The WLM phase corrections were applied to all of the data into the OVRO test track. 3C84 was used as the phase calibrator and to remove instrumental drifts. No gain calibration was applied to the data. Cleaned images of the quasar 0309+411 were then made using the IMAGR task in AIPS. This figure highlights the change in the image quality after applying the full phase corrections using the WLM data.

The top panels of this figure show the resulting images before applying any water line corrections. Images are made using data from the entire track, the first half only, and the second half of the track where the phase stability was the worst. The bottom panels show the corresponding images after applying the water line corrections. The color stretch and contour levels are the same in each panel. The "before" images show extended emission up to 2 arcseconds in angular extent which is caused by phase errors in the astronomy data. After applying the WLM phase corrections, the phase errors are reduced, as evidenced by the fact that the source is more compact and the amplitude is larger.