Automatic Solar Seeing Observations at Mt. Wumingshan in Western China

Song, Tengfei; Wen, Yumei; Liu, Yu; Elmhamdi, A.; Kordi, A. S.; Zhang, Xiaofu; Li, X. B.; Wang, J. X.; Fu, You‐Jun; Cheng, Xiaojin; Xu, Fang-Yu

doi:10.1007/s11207-018-1254-0

Cited by 14 publications

(7 citation statements)

References 19 publications

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“…Saishiteng is enough and comparable to that in Haleakala, Hawaii for Daniel K. Inoue Solar Telescope (DKIST) with a diameter of 4 m (Özişik & Ak 2004). The median value of Fried parameter r 0 in Daocheng, Sichuan is 7.2 cm (Song et al 2018).…”

Section: Discussionmentioning

confidence: 88%

“…The altitude of Ali station is 5100 m above sea level and its logistic is poor and living conditions aretough. The site test survey of Daocheng in the daytime has been done for more than one year (Song et al 2018). The weather station was installed at Nanshan, Ali, and Delingha stations and a precipitable water vapor spectrometer was deployed at Delingha Station.…”

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confidence: 99%

See 1 more Smart Citation

The AIMS Site Survey

Bao,

Wang,

Jing

et al. 2023

Res. Astron. Astrophys.

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This paper reports site survey results for the Infrared System for theAccurate Measurement of Solar Magnetic Field, especially in Saishiteng Mountain, Qinghai, China. Since 2017, we have installed weather station, spectrometer for precipitable water vapor (PWV) and S-DIMM and carried out observation on weather elements, precipitable water vapor and daytime seeing condition for more than one year in almost all candidates. At Mt. Saishiteng, the median value of day time precipitable water vapor (pwv) is 5.25 mm and its median value in winter seasons is 2.1 mm. The median value of Fried parameter of day-time seeing observation at Saishiteng Mountain is 3.42 cm. Its solar direct radiation data shows that solar average observable time is 446 minutes per day and premium time is 401 minutes per day in August 2019.

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Section: Discussionmentioning

confidence: 88%

mentioning

confidence: 99%

The AIMS Site Survey

Bao,

Wang,

Jing

et al. 2023

Res. Astron. Astrophys.

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“…For instance, the solar equivalent of a Differential Image Motion Monitor involves the use of a specially designed telescope with two apertures and a prism to split the light from the solar limb. The seeing condition is then quantified by measuring the differential motion between images of the solar limb (e.g., Beckers 2001;Ozışık & Ak 2004;Kawate et al 2011;Irbah et al 2016;Song et al 2018). Once the setup is installed, the telescope becomes dedicated solely to seeing monitoring.…”

Section: Introductionmentioning

confidence: 99%

Solar Image Quality Assessment: A Proof of Concept Using Variance of Laplacian Method and its Application to Optical Atmospheric Condition Monitoring

So,

Yuen,

Leung

et al. 2024

PASP

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Here we present a proof of concept for the application of the Variance of Laplacian (VL) method in quantifying the sharpness of optical solar images. We conducted a comprehensive study using over 65,000 individual solar images acquired on more than 160 days. Each image underwent processing using a VL image processing algorithm, which assigns a “score” based on the sharpness of the solar disk’s edges. We studied the scores obtained from images acquired at different conditions. Our findings demonstrate that the sharpness of the images exhibits daily trends that are closely linked to the altitude of the Sun at the observation site. We observed a significant degradation in image quality only below a certain altitude threshold. Furthermore, we compared airmass formulae from the literature with our sharpness observations and concluded that the degradation could be modeled as an Image Sharpness Function (ISF), which exhibits similarities to airmass variations. In addition to assessing image quality, our method has the potential to evaluate the optical atmospheric conditions during daytime observations. Moreover, this technique can be easily and cost-effectively applied to archival or real-time images of other celestial bodies, such as the Moon, bright planets and defocused stars. Given that ISF is unique to each location and sensitive to sky conditions, the development of an ISF is not only beneficial for routine observation preparation but also essential for long-term site monitoring.

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“…The DIMM has become the standard equipment for assessing the atmospheric 'seeing' at astronomical sites (Xu et al 2020). DIMMs are used for measurements pointing at not only the stellar image but also the Sun (Kawate et al 2011;Song & Cai et al 2020;Song et al 2018). After that, the S-DIMM+ technique was used to measure daytime turbulence profiles above the 1.6-m New Solar Telescope (NST) with 15 sub-apertures of SHWFS (Shack-Hartmann Wavefront Sensor), which yielded a turbulence profile of 4 layers up to 8 km (Kellerer et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Two-telescope-based solar seeing profile measurement simulation

Wang¹,

Ren²,

Saadetian³

2021

Res. Astron. Astrophys.

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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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Automatic Solar Seeing Observations at Mt. Wumingshan in Western China

Cited by 14 publications

References 19 publications

The AIMS Site Survey

The AIMS Site Survey

Solar Image Quality Assessment: A Proof of Concept Using Variance of Laplacian Method and its Application to Optical Atmospheric Condition Monitoring

Two-telescope-based solar seeing profile measurement simulation

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