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We present multi-wavelength monitoring results for the broad-line radiogalaxy 3C 120 in the MeV/GeV, sub-millimeter, and 43 GHz bands over six years.Over the past two years, Fermi-LAT sporadically detected 3C 120 with highsignificance and the 230 GHz data also suggest an enhanced activity of thesource. After the MeV/GeV detection from 3C 120 in MJD 56240-56300, 43 GHz VLBAmonitoring revealed a brightening of the radio core, followed by the ejectionof a superluminal knot. Since we observed the gamma-ray and VLBA phenomena intemporal proximity to each other, it is naturally assumed that they arephysically connected. This assumption was further supported by the subsequentobservation that the 43 GHz core brightened again after a gamma-ray flareoccurred around MJD 56560. We can then infer that the MeV/GeV emission tookplace inside an unresolved 43 GHz core of 3C 120 and that the jet dissipationoccurred at sub-parsec distances from the central black hole, if we take thedistance of the 43 GHz core from the central black hole as ~ 0.5 pc, aspreviously estimated from the time lag between X-ray dips and knot ejections(Marscher et al. 2002; Chatterjee et al. 2009). Based on our constraints on therelative locations of the emission regions and energetic arguments, we concludethat the gamma rays are more favorably produced via the synchrotronself-Compton process, rather than inverse Compton scattering of externalphotons coming from the broad line region or hot dusty torus. We also derivedthe electron distribution and magnetic field by modeling the simultaneousbroadband spectrum.

the astrophysical journal. letters

Six Years of Fermi-LAT and Multi-wavelength Monitoring of the Broad-Line  Radio Galaxy 3C 120: Jet Dissipation at Sub-parsec Scales from the Central  Engine