  Studies have shown that remnants of destroyed planets and debris-disk
planetesimals can survive the volatile evolution of their host stars into white
dwarfs, but detection of intact planetary bodies around white dwarfs are few.
Simulations predict that planets in Jupiter-like orbits around stars of $\lt 8
M_\odot$ avoid being destroyed by the strong tidal forces of their stellar
host, but as yet there has been no observational confirmation of such a
survivor. Here we report on the non-detection of a main-sequence lens star in
the microlensing event MOA-2010-BLG-477Lb using near-infrared observations from
the Keck Observatory. We determine this system contains a $0.53\pm0.11$ solar
mass white dwarf host orbited by a $1.4 \pm 0.3$ Jupiter mass planet with a
separation on the plane of the sky of $2.8\pm 0.5$ AU, which implies a
semi-major axis larger than this. This system is evidence that planets around
white dwarfs can survive the giant and asymptotic giant phases of their host's
evolution, and supports the prediction that over half of white dwarfs are
predicted to have Jovian planetary companions. Located at approximately 2.0 kpc
toward the center of our Galaxy, it likely represents an analog to the end
stages of the Sun and Jupiter in our own Solar System.
