  Using a numerical simulation of an isolated barred disc galaxy, we first
demonstrate that the resonances of the inner bar structure induce more
prominent features in the action space distribution for the kinematically
hotter stars, which are less sensitive to the local perturbation, such as the
transient spiral arms. Then, we analyse the action distribution for the
kinematically hotter stars selected from the Gaia EDR3 data as the stars with
higher values of radial and vertical actions. We find several resonance
features, including two new features, in the angular momentum distribution
similar to what are seen in our numerical simulations. We show that the bar
pattern speeds of about $\Omega_{\rm bar}\sim34$~km~s$^{-1}$~kpc$^{-1}$ and
42~km~s$^{-1}$~kpc$^{-1}$ explain all these features equally well. The
resonance features we find correspond to the inner 4:1, co-rotation, outer 4:1,
outer Lindblad and outer 4:3 (co-rotation, outer 4:1, outer Lindblad, outer 4:3
and outer 1:1) resonances, when $\Omega_{\rm bar}\sim34$ (42)
km~s$^{-1}$~kpc$^{-1}$ is assumed.
