Light curves of the blazar TXS 2013+370 at different frequencies. From top to bottom: Fermi-LAT 0.1–100 GeV with 1-month binning, flux plotted vs. time for 226 GHz SMA, and 15 GHz OVRO. The dashed vertical lines indicate the estimated ejection times of the components N, N1 (Traianou et al. 2020), and the new knot N2, respectively, whereas the width of the shadow areas designates the uncertainty of these estimations. For N2, the uncertainty is based on the uncertainty of component A1 as it was found in Traianou et al. (2020). The dashed gray line indicates a new flaring activity in the source.