{ "id": "2005.06178", "version": "v1", "published": "2020-05-13T06:43:45.000Z", "updated": "2020-05-13T06:43:45.000Z", "title": "The optical polarization of the blazar PKS 2155$-$304 during an optical flare in 2010", "authors": [ "N. W. Peceur", "A. R. Taylor", "R. C. Kraan-Korteweg" ], "comment": "8 pages, 9 figures", "categories": [ "astro-ph.HE" ], "abstract": "An analysis is presented of the optical polarimetric and multicolour photometric ($BVRJ$) behaviour of the blazar PKS 2155$-$304 during an outburst in 2010. This flare develops over roughly 117 days, with a flux doubling time $\\tau \\sim 4$ days that increases from blue to red wavelengths. The polarization angle is initially aligned with the jet axis but rotates by roughly $90^\\circ$ as the flare grows. Two distinct states are evident at low and high fluxes. Below 18 mJy, the polarization angle takes on a wide range of values, without any clear relation to the flux. In contrast, there is a positive correlation between the polarization angle and flux above 18 mJy. The polarization degree does not display a clear correlation with the flux. We find that the photopolarimetric behaviour for the high flux state can be attributed to a variable component with a steady power-law spectral energy distribution and high optical polarization degree (13.3%). These properties are interpreted within the shock-in-jet model, which shows that the observed variability can be explained by a shock that is seen nearly edge-on. Some parameters derived for the relativistic jet within the shock-in-jet model are: $B=0.09$ G for the magnetic field, $\\delta=22.3$ for the Doppler factor and $\\Phi=2.6^\\circ$ for the viewing angle.", "revisions": [ { "version": "v1", "updated": "2020-05-13T06:43:45.000Z" } ], "analyses": { "keywords": [ "blazar pks", "optical flare", "polarization angle", "steady power-law spectral energy distribution", "shock-in-jet model" ], "note": { "typesetting": "TeX", "pages": 8, "language": "en", "license": "arXiv", "status": "editable" } } }