| NGC 4589 | |
|---|---|
NGC 4589 imaged by the Hubble Space Telescope
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| Observation data (J2000 epoch) | |
| Constellation | Draco |
| Right ascension | 12h37m 24.9875s[1] |
| Declination | +74° 11′ 30.903″[1] |
| Redshift | 0.006617[2] |
| Heliocentric radial velocity | 2,002 km/s[3] |
| Galactocentric velocity | 2,154 km/s[3] |
| Distance | 73.03 ± 0.46 Mly (22.39 ± 0.14 Mpc)[3] |
| Apparent magnitude (V) | 10.73±0.15[4] |
| Apparent magnitude (B) | 11.69±0.15[4] |
| Absolute magnitude (V) | −21.41±0.23[4] |
| Characteristics | |
| Type | E2[4] |
| Apparent size (V) | 3.47′ × 2.75′[5] |
| Other designations | |
| IRAS F12353+7428, NGC 4589, UGC 7797, LEDA 42139[6] | |
NGC 4589 is an elliptical galaxy located in the Draco constellation.[7][8][9] It was discovered by German-British astronomer William Herschel on November 22, 1797. This galaxy lies at a distance of 73.0 million light-years (22.39 Mpc) from the Milky Way, and is receding with a heliocentric radial velocityof2,002 km/s.[3] It is known by its designations PGC 42139 or UGC 7797.[6]
The morphological classification of NGC 4589 is E2 in the De Vaucouleurs system, Indicating this is an elliptical galaxy with a ratio of 5:4 between the major and minor axes. It is a bright source of X-ray emission and is a LINER-type galaxy. There is a dusty disk that is aligned with the minor axis, which is likely the remnant of a merger with a gas-rich galaxy. NGC 4589 has a large population of globular clusters, estimated at 640±50. A small population of young star clusters with an age of less than a billion years are located in the central region.[4]
The calcium-rich type Ib supernova SN 2005cz was discovered on July 28, 2005.[10] The progenitor star may have formed near the young stellar clusters at the core of NGC 4589.[4]
Media related to NGC 4589 at Wikimedia Commons|
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