|System:||Cassurindui - All bodies|
|Distance to Sol:||163.39 ly|
|Spectral Class:||T - Not Scoopable|
|Distance To Arrival:||5,405 ls|
|Luminosity Class:||V - Main-sequence star (dwarf)|
|Age:||12,820 Million years|
|Surface Temperature:||1,027 K|
|Orbital Period:||211.7 D|
|Semi Major Axis:||0.28 AU|
|Orbital Inclination:||12.47 °|
|Arg Of Periapsis:||198.59 °|
Class T dwarfs are brown dwarfs with a surface temperature between 700 and 1,300 K. They are sometimes known as Methane Dwarfs due to the prominence of methane in their composition. They are on the borderline between what might be considered a very large gas giant planet and a star.
The term dwarf star refers to a variety of distinct classes of stars. The term was originally coined in 1906 when the Danish astronomer Ejnar Hertzsprung noticed that the reddest stars - classified as K and M in the Harvard scheme - could be divided into two distinct groups. They are either much brighter than the Sun, or much fainter. To distinguish these groups, he called them "giant" and "dwarf" stars, the dwarf stars being fainter and the giants being brighter than the sun.