Flux densities of the H₂O maser features in the whole region around NIRS 3, the NE lobe, central (continuum) position, and the SW lobe observed with VERA (the corresponding spectra are shown in Fig. 10). The flux densities were computed by integrating the emission over the velocity range between − 15 and + 25 km s⁻¹. The error bars represent the 30% flux uncertainty. A dashed vertical line indicates January 01, 2017.