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
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]
Helio 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]

Appearance

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]

Gallery

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  There are about 2.3 million light years between UGC 4879 and its closest neighbour, Leo A.[5]

References

External links

Wikimedia Commons has media related to UGC 4879.

• C2.staticflickr.com