Gravitational wave observations of neutron star systems are very important to constrain the neutron star equation of state. Empirical relations between the characteristics of the gravitational wave signal and stellar parameters of static stars are employed to connect the observable signal with the underlying physics. Here, we consider empirical relations linking the frequency of the fundamental quadrupolar fluid mode in isolated neutron stars and the dominant post-merger oscillation frequency in binary neutron star mergers to the radius of static stars. We consider how individual data points distribute with respect to the corresponding fit to all points for both neutron star systems. We find that the deviations from the respective fit follow a very similar behavior in these two systems. We outline how to employ the scatter of the points to more accurately relate the radius and the tidal deformability.