The wavefront correction system for the Advanced Technology Solar Telescope

Rimmelé, Thomas; Richards, Kit; Roche, Jacqueline M.; Hegwer, S.; Hubbard, Rob; Hansen, Eric R.; Goodrich, Bret; Upton, Robert S.

doi:10.1117/12.672330

Cited by 8 publications

(6 citation statements)

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“…The bandwidth error is a result of the finite (2 kHz) update rate of the AO. During the systems-engineering process and also driven by science-productivity considerations, the number of actuators and sub-apertures was increased to 1600 and 1457 respectively, compared to earlier designs (Rimmele et al, 2006). The AO system is capable of correcting up to approximately 1400 Karhunen-Loève (KL) modes.…”

Section: Wavefront Correction Systemmentioning

confidence: 98%

“…The instruments are installed on a rotating platform (Jeffers et al, 2016), which also serves as image de-rotator and allows for alignment of the spectrograph slits, for example, parallel or perpendicular to the limb. The tip-tilt mirror and the deformable mirror of the conventional high-order AO system (Rimmele et al, 2006;Richards et al, 2010;Johnson et al, 2018) are integrated into the transfer optics. The AO-corrected light beam feeds the four instruments that are designed to perform diffraction-limited observations at visible and near-infrared wavelengths, and which can operate simultaneously.…”

Section: Science Requirements Definitionmentioning

confidence: 99%

“…The wavefront-correction system is a key component of DKIST (Rimmele et al, 2006;Richards et al, 2010;Johnson et al, 2016) that enables both seeing-limited and diffractionlimited observations. This subsystem includes: i) A solar AO system that corrects atmospheric seeing and residual optical aberrations at 2 kHz rates.…”

Section: Wavefront Correction Systemmentioning

confidence: 99%

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The Daniel K. Inouye Solar Telescope – Observatory Overview

et al. 2020

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We present an overview of the National Science Foundation’s Daniel K. Inouye Solar Telescope (DKIST), its instruments, and support facilities. The 4 m aperture DKIST provides the highest-resolution observations of the Sun ever achieved. The large aperture of DKIST combined with state-of-the-art instrumentation provide the sensitivity to measure the vector magnetic field in the chromosphere and in the faint corona, i.e. for the first time with DKIST we will be able to measure and study the most important free-energy source in the outer solar atmosphere – the coronal magnetic field. Over its operational lifetime DKIST will advance our knowledge of fundamental astronomical processes, including highly dynamic solar eruptions that are at the source of space-weather events that impact our technological society. Design and construction of DKIST took over two decades. DKIST implements a fast (f/2), off-axis Gregorian optical design. The maximum available field-of-view is 5 arcmin. A complex thermal-control system was implemented in order to remove at prime focus the majority of the 13 kW collected by the primary mirror and to keep optical surfaces and structures at ambient temperature, thus avoiding self-induced local seeing. A high-order adaptive-optics system with 1600 actuators corrects atmospheric seeing enabling diffraction limited imaging and spectroscopy. Five instruments, four of which are polarimeters, provide powerful diagnostic capability over a broad wavelength range covering the visible, near-infrared, and mid-infrared spectrum. New polarization-calibration strategies were developed to achieve the stringent polarization accuracy requirement of 5×10−4. Instruments can be combined and operated simultaneously in order to obtain a maximum of observational information. Observing time on DKIST is allocated through an open, merit-based proposal process. DKIST will be operated primarily in “service mode” and is expected to on average produce 3 PB of raw data per year. A newly developed data center located at the NSO Headquarters in Boulder will initially serve fully calibrated data to the international users community. Higher-level data products, such as physical parameters obtained from inversions of spectro-polarimetric data will be added as resources allow.

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Section: Wavefront Correction Systemmentioning

confidence: 98%

Section: Science Requirements Definitionmentioning

confidence: 99%

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The Daniel K. Inouye Solar Telescope – Observatory Overview

et al. 2020

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“…The WFC is comprised of the aO, the QSA and the HOAO. The ATST will be operated in different observing modes that drive requirements and specifications as well as operations procedures for the WFC subsystems and were described in a previous paper 3 . To summarize briefly the observing modes that drive the WFC design are:…”

Section: Introductionmentioning

confidence: 99%

The adaptive optics and wavefront correction systems for the Advanced Technology Solar Telescope

et al. 2010

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The high order adaptive optics (HOAO) system is the centerpiece of the ATST wavefront correction system. The ATST wavefront correction system is required to achieve a Strehl of S = 0.6 or better at visible wavelength. The system design closely follows the successful HOAO implementation at the Dunn Solar Telescope and is based on the correlating Shack-Hartmann wavefront sensor. In addition to HOAO the ATST will utilize wavefront sensors to implement active optics (aO) and Quasi Static Alignment (QSA) of the telescope optics, which includes several off-axis elements. Provisions for implementation of Multi-conjugate adaptive optics have been made with the design of the optical path that feeds the instrumentation at the coudé station. We will give an overview of the design of individual subsystems of the ATST wavefront correction system and describe some of the unique features of the ATST wavefront correction system, such as the need for thermally controlled corrective elements.

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“…It is therefore not surprising that the first successful on-the-sky MCAO experiments were performed at the Dunn Solar Telescope and at a solar telescope on the Canary Islands. However, further development is needed before operational solar MCAO can be implemented at future large aperture solar telescopes such as the ATST on Haleakala [6]. MCAO development must progress beyond these initial proof-of-concept experiments and should include laboratory experiments and on-sky demonstrations under controlled or well characterized conditions as well as quantitative performance analysis and comparison to model predictions.…”

Section: Introductionmentioning

confidence: 99%

Solar multiconjugate adaptive optics at the Dunn Solar Telescope

et al. 2010

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Abstract. Solar observations are performed over an extended field of view and the isoplanatic patch over which conventional adaptive optics (AO) provides diffraction limited resolution is a severe limitation. The development of multi-conjugate adaptive optics (MCAO) for the next generation large aperture solar telescopes is thus a top priority. The Sun is an ideal object for the development of MCAO since solar structure provides ,,multiple guide stars" in any desired configuration. At the Dunn Solar Telescope (DST) we implemented a dedicated MCAO bench with the goal of developing well-characterized, operational MCAO. The MCAO system uses 2 deformable mirrors conjugated to the telescope entrance pupil and a layer in the upper atmosphere, respectively. DM2 can be placed at conjugates ranging from 2km to 10km altitude. We have successfully and stably locked the MCAO system on artificial objects (slides), for which turbulence screens are generated directly in front of the DMs, as well as solar structure. We present preliminary results and discuss future plans.

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The wavefront correction system for the Advanced Technology Solar Telescope

Cited by 8 publications

References 0 publications

The Daniel K. Inouye Solar Telescope – Observatory Overview

The Daniel K. Inouye Solar Telescope – Observatory Overview

The adaptive optics and wavefront correction systems for the Advanced Technology Solar Telescope

Solar multiconjugate adaptive optics at the Dunn Solar Telescope

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