  It has been argued in the literature that the star HV~2112 in the Small
Magellanic Cloud is the first known example of a T\.ZO, a Red Supergiant with a
degenerate neutron core. This claim is based on the star having a high
luminosity ($\log (L/L_\odot)$~> 5), an extremely cool effective temperature,
and a surface enriched in in lithium, calcium and various $irp$-process
elements. In this paper we re-examine this evidence, and present new
measurements of the stellar properties. By compiling archival photometry from
blue to mid-IR for HV~2112 and integrating under it's spectral energy
distribution we find a bolometric luminosity in the range of $\log
(L/L_\odot)$=4.70-4.91, lower than that found in previous work and comparable
to bright asymptotic giant branch (AGB) stars. We compare a VLT+XSHOOTER
spectrum of HV~2112 to other late type, luminous SMC stars, finding no evidence
for enhancements in Rb, Ca or K, though there does seem to be an enrichment in
Li. We therefore conclude that a much more likely explanation for HV~2112 is
that it is an intermediate mass($\sim$5M$_\odot$) AGB star. However, from our
sample of comparison stars we identify a new T\.ZO candidate, HV~11417, which
seems to be enriched in Rb but for which we cannot determine a Li abundance.
