  Observers experience a series of limitations when measuring galaxy
kinematics, such as variable seeing conditions and aperture size. These effects
can be reduced using empirical corrections, but these equations are usually
applicable within a restrictive set of boundary conditions (e.g. S\'ersic
indices within a given range) which can lead to biases when trying to compare
measurements made across a full kinematic survey. In this work, we present new
corrections for two widely used kinematic parameters, $\lambda_R$ and
$V/\sigma$, that are applicable across a broad range of galaxy shapes,
measurement radii and ellipticities. We take a series of mock observations of
N-body galaxy models and use these to quantify the relationship between the
observed kinematic parameters, structural properties and different seeing
conditions. Derived corrections are then tested using the full catalogue of
galaxies, including hydro-dynamic models from the EAGLE simulation. Our
correction is most effective for regularly-rotating systems, yet the kinematic
parameters of all galaxies -- fast, slow and irregularly rotating systems --
are recovered successfully. We find that $\lambda_R$ is more easily corrected
than $V/\sigma$, with relative deviations of 0.02 and 0.06 dex respectively.
The relationship between $\lambda_R$ and $V/\sigma$, as described by the
parameter $\kappa$, also has a minor dependence on seeing conditions. These
corrections will be particularly useful for stellar kinematic measurements in
current and future integral field spectroscopic (IFS) surveys of galaxies.
