Development of a Canadian large optical telescope

Roberts, Scott

doi:10.1117/12.567520

Cited by 3 publications

(3 citation statements)

References 10 publications

(10 reference statements)

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“…Assuming that the reliability issue is resolved, we consider two families of designs based on two-mirror basic configurations: Ritchey-Chrétien and aplanatic Gregorian systems. Many variants of such two-mirror telescopes exist with apertures of 8-10 m. Current ELT projects [3][4][5][6][7][8][9] feature similar twomirror basic configurations, except for the European ELT and OWL designs [2,10]. One of the reasons for high popularity of the two-mirror designs is their relatively straightforward configurability to provide gravity stable foci on the Nasmyth platforms, which are essential for many science instruments.…”

Section: Fully Integrated Mcao Systemsmentioning

confidence: 99%

“…Recent advances in adaptive optics (AO) [1] allowed astronomers to improve the angular resolution of existing telescopes by reducing the atmosphere-induced blurring effects. The current plans for building the future extremely large telescopes (ELTs) [2][3][4][5][6][7][8][9][10] featuring multi-conjugate AO (MCAO) systems [11][12][13][14][15][16][17][18][19][20] are justified by their potential to reach the diffraction limit over an extended field of view (FoV) with the resolution of a few milliarcseconds. Current difficulties in manufacturing large deformable mirrors (DMs) limit their direct use in the main telescope system [21].…”

Section: Introductionmentioning

confidence: 99%

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Future giant telescopes: integration of MCAO into telescope design

2008

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Ground-based optical telescopes are still the fundamental tool in observational astronomy. Building future extremely large telescopes featuring AO systems is on the way with a prime goal to reach the diffraction limit in resolution with a few milliarcseconds over extended field. Current difficulties in manufacturing large deformable mirrors (DMs) limit their direct use in the main telescope system, yet it might be feasible in the future. The present paper deals with optical systems with integrated 2-3 DMs into the telescope design. Using DMs of larger diameter in the telescope, one could minimize the number of reflecting surfaces and increase the number of actuators across the DMs, hence improving throughput and reducing the AO fitting error. We present several optical designs with fully-integrated AO that provides conjugations to various heights. A comparative analysis of the imaging quality is given together with recommendations for optimal pupil diameter for each optical configuration.

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Section: Fully Integrated Mcao Systemsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Future giant telescopes: integration of MCAO into telescope design

2008

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“…1 illustrates the telescope reference design that has been synthesized from previous studies by the individual partners. 1,2,3 The Gregorian optical design consists of a 30m, f/1, parabolic primary mirror (M1) and a 3.6m concave, ellipsoidal secondary (M2). The output focal ratio is f/15, and the design has been optimized for a 20 arc minute fieldof-view (FOV).…”

Section: Introductionmentioning

confidence: 99%

Adaptive optics for the Thirty Meter Telescope

et al. 2005

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Adaptive Optics (AO) will be essential for at least seven of the eight science instruments currently planned for the Thirty Meter Telescope (TMT). These instruments include three near infra-red (NIR) imagers and spectrometers with fields of view from 2 to 30 arc seconds, a mid-IR echelle spectrometer, a planet formation imager/spectrometer, a wide field optical spectrograph, and a NIR multi-object spectrometer with multiple integral field units deployable over a 5 arc minute field of regard. In this paper we describe the overall AO reference design that supports these instruments, which consists of a facility AO system feeding the first three instruments and dedicated AO systems for the remaining four.Key design challenges for these systems include very high-order, large-stroke wavefront correction, tip-tilt sensing with faint natural guide stars to maximize sky coverage, laser guidestar wavefront sensing on a very large aperture, and achieving extremely high contrast ratios for the detection of extra-solar planets and other faint companions of bright stars. We describe design concepts for meeting these challenges and summarize our supporting plans for AO component development.

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Orthogonal ray scheme: a method for processing interference patterns and reconstructing the shape of a test convex mirror

Gavlina

Novikov

Askerko

2021

J. Phys.: Conf. Ser.

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This report is devoted to the processing of the interference pattern of the tested mirror, obtained using the orthogonal ray scheme, where the convex testing surface is illuminated by a collimated beam, which is perpendicular to the optical axis of the surface. The interference pattern is created by two wavefronts, one of which is reflected from the mirror, while the other wavefront bypasses the mirror and travels directly to the detector plane. The result of interference pattern processing is a topography map formed by several tangential profiles. The proposed method is suited for large diameter convex spherical and aspherical mirrors and does not require a priori information of surface under the test, such as the vertex radius of curvature and the conical constant. Theoretical foundation of the data processing method are presented.

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Development of a Canadian large optical telescope

Cited by 3 publications

References 10 publications

Future giant telescopes: integration of MCAO into telescope design

Future giant telescopes: integration of MCAO into telescope design

Adaptive optics for the Thirty Meter Telescope

Orthogonal ray scheme: a method for processing interference patterns and reconstructing the shape of a test convex mirror

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