An XMM-Newton Survey of the Soft X-ray Background. III. The Galactic
  Halo X-ray Emission
  We present measurements of the Galactic halo's X-ray emission for 110
XMM-Newton sight lines, selected to minimize contamination from solar wind
charge exchange emission. We detect emission from few million degree gas on
~4/5 of our sight lines. The temperature is fairly uniform (median = 2.22e6 K,
interquartile range = 0.63e6 K), while the emission measure and intrinsic
0.5--2.0 keV surface brightness vary by over an order of magnitude (~(0.4-7)e-3
cm^-6 pc and ~(0.5-7)e-12 erg cm^-2 s^-1 deg^-2, respectively, with median
detections of 1.9e-3 cm^-6 pc and 1.5e-12 erg cm^-2 s^-1 deg^-2, respectively).
The high-latitude sky contains a patchy distribution of few million degree gas.
This gas exhibits a general increase in emission measure toward the inner
Galaxy in the southern Galactic hemisphere. However, there is no tendency for
our observed emission measures to decrease with increasing Galactic latitude,
contrary to what is expected for a disk-like halo morphology. The measured
temperatures, brightnesses, and spatial distributions of the gas can be used to
place constraints on models for the dominant heating sources of the halo. We
provide some discussion of such heating sources, but defer comparisons between
the observations and detailed models to a later paper.
