Determine the three-dimensional origin of the extended CO component

Determine whether the extended, redshifted CO emission in the northern region of the Gomez’s Hamburger disk arises from the front side, back side, or both sides of the disk, thereby constraining the geometry of the potential outflow or disk wind.

Background

The paper identifies extended, non-Keplerian 12^{12}CO and 13^{13}CO emission toward the northern part of the nearly edge-on Gomez’s Hamburger disk. The morphology may be consistent with outflowing gas, external photoevaporation, or a magnetohydrodynamic disk wind, but projection effects prevent the authors from locating the emitting material unambiguously along the line of sight.

Resolving this ambiguity requires dedicated kinematic modeling and observations capable of tracing the spatial extent, excitation, and velocity structure of the suspected wind or outflow.

References

The redshifted velocities of these features suggest that material entrained in this potential wind is moving away from the observer, but due to projection effects and in the absence of a dedicated kinematic model, it is not clear if it arises from the front or back (or both) sides of the disk.

— The ALMA View of the Edge-on Gomez's Hamburger System: A Highly-Dynamic, Asymmetric Protoplanetary Disk Reveals the Earliest Phases of Giant Planet Formation  (2609.09290 - Law et al., 8 Sep 2026) in Section 3.2, “Possible Disk Wind Signatures in $^{12}$CO and $^{13}$CO”