  We investigate the shape of the Rotation Curves (RCs) of $z\sim 1$
star-forming galaxies and compare them with the local star-forming galaxies.
For this purpose, we have used $409$ galaxies from the K-band Multi-Object
Spectrograph (KMOS) for Redshift One Spectroscopic Survey (KROSS). This sample
covers the redshift range $0.57\leq z \leq 1.04$, effective radii $0.69 \leq
R_e \left[kpc \right] \leq 7.73$, absolute H-band magnitude $-24.46 \leq M_H
\leq -18.85$ with median stellar mass $log\left(M_* \ \left[M_\odot
\right]\right)=9.95$ and median total star-formation rate $log\left(SFR_{tot} \
\left[M_\odot \ yr^{-1} \right]\right)=1.49$. Using $^{3D}$BAROLO (Barolo), we
extract $H\alpha$ kinematic maps and corresponding Rotation Curves (RCs). The
main advantage of Barolo is that it incorporates the beam smearing in the 3D
observational space, which provide us with the intrinsic rotation velocity even
in the low spatial resolution data. Using Asymmetric Drift Correction (ADC), we
have corrected the RCs for the pressure gradient effect, which seems to be a
more dominant effect than beam smearing in high-z galaxies. Nearly all objects
($0.1 <v/ \sigma< 15$) are affected by the pressure gradient, and we noticed
that ADC improves the rotation velocity of these systems by $\sim 10-87\%$.
Only a combination of the three techniques (3D-kinematic modelling +
3D-Beamsmearing correction + ADC ) yields the intrinsic RC of an individual
galaxy. Further, we present the co-added RCs constructed out of 237
high-quality objects to obtain intrinsic RC shapes out to 6.4 $\times$ disk
scale length. We do not see any change in the shape of RCs with respect to the
local star-forming disk-type galaxies. In contrast, we do find a significant
evolution in the stellar-disk length ($R_D$) of the galaxies. Therefore, we
conclude stellar disk evolves over cosmic time while total mass distribution
stays constant.
