  We investigate the effect of star formation on turbulence in the Orion A and
Ophiuchus clouds using principal component analysis (PCA). We measure the
properties of turbulence by applying PCA on the spectral maps in $^{13}$CO,
C$^{18}$O, HCO$^+$ $J=$1$-$0, and CS $J=$2$-$1. First, the scaling relations
derived from PCA of the $^{13}$CO maps show that the velocity difference
($\delta v$) for a given spatial scale ($L$) is the highest in the integral
shaped filament (ISF) and L1688, where the most active star formation occurs in
the two clouds. The $\delta v$ increases with the number density and total
bolometric luminosity of the protostars in the sub-regions. Second, in the ISF
and L1688 regions, the $\delta v$ of C$^{18}$O, HCO$^+$, and CS are generally
higher than that of $^{13}$CO, which implies that the dense gas is more
turbulent than the diffuse gas in the star-forming regions; stars form in dense
gas, and dynamical activities associated with star formation, such as jets and
outflows, can provide energy into the surrounding gas to enhance turbulent
motions.
