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The strength and vertical distribution of atmospheric turbulence is a keyfactor determining the performance of optical and infrared telescopes, with andwithout adaptive optics. Yet, this remains challenging to measure. We describea new technique using a sequence of short-exposure images of a star field,obtained with a small telescope. Differential motion between all pairs of starimages is used to compute the structure functions of longitudinal andtransverse wavefront tilt for a range of angular separations. These arecompared with theoretical predictions of simple turbulence models by means of aMarkov-Chain Monte-Carlo optimization. The method is able to estimate theturbulence profile in the lower atmosphere, the total and free-atmosphereseeing, and the outer scale. We present results of Monte-Carlo simulations usedto verify the technique, and show some examples using data from the second AST3telescope at Dome A in Antarctica.

Multi-star Turbulence Monitor: A new technique to measure optical turbulence profiles