Overlay of the 25 GHz continuum emission (gray scale and white contours) and the 0th moment images of the NH₃ (6, 6), (9, 9), (10, 10), and (13, 13) thermal emission lines (cyan, blue, orange, and red contours, respectively) imaged with the JVLA in W51 IRS2. The 25 GHz continuum contours indicate 1 and 3 mJy flux levels per beam, respectively (the peak is ~160 mJy beam^-1 and the rms is 0.4 mJy beam^-1). The NH₃ contours are 20% to 100% with steps of 10% of the line peak for the (6, 6) line (119 mJy beam^-1 km s^-1) and the (9, 9) line (63 mJy beam^-1 km s^-1), and 30%, 60%, 90% of the line peak for the (10, 10) (66 mJy beam^-1 km s^-1) and the (13, 13) lines (65 mJy beam^-1 km s^-1). The intensity was integrated in the velocity range from 50.3 to 70.7 km s^-1 for the (6, 6) line, +50.4 to +66.0 km s^-1 for the (9, 9) line, +50.2 to +66.2 km s^-1 for the (10, 10) line, and +50.0 to +66.8 km s^-1 for the (13, 13) line, respectively. The big white plus marks the position of the (6, 6), (7, 7), and (9, 9) NH₃ masers. The small white plus marks the position of the W51-North protostar as inferred from SiO masers (Eisner et al. 2002). We note that the most highly excited lines, the (10, 10) and (13, 13) transitions, show a peak at the NH₃ maser position. The images displayed are not corrected for primary beam effects.