Illustration of the systematic distortion of seemingly photospheric absorption lines of Be stars in binaries due to unnoticed weak emission from the envelope with phase-locked V/R changes. Top: sketch of the Be-star circumstellar disk located inside the Roche lobe of a binary system (with a mass ratio of 0.1 in this example). Bottom: plot shows a superposition of the true rotationally broadened photospheric line profile (green) with a weak double-peak emission having V/R > 1 (simulated by the blue and red Gaussians). The resulting (black) profile has a more positive RV than the original profile. This situation corresponds to an observation at the elongation with the Be component receding from us. Just the opposite happens at the other elongation.