## 1 Introduction  
Multi-conjugate adaptive optics (MCAO) [1; 2; 3] is attractive for the large-field-of-view high-resolution imaging requirements of astronomical observations, which heavily rely on the intensity distribution information of turbulence. Therefore, the intensity distribution of atmospheric optical turbulence is essential prior information for the MCAO system. For a ground-layer adaptive optics (GLAO) [4] system, the intensity and distribution of turbulence are fundamental for analyzing performance. Measuring the atmospheric optical turbulence intensity and its distribution information is necessary. Additionally, the intensity and distribution of atmospheric turbulence positively impact the development of future intelligent adaptive optical systems and the post-reconstruction of astronomical images. There are currently many methods for measuring atmospheric turbulence in the visible and infrared bands, such as SCIntillation Detection and Ranging (SCIDAR [5]), Stereo-SCIDAR [6; 7; 8], SLOpe Detection and Ranging (SLODAR [9; 10; 11; 12]), the Multi-ApertureScintillation Sensor (MASS [13; 14]), the Multiple-Aperture Seeing Profiler (MASP [15; 16]), the Ring-Image Next-Generation Scintillation Sensor (RINGSS [17]), the Differential Image Motion Monitor (DIMM [18]), Solar DIMM(SDIMM [19; 20; 21]), S-DIMM+ [22; 23; 24], and the Profiler of the Differential Solar Limb (PDSL [25]). Most of these numerous algorithms serve the site selection process of large-aperture telescopes by monitoring the atmospheric turbulence at the site for a long time to obtain a comprehensive evaluation of the turbulence situation at the site. Most methods have developed into independent small instruments for easy installation at different sites. However, atmospheric turbulence is variable, and atmospheric turbulence at different times may be completely different. When operating the large-aperture telescope and MCAO system, we need to detect the intensity and distribution of atmospheric turbulence in real time to better optimize the MCAO system parameters. Under the conditions of large-aperture telescopes and MCAO systems, the use of additional small portable devices is unnecessary. It is feasible to directly use large-aperture telescopes with wavefront sensors to detect atmospheric turbulence, and various methods have been tested, such as MASS and Stereo-SCIDAR [8], based on scintillation for nighttime observations, and SLODAR [11] and S-DIMM+ [22; 23; 24] for daytime measurements. These two algorithms are feasible for use in the turbulence measurement system on the 1-m New Vacuum Solar Telescope (NVST). Both SLODAR and S-DIMM+ originated from the DIMM method proposed in 1990 [18], which is a widely employed method for measuring the intensity of atmospheric optical turbulence. Based on the Kolmogorov turbulence theory, the relationship between the wavefront variance of atmospheric optical turbulence and the atmospheric coherence length could be established. By measuring wavefront fluctuations of a target passing through atmospheric optical turbulence using two apertures spaced at a predetermined distance, the atmospheric coherence length can be determined. This method has become the predominant approach for quantifying the intensity of atmospheric optical turbulence at astronomical sites. The SLODAR or S-DIMM+ method needs wavefront information from different guide stars (regions) for measuring the intensity and distribution of atmospheric turbulence. The SLODAR method employs slope correlation to achieve layered detection of atmospheric optical turbulence, thereby obtaining the intensity distribution information of atmospheric optical turbulence. This method has primarily been used in nighttime astronomical observations and gradually employed in daytime solar observations based on wide-field wavefront sensors [26]. In 2021, [PERSON] et al. [27] incorporated temporal movement to supplement the spatial guide region by utilizing a single field of view of the Shack-Hartmann wavefront sensor.