  Observations of the hot X-ray emitting interstellar medium in the Milky Way
are important for studying the stellar feedback and understanding the formation
and evolution of galaxies. We present measurements of the soft X-ray background
emission for 130 Suzaku observations at $75^\circ<l < 285^\circ$ and
$|b|>15^\circ$. With the standard soft X-ray background model consisting of the
local hot bubble and the Milky Way halo, residual structures remain at 0.7--1
keV in the spectra of some regions. Adding a collisional-ionization-equilibrium
component with a temperature of $\sim$0.8 keV, much higher than the virial
temperature of the Milky Way, significantly reduces the derived C-statistic for
56 out of 130 observations. The emission measure of the 0.8 keV component
varies by more than an order of magnitude: Assuming the solar abundance, the
median value is 3$\times 10^{-4}~ \rm{cm^{-6} pc}$ and the 16th-84th percentile
range is (1--8)$\times 10^{-4}~ \rm{cm^{-6} pc}$. Regions toward the
Orion-Eridanus Superbubble, a large cavity extending from the Ori OB1
association, have the highest emission measures of the 0.8 keV component. While
the scatter is large, the emission measures tend to be higher toward the lower
Galactic latitude. We discuss possible biases caused by the solar wind charge
exchange, stars, and background groups. The 0.8 keV component is probably
heated by supernovae in the Milky Way disk, possibly related to galactic
fountains.
