Comparison of the H₂O maser features detected toward VLA 2 (left panel) in the four EVN epochs (2014.46, 2016.45, 2018.44, and 2020.82) and superimposed to the natural-weighted continuum map at K-band (central frequency 22 GHz) of the thermal, collimated ionized wind emitted by VLA 2 obtained with the VLA by Carrasco-González et al. (2015). The light gray contours are 5, 10, 15, 20, 25, 50, and 75 times σ = 10 μJy beam⁻¹ and the VLA beam is shown on the bottom right corner. The positions of the maser features are corrected assuming the proper motion of the subregion W75N(B) equal to the median proper motion measured for the 6.7 GHz CH₃OH maser features by Rygl et al. (2012), ⟨μ_α⟩ = (−1.97 ± 0.10) mas yr⁻¹ and ⟨μ_δ⟩ = (−4.16 ± 0.15) mas yr⁻¹. The size of the symbols are ten times the uncertainties of the absolute positions of the maser features (see Table 2). For clarity, we show the parabolic fit of the maser features of zone 1 and the linear fit of the maser features of zone 2 (north features) and zone 4 for each epoch (right panel). The reference position is α₂₀₀₀ = 20^h38^m36^s​.43399 and δ₂₀₀₀ = +42° 37′34.​​″8710. The parameters of the linear and parabolic fits are reported in Tables 4 and 5, respectively.