X-ray Emission and Radio Emission from the Jets and Lobes of the
  Spiderweb Radio Galaxy
  Deep Chandra and VLA imaging reveals a clear correlation between X-ray and
radio emission on scales $\sim 100$~kpc in the Spiderweb radio galaxy at
z=2.16. The X-ray emission associated with the extended radio source is likely
dominated by inverse Compton up-scattering of cosmic microwave background
photons by the radio emitting relativistic electrons. For regions dominated by
high surface brightness emission, such as hot spots and jet knots, the implied
magnetic fields are $\sim 50~\mu$G to $70~\mu$G. The non-thermal pressure is
these brighter regions is then $\sim 9\times 10^{-10}$ dyne cm$^{-2}$, or three
times larger than the non-thermal pressure derived assuming minimum energy
conditions, and an order of magnitude larger than the thermal pressure in the
ambient cluster medium. Assuming ram pressure confinement implies an average
advance speed for the radio source of $\sim 2400$ km s$^{-1}$, and a source age
of $\sim 3\times 10^7$ years. Considering the lower surface brightness, diffuse
radio emitting regions, we identify an evacuated cavity in the Ly$\alpha$
emission coincident with the tail of the eastern radio lobe. Making reasonable
assumptions for the radio spectrum, we find that the relativistic electrons and
fields in the lobe are plausibly in pressure equilibrium with the thermal gas,
and close to a minimum energy configuration. The radio morphology suggests that
the Spiderweb is a high-$z$ example of the rare class of hybrid morphology
radio sources (or HyMoRS), which we attribute to interaction with the
asymmetric gaseous environment indicated by the Ly$\alpha$ emission.
