tokens: 11 shows the relation between the position of a meteor in the image and the estimated errors in radiant. Since the pointing of the camera and the radiant of the simulated shower was set to the local zenith, the angular separation between the radiant and position of a meteor in the image corresponds to the elevation angle of the meteor. The median for the estimated errors in the speed for these 161 meteors was 0.12 km s −1 . The median of the estimated errors for 192 un-shuttered synthetic meteors, for which the residuals in magnitude Δmag were 0.5 m, was +0.01 m with a median deviation of 0.02 m. Fig. 11. Plot showing the relation between the angular separation and the estimated uncertainties in right ascension (filled circles) and declination (open circles). 5.2. Real meteor data We applied our software to three hours of double-station SPOSH image data acquired during an observing campaign held in Greece (i.e. at ∼37 ∘ N latitude ) on 12 August 2015 from 23 to 02 UT. The cameras were pointing to the zenith with their x -axis orientated to the north. The baseline between the two sites was 51.5 km. We reduced 177 meteor image pairs and determined their trajectories, velocities and heliocentric orbits. We focus on a 20 × 20 ∘ area centred at RA = 46 ∘ , Dec = 58 ∘ , close to the nominal radiant position of the Perseids (Fig. 12 ). To distinguish between Perseid and non-Perseid meteors, we performed a classification based on radiant position and speed as follows: 132 meteors were found to radiate from within this area. We determine the radiant of the Perseid shower as the median value of these radiants: RA = 45.96 ∘ and Dec = 57.77 ∘ . We assume that most of the meteors are Perseids and we find the 1 σ uncertainty in RA and Dec to be 3.29 ∘ and 2.27 ∘ , respectively. The geocentric speeds V G have a median value at 58.97 km s −1 and a median propagated error of 1.21 km s −1 (Fig. 13 ). We classify all meteors with speeds closer to this median speed than four times the median propagated error, as Perseids. In this way, we identified 71 meteors belonging to the Perseids meteor shower (Fig. 12 ). Their median speed V G was found to be 59.58 km s −1 with a median deviation of the observed uncertainties of 0.48 km s −1 . Statistical properties are given in Table 2 . As the aim of our example is to demonstrate the successful usage of our software using real data, we neglected the effect of radiant drift. Fig. 12. Geocentric radiants of 132 meteors originating close to the Perseid radiant. The ellipse defines the area occupied by Perseids. Meteors classified as Perseids according to their speed are shown as filled circles (•). All other meteors not meeting the requirements to be classified as Perseids are shown as open circles (∘). Fig. 13. Speed distribution of 132 meteors originating from an area close to the Perseid radiant. The dashed line shows computed median speed of 59.58 km s −1 . The bars in dark grey show the distribution of speeds for
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