  The low resolution X-ray spectra around $\eta$ Car covering Tr 16 and part of
Tr 14 have been extracted from a Chandra CCD ACIS image. Various analysis
techniques have been applied to the spectra based on their count rates. The
spectra with the greatest number of counts (HD 93162 = WR 25, HD 93129AB, and
HD 93250) have been fit with a wind model, which uses several components with
different temperatures and depths in the wind. Weaker spectra have been fit
with Raymond-Smith models. The weakest spectra are simply inter-compared with
strong spectra. In general, fits produce reasonable parameters based on
knowledge of the extinction from optical studies and on the range of
temperatures for high and low mass stars. Direct comparisons of spectra confirm
the consistency of the fitting results and also hardness ratios for cases of
unusually large extinction in the clusters. The spectra of the low mass stars
are harder than the more massive stars. Stars in the sequence evolving from the
main sequence (HD 93250) through the system containing the O supergiant (HD
93129AB) and then through the Wolf-Rayet stage (HD93162), presumably ending in
the extreme example of $\eta$ Car, share the property of being unusually
luminous and hard in X-rays. For these X-ray luminous stars, their high mass
and evolutionary status (from the very last stages of the main sequence and
beyond) is the common feature. Their binary status is mixed, and magnetic
status is still uncertain.
