Wavefront sensing within the VISTA infrared camera

Clark, Paul; Berry, P.F.; Bingham, R. G.; Bissonauth, Nirmal; Caldwell, M.; Dipper, N. A.; Dunlop, Colin; Henry, David; Luke, Peter; Myers, R; Robertson, David J.

doi:10.1117/12.552033

Cited by 10 publications

(6 citation statements)

References 5 publications

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“…After obtaining the expression for a single wavelength, the intensity of the interference between different wavelengths,

, can be obtained as follows (

is a matrix whose rows correspond to the spectral response function of the detector) [ 15 , 16 , 17 ]:

where

is the wavelength, and the filter function includes the shape of the passband and frequency response of the detector. Using these equations, we can obtain a quantitative description of the fringes arising from the two-path interference under non-narrow bands.…”

Section: Methodsmentioning

confidence: 99%

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Photonics Scanning Pentaprism System for the Integrated Inspection of Large-Aperture Telescopes

Zhang

Wang

et al. 2023

Sensors

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To improve their spatial resolution and detection capabilities, future ground-based optical telescopes will have a size of 30 m, and the aperture of space telescopes will be increased to 10 m. Such large optical systems necessitate the development of large integrated testing equipment. In this study, spectrum and system alignment measurements and wavefront quality checking were performed using the sub-aperture detection method and a fiber-connected Photonics Scanning Pentaprism (PSP). First, the system was aligned using an optical truss, ensuring that the optical axis was properly positioned. Second, using a sub-aperture light beam though the entrance pupil, light spots were formed on the focal plane and transmitted to the spectrometer via fibers to obtain the corresponding spectral components. Then, by taking measurements at different system positions, a full-aperture spectrum response could be reached. Lastly, by photon-integrated interference on the focal plane, intensity interference fringes could be projected at the entrance pupil of the system. And the wavefront quality of the system could be verified by observing the fringe deformation. The measurement accuracy of the optical axis of the system is better than 2 mrad. The spectral measurement accuracy was better than 5%, and the wavefront measurement accuracy surpassed 0.1 wavelengths (1 wavelength = 633 nm). This study effectively enhanced the detection and in situ calibration capabilities of large telescope systems, ensuring that the performance requirements can be met in the design of future telescopes.

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“…After obtaining the expression for a single wavelength, the intensity of the interference between different wavelengths,

, can be obtained as follows (

is a matrix whose rows correspond to the spectral response function of the detector) [ 15 , 16 , 17 ]:

where

Section: Methodsmentioning

confidence: 99%

“…After obtaining the expression for a single wavelength, the intensity of the interference between different wavelengths, I(λ, u), can be obtained as follows (P(λ) is a matrix whose rows correspond to the spectral response function of the detector) [15][16][17]:…”

Section: Basic Principles Of Wavefront Detection and Spectral Detectionmentioning

confidence: 99%

Photonics Scanning Pentaprism System for the Integrated Inspection of Large-Aperture Telescopes

Zhang

Wang

et al. 2023

Sensors

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“…For details see Patterson and Sutherland 26 , Clark et al 27 , Bissonauth et al 28 , Terrett et al 29 , Terrett and Sutherland 30 . Both high-order and low-order curvature sensing systems have worked well.…”

Section: M2 Support Unit and Curvature Sensorsmentioning

confidence: 97%

VISTA: status and performance

Emerson

Sutherland

2010

SPIE Proceedings

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VISTA, the Visible and Infrared Survey Telescope for Astronomy, is a 4-m class 1.65-degree wide field near-IR survey telescope with 0.34 arcsec pixels. VISTA was successfully commissioned and has been making surveys since 15 October 2009, and was formally accepted as a part of ESO's Cerro Paranal Observatory on 10 December 2009. We summarise the design and build process, report on commissioning and the as-built status. The most novel aspects of the system design have proved to all work well. We report the measured on-sky system performance that confirms that VISTA works as expected.

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“…Currently operating wide field survey telescopes all use wavefront sensing based on image analysis from area detectors. The VISTA telescope, an infrared survey telescope, utilizes a pair of curvature sensors and forward modeling of low order aberrations to provide optical feedback [4,5]. Similarly, the Dark Energy Camera employs 8 2k×2k sensors around the focal plane both in and out of focus to forward model the resulting donut images [6].…”

Section: Introductionmentioning

confidence: 99%

Curvature wavefront sensing for the large synoptic survey telescope

et al. 2015

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The Large Synoptic Survey Telescope (LSST) will use an active optics system (AOS) to maintain alignment and surface figure on its three large mirrors. Corrective actions fed to the LSST AOS are determined from information derived from 4 curvature wavefront sensors located at the corners of the focal plane. Each wavefront sensor is a split detector such that the halves are 1mm on either side of focus. In this paper we describe the extensions to published curvature wavefront sensing algorithms needed to address challenges presented by the LSST, namely the large central obscuration, the fast f /1.23 beam, off-axis pupil distortions, and vignetting at the sensor locations. We also describe corrections needed for the split sensors and the effects from the angular separation of different stars providing the intra-and extra-focal images. Lastly,we present simulations that demonstrate convergence, linearity, and negligible noise when compared to atmospheric effects when the algorithm extensions are applied to the LSST optical system. The algorithm extensions reported here are generic and can easily be adapted to other wide-field optical systems including similar telescopes with large central obscuration and off-axis curvature sensing.

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Wavefront sensing within the VISTA infrared camera

Cited by 10 publications

References 5 publications

Photonics Scanning Pentaprism System for the Integrated Inspection of Large-Aperture Telescopes

Photonics Scanning Pentaprism System for the Integrated Inspection of Large-Aperture Telescopes

VISTA: status and performance

Curvature wavefront sensing for the large synoptic survey telescope

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