This distribution of globular cluster luminosities is called the Globular Cluster Luminosity Function (GCLF). Galaxies with luminosities above are ultraluminous infrared galaxies (ULIRGs). It shines with a luminosity of only 0.34 solar luminosities. Seyfert galaxies have extremely bright nuclei, with luminosities ranging between 10 and 10 solar luminosities. Quasar luminosities can vary considerably over time, depending on their surroundings. Quasars' luminosities are variable, with time scales that range from months to hours. At low luminosities, the objects to be unified are Seyfert galaxies. The funnels collimate the radiation into beams with highly super-Eddington luminosities. Older models had produced temperatures around 45,000 K and hence dramatically lower luminosities. Lower surface gravity often indicates larger stars, and hence, higher luminosities. If not, this will induce systematic errors in the determination of stellar luminosities. This effectively restricts stars from shining at higher luminosities for long periods. However, stars have a wide range in luminosities. Only highly unstable objects are found, temporarily, at higher luminosities. This would require a massive object, which would also explain the high luminosities.