| Galaxy | Const | Type | Distance | Luminosity | Mass | Comment |
|---|---|---|---|---|---|---|
| Milky Way | [Sgr] | Sbc | 0.028 | 1.9 | 2 | Sgr A, Galactic Center |
| M31 | And | Sb | 2.9 | 5.2 | 30 | Andromeda Galaxy |
| M32 | And | E2 | 2.9 | 0.25 | 3 | Satellite of M31 |
| NGC 3115 | Sex | SO | 27 | 14.2 | 2 | |
| M 106 | CVn | Sbc | 24 | 1.3 | 40 | Maser Detection |
| NGC 4261 | Vir | E2 | 90 | 33 | 400 | |
| M87 | Vir | E0 | 60 | 56 | 3000 | |
| M104 | Vir | Sa | 50 | 47 | 1000 | Sombrero Galaxy |
| NGC 3377 | Leo | E5 | 38 | 5.2 | 100 | |
| M105 | Leo | E1 | 38 | 13 | 50 | |
| NGC 4486B | Vir | E0 | 60 | 0.82 | 500 | Satellite of M87 |
| M77 | Cet | Sb | 60 | Caltech IR detection | ||
| M84 | Vir | S0 | 60 | 56 | 300 | HST STIS (May 1997) |
Key:
This table summarizes data for some of the well-established massive dark objects in the nuclei of galaxies. The masses of these objects are usually estimated from the orbital velocity of stars or gas orbiting the objects at distances of some tens or hundreds of light years, which shows that enormous masses are concentrated in small volumes. Many of these central objects exhibit other signs of violent gravitational action: Accretion disks, emission of strong radio and/or high-energy radiation, or jets of highly accelerated material.
What may be the nature of these mysterious objects ? Many astronomers take it for granted that these objects are supermassive black holes, but none of them is really resolved. To get truely compelling evidence, or better, to reveal the true nature of the massive dark objects, a resolution would be required of the order of the Schwarzschild radius (the "horizon" radius of a black hole acording to Einstein's General Relativity theory). The Schwarzschild radius is simply correlated to the mass of an object, as it is defined as that radius where the escape velocity from the mass equals light velocity; this means that it is propoertional to the mass. The formal relation can be given as
The table above is partly based on STScI-PR97-01.
Last Modification: 14 Feb 1998, 17:30 MET