| NGC 7679 | |
|---|---|
 Hubble Space Telescope (HST) image of the galaxy | |
| Observation data (J2000epoch) | |
| Constellation | Pisces |
| Right ascension | 23h 28m 46.7s[1] |
| Declination | +03° 30′ 41″[1] |
| Redshift | 0.017139 ± 0.000013 |
| Heliocentric radial velocity | 5,138 ± 4 km/s[1] |
| Distance | 191 ± 11Mly (58.6 ± 3.3Mpc)[1] |
| Apparent magnitude (V) | 12.5[2] |
| Characteristics | |
| Type | SB0 pec[1] |
| Apparent size (V) | 1.3′ × 0.9′[1] |
| Notable features | Seyfert galaxy,starburst |
| Other designations | |
| Arp 216,UGC 12618,MCG +00-59-046,Mrk 534,PGC 71554,CGCG 380-061,VV 329[1] | |
NGC 7679 is alenticular galaxy with a peculiar morphology in theconstellationPisces. It is located at a distance of about 200 millionlight years from Earth, which, given its apparent dimensions, means that NGC 7679 is about 60,000 light years across. It was discovered byHeinrich d'Arrest on September 23, 1864.[3] The totalinfrared luminosity is1011.05 L☉, and thus it is categorised as aluminous infrared galaxy.[4] NGC 7679 is both astarburst galaxy and aSeyfert galaxy.[5]
NGC 7679 is abarred lenticular galaxy seen face on,[6] and is noted for its distorted shape. The galaxy has two plumes in opposite directions, possibly the result of tidal interaction with NGC 7682, and smooth outer arms. The inner region is of high surface brightness with many knots and a high star formation rate.[7] The star formation rate of the galaxy is estimated to be 80M☉ per year based on the x-ray luminosity observed byXMM-Newton,[8] and on theH-alpha luminosity of 21.2 ± 0.2M☉ per year while observations in infrared indicate a star formation of 11.35 ± 0.6M☉ per year.[9]
There is evidence of massivestarburst activity in the circumnuclear region, with 35% of the stars there being aged less than 10 million years.[10] A ring of ionised gas dominates both the optical and infrared wavelengths and is the locus of the starburst activity.[11]
The nucleus of NGC 7679 has been found to beactive and has been categorised as aSeyfert galaxy. The most accepted theory for the energy source of Seyfert galaxies is the presence of anaccretion disk around asupermassive black hole. NGC 7679 is believed to host a supermassive black hole whose mass is estimated to be5.9×106 (106.77)M☉ based onvelocity dispersion.[12]
TheX-ray spectrum fromBeppoSAX shows no significant absorption above 2 MeV and the iron Ka line was marginally detected.[13] However, the galaxy shows signs of obstruction in visual light, as it lacks broademission lines. Two possible reasons are the presence of dust or theaccretion disk that produces X-rays is not obstructed but the broad line region is.[14] The lack of X-ray absorption along with the presence of broad H-alpha lines but not broad H-beta mean that it cannot be easily categorised as a particular type of Seyfert galaxy.[5]
NGC 7679 forms a pair withNGC 7682. NGC 7682 lies at a distance of 269.7 arcseconds, which corresponds to a projected distance of 97 kpc.[8] The two galaxies are connected by a hydrogen bridge, a sign of a closer encounter in the past 500 million years.[11] It is possible that the interaction of the two galaxies caused star formation in NGC 7679.[6] A fainter galaxy has been found superimposed on the eastern arm of the galaxy, but it is actually located in the background.[11]
Media related toNGC 7679 at Wikimedia Commons