Spatially resolved spectra of two vibrationally excited H₂O lines detected toward W Hya. Panel (a): The continuum-subtracted intensity map of the 268 GHz H₂O line (v₂ = 2, 6_5, 2–7_4, 3) integrated from V_rel = −1.5 to 1.5 km s⁻¹ to show the most prominent emission components. The crosses and numbers correspond to the positions where the spatially resolved spectra shown in the lower two columns were obtained (the spectra were extracted at the marked pixels). Panels (b)–(i): Spatially resolved spectra obtained at positions 1–4 over the stellar disk and positions 5–8 off the limb of the stellar disk. The orange and blue lines show the continuum-subtracted spectra of the H₂O lines v₂ = 2, 6_5, 2–7_4, 3 (268 GHz) and v₂ = 2, 9_2, 8–8_3, 5 (251 GHz), respectively. In panels (f)–(i), the left and right ordinates correspond to the intensity of the lines at 268 and 251 GHz, respectively. The spectra of the v₂ = 2, 9_2, 8–8_3, 5 line are shown only up to V_rel = 3.2 km s⁻¹, because the data at more redshifted velocities are affected by the blend due to the adjacent Si¹⁷O line at 250.744695 GHz. The weak emission seen at V_rel < −20 km s⁻¹ in the 268 GHz line in panels (f)–(i) is due to the SO₂ (v₂ = 1, 11_3, 9–11_2, 10) line at 268.169791 GHz. The dotted lines in panels (b)–(e) mark the RMS noise level.