NGC 7319 | |
---|---|
Observation data (J2000 epoch) | |
Constellation | Pegasus |
Right ascension | 22h 36m 03.56s[1] |
Declination | +33° 58′ 32.7″[1] |
Redshift | 0.022[1] |
Heliocentric radial velocity | 6,740 km/s[2] |
Distance | 311 Mly (95.3 Mpc)[1] |
Apparent magnitude (V) | 14.1[3] |
Characteristics | |
Type | SB(s)bc pec[3] |
Apparent size (V) | 1′.7 × 1′.3[3] |
Other designations | |
NGC 7319, UGC 12102, LEDA 69269, PGC 69269[4][3] |
NGC 7319 is a highly distorted barred spiral galaxy that is a member of the compact Stephan's Quintet[5] group located in the constellation Pegasus, some 311 megalight-years distant from the Milky Way.[1] The galaxy's arms, dust and gas have been highly disturbed as a result of the interaction with the other members of the Quintet. Nearly all of the neutral hydrogen has been stripped from this galaxy, most likely as a result of a collision with NGC 7320c some 100 million years ago.[6] A pair of long, parallel tidal tails extend southward from NGC 7319 in the direction of NGC 7320c, and is undergoing star formation.[7]
This is a type 2 Seyfert galaxy[1] with one of the largest circumnuclear outflows known in galaxies of this type. This outflow reaches velocities of up to 500 km/s and spans 13 kly. The star formation rate appears normal for a spiral galaxy at 1.98±0.58 M☉ yr−1, and the majority (68%) is occurring in the spiral arms.[7] The core appears faint in the ultraviolet band, indicating heavy extinction within the active galactic nucleus.[7] There is a three component radio source with an overall size of 5.5 kly that is straddling the nucleus.[8] A strong X-ray source with a high redshift has been detected at a separation of 8″ from the galactic nucleus, a quasi-stellar object.[2]
One supernova has been observed in NGC 7319: On 19 August 1971, Leonida Rosino discovered SN 1971P (type unknown, mag. 16.8).[9]