Description
HESS J1640-465 is a powerful source of very high energy γ-rays and possibly the most luminous
TeV source in the Milky Way. It is also associated with a radio supernova remnant (SNR) and an
X-ray PWN powered by an energetic pulsar. Determining the origin of the VHE γ-rays requires
measuring, and modeling the broadband non-thermal emission of this source. My recent analysis
of the X-ray PWN and associated γ-ray emission indicates that a PWN powered by the energetic
pulsar could produce the observed γ-rays under some peculiar conditions; a conclusion testable
by measuring the previously undetected radio properties of this PWN. I was recently awarded a
MeerKAT observation to do that, and in this talk, I will present the properties of the detected PWN
and the additional information it provides.
