| NGC 4485 | |
|---|---|
 | |
| Observation data (J2000epoch) | |
| Constellation | Canes Venatici[1] |
| Right ascension | 12h 30m 31.113s[2] |
| Declination | +41° 42′ 04.22″[2] |
| Redshift | 0.0016[3] |
| Heliocentric radial velocity | 483[4] |
| Distance | 29.1 Mly (8.91 Mpc)[4] |
| Apparent magnitude (V) | 11.93[3] |
| Apparent magnitude (B) | 12.32[3] |
| Characteristics | |
| Type | IB(s)m pec[5] |
| Size | 11000 ly |
| Other designations | |
| 2MASX J12303111+4142042,NGC 4485,UGC 7648,MCG +07-26-013,PGC 41326,VV 30b,KPG 341a[3] | |
NGC 4485 is anirregular galaxy located in the northernconstellation ofCanes Venatici. It was discovered January 14, 1788 byWilliam Herschel.[6] This galaxy is located at a distance of 29[4] millionlight years and is receding with a heliocentricradial velocity of 483 km/s.[4]
NGC 4485 isinteracting with the spiral galaxyNGC 4490 and as a result both galaxies are distorted and are undergoing intense star formation. They have a projected separation of9.3 kpc and are surrounded by an extended hydrogen envelope with a dense bridge of gas joining the two. Both galaxies are otherwise isolated and of low mass. The star formation rate in NGC 4485 is0.22 M☉·yr−1.[7]
![Interaction between them created a stream of material about 25 000 light-years long.[8]](/mt/?noimg=&dark=on&url=http%3a%2f%2fen.wikipedia.org%2fwiki%2fFile%3aOn_the_verge_NGC_4485.jpg)
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