Extended Data Fig. 1: The logarithmic far-UV flux distribution of J1858 during our observations.
From: A persistent ultraviolet outflow from an accreting neutron star binary transient
The distribution is clearly bimodal, consistent with the visual impression from the light curve (Fig. 1b) of the variability being due to a flaring component that is superposed on a roughly constant component. The grey line is the optimal decomposition of the distribution into two Gaussians, as suggested by the KMM algorithm42. The blue and red lines correspond to the individual Gaussians. KMM rejects the null hypothesis of a single component with extremely high significance (p < 10−43).
