Best-fit stellar patch model with an inhomogeneous velocity field for Antares observed in 2009. Panels a)–d) show model images in the continuum, blue wing, line center, and red wing within the same CO line profile as shown in Fig. 5. The wavelengths of these images are marked with black, blue, green, and red dots in panel e), where the observed and model spectra are plotted by the filled diamonds and the black solid line, respectively. Panels f)–h) show the best-fit continuum-subtracted model images convolved with the same beam as the observed images. Therefore, these model images can be compared to the images shown in Figs. 5j–5l.