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Using a simple relation between the radial expansion velocity of diffuse gasin the Central Molecular Zone (CMZ) of the Galaxy and its distance from SgrA$^\ast$ we estimate the physical depths within the CMZ of Star $\iota$ (2MASS$J$17470898-2829561) and two Sgr B2 far-infrared continuum sources with respectto the location of Sgr A$^\ast$. To do this we use velocity profiles ofmid-infrared absorption lines of H$_3^+$ and of far-infrared absorption linesof H$_2$O$^+$, OH$^+$, and $^{13}$CH$^+$. The distances to Star $\iota$ and tothe Sgr B2 sources are found to be $\sim$90 pc greater than the distance to SgrA$^\ast$. Our conclusion that Sgr B2 lies toward the rear of the CMZ iscontrary to many previous models in which it has been placed shallower than SgrA$^\ast$.

The Central 300 pc of the Galaxy Probed by Infrared Spectra of H$_3^+$ and CO: III. Locations of Sgr B2 and Star $\iota$