  Chandra ACIS-I data of the molecular cloud and HII region complex NGC 6334
were analyzed. The hard X-ray clumps detected with ASCA (Sekimoto et al. 2000)
were resolved into 792 point sources. After removing the point sources, an
extended X-ray emission component was detected over a 5x9 pc2 region, with the
0.5-8 keV absorption-corrected luminosity of 2x10^33 erg/s. The contribution
from faint point sources to this extended emission was estimated as at most ~20
%, suggesting that most of the emission is diffuse in nature. The X-ray
spectrum of the diffuse emission was observed to vary from place to place. In
tenuous molecular cloud regions with hydrogen column density of 0.5~1x10^22
cm-2, the spectrum can be represented by a thermal plasma model with
temperatures of several keV. The spectrum in dense cloud cores exhibits harder
continuum, together with higher absorption more than ~3x10^22 cm-2. In some of
such highly obscured regions, the spectrum show extremely hard continua
equivalent to a photon index of ~1, and favor non-thermal interpretation. These
results are discussed in the context of thermal and non-thermal emissions, both
powered by fast stellar winds from embedded young early-type stars through
shock transitions.

Astrophysics