This is based on the topography map from the Dr. Schenk's blog, rendered with MATLAB R2016a. When the Voyager 2 probe flew by the Uranian System, it took very few pictures of Miranda. About a half of its surface is known, so the topography that can be deduced from photometry is reduced to a little patch. The rest was filled by interpolation.
The file's names explained: name_1_x_10_y.stl is 1 : x * 10y. So _1_6_10_7 is 1:600000000 or one in 60 million.
Like most of the Uranian System, only Miranda's southern hemisphere is known because at the time of the Voyager 2 flyby, the south of the system was pointing toward the Sun. Like most of the icy moons of the Solar System, its surface show signals of geologic activity. It is the smallest of the principal moons of Uranus, about the size of Mimas or Enceladus, of the Saturnian System.
Orbital period: 1.413 d.
Composition: Icy body.
Density: 1.2 g/cm3.
Dimensions: 480 km × 468.4 km × 465.8 km
Model scale: 1:1x107 (5cm) 1:4x106 (12cm)