  We study the effects of planetary late migration on the gas giants
obliquities. We consider the planetary instability models from Nesvorny &
Morbidelli (2012), in which the obliquities of Jupiter and Saturn can be
excited when the spin-orbit resonances occur. The most notable resonances occur
when the $s_7$ and $s_8$ frequencies, changing as a result of planetary
migration, become commensurate with the precession frequencies of Jupiter's and
Saturn's spin vectors. We show that Jupiter may have obtained its present
obliquity by crossing of the $s_8$ resonance. This would set strict constrains
on the character of migration during the early stage. Additional effects on
Jupiter's obliquity are expected during the last gasp of migration when the
$s_7$ resonance was approached. The magnitude of these effects depends on the
precise value of the Jupiter's precession constant. Saturn's large obliquity
was likely excited by capture into the $s_8$ resonance. This probably happened
during the late stage of planetary migration when the evolution of the $s_8$
frequency was very slow, and the conditions for capture into the spin-orbit
resonance with $s_8$ were satisfied. However, whether or not Saturn is in the
spin-orbit resonance with $s_8$ at the present time is not clear, because the
existing observations of Saturn's spin precession and internal structure models
have significant uncertainties.
