Adding multi-conjugate adaptive optics to the Daniel K. Inouye Solar Telescope

AbstractThe Indian National Large Solar Telescope (NLST) will be a state-of-the-art 2-m class telescope for carrying out high resolution studies of the solar atmosphere. Sites in the Himalayan region at altitudes greater than 4000-m that have extremely low water vapor content and are unaffected by monsoons are under evaluation. This project is led by the Indian Institute of Astrophysics and has national and international partners.NLST is an on-axis alt-azimuth Gregorian multi-purpose open telescope with the provision of carrying out night time stellar observations using a spectrograph. The telescope utilizes an innovative design with low number of reflections to achieve a high throughput and low instrumental polarization. High order adaptive optics is integrated into the design that works with a modest Fried's parameter of 7-cm to give diffraction limited performance. The telescope will be equipped with a suite of post-focus instruments including a high resolution spectrograph and a polarimeter. A detailed concept design of the telescope is presently being finalized and fabrication is expected to begin in 2010 with first light in 2014.

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Results of the multi-conjugate adaptive optics system at the German solar telescope, Tenerife

10.1117/12.619132 ◽

2005 ◽

Cited By ~ 4

Author(s):

Thomas Berkefeld ◽

Dirk Soltau ◽

Oskar von der Luehe

Keyword(s):

Adaptive Optics ◽

Solar Telescope ◽

Adaptive Optics System

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Multi-Conjugate Adaptive Optics - relay optical designs for a 4-m off-axis solar telescope

10.1117/12.509196 ◽

2004 ◽

Author(s):

Gilberto Moretto ◽

Thomas R. Rimmele ◽

Maud Langlois

Keyword(s):

Adaptive Optics ◽

Solar Telescope

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

10.1117/12.857515 ◽

2010 ◽

Cited By ~ 3

Author(s):

K. Richards ◽

T. Rimmele ◽

S. L. Hegwer ◽

R. S. Upton ◽

F. Woeger ◽

...

Keyword(s):

Adaptive Optics ◽

Advanced Technology ◽

Solar Telescope ◽

Wavefront Correction

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Project of the Large Solar Telescope with mirror 3 m in diameter

Solar-Terrestrial Physics ◽

10.12737/stp-62202002 ◽

2020 ◽

Vol 6 (2) ◽

pp. 14-29 ◽

Cited By ~ 2

Author(s):

Victor Grigoryev ◽

Mikhail Demidov ◽

Dmitriy Kolobov ◽

Vasiliy Pulyaev ◽

Valery Skomorovsky ◽

...

Keyword(s):

Adaptive Optics ◽

Near Infrared ◽

Solar Physics ◽

Solar Observatory ◽

Spectral Lines ◽

Small Scale ◽

Solar Telescope ◽

Rotating Platform ◽

Solar Telescopes ◽

Under Construction

One of the most important problems of modern solar physics is the observation of the small-scale structure of the solar atmosphere at various heights (including the chromosphere and corona) in different spectral lines. Such observations can be made only with large solar telescopes whose main mirror has a diameter of at least 3 m. Currently, several large solar telescopes are under construction or development in the world. In 2013 in Russia, the work began on the development of a national large solar telescope with a mirror 3 m in diameter (LST-3), which is a part (subproject) of the National Heliogeophysical Complex of the Russian Academy of Sciences. The telescope is planned to be located in the Sayan Solar Observatory at an altitude of more than 2000 m. The choice was made in favor of the classic axisymmetric Gregory optical layout on an alt-azimuth mount. The scientific equipment of LST-3 will consist of several systems of narrow-band tunable filters and spectrographs for various wave ranges. The equipment will be placed both in the main coude focus on a rotating platform and in the Nasmyth focus. To achieve a diffraction resolution, high-order adaptive optics (AO) will be used. It is assumed that with a certain modification of the optical configuration, LST-3 will work as a 0.7 m mirror coronograph in near infrared lines and can also be used for observing astrophysical objects in the nighttime.

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Two-telescope-based solar seeing profile measurement simulation

Research in Astronomy and Astrophysics ◽

10.1088/1674-4527/21/12/298 ◽

2022 ◽

Vol 21 (12) ◽

pp. 298

Author(s):

Zi-Yue Wang ◽

De-Qing Ren ◽

Raffi Saadetian

Keyword(s):

Numerical Simulations ◽

Atmospheric Turbulence ◽

Adaptive Optics ◽

Solar Observatory ◽

Performance Estimation ◽

Image Motion ◽

Profile Measurement ◽

Solar Telescope ◽

National Solar Observatory ◽

Bear Lake

Abstract Measurements of the daytime seeing profile of the atmospheric turbulence are crucial for evaluating a solar astronomical site so that research on the profile of the atmospheric turbulence as a function of altitude C n 2 ( h n ) becomes more and more critical for performance estimation and optimization of future adaptive optics (AO) including the multi-conjugate adaptive optics (MCAO) systems. Recently, the S-DIMM+ method has been successfully used to measure daytime turbulence profiles above the New Solar Telescope (NST) on Big Bear Lake. However, such techniques are limited by the requirement of using a large solar telescope which is not realistic for a new potential astronomical site. Meanwhile, the A-MASP (advanced multiple-aperture seeing profiler) method is more portable and has been proved that can reliably retrieve the seeing profile up to 16 km with the Dunn Solar Telescope (DST) on the National Solar Observatory (Townson, Kellerer et al.). But the turbulence of the ground layer is calculated by combining A-MASP and S-DIMM+ (Solar Differential Image Motion Monitor+) due to the limitation of the two-individual-telescopes structure. To solve these problems, we introduce the two-telescope seeing profiler (TTSP) which consists of two portable individual telescopes. Numerical simulations have been conducted to evaluate the performance of TTSP. We find our TTSP can effectively retrieve seeing profiles of four turbulence layers with a relative error of less than 4% and is dependable for actual seeing measurement.

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