  Star formation is a complex process that typically occurs in dense regions of
molecular clouds mainly regulated by magnetic fields, magnetohydrodynamic (MHD)
turbulence, and self-gravity. However, it remains a challenging endeavor to
trace the magnetic field and determine regions of gravitational collapse where
the star is forming. Based on the anisotropic properties of MHD turbulence, a
new technique termed Velocity Gradient Technique (VGT) has been proposed to
address these challenges. In this study, we apply the VGT to two regions of the
giant California Molecular Cloud (CMC), namely, L1478 and L1482, and analyze
the difference in their physical properties. We use the $^{12}$CO (J = 2 - 1),
$^{13}$CO (J = 2 - 1), and C$^{18}$O (J = 2 - 1) emission lines observed with
the Heinrich Hertz Submillimeter Telescope. We compare VGT results calculated
in the resolutions of $3.3'$ and $10'$ to Planck polarization at 353 GHz and
$10'$ to determine areas of MHD turbulence dominance and self-gravity
dominance. We show that the resolution difference can introduce misalignment
between the two measurements. We find the VGT-measured magnetic fields globally
agree with that from Planck in L1478 suggesting self-gravity's effect is
insignificant. The best agreement appears in VGT-$^{12}$CO. As for L1482, the
VGT measurements are statistically perpendicular to the Planck polarization
indicating the dominance of self-gravity. This perpendicular alignment is more
significant in VGT-$^{13}$CO and VGT-C$^{18}$O.
