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(X/peanut)-shaped features observed in a significant fraction of diskgalaxies are thought to have formed from vertically buckled bars. Despite beingthree dimensional structures, they are preferentially detected in near edge-onprojection. Only a few galaxies are found to have displayed such structureswhen their disks are relatively face-on - suggesting that either they aregenerally weak in face-on projection or many may be hidden by the light oftheir galaxy's face-on disk.  Here we report on three (collisionless) simulated galaxies displayingpeanut-shaped structures when their disks are seen both face-on and edge-on -resembling a three-dimensional peanut or dumbbell. Furthermore, thesestructures are accompanied by ansae and an outer ring at the end of the bar ---as seen in real galaxies such as IC~5240.  The same set of quantitative parameters used to measure peanut structures inreal galaxies have been determined for the simulated galaxies, and a broadagreement is found. In addition, the peanut length grows in tandem with thebar, and is a maximum at half the length of the bar. Beyond the cutoff of thesepeanut structures, towards the end of the bar, we discover a newpositive/negative feature in the $B_6$ radial profile associated with theisophotes of the ansae/ring.  Our simulated, self-gravitating, three-dimensional peanut structures displaycylindrical rotation even in the near-face-on disk projection. In addition, wereport on a kinematic pinch in the velocity map along the bar minor-axis,matching that seen in the surface density map.

Building the peanut: simulations and observations of peanut-shaped structures and ansae in face-on disk galaxies