Umbral region of NOAA 10808, before and after flare iii. Top row: the TRACE whitelight intensity image on the left side in the upper row was recorded at 19:36 and rotated and scaled to the SOLIS-VSM data. The green contours are locations where the continuum intensity is below  ~20% of the quiet Sun continuum. These regions marked as A and B are also locations of low polarization signals. The second panel in the upper row is the SOLIS magnetogram that was obtained from the Stokes V profiles (see main text for details) recorded at about 19:56 UT. The last two panels, magnetic field strength in kG and inclination angle γ, are the result of LILIA inversions of the SOLIS-VSM full Stokes profiles recorded around 19:56 UT at optical depth log (τ_500   nm) = -1. The inclination angle is shown in degrees, with a magnetic field vector along the line of sight pointing out of the solar surface with an inclination angle of 0° . The black lines are contours obtained by choosing cutoff levels of 0.002 and −0.002 for the magnetogram. The black areas in the inversion results are uninverted pixels. The noise produced by the deteriorating polarization modulator propagates into the inversion results. Bottom row: the first panel shows the TRACE whitelight image at 20:10 UT. The last three panels in the lower row are the magnetogram and the inversion results obtained from SOLIS data recorded around 20:05 UT. The Stokes profiles found at locations P i to P iv are discussed in Sect. 3.2.