PKS 2349−014 is aSeyfert type 1 galaxy and a low-redshiftquasar located in the constellation ofPisces. Theredshift of the object is (z) 0.173[1] and it was first discovered by J.G. Bolton as aradio source in 1968 where it was designated asPKS 2349−01.[2] It is also classified as a broad-lineradio galaxy and is radio-loud.[3][4]
PKS 2349−014 is classified as a radio-loud luminous quasar.[5][6] The host galaxy is anelliptical galaxy based on ade Vaucouleurs model.[7][8] Imaging by theHubble Space Telescope (HST), described it as having a highly disturbed appearance, with large tidal arms depicted as oddly shaped, indicating aninteraction with a nearby companion galaxy described as having a faintmagnitude of 21.0 ± 0.3.[6][9] There are several other galaxies located around the field of the object.[10]
Two smooth wisp features are found to surround PKS 2349−014, forming an almost completering-like structure with an extent of 20kiloparsecs and brighter when closer to the center of the object. One of the wisps on the eastern side seems to penetrate its companion.[10] Evidence pointed out these wisps are the remains of a bright galaxy tidally accreted by the host galaxy, indicating a completemerger prior to the interaction with the companion.[11]
The object shows an unresolved central nucleus. There is also a faint off-centerednebula extension with a low averagesurface brightness of 24.4 mag arcsec-2, a major and minor axis extension of 48 and 34 kiloparsecs respectively.[10][12] From the nucleus on the northeast region, several traces ofdust lane remnants can be seen.[10]
Thespectrum of PKS 2349−014 is mainly dominated by both narrow forbidden and strong broad permittedemission lines.[13] It is also shown the object has a post starburststellar population mostly made up of oldstars of 12 billion years with evidence of younger stars aged around 500 million years.[14][15] The totalstellar mass is estimated to be 12.2 x 1011 Mʘ while thestar formation rate is approximately 8.3 Mʘ per year.[13] Asupermassive black hole mass of 8.41 ± 0.06 Mʘ was calculated for PKS 2349−014 based on aHβ line.[16]
