| NGC 4670 | |
|---|---|
 NGC 4670 byHubble Space Telescope | |
| Observation data (J2000epoch) | |
| Constellation | Coma Berenices |
| Right ascension | 12h 45m 17.1s[1] |
| Declination | +27° 07′ 32″[1] |
| Redshift | 0.003630 ± 0.000005[1] |
| Heliocentric radial velocity | 1,088 ± 1km/s[1] |
| Distance | 57.6 ± 17Mly (17.7 ± 4.7Mpc)[1] |
| Apparent magnitude (V) | 12.2[2] |
| Characteristics | |
| Type | SB(s)0/a pec[1] |
| Apparent size (V) | 1.4′ × 1.1′[1] |
| Notable features | Blue compact dwarf |
| Other designations | |
| UGC 7930,Arp 163, Haro 9,MCG +05-30-072, KUG 1242+273, IRAS 12428+2724,PGC 42987 | |
NGC 4670 is ablue compact galaxy in the constellationComa Berenices. The galaxy lies about 60 millionlight years away from Earth, which means, given its apparent dimensions, that NGC 4670 is approximately 25,000 light years across.[1] It was discovered byWilliam Herschel on April 6, 1785.[3]
The overall shape of the galaxy is categorised aspeculiar and it has been categorised as amorphous or as barred lenticular galaxy. NGC 4670 is included in the Atlas of Peculiar Galaxies in the galaxies with diffuse counter tails category. The gas kinematics indicate the presence of acentral bar.[4] The galaxy is seen with an 28° inclination but it is possibly warped.[5]
NGC 4670 is characterised by its blue color, which was noted byGuillermo Haro in a study published in 1956.[6] Such galaxies are characterised by episodes of intensestar formation. The centre of NGC 4670 hosts a supergiantHII region and also hosts most of the hydrogen of the galaxy. The hydrogen lies in three clouds with an estimated mass of108 M☉.[5] Four other HII regions are visible near the central region.[7]
The galaxy has also ionised gas outside of the central region, forming bubbles and filaments. The two larger filaments extend to the southwest and northeast and a have a calculated length of 7.5 and 6.5 kpc respectively.[4]
An X-ray and radio source has been detected in the galaxy at the location of a star cluster complex but its nature is uncertain. It could be a massiveblack hole, an ultraluminousX-ray bubble, anX-ray binary star or asupernova remnant.[8]
NGC 4670 is considered to be a member of theNGC 4565 Group, which also includes, apart fromNGC 4565, the galaxiesNGC 4494,NGC 4562,NGC 4725, andNGC 4747.[9]
