The Advanced Technology Solar Telescope: beginning construction of the world's largest solar telescope

Rimmelé, Thomas; Wagner, J.; Keil, Stephen L.; Elmore, D.; Hubbard, Robert P.; Hansen, Eric R.; Warner, Mark; Jeffers, Paul; Phelps, LeEllen; Marshall, Heather K.; Goodrich, Bret; Richards, Kit; Hegwer, S.; Kneale, Ruth; Ditsler, J.

doi:10.1117/12.857714

Cited by 20 publications

(11 citation statements)

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“…The strong scientific case for the ATST has been presented in previous publications [1] [2]. The science drivers lead to a versatile ATST design that supports diffraction-limited imaging, spectroscopy and, in particular, magnetometry at visible and near-and far-infrared wavelengths, and infrared coronal observations near the limb of the Sun [3]. A main scientific objective of the ATST is to precisely measure the three-dimensional structure of the magnetic field that drives the variability and activity of the solar atmosphere.…”

Section: Introductionmentioning

confidence: 99%

The Advanced Technology Solar Telescope: design and early construction

et al. 2012

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The National Solar Observatory's (NSO) Advanced Technology Solar Telescope (ATST) is the first large U.S. solar telescope accessible to the worldwide solar physics community to be constructed in more than 30 years. The 4-meter diameter facility will operate over a broad wavelength range (0.35 to 28 µm ), employing adaptive optics systems to achieve diffraction limited imaging and resolve features approximately 20 km on the Sun; the key observational parameters (collecting area, spatial resolution, spectral coverage, polarization accuracy, low scattered light) enable resolution of the theoretically-predicted, fine-scale magnetic features and their dynamics which modulate the radiative output of the sun and drive the release of magnetic energy from the Sun's atmosphere in the form of flares and coronal mass ejections.In 2010, the ATST received a significant fraction of its funding for construction. In the subsequent two years, the project has hired staff and opened an office on Maui. A number of large industrial contracts have been placed throughout the world to complete the detailed designs and begin constructing the major telescope subsystems. These contracts have included the site development, A&E designs, mirrors, polishing, optic support assemblies, telescope mount and coudé rotator structures, enclosure, thermal and mechanical systems, and high-level software and controls. In addition, design development work on the instrument suite has undergone significant progress; this has included the completion of preliminary design reviews (PDR) for all five facility instruments. Permitting required for physically starting construction on the mountaintop of Haleakalā, Maui has also progressed. This paper will review the ATST goals and specifications, describe each of the major subsystems under construction, and review the contracts and lessons learned during the contracting and early construction phases. Schedules for site construction, key factory testing of major subsystems, and integration, test and commissioning activities will also be discussed.

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Section: Introductionmentioning

confidence: 99%

The Advanced Technology Solar Telescope: design and early construction

et al. 2012

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“…The Daniel K. Inouye Solar Telescope (DKIST) is a 4-meter solar observatory under construction at Haleakala, Hawaii [1]. The observatory will consist of a suite of facility instruments that study the outer solar atmosphere using a combination of visible and polarimetric data acquisition techniques.…”

Section: Introductionmentioning

confidence: 99%

DKIST controls model for synchronization of instrument cameras, polarization modulators, and mechanisms

et al. 2014

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The Daniel K. Inouye Solar Telescope (DKIST) will include facility instruments that perform polarimetric observations of the sun. In order for an instrument to successfully perform these observations its Instrument Controller (IC) software must be able to tightly synchronize the activities of its sub-systems including polarization modulators, cameras, and mechanisms. In this paper we discuss the DKIST control model for synchronizing these sub-systems without the use of hardware trigger lines by using the DKIST Time Reference And Distribution System (TRADS) as a common time base and through sub-system control interfaces that support configuring the timing and cadence of their behavior.The DKIST Polarization Modulator Controller System (PMCS) provides an interface that allows the IC to characterize the rotation of the modulator in terms of a reference time (t0), rate, and start state. The DKIST Virtual Camera (VC) provides a complimentary interface that allows data acquisitions and accumulation sequences to be specified using a reference time (t0), rate, and execution block time slices, which are cumulative offsets from t0. Re-configuration of other instrument mechanisms such as filter, slits, or steering mirrors during the observation is the responsibility of the IC and must be carefully scheduled at known and pre-determined gaps in the VC data acquisition sequence.The DKIST TRADS provides an IEEE-1588-2008 Precision Time Protocol (PTP) service that is used to synchronize the activities of instrument sub-systems. The modulator, camera, and mechanism sub-systems subscribe to this service and can therefore perform their tasks according to a common time base.In this paper we discuss the design of the PMCS, VC, and mechanism control interfaces, and how the IC can use them to configure the behavior of these sub-systems during an observation. We also discuss the interface to TRADS and how it is used as a common time base in each of these sub-systems. We present our preliminary results of the system performance against known instrument use cases.

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“…Diffraction-limited observations of the solar atmosphere are a key science driver for the Advanced Technology Solar Telescope (ATST) 1,2 . As a consequence the ATST wavefront correction system (WFC) is a centerpiece of the telescope facility.…”

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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The Advanced Technology Solar Telescope: beginning construction of the world's largest solar telescope

Cited by 20 publications

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The Advanced Technology Solar Telescope: design and early construction

The Advanced Technology Solar Telescope: design and early construction

DKIST controls model for synchronization of instrument cameras, polarization modulators, and mechanisms

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

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