Wide Field Wavefront Sensing
  When observing from the ground one has to deal with the turbulence from the atmosphere and the turbulence caused by the telescope's surroundings. In order to find the best sites for future solar telescopes and develop multi-conjugate adaptive optics (MCAO) for them, the contributions to seeing have to be characterized for heights up to at least 12 km above the telescope.   This characterization is done with a method that measures differential image displacements using several subapertures. By extending the ordinary DIMM- and S-DIMM-methods to measure displacements at different field angles, the height distribution of seeing can be measured. This extended method is called S-DIMM+, where the letter S denotes the use of the Sun as source and the + signifies that it is an extension of the former methods.   Observations are made with the Wide Field Wavefront Sensor (WFWFS) mounted at the Swedish 1-m Solar Telescope (SST) at La Palma. The results from these measurements are compared with the Shadow Band Ranger (SHABAR), also mounted on the SST.   The first results of these comparisons show good correlation between the two instruments for heights up to 500 m. Results from the WFWFS also show that the dominant seeing at this site comes from layers close to the ground and at high altitude and that Fried's parameter, r_0, is larger than 40 cm for the intermediate layers. 
Maria Tham
astro-ph.SR astro-ph.IM physics.optics