  A significant part of barred disc galaxies exhibits boxy/peanut-shaped
structures (B/PS bulges) at high inclinations. Another structure also
associated with the bar is a barlens, often observed in galaxies in a position
close to face-on. At this viewing angle, special kinematic tests are required
to detect a 3D extension of the bars in the vertical direction (B/PS bulges).
We use four pure $N$-body models of galaxies with B/PS bulges, which have
different bar morphology from bars with barlenses to the so-called face-on
peanut bars. We analyse the kinematics of our models to establish how the
structural features of B/PS bulges manifest themselves in the kinematics for
galaxies at intermediate inclinations and whether these features are related to
the barlenses. We apply the dissection of the bar into different orbital groups
to determine which of them are responsible for the features of the LOSVD
(line-of-sight velocity distribution), i.e., for the deep minima of the $h_4$
parameter along the major axis of the bar. As a result, we claim that for our
models at the face-on position, the kinematic signatures of a `peanut' indeed
track the vertical density distribution features. We conclude that orbits
responsible for such kinematic signatures differ from model to model. We pay
special attention to the barlens model. We show that orbits assembled into
barlens are not responsible for the kinematic signatures of B/PS bulges. The
results presented in this work are applicable to the interpretation of IFU
observations of real galaxies.
