Advanced Technology Solar Telescope optical design

Hansen, Eric R.; Price, R.; Hubbard, Rob

doi:10.1117/12.670076

Cited by 10 publications

(4 citation statements)

References 2 publications

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“…Thinner substrates dramatically reduce the thermal time lag and thus simplify the closed-loop thermal control. Modeling and tests have confirmed the ability of the M1 cooling system to control the M1 mirror surface to specifications (Hansen, Price, and Hubbard, 2006;Hansen, Bulau, and Phelps, 2008). Air-jet cooling from the back side is also used to cool smaller, fast tip-tilt mirrors.…”

Section: Thermal Control Of Opticsmentioning

confidence: 86%

“…To achieve the telescope scattered-light performance required for sensitive coronal magnetometry, DKIST uses an unobstructed, fast, off-axis optical configuration that recent solar telescopes have adopted (Kuhn et al, 2003;Goode and Cao, 2012a). Aspects of the optical design of DKIST evolved from an early design presented by Rimmele et al (2003b) and Hansen, Price, and Hubbard (2006). While the design of the main telescope (i.e.…”

Section: Dkist Optical System Designmentioning

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: Thermal Control Of Opticsmentioning

confidence: 86%

Section: Dkist Optical System Designmentioning

confidence: 99%

The Daniel K. Inouye Solar Telescope – Observatory Overview

et al. 2020

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“…2). 13,14 The above simplified heat transfer model can be described by a one-dimensional (1-D) transient heat transfer model (Fig. 3).…”

Section: Heat Transfer Model Of Primary Mirrormentioning

confidence: 99%

Noncontact temperature estimation method on the actively cooled primary mirror surface of large ground-based solar telescope

Liu

Rao

2017

J. Astron. Telesc. Instrum. Syst

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, "Noncontact temperature estimation method on the actively cooled primary mirror surface of large ground-based solar telescope," J. Abstract. To control the mirror seeing effect and the thermal deformation, the actively cooled primary mirror is utilized in a large ground-based solar telescope. Due to direct solar illumination and high reflectivity of the mirror surface coating, the traditional contact or noncontact temperature measuring methods of the mirror surface are not available. A noncontact temperature estimation method based on the analytical heat transfer model of actively cooled primary mirror of a solar telescope is proposed. The experimental validation has been carried out on the actively cooled honeycomb mirror with 600-mm diameter. When the temperature on the mirror surface fluctuates between 23.7 deg and 26 deg, the corresponding estimation error is not more than 0.4 deg. The experimental results validate the correctness and accuracy of the proposed method.

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“…2 The 4m Advanced Technology Solar Telescope (ATST) (see Figure 1), with its integrated high-order adaptive optics (AO) system, will enable observations at a resolution of 0.022arcsec at 430nm, enabling precise measurements of solar magnetic fields at their fundamental scales. This complex, high-performance optical system, 3 which will include wavefront control, 4 integrated polarimetry, 5 and powerful post-focus instrumentation, 6 will be the solar polarimetric microscope that will unravel many of the remaining mysteries of solar magnetism. ATST, slated for first light in 2015, will be the largest and most capable solar telescope ever built.…”

mentioning

confidence: 99%