When I discovered this, I wondered what it would be like to stand on the surface of the primary of 2006 CH69 and look up at the secondary over the course of their mutual orbit. Using a rough calculation of the size of the secondary body, I determined its apparent size as seen from the surface of the primary, and compared it to the apparent size of the full moon (our 'secondary') as seen from the surface of the Earth (our 'primary').
At the time, I was just learning the ropes of how to make effective visualizations, but I put the following animation together:
On the right you see the apparent size of the secondary - here referred to with its earlier designation of L5c02b - as seen from the surface of the system primary. The animation starts with the system at their most widely separated, with the secondary appearing roughly 1/5th the size of the full moon. At their closest half an orbit later, L5c02b grows to appear over 3 times the size of the full moon on the sky!
I took some liberties with this animation - we don't know what the rotation period of L5c02b is, nor do we know if it has any surface markings, or even if it has a round shape! Future, more detailed studies will be needed to refine our understanding of the system.
I later made an animation showing the motion of six of the systems I studied, as seen from the Earth, and the observations we collected of them over the course of a decade.