Brown dwarfs are typically detected through photometry, which involves measuring their brightness at different wavelengths.

The Wide-field Infrared Survey Explorer (WISE) mission has produced the most comprehensive catalog of brown dwarfs to date.

Brown dwarfs typically have temperatures ranging from 1,000 to 2,000 Kelvin.

Brown dwarfs are often classified as L, T, or Y dwarfs based on their spectral features.

Brown dwarfs typically have masses ranging from 0.01 to 0.08 solar masses.

Brown dwarfs cannot sustain nuclear fusion in their cores due to their low masses.

Gliese 229B was the first brown dwarf to be discovered in 1995.

M dwarfs are not considered brown dwarfs as they are capable of sustaining nuclear fusion.

The oldest known brown dwarf is estimated to be around 10 billion years old.

X-ray astronomy is not commonly used to study brown dwarfs.

Luhman 16 is the closest known brown dwarf to our solar system, located approximately 6.5 light-years away.

Brown dwarfs cannot become neutron stars due to their low masses.

It is estimated that there are approximately 100 billion brown dwarfs in our galaxy.

Gravitational microlensing is not a commonly used method for detecting brown dwarfs.