Slices of magnetic field magnitude highlighting the non-uniformity of the field. The non-uniformity can partly be attributed to the five magnetic stars in the cluster. The magnetic field reaches 1 mG in the cluster core and can fall to values of 0.1 μG in the cluster wind. Large asymmetries persist into the superbubble, although they smooth out slowly over time. Two main observations are (1) field amplification behind the wind termination shock (e.g. right-most panel) and (2) mixing of flow from magnetic stars into the bulk medium (e.g. left-most panel). The figure shows data for cluster III sliced along the z-axis.