  We present the results of a study of discrete X-ray sources in NGC 6946 using
a deep Chandra ACIS observation. Based on the slope of the log N-log S
distribution and the general correlation of sources with the spiral arms, we
infer that the overall discrete source sample in NGC 6946 is dominated by high
mass X-ray binaries, in contrast to the source distributions in M31 and the
Milky Way. This is consistent with the higher star formation rate in NGC 6946
than in those galaxies. We find that the strong X-ray sources in the region of
the galactic center do not correlate in detail with images of the region in the
near-IR, although one of them may be coincident with the galactic center. The
non-central ultra-luminous X-ray source in NGC 6946, previously identified with
a supernova remnant, has an X-ray spectrum and luminosity that is inconsistent
with either a traditional pulsar wind nebula or a blast wave remnant.
