| NGC 7592 | |
|---|---|
 Hubble Space Telescope (HST) image of the galaxy | |
| Observation data (J2000epoch) | |
| Constellation | Aquarius |
| Right ascension | 23h 18m 22.2s[1] |
| Declination | −04° 25′ 01″[1] |
| Redshift | 0.024444 ± 0.000113 |
| Heliocentric radial velocity | 7,328 ± 34 km/s[1] |
| Distance | 306Mly (95Mpc)[1] |
| Apparent magnitude (V) | 13.5[2] |
| Characteristics | |
| Type | S0+ pec[1] |
| Apparent size (V) | 1.2′ × 0.9′[1] |
| Notable features | mergering galaxy pair |
| Other designations | |
| MCG -01-59-017, VV 731,PGC 70999,[1]Mrk 928 | |
NGC 7592 is aninteracting galaxy system located 300 million light years away in theconstellationAquarius. It was discovered byWilliam Herschel on September 20, 1784.[3] The totalinfrared luminosity is1011.33 L☉, and thus it is categorised as aluminous infrared galaxy.[4] One of the galaxies hosts a type 2Seyfert nucleus.[5]
NGC 7592 is an interacting galaxy system and ongoinggalaxy merger between an early type galaxy and a late typespiral galaxy.[6] The system has at least two faint diffusetidal tails, with the longer one extending about 2 arcminutes towards the south.[7] Based on the totalinfrared luminosity of the galaxy (1011.33 L☉), NGC 7592 is categorised as aluminous infrared galaxy.[4] Luminous infrared galaxies are characterised by increasedstar formation. The star formation rate of NGC 7592 is estimated to be 26M☉ per year.[7]
The two galactic nuclei, whose projected separation is 14 arcseconds, have nearly equal luminance in near infrared imaging.[8] The west nucleus is known to be aSeyfert, a type ofactive galactic nucleus (AGN). Based on its spectral lines, it has been categorised as type 1.9 or type 2.[9] The most accepted theory for the energy source of AGNs is the presence of anaccretion disk around asupermassive black hole. It has been suggested that around the Seyfert nucleus lies a rotating, star-forming knotty disk or ring with a diameter of about 1.5 kpc viewed nearly edge-on, and which is perpendicular to the galactic plane. It is possible that it is material accreted from the other galaxy. The east nucleus features a complex structure, probably due toextinction.[6] There is diffuse X-ray emission around both nuclei.[7]
At the end of one tidal tail lies a bright source in visual light that is identified as NGC 7592C.[7] It is located about 12 arcseconds south from the mid-distance of the two other nuclei.[8] It has been suggested that it is another galaxy taking part in the merger, however itsinfrared emission is fainter than the other two nuclei and it has not been detected in x-rays byChandra X-ray Observatory.[10] Its spectrum, both optical and infrared, suggests it is an extranuclearstar formation region.[7] Based on its kinematics, the south condensation is part of the spiral galaxy.[6]
Media related toNGC 7592 at Wikimedia Commons