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Black hole neutron star (BHNS) mergers have recently been detected throughtheir gravitational-wave (GW) emission. BHNS mergers could also produceelectromagnetic (EM) emission as a short gamma-ray burst (sGRB), and/or an sGRBafterglow upon interaction with the circummerger medium. Here, we makepredictions for the expected detection rates with the Square Kilometre ArrayPhase 1 (SKA1) of sGRB radio afterglows associated with BHNS mergers. We alsoinvestigate the benefits of a multimessenger analysis in inferring theproperties of the merging binary. We simulate a population of BHNS mergers andestimate their sGRB afterglow flux to obtain the detection rates with SKA1. Weinvestigate how this rate depends on the GW detector sensitivity, the primaryblack hole (BH) spin, and the neutron star equation of state. We then perform amultimessenger Bayesian inference study on a fiducial BHNS merger. We simulateits sGRB afterglow and GW emission and take systematic errors into account. Theexpected rates of a combined GW and radio detection with the current generationGW detectors are likely low. Due to the much increased sensitivity of future GWdetectors like the Einstein Telescope, the chances of an sGRB localisation andradio detection increase substantially. The unknown distribution of the BH spinhas a big influence on the detection rates, however, and it is a large sourceof uncertainty. Furthermore, for our fiducial BHNS merger we are able to inferboth the binary source parameters as well as the parameters of the sGRBafterglow simultaneously when combining the GW and radio data. The radio dataprovides useful extra information on the binary parameters such as the massratio but this is limited by the systematic errors involved. A betterunderstanding of the systematics will further increase the amount ofinformation on the binary parameters that can be extracted from this radiodata.

Investigating the detection rates and inference of gravitational-wave and radio emission from black hole neutron star mergers