Cygnus A, the archetype of powerful Fanaroff-Riley class II radio galaxies, is hosted by the central galaxy of a cool core cluster, in a dense, high pressure environment. I will focus on what deep Chandra observations of Cygnus A have revealed about the radio galaxy and interactions with its environment. Measuring properties of its cocoon shocks has revealed that the pressure is relatively...
Observations performed in the last decades have shown that supermassive black holes (SMBHs) and cosmic structures are not separate elements of the Universe. While galaxies have sizes roughly ten orders of magnitude larger than SMBHs, black holes would not exist without matter feeding them, and cosmic structures would not be the same without feedback from SMBHs. Powerful winds/jets in active...
The broad-line radio galaxy 3C 120 has the properties of a Seyfert galaxy at optical through X-ray frequencies, and a quasar-like blazar at radio frequencies. It is one of a very small number - and probably the best - of active galaxies suitable for probing the relationship between the accretion disk/corona and a relativistic jet. We recently monitored 3C 120 with Swift at optical/UV/X-ray...
We present results from two observations of the M87 jet taken with the Chandra High Resolution Camera (HRC) separated by ~5 years. We detect proper motions in knot HST-1 and knot D of 24.1pm1.6 mas/yr and 9.2pm2.6 mas/yr, respectively. This corresponds to superluminal velocities of 6.3pm0.4c and 2.4pm0.6c, respectively, along the axis of the jet. These velocities are consistent with the...
The change in a boundary shape of a jet in M87 was discovered first by Asada and Nakamura (2012). This jet is characterized by the initially quasi-parabolic flow changing into the approximately conical one. We propose that the change in a jet boundary shape is due to a transition of an outflow from the Poynting dominated to particle-dominated (equipartition) regime. We propose a model with an...
In this contribution, I will present the results of a paper on the Flat Spectrum Radio Quasar 3C 279. We use light curves that cover a time-frame of six years, at different wavelengths: Gamma-rays, X-rays, UV 3000 Å continuum, optical V band, Near-Infrared (NIR) JHK bands, 1mm, as well as optical spectropolarimetry.
By applying cross-correlation analysis, We find that the UV continuum,...
