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The shape of the ion energy spectra plays a critical role toward determiningthe ion energetics, the acceleration mechanisms and the possible sources ofdifferent plasma and suprathermal ion populations. The determination of theexact shape of the total particle spectrum, provide the necessary means toaddress the inner heliosheath (IHS) dynamics. Apart from various modelingefforts, a direct fit to the measured ion spectra for an extended energy rangeof $\sim$0.11 to 344 MeV has not been performed to date.  We use an extended set of combined 0.11-55 keV ENA measurements from theInterstellar Boundary Explorer (IBEX-Lo and IBEX-Hi) and Cassini/Ion andNeutral Camera (INCA), converted to protons, together with $\sim$28 keV to 344MeV ion measurements from the Low Energy Charged Particle (LECP) and Cosmic RaySubsystem (CRS) experiments on Voyager 2, over the declining phase of SolarCyle 23 (SC23) and ascending phase Solar Cylce 24 (SC24) (2009-2016) to studythe characteristics of the particle energy spectrum.  We fit the 0.11 keV to 344 MeV composite spectra with a set of regularizedisotropic $\kappa$-distribution functions (RKD) allowing the determination ofthe macroscopic physical properties.  We demonstrate that the 2009-2012 spectrum that corresponds to the decliningphase of SC23 is well fitted by three different RKDs, while the 2013-2016spectrum, associated with the rise of SC24, can only be approximated with sixdifferent RKDs.  Our results are generally consistent with shock accelerated particles thatundergo additional acceleration inside the IHS. We identify a low energytransmitted population of particles, a suprathermal reflected population and avery high energy component that is modulated by GCRs. The 2013-2016 time periodis most likely associated with a mixture of particles from SC23 and SC24, whichis reflected by the need to employ six RDKs.

On the properties of 0.11 keV to 344 MeV ion spectra in the inner heliosheath using regularized $\kappa$-distributions