  We investigate the stellar kinematics of the bulge and disk components in 826
galaxies with a wide range of morphology from the Sydney-AAO Multi-object
Integral-field spectroscopy (SAMI) Galaxy Survey. The spatially-resolved
rotation velocity (V) and velocity dispersion ($\sigma$) of bulge and disk
components have been simultaneously estimated using the penalized pixel fitting
(pPXF) method with photometrically defined weights for the two components. We
introduce a new subroutine of pPXF for dealing with degeneracy in the
solutions. We show that the V and $\sigma$ distributions in each galaxy can be
reconstructed using the kinematics and weights of the bulge and disk
components. The combination of two distinct components provides a consistent
description of the major kinematic features of galaxies over a wide range of
morphological types. We present Tully-Fisher and Faber-Jackson relations
showing that the galaxy stellar mass scales with both V and $\sigma$ for both
components of all galaxy types. We find a tight Faber-Jackson relation even for
the disk component. We show that the bulge and disk components are
kinematically distinct: (1) the two components show scaling relations with
similar slopes, but different intercepts; (2) the spin parameter $\lambda_R$
indicates bulges are pressure-dominated systems and disks are supported by
rotation; (3) the bulge and disk components have, respectively, low and high
values in intrinsic ellipticity. Our findings suggest that the relative
contributions of the two components explain, at least to first order, the
complex kinematic behaviour of galaxies.
