  VLA 1623 West is an ambiguous source that has been described as a shocked
cloudlet as well as a protostellar disk. We use deep ALMA 1.3 and 0.87
millimeter observations to constrain its shape and structure to determine its
origins better. We use a series of geometric models to fit the uv visibilities
at both wavelengths with GALARIO. Although the Real visibilities show
structures similar to what has been identified as gaps and rings in
protoplanetary disks, we find that a modified Flat-Topped Gaussian at high
inclination provides the best fit to the observations. This fit agrees well
with expectations for an optically thick, highly inclined disk. Nevertheless,
we find that the geometric models consistently yield positive residuals at the
four corners of the disk at both wavelengths. We interpret these residuals as
evidence that the disk is flared in the millimeter dust. We use a simple toy
model for an edge-on flared disk and find that the residuals best match a disk
with flaring that is mainly restricted to the outer disk at $R \gtrsim 30$ au.
Thus, VLA 1623W may represent a young protostellar disk where the large dust
grains have not yet had enough time to settle into the mid-plane. This result
may have implications for how disk evolution and vertical dust settling impact
the initial conditions leading to planet formation.
