  Massive protostars generate strong radiation feedback, which may help set the
mass they achieve by the end of the accretion process. Studying such feedback
is therefore crucial for understanding the formation of massive stars. We
report the discovery of a photoionized bipolar outflow towards the massive
protostar G45.47+0.05 using high-resolution observations at 1.3 mm with the
Atacama Large Millimeter/Submillimeter Array (ALMA) and at 7 mm with the Karl
G. Jansky Very Large Array (VLA). By modeling the free-free continuum, the
ionized outflow is found to be a photoevaporation flow with an electron
temperature of 10,000 K and an electron number density of ~1.5x10^7 cm^-3 at
the center, launched from a disk of radius of 110 au. H30alpha hydrogen
recombination line emission shows strong maser amplification, with G45 being
one of very few sources to show such millimeter recombination line masers. The
mass of the driving source is estimated to be 30-50 Msun based on the derived
ionizing photon rate, or 30-40 Msun based on the H30alpha kinematics. The
kinematics of the photoevaporated material is dominated by rotation close to
the disk plane, while accelerated to outflowing motion above the disk plane.
The mass loss rate of the photoevaporation outflow is estimated to be
~(2-3.5)x10^-5 Msun/yr. We also found hints of a possible jet embedded inside
the wide-angle ionized outflow with non-thermal emissions. The possible
co-existence of a jet and a massive photoevaporation outflow suggests that, in
spite of the strong photoionization feedback, accretion is still on-going.
