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Detecting the thermal emission from double neutron star merger events is achallenging task because of the quick fading of the observed flux. In order tocreate an efficient observing strategy for their observing method it is crucialto know their intrinsic rate. Unfortunately, the numerous models existing todaypredict this rate on a vary wide range. Hence, our goal in this paper is toinvestigate the effect of different level of approximations on the relativerate predictions. Also, we study the effect of distinct ejecta mass lay-outs onthe light curve. We find that the ratio of the expected kilonova detections ofthe spherical to axisymmetrical models is 6:1 (or 2:1, depending on the inputparameter set applied in our work). Nevertheless, the light curve shape is onlyslightly affected by the various ejecta alignments. This means that differentejecta layouts can produce light curves with similar shapes making it achallenging task to infer the structure of the matter outflow. Thus, weconclude that the uncertainty in the rate predictions arising from the variousejecta mass distribution models is negligible compared to the errors present inother input parameters (e.g. binary neutron star merger rate). In addition, weshow that up to moderate redshifts (z < 0.2) the redshift distribution type(observed or uniform in volume) does not affect the expected relative rateestimations.

Kilonova rates from spherical and axisymmetrical models