  New abundances of N, O, Na, Mg, Si, Ca, Sc, Ti, Cr, Fe, Sr, Zr, and Ba are
presented for 10 A-type supergiants in the SMC, plus upper limits for C. In
interpreting the CNO results for constraints on stellar evolution theories,
careful attention has been paid to the comparison abundances, i.e., the present
day abundances of SMC nebulae and B-dwarf stars. These new results are also
compared to published results from F-K supergiant analyses, and found to be in
good agreement when both sets of data are carefully examined as differential
(SMC minus Galactic standard) abundances.
  With the exception of nitrogen, very small star-to-star abundance variations
are found for all elements in this analysis. The N variations are not predicted
by standard stellar evolution models. Instead, the results support the new
predictions reported from rotating stellar models, where the range in nitrogen
is the result of partial mixing of CN-cycled gas from the stellar interior due
to main-sequence rotation at different rates (c.f., Langer & Heger 1998). The
overall overabundance of nitrogen in the sampled stars also implies these stars
have undergone the first dredge-up in addition to having been mixed while on
the main-sequence.
  The alpha-elements (O, Mg, Si, Ca, Ti) have similar underabundances to Fe,
which is not the same as seen in metal-poor stars in the solar neighborhood of
the Galaxy. In addition, certain light s-process elements (Zr, Ba) are slightly
more underabundant than Fe, which is predicted by the bursting chemical
evolution model presented by Pagel & Tautvaisiene (1998) for the SMC.
