IRAS 17208-0014 | |
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![]() SDSS image of IRAS 17208-0014. | |
Observation data (J2000 epoch) | |
Constellation | Ophiuchus |
Right ascension | 17h 23m 21.951s [1] |
Declination | −00° 17′ 00.74″ [1] |
Redshift | 0.042810 [1] |
Heliocentric radial velocity | 12,824 km/s [1] |
Distance | 617 Mly |
Apparent magnitude (B) | 15.1 |
Characteristics | |
Type | LINER [1] |
Size | ~113,700 ly (34.86 kpc) (estimated) [1] |
Notable features | Ultraluminous inflared galaxy |
Other designations | |
NSA 147958, PGC 60189, C-GOALS 32, NVSS J172321-001702, PMN J1723-0016 [1] |
IRAS 17208-0014 is an ultraluminous infrared galaxy located about 617 million light-years from Earth in the southern constellation of Ophiuchus. [1] This is a well-studied galaxy hosting an hydroxyl (OH) megamaser, [2] first discovered by the Nancay radio telescope in 1985. [3] The redshift of the galaxy is (z) 0.0428 and it has a total infrared luminosity of 1012.4 Lʘ. [4]
IRAS 17208-0014 is categorized an advanced galaxy merger, a result of two disk galaxies colliding with one another. It is known to display two tidal tails that are protruding out from the galaxy by 20 kiloparsecs with a distorted central body. [5] [6] The outer disk of the galaxy is disturbed and it has an extended nucleus when shown in near-infrared imaging bands, captured by the Hubble Space Telescope NICMOS camera. [7] The nucleus of the galaxy is compact and elongated along the position angle of 90° to 110°. [8] It is surrounded by both absorption features and condensations. [9] Observations also showed it has a buried active galactic nucleus (AGN) in the western disk of the galaxy. [4] The galaxy has a supermassive black hole located in the center, with a mass of 2.3 x 108 Mʘ based on a stellar velocity dispersion. [10]
IRAS 17208-0014 is described as a LINER. It has an X-ray luminosity measured as 1 x 1042 erg s-1 when observed by BeppoSAX. [11] There are several star clusters located within the inner region of the galaxy, said to be proto globular systems. [5] The galaxy is powered by intense starbursts with a star formation of 84 ± 13 Mʘ per year; fueled by a molecular gas reservoir. [12] [13] Carbon monoxide line emission was also detected mainly originating from a molecular disk, found as spatially resolved and measuring a diameter of 2.7 x 1.8 kiloparsecs. [14] [15] There is also evidence of a detached clump and three faint protrusions pushing the disk's emission out to 1.8 kiloparsecs. The mass of the molecular gas outflow is estimated to be 2 x 108 Mʘ. [15]
Three nuclear regions have been identified in IRAS 17208-0014, found aligned in a linear pattern along east to west. When imaged by matched resolution at 15 and 33 GHz frequencies by Very Large Array, they are combined into a larger region. [16] A deep study on the OH megamaser in IRAS 17208-0014 showed it having an area of around 170 x 110 parsecs in diameter and mainly found in two dominant regions. [17] The galaxy also shows HCO+ emission. [18]