Astroclimatic conditions characterize the quality of an astronomical site. The Terskol Observatory was founded over 42 years ago in 1980. The astronomical site (coordinates 43◦16′29′′ N,42◦30′03′′ E) is located about 10km from Mt. Elbrus in the northern Caucasus Mountains. The paper presents the results of an analysis astroclimatic parameters such as total cloud cover, precipitable water vapor, and wind speed at a level of 200hPa. above the Terskol Observatory using atmospheric ERA5 Reanalysis data from the European Center for Medium-Range Weather Forecast, as well as acoustic station data and optical measurements. The study of seasonal changes in the astroclimate parameters: wind speed at a level of 200mbar, as a parameter of applicability of adaptive optics (AO), altitude distribution of wind speed, which determines the requirements for AO performance, moisture content for assessing the possibility of AO operation in the IR range. The statistics of the seeing for 2023 are also provided.
The paper discusses the issues of choosing a site for a new large ground-based radio telescope. One of the most important characteristic that determines the optical atmospheric thickness, in particular, the precipitable water vapor in the atmosphere, is considered. We estimated reference precipitable water vapor height scale in the atmosphere at a number of reference sites within region perspective for creation of ground-based radio telescope. Using the method for correction of precipitable water vapor values, we showed that the sites in the vicinity of the lake Karakul are suitable for placement of large ground-based radio telescope.
This paper is aimed at finding suitable sites for a large ground-based millimeter/submillimeter telescopes. We discuss the most promising regions in the world in terms of low values of precipitable water vapor. A separate issue is the regions with low values of precipitable water vapor within Russia, China and Uzbekistan.
The paper describes the results of measuring the structural parameters of optical turbulence for different altitudes in the atmosphere above the Large Solar Vacuum Telescope of the Baikal Astrophysical Observatory. The structural parameters of optical turbulence we estimated from the measurement data of the Shack-Hartmann sensor for individual atmospheric layers by applying the analysis of wavefront distortions in crossed optical beams. To estimate the structural parameters of optical turbulence, we propose an approach based on statistical averaging normalized dimensionless characteristics of turbulence, the Fried parameter and averaged profile of optical turbulence at a given site.
For adaptive optics systems, one of the fundamental task to be decided is determination of the frequency characteristics of wavefront distortion variations in the focus of a ground-based solar telescope. It is a classical approach to use the atmospheric coherence time related to the vertical distribution of turbulence and wind speed. Besides, small-scale variations of wavefront induced due to turbulence for understanding the large-scale structure of atmospheric turbulence it is important to estimate frequencies of large-scale (low-frequency) turbulent components. The paper presents the results of the analysis of the frequency characteristics of wavefront distortion variations recorded in the adaptive optics system of the Large Solar Vacuum Telescope of the Baikal Astrophysical Observatory.
The paper presents the first results of comparative study of the optical turbulence at the sites of the Fuxian Lake Solar Observatory (FSO) and the Baikal Astrophysical Observatory (BAO). The distributions of the probability of the Fried parameter estimated from Shack-Hartmann wavefront sensor measurements are analyzed.
A multi-cascade adaptive optical system for imaging and image stabilization for the Large Solar Vacuum Telescope is described. This system was created in 2017 by specialists of the V.E. Zuev Institute of Atmospheric Optics SB RAS, Tomsk, with the technical support of the Institute of Solar-Terrestrial Physics SB RAS, Irkutsk. The system has been tested at the Large Solar Vacuum Telescope (Baikal Astrophysical Observatory) and demonstrated its efficiency. Along with the first cascade of adaptive image stabilization by a tip-tilt corrected mirror, this system employs the second imaging cascade based on correction with a flexible mirror controlled by a specialized wavefront sensor, as well as the third cascade for real-time post-detector processing of video camera frames. Reliable experimental data confirming the efficiency of the multi-cascade adaptive system for image formation and stabilization have been obtained. Three highrate digital video cameras recording simultaneously digital images with rates from 300 to 980 frames per second were used to test the system. The mirror correcting wavefront tilts and operating in a closed optical feedback loop was controlled by the specially developed software including the fast correlation tracking algorithm. The post-detector digital imaging was performed with a special software for processing of video camera frames in real time with the use of modern high-speed parallel algorithms based on the Intel MKL and IPP libraries.
In the paper we review the widefield adaptive optics systems including GeMS, LINC-NIRVANA, MAD, `Imaka, CANARY, RAVEN, MCAO installed on such telescopes as VTT, GREGOR, NST and DST. Review is relevant for the design Russian project of the Large solar telescope LST-3. The heights of the optical conjugation of the adaptive optics elements with turbulence layers as well as peculiarities in the MCAO systems` design are compared for different sites.
In the paper we discuss the results of the measurements of the nighttime optical turbulence parameters performed by the mobile astronomical telescope MEADE at the Large solar vacuum telescope of the Baykal Astrophysical Observatory site. Measurements have been performed in the clear sky, when the surface-layer wind speed < 2 m/sec. The studies of the optical turbulence in the nighttime are relevant for improving our knowledge about mechanisms of the turbulence generation and dissipation at this site. It is known that diurnal variations in the energy and momentum fluxes, turbulence strength are modulated by topography. Regional peculiarities of the energetic structure of atmospheric fluctuations (including optical turbulence) is the basis for development of the parametrization methods.
We propose the concept of the new SCIDAR-based method to determine the characteristics of the atmospheric turbulent layers including its heights and strength. In this paper we discuss the possibility of the estimating of the heights of the atmospheric turbulent layers from the vertical profiles (along line of sight) of dimensionless characteristics of turbulence. The method is based on the analysis of the scintillation in crossed optical beams (with temporal lag) on the spaced subapertures of single Shack-Hartmann sensor (with field of view of order 40 arc.sec.) conjugated with the aperture.
The spatial analysis of the wavefront distortions registered by the Shack-Hartmann sensor of the adaptive optics (AO) system of Large solar vacuum telescope have been performed. In the paper the results of analysis of spatial structure of the wavefront within the field of view ~35 arcsec are discussed. It is shown that the wavefront distortions formed within the field of view ~35 arcsec are not random. There are the repetitive hills of spatial crosscorrelation functions in the field of view at the same intervals for different space subapertures. It is shown that spatial crosscorrelation functions do not contain pronounced kernel for finding the exact position of the atmospheric layer contributing to significant distortions in the wavefront incident on the telescope aperture.
To restore the height profiles of the atmospheric turbulence we used the analysis of the spatial crosscorrelation functions of wavefront distortions registered by the Shack-Hartmann sensor of the adaptive optics (AO) system of Large solar vacuum telescope. In the paper the results of analysis of spatial crosscorrelation function within the field of view ~35 arcsec are discussed. It is shown that the wavefront distortions formed within the field of view ~35 arcsec are not random. There are the repetitive hills of spatial crosscorrelation functions in the field of view at the same intervals for different space subapertures. It is shown that spatial crosscorrelation functions do not contain pronounced kernel for finding the exact position of the atmospheric layer contributing to significant distortions in the wavefront incident on the telescope aperture.
The paper discusses the problem of finding solar-terrestrial relations. The features of the possible optical screen influence of the atmosphere on the propagation of solar radiation in different phases of solar activity are considered. Changes of the scattered radiation at different heights are analyzed separately. Considering the small amplitudes of fluctuations in the level of diffuse radiation due to solar activity, the possible causes of disynchronization in changes in Wolf numbers and diffuse radiation are discussed. The concept of the work is modulation of incoming solar energy may be due to changes in the optical properties of the earth's atmosphere, including its transparency.
One of the approach to calculate the characteristics of the air refractive index fluctuations along line of sight for multiconjugated adaptive optics is based on the triangulating the wavefront distortions or/and scintillation amplitudes analysis. The description of the experiments aimed to measurements of the wavefront distortions and scintillation fluctuations is given. The scheme for recovering the optical distortions (wavefront) at the different heights is discussed. The results of changes of the wavefront distortions measured by Shack-Hartmann sensor in the spaced regions of images are discussed. The results obtained may be used for estimation of the real amplitudes of the wavefront distortions in crossed optical beams at the different heights using such method as SDimm+[ 5].
The article proposes a design of sensor of optical distortions in a wide field of view for the adaptive optical system of the Large Solar Vacuum Telescope. The calculation of the optical scheme of the sensor based on the use of two wavefront sensors was performed. The working field of view of the adaptive system with an additional sensor for determining the distortions of the wavefront is 120 arc sec. Adjusting the field of view of each Shack-Hartmann sensor up to 30 arc sec is provided by field diaphragms. It is shown that for the used second imager, the quality of subimages remains high, the standard deviation is λ /80.
We study seasonal variations of the vertical distribution of wind speed at the Baikal Astrophysical Observatory (BAO) using NCEP/NCAR Reanalysis data base for development of adaptive optical system of Large Solar Vacuum Telescope (LSVT). The statistics of wind speed including mean and median profile, the first and third quartiles are calculated. Also we analyzed seasonal variations of wind speed on the pressure level 200-mbar, as parameter for estimation of suitable of the site for adaptive optics and level of atmospheric optical turbulence.
The work discusses the optical turbulence structure and dynamics at the Baykal Astrophysical Observatory (BAO) site. The characteristics of the optical turbulence including Fried radius, isoplanatic angle are analyzed. Estimates of the variations of the height profiles of the air refraction index turbulent fluctuations at the Baykal Astrophysical Observatory are given. Using the mean height profile of the structure characteristic of the air refraction index turbulent fluctuations, diurnal variations of the Fried radius at the BAO site are estimated.
The Baikal Astrophysical Observatory of Institute Solar- Terrestrial Physics of Siberian Branch of Russian Academy Sciences is located at an altitude of about 700 meter above sea level on the shore of Lake Baikal, Russian Federation. Large Solar Vacuum Telescope (LSVT) is the main telescope of the Baikal Astrophysical Observatory. We develop models of vertical profile of atmospheric turbulence (the refractive-index structure constant) and wind speed at the BAO for adaptive optical system design of LSVT. We also presented vertical profile wind speed and the refractive-index structure constant is obtained from NCEP/NCAR Reanalysis base.
The optical turbulence characteristics statistics including "seeing", Fried radius, wind speed height profiles are discussed. Distribution of the mean Fried radius obtained from the data of image motion measurements by the Brandt sensor is given. Also, the Fried radius values calculated from the Shack-Hartmann data are given. Using the height profile of the structure characteristic of air refractive index fluctuations obtained from spectral multiscale turbulence model the results of the Fried radius simulations from micrometeorological mast measurement data given.
The work discusses the spatial scales of atmospheric optical distortions including the outer scale of turbulence and the Fried radius. It is assumed that the energy spectrum of atmospheric turbulence is not limited strictly [6] and the outer scale is considered in application to astronomical telescopes. In the case when the telescope diameter is larger or comparable with the outer scale the optical distortions substantially differ from the results of the Kolmogorov model. For a given diameter it is possible to introduce a certain spatial scale at distances larger than the size of which the refractive index fluctuations no longer have a significant effect on the quality of astronomical images. Estimates of the outer scale of turbulence are reported for both a atmospheric layer from 0 up to 20 km and surface layer.
The dynamics of turbulent characteristics including air index refraction vertical variations as well as effective turbulent velocity important for the functioning of the Large solar vacuum telescope (LSVT) adaptive optics system is considered. Long-term changes of the effective turbulent velocity and Fried radius in the atmospheric layer from 0 to 20 km are estimated using model of turbulence taking into account the shape of the energy spectrum over a wide range of spatial and temporal scales. The possible experimental local model of Fried radius changes is discussed for the Large solar vacuum telescope site.
According to the work plan for the RSF project, during 2016 measurements were taken in all seasons of the year: February, April, May, August and October. With the use of the whole set of equipment of the stand on the BSVT, the task was set to work out methods for recording and correcting the distortions of the phase of optical radiation passing through a layer of turbulent atmosphere. Complex on-site meteorological observations were organized and conducted at the site of the BSVT. Observations were carried out with the aim of developing and improving the local computational model of turbulent characteristics in the entire thickness of the active atmosphere in the "optical turbulence" range, including the surface layer. As the initial meteorological information for calculations, the model uses two-level data of pulsating observations of temperature and wind speed at the BSVT site, as well as current NCEP/NCAR archival data for the period from 1948 to 2015.
The results of optical measurements of the quality of astronomical seeing on the Large solar vacuum telescope (LSVT) in spring and summer are shown. It is noticed that in the summer measurements, the quality of vision is higher on average 2.5 times than in the spring. Information on the seasonal variability of the astronomical quality of vision can be useful in the planning of scientific experiments for the LSVT, as well as to improve the performance of existing adaptive system
The features of air index refraction vertical variations up to 20 km at the Large solar vacuum telescope site are discussed. The possible local model of air index refraction fluctuations are supposed at the Large solar vacuum telescope site.
The problem of selection of sites for modern telescopes which are characterized by favorable conditions for astronomical observations is discussed. A number of new sites to telescope construct with separate mountain peaks (above 2 km) as well as high image quality (astronomical seeing) and low level of cloud are pointed.
In this article, we describe the development of the newest adaptive optics system for the Big Solar Vacuum Telescope of the Baikal Astrophysical Observatory. This system is a result of collaboration between VE Zuev Institute of Atmospheric Optics SB RAS, Tomsk, and Institute of Solar-Terrestrial Physics SB RAS, Irkutsk. The system includes two active mirrors for the correction: domestic tip-tilt and bimorph deformable (Active Optics NightN Ltd.), and separate wavefront sensors (WFS). A correlation S-H wave-front sensor is based on a Allies Prosilica GX-1050 GigE camera with speed of 309 Hz and frame size of 1248x1248 pixels. A personal computer is used for bimorph deformable mirror image processing. The mirror was successfully used during the 2010–2014 observing seasons. The system developed is capable of correcting up to 35 modes, thus providing diffraction limited images at visible wavelengths.
The estimations of the Fried parameter according to micrometeorological and optical measurements in the atmospheric surface layer in the area of l. Baikal, Baikal astrophysical Observatory (BAO). According to the archive of NCEP/NCAR Reanalysis data obtained vertical distribution of temperature pulsations, and revealed the most pronounced atmospheric layers with high turbulence. It is established that the values of the fried parameter at the location of the BAO are in the range from 1.5 to 5.5 cm in inter, the atmospheric coherence radius is characterized by low values of the Fried parameter. Turbulyzed atmospheric layers of the atmosphere located at an altitude of about 2.5 km and 11.5 km above the observatory, respectively. The average values of the fried radius is 4.6 cm.
The criteria image qualities based on wave front aberration caused by atmospheric turbulence using in adaptive optics are summarized. Atmospheric turbulence profile for Big Solar Vacuum Telescope (BSVT) observatory is obtained based on satellite date. On this based the development of adaptive optics systems of BSVT are discussed.
The estimations of the fried parameter according to micrometeorological and optical measurements in the atmospheric surface layer in the area of lake Baikal, Baikal astrophysical Observatory. According to the archive of NCEP/NCAR Reanalysis data obtained vertical distribution of temperature pulsations, and revealed the most pronounced atmospheric layers with high turbulence. A comparison of astronomical conditions vision in winter and in summer. By the registration of optical radiation of the Sun with telescopes, ground-based there is a need to compensate for the effects of atmospheric turbulence. Atmospheric turbulence reduces the angular resolution of the observed objects and distorts the structure of the obtained images. To improve image quality, and ideally closer to angular resolution, limited only by diffraction, it is necessary to implement and use adaptive optics system. The specificity of image correction using adaptive optics is that it is necessary not only to compensate for the random jitter of the image as a whole, but also adjust the geometry of the individual parts of the image. Evaluation of atmospheric radius of coherence (Fried parameter) are of interest not only for site-testing research space, but also are the basis for the efficient operation of adaptive optical systems 1 .
It is shown that atmospheric turbulence is not suppressed completely in strongly stably stratified conditions when Richardson's number exceeds its critical value. It is worth to note that airflow is laminar according classical ideas of the turbulence theory when Richardson's number values are supercritical. It is shown that in the stably stratified atmospheric surface layer under conditions of large vertical temperature gradients and low wind speeds, atmospheric turbulence is often characterized by intermittent structure and in some parts of space intensity of fluctuations can reach high values. The results of experimental investigations of optical instability conducted out along the horizontal path in the stably stratified atmospheric surface layer are discussed.
The results of investigations of small-scale atmospheric turbulence are discussed. The differences of the shapes of smallscale atmospheric turbulence spectra in the free atmosphere and the boundary layer are in the focus of the paper. The obtained results may allow us to estimate the characteristics of small-scale (optical) atmospheric turbulence parameters and adaptive optics systems.
The results of investigations of vertical profile of turbulent inhomogeneities of the air refractive index using NCEP / NCAR Reanalysis data are discussed in this paper. Model used for calculations is based on the spectral features of atmospheric turbulence characteristics in a wide range of scales. The differences of the shapes of small-scale atmospheric turbulence spectra in the free atmosphere and the boundary layer are in the focus of the paper. The obtained results may allow us to estimate characteristics of turbulent and, thus, parameters of adaptive optics systems.
Energy spectra of wind speed fluctuations and temperature fluctuations are calculated at altitudes between 2 and 301 m
for the period from January 1, 2008 to 31 December, 2008 by using results of numerical analysis of high-altitude
meteorological mast data. Comparison of the shape of the calculated spectra with known shapes has confirmed presence
of two basic regions of wavenumbers with an approximate "-3" dependence and "-5/3" dependence. The result obtained
has been used for estimating of high-frequency characteristics of atmospheric turbulence using network meteorological
data.
Access to the requested content is limited to institutions that have purchased or subscribe to SPIE eBooks.
You are receiving this notice because your organization may not have SPIE eBooks access.*
*Shibboleth/Open Athens users─please
sign in
to access your institution's subscriptions.
To obtain this item, you may purchase the complete book in print or electronic format on
SPIE.org.
INSTITUTIONAL Select your institution to access the SPIE Digital Library.
PERSONAL Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.