Kinematics and Dynamics of kiloparsec-scale Jets in Radio Galaxies with
  SKA
  We explore the use of SKA to deduce the physical parameters of
kiloparsec-scale jet flows in radio galaxies. Jets in Active Galactic Nuclei
are relativistic where they are first formed, but their speeds and compositions
change as they propagate. It has long been known that kiloparsec-scale jets in
radio galaxies can be divided into two flavours: strong (found in powerful
sources, narrow and terminating in compact hot-spots) and weak (found in
low-luminosity sources, geometrically flaring, unable to form hot-spots and
terminating in diffuse lobes or tails). We have developed methods to model AGN
jets as intrinsically symmetrical, relativistic flows by fitting to deep,
well-resolved radio images in Stokes I, Q and U. This has yielded a wealth of
information about the brightest few weak-flavour jets. Our first key objective
is to observe large samples of weak and transition jets at 0.1 - 0.5 arcsec
resolution with SKA1-MID. This would allow us to see how jet propagation
depends on power and environment and to quantify the energy and momentum input
into the IGM. We will require typical noise levels of 1 microJy/beam, and may
be able to exploit survey imaging in some cases. Our second, more challenging,
application is to determine the velocity fields in strong-flavour jets. Do they
have very fast spines with bulk Lorentz factors of 5 - 10? Is there evidence
for magnetic confinement by a toroidal field? What are their energy fluxes?
This is a major imaging challenge for SKA2: we need resolution better than 0.05
arcsec, ideally in the 1 - 10 GHz frequency range, with rms noise levels of
roughly 10 nJy/beam and extremely high dynamic range, imaging fidelity and
polarization purity.
