3C 432 | |
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![]() The quasar 3C 432. | |
Observation data (J2000.0 epoch) | |
Constellation | Pegasus |
Right ascension | 21h 22m 46.319s [1] |
Declination | +17° 04′ 37.983″ [1] |
Redshift | 1.785000 [1] |
Heliocentric radial velocity | 535,130 km/s [1] |
Distance | 9.678 Gly |
Apparent magnitude (V) | 17.96 |
Apparent magnitude (B) | 18.18 |
Characteristics | |
Type | RL1 [1] |
Other designations | |
4C +16.72, PKS 2120+16, LEDA 2817730, OX +134.2, NRAO 0656, TXS 2120+168, IERS B2120+168 [1] |
3C 432 is a quasar located in the constellation of Pegasus. It has a redshift of (z) 1.785 [1] and it was first discovered in 1966 during the Third Cambridge Catalogue of Radio Sources survey. [2] This is a powerful radio-loud object classified as a lobe-dominated quasar, [3] with a Type II Fanaroff Riley class source. [4] [5]
The source of 3C 432 is small. [6] When observed with Very Large Array radio imaging, it is made up of bright radio lobes which are placed asymmetrically around its central feature, interpreted as the radio core. [6] There are two detected hot spots; one located on the lobe extreme edge and the other located towards the lobe inner edges. [4] A jet displaying an elongated jet knot, is found pointing towards the direction of the brightest hot spot region. [6] This jet is estimated to have an extension of 155 kiloparsecs. [7] On the western edge of its southeast lobe, there is a ring feature girding the jet's path with an absence of a counter-jet. Strong polarization has been found in the southeast lobe's west side, mainly between 30% to 50%, while the southeast hot spot and the jet shows no traces of polarization. [6] In both the core and lobes, radio emission are present. [8]
The host galaxy of 3C 432 is compact. Based on imaging by Hubble Space Telescope, it is found to have an orientation of 45° along its position angle with a diameter of 1.2 fractional arcseconds. There is also a detection of a secondary radio emission plume that has a position angle of 135°. [9] In additional, the host galaxy is experiencing a starburst with its total star formation rate being 420 Mʘ per year. [10] It is also undergoing a galaxy merger. [11]
Observations made using the AGN radio-to-X-ray spectral energy distribution model fitting code, found the torus emission of the accretion disk of 3C 432, has a best fit by combining clumps and a homogenous disk that is described having a high opacity, with a viewing inclination angle of 33°. [7] A central supermassive black hole mass of 9.72 Mʘ was also calculated for the quasar, with its broad-line luminosity estimating to be 45.57 LBLR. [11] [12]