NGC 4800
Galaxy in constellation Canes Venatici
From Wikipedia, the free encyclopedia
NGC 4800 is an isolated[6] spiral galaxy in the constellation Canes Venatici, located at a distance of 95 megalight-years from the Milky Way.[3] It was discovered by William Herschel on April 1, 1788.[7] The morphological classification of this galaxy is SA(rs)b,[5] indicating a spiral galaxy with no visual bar at the nucleus (SA), an incomplete ring structure (rs), and moderately-tightly wound spiral arms (b). The galactic plane is inclined to the line of sight by an angle of 43°, and the long axis is oriented along a position angle of 25°.[8] There is a weak bar structure at the nucleus that is visible in the infrared.[6]
| NGC 4800 | |
|---|---|
Hubble Space Telescope image of NGC 4800 | |
| Observation data (J2000 epoch) | |
| Constellation | Canes Venatici |
| Right ascension | 12h 54m 37.78208s[1] |
| Declination | +46° 31′ 52.2815″[1] |
| Redshift | 0.002972[2] |
| Heliocentric radial velocity | 891±17 km/s[2] |
| Distance | 95 Mly (29.0 Mpc)[3] |
| Apparent magnitude (B) | 12.0[4] |
| Characteristics | |
| Type | SA(rs)b[5] |
| Other designations | |
| NGC 4800, LEDA 43931, 2MASX J12543777+4631521[4] | |
The galaxy has a low-luminosity active galactic nucleus with an HII region at the core.[5] The circumnuclear zone contains a double ring structure of "ultra-compact nuclear rings"; the inner ring has a radius of 30 pc and the outer ring's radius is about 130 pc.[6] The upper limit on the mass of the central supermassive black hole is estimated as 2.0×107 M☉, or 20 million times the mass of the Sun.[9]
NGC 4800 is isolated within the Ursa Major Cloud, which is part of the Virgo Supercluster.[10]
