeau interferometric cophasing of segmented mirrors’ (Cheetham et al)
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How do you Solve a Problem like A Mirror?
› We want a ‘tweeter’ on top of coarse phasing with FICSM
› Martinache (2013) theory says you need an asymmetric pupil
› We could do this with bars – or single segments
› That does work – but you still have planes of mirror symmetry for which the sensor is weak
› If you take out the same pattern you included with FICSM, you have no symmetries
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Pupil Modes
› Below: examples of normal modes of the discrete pupil model used in our experiment
› These play the role of the Zernike basis for expanding optical aberrations on a circular pupil
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Degrading the Wavefront
› Wavelength: 1600 nm
› MEMS settings disturbed by random tips, tilts and pistons nm
› Right: Wavefront reconstruction
› Can we fix this?
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Wavefront Restoration
› Yes we can!
› Right: reconstructed wavefront
› Don’t let the colourbar scare you – there are a couple of bad points
› Actual RMS piston error reduced < 10nm on all segments
› Strehl > 99%!
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Quick and Dirty
› While we found that the not-at-all symmetric segment tilting worked best, can we get away with doing fewer segments?- Better if moving mirrors is risky, expensive
or slow
› Yes we can! A single asymmetry (particularly in the outer ring) was found to work (top)- Has some issues with sensing modes
symmetric with respect to the line of reflection symmetry
› A wedge asymmetry (3 in outer ring, one in inner) also works (bottom)
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How well can we Measure a Single Segment?
› Pistoned a single segment (3) in 20 nm steps from -300 to +300
› Reconstruction is very accurate… within limits
› You lose it when linearity fails
› Phases are also correlated – sensing modes globally is a bad way to reconstruct phases on a single segment
› When phasing the whole mirror in closed loop, this correlated error beats down to zero as you make the whole thing flat
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Restoring a PSF
› Left: animation of a stretched PSF as our algorithm converges
› This is with a scalene triangle of segments removed
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Restoring a PSF
› Also works with a wedge removed
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Restoring a PSF
› Or in fact a single segment!
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Oxford-SWIFT at Palomar
› Hale 200-inch telescope has the PALM-3000 extreme AO system – the highest order AO currently available for experiments
› Oxford has the Short Wavelength Integral Field specTrograph (SWIFT) on P3K – a high spatial and spectral resolution IFU from 650-1000 nm
› SWIFT has historically had problems with non common path error – never achieves even internal diffraction limit- Hard to correct with conventional methods, because of the optical layout
› Ideal test case for our wavefront sensing method
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HODM Mask
› Right: the mask we placed over the high order DM to get the pupil asymmetry
› This was probably overkill, but we wanted to make sure it worked the first time!
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Results
› Left top: 940nm ; bottom, 970 nm PSF› You can see two, maybe 3 Airy rings› This would not ordinarily be especially
impressive – but SWIFT has an internally very complicated layout and has never seen Airy rings before!
› This was achieved with only the LODM› HODM correction should get it to the
diffraction limit!
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The Phase Map
› Right: Final phase map subtracted from LODM offsets
› Could maybe have improved – but had to stop to do science observations!
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Next Directions
› Now that we’ve demonstrated this in the lab and on Palomar…- JWST needs phasing! But can we maybe get a ‘spider
sense’ from using the spiders as the asymmetric mask?- HARMONI, the first-light IFS for the E-ELT is predicted to
suffer from very bad non common path error – ideal case!- Project 1640 – another Palomar IFS for exoplanet studies
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Thanks!
Thank you for listening!