Overview of the ¹⁰Be anomaly, clusters proximity to the Solar System, and the associated SN probability. Top left: ¹⁰Be decay corrected profile (¹⁰Be_dc), normalized by the ¹⁰Be mean equilibrium surface concentration (¹⁰Be_m), for the crust VA13/2-237KD-a, as reported in Fig. 4 of Koll et al. (2025) (kindly provided in a processed form by the authors upon request). A Gaussian centered at 10.1 Myr, with a full width at half maximum of 1.4 Myr, is overplotted in blue. The two vertical black lines mark the onset and end of the anomaly. Bottom left: Distance between the Sun and the four clusters discussed in Sect. 4 over the past 20 Myr. The color bar saturates at 100 pc, the threshold distance adopted in this work for the SN probability study. If a cluster formed within this time interval, its formation time is marked by a star, and an error bar indicates the associated uncertainty. Right: Probability of having at least one SN event between the onset and the peak of the anomaly (11.5–10.1 Myr ago) as a function of distance. The total probability for all clusters considered in this study, as well as for each of the four main clusters, is shown. Statistical errors for the data points are within 3%. The numerical values corresponding to this figure are reported in Table B.3.