latter star and ignite to form a supergiant. Later this will become an extreme helium star before cooling to become a white dwarf. While RR Telescopii, also designated Nova Telescopii 1948, is often called a slow nova, it is now classified as a symbiotic nova system composed of an M5III pulsating red giant and a white dwarf; between 1944 and 1948 it brightened by about 7 magnitudes before being noticed at apparent magnitude 6.0 in mid-1948. It has since faded slowly to about apparent magnitude 12. QS Telescopii is a binary system composed of a white dwarf and main sequence donor star, in this case the two are close enough to be tidally locked, facing one another. Known as polars, material from the donor star does not form an accretion disk around the white dwarf, but rather streams directly onto it. This is due to the presence of the white dwarf's strong magnetic field. Although no star systems in Telescopium have confirmed planets, several have been found to have brown dwarf companions. A member of the 12-million-year-old Beta Pictoris moving group of stars that share a common proper motion through space, Eta Telescopii is a young white main sequence star of magnitude 5.0 and spectral type A0V. It has a debris disk and brown dwarf companion of spectral type M7V or M8V that is between 20 and 50 times as massive as Jupiter. The system is complex, as it has a common proper motion with (and is gravitationally bound to) the star HD 181327, which has its own debris disk. This latter star is a yellow-white main sequence star of spectral type F6V of magnitude 7.0. PZ Telescopii is another young star with a debris disk and substellar brown dwarf companion, though at 24 million years of age appears too old to be part of the Beta Pictoris moving group. HD 191760 is a yellow subgiant—a star that is cooling and expanding off the main sequence—of spectral type G3IV/V. Estimated to be just over four billion years old, it is slightly (1.1 to 1.3 times) more massive as the Sun, 2.69 times as luminous, and has around 1.62 times its radius. Using the High Accuracy Radial Velocity Planet Searcher (HARPS) instrument on the ESO 3.6 m Telescope, it was found to have a brown dwarf around 38 times as massive as Jupiter orbiting at an average distance of 1.35 AU