A Multi-Wavelength Polarimetric Study of the Blazar Cta 102 During a Gamma-Ray Flare in 2012

We perform a multi-wavelength polarimetric study of the quasar CTA 102 during an extraordinarily bright γ -ray outburst detected by the Fermi Large Area Telescope in 2012 September–October when the source reached a flux of F >100 MeV = 5.2 ± 0.4 × 10 −6 photons cm −2 s −1 . At the same time, the source displayed an unprecedented optical and near-infrared (near-IR) outburst. We study the evolution of the parsec-scale jet with ultra-high angular resolution through a sequence of 80 total and polarized intensity Very Long Baseline Array images at 43 GHz, covering the observing period from 2007 June to 2014 June. We find that the γ -ray outburst is coincident with flares at all the other frequencies and is related to the passage of a new superluminal knot through the radio core. The powerful γ -ray emission is associated with a change in direction of the jet, which became oriented more closely to our line of sight ( θ ∼ 1 2) during the ejection of the knot and the γ -ray outburst. During the flare, the optical polarized emission displays intra-day variability and a clear clockwise rotation of electric vector position angles (EVPAs), which we associate with the path followed by the knot as it moves along helical magnetic field lines, although a random walk of the EVPA caused by a turbulent magnetic field cannot be ruled out. We locate the γ -ray outburst a short distance downstream of the radio core, parsecs from the black hole. This suggests that synchrotron self-Compton scattering of NIR to ultraviolet photons is the probable mechanism for the γ -ray production.