  We present Chandra and XMM-Newton X-ray data of NGC5253, a local starbursting
dwarf elliptical galaxy, in the early stages of a starburst episode.
Contributions to the X-ray emission come from discrete point sources and
extended diffuse emission, in the form of what appear to be multiple
superbubbles, and smaller bubbles probably associated with individual star
clusters. Chandra detects 17 sources within the optical extent of NGC5253 down
to a completeness level corresponding to a luminosity of 1.5E37 erg/s.The slope
of the point source X-ray luminosity function is -0.54, similar to that of
other nearby dwarf starburst galaxies. Several different types of source are
detected within the galaxy, including X-ray binaries and the emission
associated with star-clusters.
  Comparison of the diffuse X-ray emission with the observed Halpha emission
shows similarities in their extent. The best spectral fit to the diffuse
emission is obtained with an absorbed, two temperature model giving
temperatures for the two gas components of ~0.24keV and ~0.75keV.The derived
parameters of the diffuse X-ray emitting gas are as follows: a total mass of
\~1.4E6 f^{1/2} Msun, where f is the volume filling factor of the X-ray
emitting gas, and a total thermal energy content for the hot X-ray emitting gas
of \~3.4E54 f^{1/2} erg. The pressure in the diffuse gas is P/k ~
1E6f^{-1/2}K/cm3. We find that these values are broadly commensurate with the
mass and energy injection from the starburst population. Analysis of the
kinematics of the starburst region suggest that the stellar ejecta contained
within it can escape the gravitational potential well of the galaxy, and
pollute the surrounding IGM.
