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We present multicolour Hubble Space Telescope images of the powerful z=2.4radio galaxy MRC 0406-244 and model its complex morphology with severalcomponents including a host galaxy, a point source, and extended nebular andcontinuum emission. We suggest that the main progenitor of this radio galaxywas a normal, albeit massive (M ~10^{11} solar masses), star-forming galaxy.The optical stellar disc of the host galaxy is smooth and well described by aS\'ersic profile, which argues against a recent major merger, however there isalso a point-source component which may be the remnant of a minor merger. Thehalf-light radius of the optical disc is constrained to lie in the range 3.5 to8.2kpc, which is of similar size to coeval star forming galaxies.  Biconical shells of nebular emission and UV-bright continuum extend out fromthe host galaxy along the radio jet axis, which is also the minor axis of thehost galaxy. The origin of the continuum emission is uncertain, but it is mostlikely to be young stars or dust-scattered light from the AGN, and it ispossible that stars are forming from this material at a rate of200^{+1420}_{-110} solar masses per year.

The host galaxy of the z=2.4 radio-loud AGN MRC 0406-244 as seen by HST