Wind and C(2)(N) profiling by single-star scintillation analysis

Wind profiling based on the optical beam intensity statistics in a turbulent atmosphere

Reconstruction of the wind profile from the statistics of intensity fluctuations of an optical beam propagating in a turbulent atmosphere is considered. The equations for the spatiotemporal correlation function and the spectrum of weak intensity fluctuations of a Gaussian beam are obtained. The algorithms of wind profile retrieval from the spatiotemporal intensity spectrum are described and the results of end-to-end computer experiments on wind profiling based on the developed algorithms are presented. It is shown that the developed algorithms allow retrieval of the wind profile from the turbulent optical beam intensity fluctuations with acceptable accuracy in many practically feasible laser measurements set up in the atmosphere.

First retrieval of vertical profiles of turbulence characteristics and horizontal wind velocity from solar transmission measurements at 212 and 405 GHz

We report on the investigation and successful application of vertical profiling of the structure parameter C2m and of the outer scale L0 of absorption fluctuations and of the horizontal wind velocity (vector) during daytime by the analysis of solar transmission measurements. The method is relatively simple and straightforward so that the presented (or a similar) technique could be used in the routine remote sensing of daytime C2m, L0, and wind profiles. It requires multiple beams pointing in different directions at the Sun. The retrieved profiles are consistent with the current knowledge of atmospheric physics. Simultaneous in situ wind velocity measurements agree with the retrieved wind velocity in the lowest 100 m above ground within the measurement uncertainties of less than +/-2 m/s. The derived values of C2m at 200 m above ground are in good agreement (within a factor of 1.5) with the findings of an earlier investigation at the same test site. Finally, it is shown that irradiance fluctuations of millimeter and submillimeter waves are dominantly affected by humidity fluctuations, even at a dry and elevated site.

Wind-flow measurement over the Subaru Telescope

Wind flows over the 8.2-m Subaru Telescope at Mauna Kea in Hawaii were analyzed with a correlation method. Three or four wind flows were detected from our measurements. Spatial and temporal resolution of the wind-flow analysis across the 8.2 m pupil were investigated experimentally. A three-dimensional spatiotemporal-frequency analysis was also applied to the wind-flow data.

Polychromatic scintillation

A formula to compute the index of stellar scintillation detected with a finite spectral bandpass and with arbitrary aperture is derived in the limit of weak perturbations. It also applies to differential scintillation (relative fluctuations of light intensity in a pair of apertures), where the effect of finite bandpass turns out to be significant. The new formula is used for measurements of free-atmosphere seeing and low-resolution turbulence profiles with concentric-ring apertures.

Application of an exclusively binarized correlation-calculation method to wind velocity measurement by use of stellar scintillation patterns

An exclusively binarized method for the correlation calculation of image processing is presented with application to velocity measurements. The exclusively binarized correlation-calculation method is capable of determining the peak position of the correlation even with a small number of random-pattern images. Because the velocity is deduced from the movement of the correlation-peak position within a time interval, the method is suitable for the velocity measurement of random patterns. The method is applied to the measurement of the upper-atmospheric wind velocity by use of stellar scintillation patterns.

Temporal coherence of individual turbulent patterns in atmospheric seeing

We used a variation of the generalized scidar (scintillation detection and ranging) technique to examine the temporal coherence of turbulent patterns at different altitudes in the atmosphere above Palomar Observatory. This enables us to test the validity of a frozen turbulence hypothesis in the local reference frame of the moving atmosphere. The data set analyzed here contains three turbulent patterns, each at a different altitude, which remain internally coherent over time scales of 0.28-0.41 s. This measurement is significant, because it is made on a 5-m aperture, allowing moving patterns to be tracked over time scales longer than their own lifetimes.

Whole atmospheric-turbulence profiling with generalized scidar

Statistical analysis of stellar scintillation on the pupil of a telescope, known as the scidar (scintillation, detection, and ranging) technique, is sensitive only to atmospheric turbulence at altitudes higher than a few kilometers. With the generalized scidar technique, recently proposed and tested under laboratory conditions, one can overcome this limitation by analyzing the scintillation on a plane away from the pupil. We report the first experimental implementation of this technique, to our knowledge, under real atmospheric conditions as a vertical profiler of the refractive-index structure constant C (N)(2) (h). The instrument was adapted to the Nordic Optical Telescope and the William Hershel Telescope at La Palma, Canary Islands. We measure the spatial autocorrelation function of double-star scintillation for different positions of the analysis plane, finding good agreement with theoretical expectations.

Interferometric seeing measurements on Mt. Wilson: power spectra and outer scales

We have measured power spectra of atmospheric phase fluctuations with the Mark III stellar interferometer on Mt. Wilson under a wide variety of seeing conditions. On almost all nights, the high-frequency portions of the temporal power spectra closely follow the form predicted by the standard Kolmogorov-Tatarski model. At lower frequencies, a variety of behavior is observed. On a few nights, the spectra clearly exhibit the low-frequency flattening characteristic of turbulence with an outer-scale length of the order of 30 m. On other nights, examination of individual spectra yields no strong evidence of an outer scale less than a few kilometers in size, but comparison of the spectra on different interferometer baselines shows a saturation of the spatial structure function on long baselines. This saturation is consistent with the assumption of an outer-scale length similar to that derived for the nights when low-frequency flattening of the spectra is clearly seen. We discuss possible explanations of this behavior and conclude that power spectra from a single interferometer baseline are a poor diagnostic for the effective outer scale compared with multiple-baseline spectra.

Structure function C(2)(n) profiling by two-color stellar scintillation with atmospheric dispersion

Two-color single-star scintillation cross-correlation functions are estimated involving the use of two wavelength filters centered on 409 and 800 nm. From these estimations and using the atmospheric dispersion theory already proposed by Hudgin, turbulent layer heights are measured. Then, vertical C(2)(n)Deltah profiles are obtained every 2 min 45 sec using the slowly decreasing elevation of Sirius. The coherence with another method proves its interest. Furthermore, when the zenith angle of the observed star exceeds ~70 degrees , turbulence heights smaller than 800 m (otherwise unattainable with stellar scintillation measurements) can be detected with a vertical resolution of 300 m.

Atmospheric optical turbulence profiling by stellar scintillometers: an instrument evaluation experiment

We operated two identical atmospheric optical turbulence profiling instruments over a period from 15 Mar. to 20 Apr. 1985 at the Air Force Maui Optical Station on Mount Haleakala. The daily average results of looking along common lines of sight through identical atmospheres show systematic differences at lower altitudes and near agreement at higher altitudes. We suspect that spatially nonuniform PMT photocathode responses and incompletely subtracted background noise could significantly affect the turbulence values measured at lower altitudes and contribute to the low altitude systematic differences. The average results of looking along two different lines of sight through different regions of the atmosphere show additional systematic differences at higher altitudes, which are not due to instrument bias. We believe these to be due to genuine horizontal structure in the distribution of atmospheric optical turbulence above the 10-km level.