UGC 5460

UGC 5460 is a barred spiral galaxy in the constellation of Ursa Major. Its velocity with respect to the cosmic microwave background for is 1,276±14 km/s, which corresponds to a Hubble distance of 61.4 ± 4.4 Mly (18.82 ± 1.34 Mpc).^[1] In addition, two non redshift measurements give a distance of 58.1 ± 6.8 Mly (17.8 ± 2.1 Mpc).^[2] The first known reference to this galaxy comes from Part 1 of the Morphological Catalogue of Galaxies, where it is listed as MCG +09-17-028.

UGC 5460
UGC 5460 imaged by the Hubble Space Telescope
Observation data (J2000 epoch)
Constellation	Ursa Major
Right ascension	10h 08m 09.1731s[1]
Declination	+51° 50′ 41.583″[1]
Redshift	0.003646[1]
Heliocentric radial velocity	1,093±5 km/s[1]
Distance	61.4 ± 4.4 Mly (18.82 ± 1.34 Mpc)[1]
Group or cluster	NGC 3079 Group (LGG 188)
Apparent magnitude (V)	13.9[1]
Characteristics
Type	SB(rs)d[1]
Size	~43,900 ly (13.46 kpc) (estimated)[1]
Other designations
IRAS F10048+5205, MCG +09-17-028, PGC 29469, CGCG 266-025[1]

The SIMBAD database lists UGC 5460 as an active galaxy nucleus candidate, i.e. it has a compact region at the center that emits a significant amount of energy across the electromagnetic spectrum, with characteristics indicating that this luminosity is not produced by the stars.^[3]

NGC 3079 Group

UGC 5460 is a member of the NGC 3079 Group (also known as LGG 188), which contains six galaxies. The other five galaxies in the group are: NGC 3073, NGC 3079, UGC 5421, UGC 5459, and UGC 5479.^[4]

Supernovae

Swift UVOT optical (left), UVOT UV (middle), and XRT X-ray (right) images of SN 2011ht and its host galaxy UGC 5460.

Two supernovae have been observed in UGC 5460:

• SN 2011ht (type IIn, mag. 17) was discovered by Tom Boles on 29 September 2011.^[5][6] This supernova was initially suspected of being a luminous blue variable.^[5] Later analysis suggested that it belongs to an unusual group of SNe IIn, including SN 1994W and SN 2009kn, and perhaps SN 2005cl, that warrants a new designation of Type IIn-P.^[7]
• SN 2015as (type IIb, mag. 16) was discovered by Ken'ichi Nishimura on 15 November 2015.^[8] Although initially classified as type II,^[9] later analysis concluded it to be type IIb.^[10]