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] |
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]
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]