UGC 5101 | |
---|---|
Observation data ( J2000 epoch) | |
Constellation | Ursa Major |
Right ascension | 09h 35m 51.6s [1] |
Declination | +61° 21′ 11″ [1] |
Redshift | 0.039367 ± 0.000007 [1] |
Heliocentric radial velocity | 11,802 ± 2 km/ s [1] |
Distance | 528 Mly (162 Mpc) [1] |
Apparent magnitude (V) | 15.1 |
Characteristics | |
Type | S? [1] |
Apparent size (V) | 0.83′ × 0.45′ [1] |
Notable features | Ultraluminous infrared galaxy |
Other designations | |
MCG +10-14-025, IRAS 09320+6134, PGC 27292 [1] |
UGC 5101 is a galaxy merger located in the constellation Ursa Major. It is located at a distance of about 530 million light years from Earth. It is an ultraluminous infrared galaxy. [1] The total infrared luminosity of the galaxy is estimated to be 1011.95 L☉ and the galaxy has a total star formation rate of 105 M☉ per year. [2]
UGC 5101 has a single nucleus surrounded by spiral isophotes. [3] The nucleus of UGC 5101 has been found to be active and it has been categorised as a type 1.5 Seyfert galaxy or a LINER based on the radio continuum. [4] [5] The most accepted theory for the energy source of active galactic nuclei is the presence of an accretion disk around a supermassive black hole. The mass of the black hole in the centre of UGC 5101 is estimated to be 108.2 (160 million) M☉ based on stellar velocity dispersion. [6] The galaxy also hosts a water megamaser, probably originating from the nucleus. [7]
The nucleus emits hard X-rays, which are strongly absorbed, while there is also a soft X-rays component, which could originate from a hidden starburst region. [8] Also NeV emission has been detected in the nucleus, indicating the presence of a hot gas in the coronal line region, while hot dust has been detected around the nucleus, as indicated by the presence of PAH emission and strong silicate absorption. [9] [10] [11] The nucleus is surrounded by a dust torus with an opening angle larger than 41° which partly obstructs the nucleus with a column density of NHLS about 1.3×1024 cm−2. The hole of the torus is covered with compton thin material. [12] The integrated intensities of HCN to 13CO indicate the gas in the torus is very dense. [13] When observed with very-long-baseline interferometry the galaxy features a ridgeline that could be compact jets generated by the active nucleus. [14]
The galaxy has a tidal tail, seen edge on, and a faint halo of stars that was created during the merger. [15] A second tidal tail appears to loop around the nucleus, forming a ring. [3]
UGC 5101 | |
---|---|
Observation data ( J2000 epoch) | |
Constellation | Ursa Major |
Right ascension | 09h 35m 51.6s [1] |
Declination | +61° 21′ 11″ [1] |
Redshift | 0.039367 ± 0.000007 [1] |
Heliocentric radial velocity | 11,802 ± 2 km/ s [1] |
Distance | 528 Mly (162 Mpc) [1] |
Apparent magnitude (V) | 15.1 |
Characteristics | |
Type | S? [1] |
Apparent size (V) | 0.83′ × 0.45′ [1] |
Notable features | Ultraluminous infrared galaxy |
Other designations | |
MCG +10-14-025, IRAS 09320+6134, PGC 27292 [1] |
UGC 5101 is a galaxy merger located in the constellation Ursa Major. It is located at a distance of about 530 million light years from Earth. It is an ultraluminous infrared galaxy. [1] The total infrared luminosity of the galaxy is estimated to be 1011.95 L☉ and the galaxy has a total star formation rate of 105 M☉ per year. [2]
UGC 5101 has a single nucleus surrounded by spiral isophotes. [3] The nucleus of UGC 5101 has been found to be active and it has been categorised as a type 1.5 Seyfert galaxy or a LINER based on the radio continuum. [4] [5] The most accepted theory for the energy source of active galactic nuclei is the presence of an accretion disk around a supermassive black hole. The mass of the black hole in the centre of UGC 5101 is estimated to be 108.2 (160 million) M☉ based on stellar velocity dispersion. [6] The galaxy also hosts a water megamaser, probably originating from the nucleus. [7]
The nucleus emits hard X-rays, which are strongly absorbed, while there is also a soft X-rays component, which could originate from a hidden starburst region. [8] Also NeV emission has been detected in the nucleus, indicating the presence of a hot gas in the coronal line region, while hot dust has been detected around the nucleus, as indicated by the presence of PAH emission and strong silicate absorption. [9] [10] [11] The nucleus is surrounded by a dust torus with an opening angle larger than 41° which partly obstructs the nucleus with a column density of NHLS about 1.3×1024 cm−2. The hole of the torus is covered with compton thin material. [12] The integrated intensities of HCN to 13CO indicate the gas in the torus is very dense. [13] When observed with very-long-baseline interferometry the galaxy features a ridgeline that could be compact jets generated by the active nucleus. [14]
The galaxy has a tidal tail, seen edge on, and a faint halo of stars that was created during the merger. [15] A second tidal tail appears to loop around the nucleus, forming a ring. [3]