5007$ with corroborating \[\] $\lambda 4959$ emission. Subsequent analysis reveals the latter emission line to be due to poorly subtracted telluric emission, and we now identify the strong emission line as H$\alpha$ (Q=3.5). The remaining cases seem to be genuine mismatches between the spectroscopic redshift and the photometric redshifts, both the individual photometric redshift of the galaxy and the SOM-based photometric redshift. Consideration of [*Hubble*]{} imaging reveals at least some of these likely due to two close-separation galaxies, where the ground-based imaging used for the photometry was unable to separate the sources.

Increased color space coverage
------------------------------

The five nights of observing in 2016A filled in $\sim$6% of the map, in addition to existing spectroscopy which already filled $\sim$50% (see Figure \[figure:som\_update\]). Thus we completed $\gtrsim$10% of the required calibration. However, some of the remaining observations may prove more challenging. Given the recent progress on bringing multiple deep fields (and their spectroscopy) onto a consistent color system, the requirements may also change to some extent, in the sense that somewhat fewer spectra are required due to the inclusion of other spectroscopic surveys.

It should also be noted that a certain fraction of the remaining cells represent faint, red sources for 