Fig. 14 shows the apparent sky-plane distribution for 3 m diameter bolides 1 day before impact. These small objects (e.g. 1–20 m) are visible for only a short time before impact and their apparent brightness is strongly affected by the phase angle so that they can only be detected near opposition. The location of 2008 TC3 three days before impact is clearly within the PS1 opposition field. PS1 would have detected 2008 TC3 since it was brighter than V = 22.7 mag (assuming H = 30.4 and G = 0.15) for 4–5 days before impact (with V = 18.9 mag at discovery 1 day before the impact) and the sky-plane motion was below the PS1 trailing cut-off of 12/day.