| NGC 4429 | |
|---|---|
 SDSS image of NGC 4429. | |
| Observation data (J2000epoch) | |
| Constellation | Virgo |
| Right ascension | 12h 27m 26.5s[1] |
| Declination | 11° 06′ 28″[1] |
| Redshift | 0.003683/1104 km/s[1] |
| Distance | 55.42Mly[2] |
| Group orcluster | Virgo Cluster |
| Apparent magnitude (V) | 11.02[1] |
| Characteristics | |
| Type | SA0^+(r)[1] |
| Size | ~82,854.8 ly (estimated)[2] |
| Apparent size (V) | 5.6 x 2.6[1] |
| Other designations | |
| PGC 40850, UGC 7568, VCC 1003[1] | |
NGC 4429 is alenticular galaxy[3] located about 55 millionlight-years away[2] in theconstellation ofVirgo.[4] NGC 4429 is tilted at an inclination of about 75° which means that the galaxy is tilted almost edge-on as seen fromEarth.[2] NGC 4429 was discovered by astronomerWilliam Herschel on March 15, 1784.[5] The galaxy is a member of theVirgo Cluster.[2][6]
NGC 4429 has a small dust disk.[7] There is also possibly a cold circumnuclear stellar disk. The cold circumnuclear stellar disk may have formed due to the infall of gas to center caused by amerger. However, since NGC 4429 does not show any signs of a recent gravitational disturbance, the merger must have happened a long time ago in the past.[8]
The dust disk[7] and the cold circumnuclear stellar disk[8] are embedded in a bright, hexagonal shaped bulge that resembles that ofNGC 7020. The zone has bright arcs near its major axis but no "spots" or extensions as in NGC 7020. The zone is also somewhat ring-like.[7]
NGC 4429 may lose a significant fraction of its gas due toram pressure stripping.[2]
The central regions of NGC 4429 are overabundant in the elementmagnesium.[2]
