Modelling astronomical adaptive optics - I. The software package caos

Carbillet, Marcel; Vérinaud, Christophe; Femenia, Bruno; Riccardi, Armando; Fini, Luca

doi:10.1111/j.1365-2966.2004.08524.x

Cited by 75 publications

(53 citation statements)

References 26 publications

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“…Since we are interested in studying the behaviour of the IBD introducing the SR constraint, we consider a set of different AOcorrected PSFs with increasing SR. The five PSFs used here (with SR from 0.17 to 0.68) have been obtained by means of the Software Package CAOS (Carbillet et al 2005), according to a precise model of the first-light AO system of LBT and the near-infrared camera LUCIFER described in a previous paper (Carbillet et al 2004b). The main parameters associated with these simulations are reported in Table 1.…”

Section: Numerical Experimentsmentioning

confidence: 99%

Strehl-constrained iterative blind deconvolution for post-adaptive-optics data

Desiderà¹,

Carbillet²

2009

A&A

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Aims. We aim to improve blind deconvolution applied to post-adaptive-optics (AO) data by taking into account one of their basic characteristics, resulting from the necessarily partial AO correction: the Strehl ratio. Methods. We apply a Strehl constraint in the framework of iterative blind deconvolution (IBD) of post-AO near-infrared images simulated in a detailed end-to-end manner and considering a case that is as realistic as possible. Results. The results obtained clearly show the advantage of using such a constraint, from the point of view of both performance and stability, especially for poorly AO-corrected data. The proposed algorithm has been implemented in the freely-distributed and CAOS-based Software Package AIRY.

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Section: Numerical Experimentsmentioning

confidence: 99%

Strehl-constrained iterative blind deconvolution for post-adaptive-optics data

Desiderà¹,

Carbillet²

2009

A&A

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“…To simulate an NGS tip/tilt correction, the overall tip/tilt is subtracted from the wavefront before the LGS sensing is done. The atmospheric phase-screens are generated using the PSG package from the CAOS software [7]. The atmospheric phase-screens are 1024 × 1024 pixels, 0.046 m/px with outer scale L 0 = 30 m. Turbulence strength of each layer is derived by the turbulence profiles measured at Mt Graham [8].…”

Section: Results From Simulationmentioning

confidence: 99%

Implementation of SLODAR atmospheric turbulence profiling to the ARGOS system

et al. 2014

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“…To predict the exact degree of correction we used "end-to-end" simulation of MagAO/VisAO with the Code for Adaptive Optics Simulation (CAOS; Carbillet et al 2005). Our CAOS simulations (assuming no extra telescope vibration) predict slightly larger wavefront errors (135 vs. 122 nm rms) than our "corrected" test tower results (Males et al 2012;Close et al 2012), hence our test tower results are quite consistent with our analytical model of MagAO.…”

Section: Our Simulated Magao/visao Error Budget Compared To On-sky Rementioning

confidence: 99%

A review of astronomical science with visible light adaptive optics

2016

Adaptive Optics Systems V

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We review astronomical results in the visible (λ<1μm) with adaptive optics. Other than a brief period in the early 1990s, there has been little (<1 paper/yr) night-time astronomical science published with AO in the visible from 2000-2013 (outside of the solar or Space Surveillance Astronomy communities where visible AO is the norm, but not the topic of this invited review). However, since mid-2013 there has been a rapid increase visible AO with over 50 refereed science papers published in just ~2.5 years (visible AO is experiencing a rapid growth rate very similar to that of NIR AO science from 1997Close 2000). Currently the most productive small (D < 2 m) visible light AO telescope is the UV-LGS Robo-AO system (Baranec, et al. 2016) on the robotic Palomar D=1.5 m telescope (currently relocated to the Kitt Peak 1.8m; Salama et al. 2016). Robo-AO uniquely offers the ability to target >15 objects/hr, which has enabled large (>3000 discrete targets) companion star surveys and has resulted in 23 refereed science publications. The most productive large telescope visible AO system is the D=6.5m Magellan telescope AO system (MagAO). MagAO is an advanced Adaptive Secondary Mirror (ASM) AO system at the Magellan 6.5m in Chile ). This ASM secondary has 585 actuators with < 1 msec response times (0.7 ms typically). MagAO utilizes a 1 kHz pyramid wavefront sensor. The relatively small actuator pitch (~22 cm/subap) allows moderate Strehls to be obtained in the visible (0.63-1.05 microns). Long exposures (60s) achieve <30mas resolutions, 30% Strehls at 0.62 microns (r') with the VisAO camera in 0.5" seeing with bright R ≤ 9 mag stars. These capabilities have led to over 22 MagAO refereed science publications in the visible. The largest (D=8m) telescope to achieve regular visible AO science is SPHERE/ZIMPOL. ZIMPOL is a polarimeter fed by the ~1.2 kHz SPHERE ExAO system (Fusco et al. 2016). ZIMPOL's ability to differentiate scattered polarized light from starlight allows the sensitive detection of circumstellar disks, stellar surfaces, and envelopes of evolved AGB stars. Here we review the key steps to having good performance in the visible and review the exciting new AO visible science opportunities and science results in the fields of: exoplanet detection; circumstellar and protoplanetary disks; young stars; AGB stars; emission line jets; and stellar surfaces. The recent rapid increase in the scientific publications and power of visible AO is due to the maturity of the next-generation of AO systems and our new ability probe circumstellar regions with very high (10-30 mas) spatial resolutions that would otherwise require much larger (>10m) diameter telescopes in the infrared.

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Modelling astronomical adaptive optics - I. The software package caos

Cited by 75 publications

References 26 publications

Strehl-constrained iterative blind deconvolution for post-adaptive-optics data

Strehl-constrained iterative blind deconvolution for post-adaptive-optics data

Implementation of SLODAR atmospheric turbulence profiling to the ARGOS system

A review of astronomical science with visible light adaptive optics

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