  In light of the recent suggestion that the nearby eclipsing binary star
system V Puppis has a dark companion on a long orbit, we present the results of
radio and X-ray observations of it. We find an upper limit on its radio flux of
about 300 $\mu$Jy and a detection of it in the X-rays with a luminosity of
about 3$\times10^{31}$ erg/sec, a value much lower than what had been observed
in some of the low angular resolution surveys of the past. These data are in
good agreement with the idea that the X-ray emission from V Puppis comes from
mass transfer between the two B stars in the system, but can still accommodate
the idea that the X-ray emission comes from the black hole accreting stellar
wind from one or both of the B stars.
