A correlation program was also written that takes the output produced by each station, finds the meteors that were visible on at least two stations, and then runs a trajectory analysis and produces a quick summary of each event. For example:
The two plots on the left show where the event was detected. The one on the top shows the zenith and azimuth angles relative to each site. The Q* angle is a measure of how good the solution is, although 'good' depends a lot on camera pixel-scale. The plot on the bottom shows the event over the camera network's region.
The two plots in the middle show the trail offset and heliocentric orbits. The trail offset plot (on the top) will show if any deceleration exists. If so, the line will curve to the left as the meteor travels to lower heights. The orbit plot (on the bottom) shows the path of the original meteoroid through space. You can see the Sun at the centre, and the orbits of the four terrestrial planets.
The two plots on the right show the measured light curve and the trajectory fit residuals. The measured light curve (on the top) is integrated in time to give an estimate of the photometric radiant energy. Assuming a luminous efficiency then gives the meteoroid mass. The residual plot (on the bottom) can give an idea of the fit precision.
In addition to these plots, the software also produces a summary list each day, which can help in recognising shower outbursts. This list also contains the meteor speed, beginning and end heights, and a list of which camera stations the meteor was seen at.