  The nature of the plasma wave modes around the ion kinetic scales in highly
Alfv\'enic slow solar wind turbulence is investigated using data from the
NASA's Parker Solar Probe taken in the inner heliosphere, at 0.18 Astronomical
Unit (AU) from the sun. The joint distribution of the normalized reduced
magnetic helicity ${\sigma}_m ({\theta}_{RB}, {\tau})$ is obtained, where
${\theta}_{RB}$ is the angle between the local mean magnetic field and the
radial direction and ${\tau}$ is the temporal scale. Two populations around ion
scales are identified: the first population has ${\sigma}_m ({\theta}_{RB},
{\tau}) < 0$ for frequencies (in the spacecraft frame) ranging from 2.1 to 26
Hz for $60^{\circ} < {\theta}_{RB} < 130^{\circ}$, corresponding to kinetic
Alfv\'en waves (KAWs), and the second population has ${\sigma}_m
({\theta}_{RB}, {\tau}) > 0$ in the frequency range [1.4, 4.9] Hz for
${\theta}_{RB} > 150^{\circ}$, corresponding to Alfv\'en ion Cyclotron Waves
(ACWs). This demonstrates for the first time the co-existence of KAWs and ACWs
in the slow solar wind in the inner heliosphere, which contrasts with previous
observations in the slow solar wind at 1 AU. This discrepancy between 0.18 and
1 AU could be explained, either by i) a dissipation of ACWs via cyclotron
resonance during their outward journey, or by ii) the high Alfv\'enicity of the
slow solar wind at 0.18 AU that may be favorable for the excitation of ACWs.
