The X-ray Emission of Low-Power Radio Galaxies

Abstract

A low-power radio galaxy generally emits X-rays from a compact X-ray core, its brighter kpc-scale radio jet, and a galaxy atmosphere. The core emission is normally predominantly radio related. The kpc-scale jet emission is synchrotron from the radio to X-ray, requiring in situ particle acceleration. The similar integrated radio to X-ray jet spectra, and different radio and X-ray substructures, are best explained if the brightest X-ray regions are sites of strong acceleration, while weaker acceleration occurs throughout the jets, and the X-ray/radio displacements are due to a combination of particle acceleration, advection, diffusion and local ageing. Galaxy atmospheres with steep pressure gradients, such as would prevent disruption of jets where their bulk deceleration is believed to be large, are detected.