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The nature of the plasma wave modes around the ion kinetic scales in highlyAlfv\'enic slow solar wind turbulence is investigated using data from theNASA's Parker Solar Probe taken in the inner heliosphere, at 0.18 AstronomicalUnit (AU) from the sun. The joint distribution of the normalized reducedmagnetic helicity ${\sigma}_m ({\theta}_{RB}, {\tau})$ is obtained, where${\theta}_{RB}$ is the angle between the local mean magnetic field and theradial direction and ${\tau}$ is the temporal scale. Two populations around ionscales are identified: the first population has ${\sigma}_m ({\theta}_{RB},{\tau}) < 0$ for frequencies (in the spacecraft frame) ranging from 2.1 to 26Hz for $60^{\circ} < {\theta}_{RB} < 130^{\circ}$, corresponding to kineticAlfv\'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 ACWsin the slow solar wind in the inner heliosphere, which contrasts with previousobservations in the slow solar wind at 1 AU. This discrepancy between 0.18 and1 AU could be explained, either by i) a dissipation of ACWs via cyclotronresonance during their outward journey, or by ii) the high Alfv\'enicity of theslow solar wind at 0.18 AU that may be favorable for the excitation of ACWs.

Kinetic Scale Slow Solar Wind Turbulence in the Inner Heliosphere: Co-existence of Kinetic Alfv\'en Waves and Alfv\'en Ion Cyclotron Waves