  We present Atacama Large Millimeter-Submillimeter Array (ALMA) observations
of CK Vulpeculae which is identified with "Nova Vulpeculae 1670". They trace
obscuring dust in the inner regions of the associated nebulosity. The dust
forms two cocoons, each extending ~5 arcsec north and south of the presumed
location of the central star. Brighter emission is in a more compact east-west
structure (2 arcsec by 1 arcsec) where the cocoons intersect. We detect line
emission in NH$_2$CHO, CN, four organic molecules and C$^{17}$O. CN lines trace
bubbles within the dusty cocoons; CH$_3$OH a north-south S-shaped jet; and
other molecules a central cloud with a structure aligned with the innermost
dust structure. The major axis of the overall dust and gas bubble structure has
a projected inclination of ~24 degrees with respect to a 71 arcsec extended
"hourglass" nebulosity, previously seen in H alpha. Three cocoon limbs align
with dark lanes in the inner regions of the same H alpha images. The central 2
arcsec by 1 arcsec dust is resolved into a structure consistent with a warped
dusty disc. The velocity structure of the jets indicates an origin at the
centre of this disc and precession with an unknown period. Deceleration regions
at both the northern and southern tips of the jets are roughly coincident with
additional diffuse dust emission over regions approximately 2 arcsec across.
These structures are consistent with a bipolar outflow expanding into
surrounding high density material. We suggest that a white dwarf and brown
dwarf merged between 1670 and 1672, with the observed structures and
extraordinary isotopic abundances generated as a result.
