2008A&A...477..671T

After proposing a new method of deriving the atmospheric time constant from the speed of focus variations (Kellerer & Tokovinin, 2007A&A...461..775K), we now implement it with the new instrument, FADE. FADE uses a 36-cm Celestron telescope that is modified to transform stellar point images into a ring by increasing the central obstruction and combining defocus with spherical aberration. Sequences of images recorded with a fast CCD detector are processed to determine the defocus and its variations in time from the ring radii. The temporal structure function of the defocus is fitted with a model to derive the atmospheric seeing and time constant. We investigated by numerical simulation the data reduction algorithm and instrumental biases. Bias caused by instrumental effects, such as optical aberrations, detector noise, acquisition frequency, etc., is quantified. The ring image must be well-focused, i.e. must have a sufficiently sharp radial profile, otherwise, scintillation seriously affects the results. An acquisition frequency of 700Hz appears adequate. FADE was operated for 5 nights at the Cerro Tololo observatory in parallel with the regular site monitor. Reasonable agreement between the results from the two instruments has been obtained.