tokens: of the largest angular scale being exceeded can be seen around zero velocity. It is important to be prudent when dealing with such data, as the potential for misinterpretation is significant. For instance, erroneously assuming a spherically symmetrical outflow for a source which is intrinsically EDE-like, or has both a radial outflow and an EDE-like component, may result in serious deviations on the estimations of the physical properties of the system. This has been shown by e.g. Homan et al. (2015) . The authors outline and quantify the uncertainties related to a misinterpretation of embedded spiral shapes in stellar winds. Their conclusions on the uncertainties, related to falsely interpreting the emission from a narrow spiral (which is effectively a kind of equatorial density enhancement) as originating from a simple spherically outflowing stellar wind, are also applicable here. 6.2. ALMA Using CASA we have simulated ALMA observations of the Keplerian disk model with a bipolar outflow. Since the considered radiative transfer model has no substructure, there is no reason to explore the effect of angular resolution. Its effect will only be of importance if the aim is to properly resolve the inner EDE, the edges of the EDE or the EDE-wind boundary. We have opted to show the effect of exceeding the chosen configuration’s largest angular scale (LAS), determined by the shortest baseline of the interferometer, on the emission distribution in the PV diagrams of the Keplerian disk model with a bipolar outflow. Table 5 The ALMA observation simulation specifications. A synthetic observation is shown in Fig. 23 , for which the main simobserve parameters are presented in Table 5 . To obtain the results in Fig. 23 we have simulated an observation with the most compact of the extended configurations, C36-1. This configuration has an angular resolution of 1.5 and a largest angular scale of 11. To properly show the effect of a decent observation, we have rescaled the pixel size to artificially place the object at the minimal distance for no EDE flux to be lost. Morphologically, the intrinsic emission and the emission in Fig. 23 are very similar, as expected. The sheer number of antennae available for cycle3 ensures even for modest integration times a decent filling of the UV-plane. The high inclination models show that even though the signature of the EDE is barely unaltered, the bipolar wind emission has exceeded the LAS of the antenna configuration around zero velocity. Some of the flux of the wind is thus lost. Because our models are confined to a numerical region, and bipolar outflows are not expected to exhibit such abrupt edges, this effect is expected to be more pronounced in real physical objects. Fig. 25 Synthetic ALMA observation simulation of the Keplerian disk model (with a bipolar outflow) with the C36-1 antenna configuration (, ), for which the original model has been rescaled to a size 18 times greater than it was in Fig. 23 . The effect
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