UGC 4879 | |
---|---|
![]() UGC 4879, taken using the
Hubble Space Telescope's
Advanced Camera for Surveys | |
Observation data ( J2000 epoch) | |
Constellation | Ursa Major |
Right ascension | 09h 16m 02.023s [1] |
Declination | +52° 50′ 42.05″ [1] |
Redshift | -0.000233 [2] |
Heliocentric radial velocity | -70 [2] |
Distance | 4.18 ± 0.41 Mly (1.283 ± 0.126 Mpc) [2] |
Group or cluster | Local Group |
Apparent magnitude (V) | 13.2 [3] |
Apparent magnitude (B) | 14.0 [3] |
Characteristics | |
Type | IAm [2] |
Size | 3,000 ly (930 pc) [2] |
Apparent size (V) | 2.5′ × 1.5′ [2] |
Notable features | Isolated dwarf galaxy in the Local Group |
Other designations | |
VV 124, MGC+09-15-113, PGC 26142 [3] |
UGC 4879, which is also known as VV 124, is the most isolated dwarf galaxy in the periphery of the Local Group. It is an irregular galaxy at a distance of 1.38 Mpc. Low-resolution spectroscopy yielded inconsistent radial velocities for different components of the galaxy, hinting at the presence of a stellar disk. There is also evidence of this galaxy containing dark matter.
UGC 4879 is a transition type galaxy, meaning it has no rings (Denoted rs). It is also a spheroidal (dSph) galaxy, meaning it has a low luminosity. It has little to no gas or dust, and little recent star formation. It is also irregular, meaning it has no specific form. [4]