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Binary neutron star mergers offer a new and independent means of measuringthe Hubble constant $H_0$ by combining the gravitational-wave inferred sourceluminosity distance with its redshift obtained from electromagnetic follow-up.This method is limited by intrinsic degeneracy between the system distance andorbital inclination in the gravitational-wave signal. Observing the afterglowcounterpart to a merger can further constrain the inclination angle, allowingthis degeneracy to be partially lifted and improving the measurement of $H_0$.In the case of the binary neutron star merger GW170817, afterglow light-curveand imagery modeling thus allowed to improve the $H_0$ measurement by a factorof 3. However, systematic access to afterglow data is far from guaranteed. Infact, though each one allows a leap in $H_0$ precision, these afterglowcounterparts should prove rare in forthcoming multimessenger campaigns. Wecombine models for emission and detection of gravitational-wave andelectromagnetic radiation from binary neutron star mergers with realisticpopulation models and estimates for afterglow inclination angle constraints.Using these models, we quantify how fast $H_0$ will be narrowed-down bysuccessive multimessenger events with and without the afterglow. We find that,because of its rareness and though it greatly refines angle estimates, theafterglow counterpart should not significantly contribute to the measurement of$H_0$ in the long run.

The potential role of binary neutron star merger afterglows in multimessenger cosmology