  Supermassive black holes (SMBHs) and their host galaxies are generally
thought to coevolve, so that the SMBH achieves up to about 0.2 to 0.5% of the
host galaxy mass in the present day. The radiation emitted from the growing
SMBH is expected to affect star formation throughout the host galaxy. The
relevance of this scenario at early cosmic epochs is not yet established. We
present spectroscopic observations of a galaxy at redshift z = 3.328, which
hosts an actively accreting, extremely massive BH, in its final stages of
growth. The SMBH mass is roughly one-tenth the mass of the entire host galaxy,
suggesting that it has grown much more efficiently than the host, contrary to
models of synchronized coevolution. The host galaxy is forming stars at an
intense rate, despite the presence of a SMBH-driven gas outflow.

Astrophysics of Galaxies;High Energy Astrophysical Phenomena