Each step of the lucky photometry process will be explained, as shown in the figure above. Let us assume that we have a frame (image) from three reference stars and one target. The first step is acquiring optimum aperture (OA) to extract the flux from each reference star in each frame, as we mentioned before. Then, the ratio of the flux of each reference star to every other reference star within a frame is calculated. This creates a pattern which describes the photometric atmospheric properties for that given frame. Once the ratio pattern has been calculated for each frame, a selection process is required to select which frames have common photometric properties. The selection process finds the most common pattern and uses it as a discriminator to reject frames from the process. After that, the selected frames are used to calculate the final lightcurve.