Low-frequency Observations as a Proxy for Jet power in RL AGN

Radio-loud Active Galactic Nuclei (AGN), powered by a supermassive black hole (SMBH), have bipolar large-scale jets of relativistic plasma. These jets cause material to propagate away from the SMBH and into radio-emitting lobes, which are built over the lifetime of the source. When looking at a low frequency SED, the two major components are the lobe emission and the jet emission. The jet emits via synchrotron emission and is relativistically beamed along the jet axis, which cause its apparent flux level to be highly affected by the orientation of the jets. The extended emission, however, emits isotopically, and so is independent of the jet orientation. This extended emission can be separated from the rest of the spectrum for a time-integrated measurement of the power of the source. Once the total spectrum is decomposed into these two components, each can be individually analyzed for parameters that hold key information about the power and orientation of the jets. These spectra will be used to revisit the “Blazar Envelope” (Meyer et al. 2011) and to look further into population statistics for these sources.