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tokens: not particularly affect the results. Missed associations in this case are due the fact that the light curve iPTF 17cw is not well sampled at early times. Our discussion in Section 4.1.1 clarifies this point. In the case of sources with redshift randomly distributed between 0.01 and 0.1 our results are, as expected, in between the two previously described cases. Specifically, 92% of all simulated sources are detected, and 87% of the detected sources are uniquely and correctly associated. In particular, 100% of the targets simulated from the templates of SN 1998bw and SN 2009bb, 69% of SN 2006aj, and 99% of iPTF 17cw are detected. Of those detected sources, 100% of the targets simulated from the templates of SN 1998bw and SN 2009bb, 48% of SN 2006aj, and 88% of iPTF 17cw are uniquely and correctly associated. For completeness, in Figure 2 we also plot the the efficiency of the optimized observing campaign as a function of total time delay for SN 2006aj-like and PTF17cw-like targets, with redshifts randomly distributed between 0.01 and 0.1. The total time delay is calculated as the sum of the delay between the explosion and the optical detection, and the delay between the optical detection and the first radio observation (which defines the urgency of the radio observing campaign; see Section 3.3 ). In this figure the efficiency (fraction of unique and correct associations) is calculated relative to the number of simulated sources that are detected in each delay bin. We note that for SN 1998bw-like and SN 2009bb-like targets, the efficiency is 100% regardless of the total time delay (and thus, regardless of the adopted observing urgency strategy in the radio). In the case of SN 2006aj-like targets, we completely miss those that are observed with total delays ≳22 days, when SN 2006aj was undetected. Figure 2. Fraction of targets that are uniquely and correctly associated as a function of the total delay between the SN explosion and the first radio observation for sources with z = 0.01–0.1. 4.1.1. Relevance of Early-time Radio Observations for Relativistic SNe In this section we assess the importance of early-time radio observations for correctly and uniquely associating relativistic SNe via an optimized radio follow-up campaign. To this end, we extrapolate the template light curves of SN 2009bb and iPTF 17cw using the early-time behavior of the much better sampled radio light curves of SN 1998bw and SN 2006aj, respectively. We choose to use SN 1998bw to extrapolate the light curve of SN 2009bb, and SN 2006aj to extrapolate the light curve of iPTF 17cw, because they are the most similar to each other. In fact, both SN 1998bw and SN 2009bb were nearby explosions that resulted in a very bright radio signal. On the other hand, both SN 2006aj and iPTF 17cw were very dim and faded away very rapidly. We repeat the simulations and optimization procedure described in the previous section including these early-time extrapolations. Since all sources