  Super-Jupiters, brown dwarfs, and stars can form from the collapse of
self-gravitating discs. Such discs are turbulent, with flocculent spiral arms
accelerating gas to transonic speeds horizontally and vertically. Objects that
fragment from gravito-turbulent discs should spin with a wide range of
directions, reflecting the random orientations of their parent eddies. We show
by direct numerical simulation that obliquities of newly collapsed fragments
can range up to 45$^\circ$. Subsequent collisions between fragments can further
alter the obliquity distribution, up to 90$^\circ$ or down to near-zero. The
large obliquities of newly discovered super-Jupiters on wide orbits around
young stars may be gravito-turbulent in origin. Obliquely spinning fragments
are born on orbits that may be inclined relative to their parent discs by up to
20$^\circ$, and gravitationally stir leftover material to many times the
pre-fragmentation disc thickness.
