The host galaxy of 3C 343.1 has a blue appearance mainly due to the presence of an early-type stellar population or a recent wave of star formation.[6] The total star formation rate of the galaxy is estimated to be 1.7+0.5-0.4 x 1011 Mʘ, with the host infraredluminosity estimated to be 2.9+0.6-0.5 x 1011Lʘ. It has a supermassive black hole mass of 28.7 x 107 Mʘ.[7] The nucleus of the galaxy has been categorized as compact.[8]
3C 343.1 has a compact source. When observed with the Very Large Array (VLA), the source has an elongated appearance in the position angle of 110°, with two clearly resolved components observed on a 15 GHz radio map.[9] An 18 centimeter observation with Very Long Baseline Interferometry (VLBI), showed the source is double with two asymmetrical components displaying high surface brightness profiles. The components also display a steep radio spectrum described as straight.[10] Newer VLBI observations made in 2021 at 327 GHz frequencies found the source displays asymmetric lobes that are separated by around 215 milliarcseconds. No radio core has been discovered, although the components have a flat radio spectrum with observed steepening at 610 MHz.[11] A radio jet is present in the source, with a linear size of 1.57 kiloparsecs.[12]
An observation conducted in 1995, found 3C 343.1 has an emission-line nebula region. The radio emission of the region is extended along the direction of the source for more than five arcseconds. making it possible that this could be classified as an extended emission-line region.[13] A linear feature is seen orientating along the east-west axis based on broad-band images.[14] The nuclear spectrum of the galaxy has been found to show either the presence of weak ionization lines or none at all. Little signs of polarization have also been detected in the galaxy.[15]
^Privon, G. C.; O’Dea, C. P.; Baum, S. A.; Axon, D. J.; Kharb, P.; Buchanan, C. L.; Sparks, W.; Chiaberge, M. (April 2008). "WFPC2 LRF Imaging of Emission-Line Nebulae in 3CR Radio Galaxies". The Astrophysical Journal Supplement Series. 175 (2): 423–461. arXiv:0710.3105. Bibcode:2008ApJS..175..423P. doi:10.1086/525024. ISSN0067-0049.
^Kawakatu, Nozomu; Nagao, Tohru; Woo, Jong-Hak (2009-03-10). "Exploring the Disk-Jet Connection From the Properties of Narrow-Line Regions in Power Young Radio-Loud Activie Galactic Nuclei". The Astrophysical Journal. 693 (2): 1686–1695. arXiv:0812.1329. doi:10.1088/0004-637x/693/2/1686. ISSN0004-637X.
^Axon, D. J.; Capetti, A.; Fanti, R.; Morganti, R.; Robinson, A.; Spencer, R. (November 2000). "The Morphology of the Emission-Line Region Of Compact Steep-Spectrum Radio Sources". The Astronomical Journal. 120 (5): 2284–2299. arXiv:astro-ph/0006355. Bibcode:2000AJ....120.2284A. doi:10.1086/316838. ISSN0004-6256.
