4C +19.46,PKS 1420+19, DA 366, OQ +134, NRAO 0443, TXS 1420+198, CoNFIG 192, Cul 1420+198[1]
3C 300 is aradio galaxy[2] located in the constellation ofBoötes. Theredshift of the object is (z) 0.270[1] and it was first discovered as aradio source in 1959.[3] It was subsequently identified with a galaxy counterpart in June 1966 and designated as4C 19.46 by theFourth Cambridge Survey in 1968.[4][5]
VLTMUSE image of the EELR with oxgen in green andH-alpha in orange.
3C 300 is a high-excitationFanaroff-Riley Class Type 2 radio galaxy,[6] hosted by a compactelliptical galaxy that is located in a poorgalaxy cluster.[7][8] The appearance of the galaxy is described as highly elongated with faint tidal distortions, a boxy isophotal structure and an apparentV magnitude of 19.0.[8][9][10] A small companion galaxy is located 8.14arcseconds away in the west direction, shown to be heavily involved in the interaction andmerging process with the galaxy.[11] There are also highsurface brightness regions in the galaxy along with a patch ofradio emission located east from its extended nucleus.[7][12] The totalstar formation of 3C 300 is 3.3+0.7-0.7 Mʘ per year, with a totalinfrared luminosity of 19.0+3.8-4.1 x 109Lʘ.[13]
Theextended emission-line region (EELR) of 3C 300,[14] has an S-shaped morphology with a total extent of 60 kiloparsecs in east to west direction and displayingrotation that is well-ordered along the position of its major radioaxis. Diffused emission is seen on the north and west side of the region.[15] Nuclear outflows are evident, with the outflow being mainly influenced by a blue component whose maximumvelocity peaks at 2160 kilometers per seconds.[16]
The radio source of 3C 300 is classified as a double, based on observations made by J.M. Riley and G.G. Pooley using the Cambridge 50-km Telescope in 1975.[17] When observed on a radio map, the source contains multiple components with a totalspectra index value of 0.83 ± 0.10.[18] High resolution imaging made by theVery Long Baseline Array (VLA) would paint a different picture for the source, describing it as asymmetrical with a hotspot located in the eastern direction. When further imaged, the hotspot has a double structure with an elongated component at its western edge and a brighter component that is being extended back towards the radio core position. Two other components are located inside a high surface brightness area.[19] The northernradio lobe of 3C 300 displays a high speed of 0.026 ± 0.045c, compared to its shorter southern radio lobe. This implies the northern radio lobe is residing within a low externalgas density area.[20]
Ajet is present inside the western radio lobe of 3C 300, from the core to the terminating point of the hotspot region. This jet might also be bent too, given the change ofangle between 10° and 15°.[19] An observation made in 1998 found the jet is straight with aflux density of 8.06GHz and has a length of 4.70 kiloparsecs.[21] Asupermassive black hole mass of 12.7+5.6-5.0 x 107 Mʘ has been estimated for the galaxy.[13]
^abFloyd, David J. E.; Axon, David; Baum, Stefi; Capetti, Alessandro; Chiaberge, Marco; Macchetto, Duccio; Madrid, Juan; Miley, George; O'Dea, Christopher P.; Perlman, Eric; Quillen, Alice; Sparks, William; Tremblay, Grant (July 2008). "Hubble Space Telescope Near-infrared Snapshot Survey of 3CR Radio Source Counterparts. II. An Atlas and Inventory of the Host Galaxies, Mergers, and Companions".The Astrophysical Journal Supplement Series.177 (1):148–173.arXiv:0712.0595.Bibcode:2008ApJS..177..148F.doi:10.1086/587622.ISSN0067-0049.
^Tremblay, G. R.; Chiaberge, M.; Donzelli, C. J.; Quillen, A. C.; Capetti, A.; Sparks, W. B.; Macchetto, F. D. (September 2007). "Isophotal Structure and Dust Distribution in Radio-loud Elliptical Galaxies".The Astrophysical Journal.666 (1):109–121.arXiv:0705.3642.Bibcode:2007ApJ...666..109T.doi:10.1086/520333.ISSN0004-637X.
