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Many manuscripts may have simply been disposed of as waste materials.
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This is confirmed by the spectroscopy of its surface, which identified water ice as the dominant surface material.A small amount of an unidentified dark material is present as well.The high albedo indicates that the surface of Tethys is composed of almost pure water ice with only a small amount of a dark material.The visible spectrum of Tethys is flat and featureless, whereas in the near-infrared strong water ice absorption bands at 1.25, 1.5, 2.0 and 3.0 μm wavelengths are visible.

Tethys orbits Saturn at a distance of about 295000 km (about 4.4 Saturn's radii) from the center of the planet.

Tethys has been approached by several space probes including Pioneer 11 (1979), Voyager 1 (1980), Voyager 2 (1981), and multiple times by Cassini since 2004.

Once Mimas and Enceladus were discovered in 1789, the numbering scheme was extended to Saturn VII by bumping the older five moons up two slots.

The surface of Tethys is one of the most reflective (at visual wavelengths) in the Solar System, with a visual albedo of 1.229.

This very high albedo is the result of the sandblasting of particles from Saturn's E-ring, a faint ring composed of small, water-ice particles generated by Enceladus's south polar geysers.