Diffuse X-ray emission from star forming galaxies
  We study the diffuse X-ray luminosity ($L_X$) of star forming galaxies using
2-D axisymmetric hydrodynamical simulations and analytical considerations of
supernovae (SNe) driven galactic outflows. We find that the mass loading of the
outflows, a crucial parameter for determining the X-ray luminosity, is
constrained by the availability of gas in the central star forming region, and
a competition between cooling and expansion. We show that the allowed range of
the mass loading factor can explain the observed scaling of $L_X$ with star
formation rate (SFR) as $L_X \propto$ SFR$^2$ for SFR $\gtrsim 1$
M$_\odot$yr$^{-1}$, and a flatter relation at low SFRs. We also show that the
emission from the hot circumgalactic medium (CGM) in the halo of massive
galaxies can explain the sub-linear behaviour of the $L_X-$SFR relation as well
as a large scatter in the diffuse X-ray emission for low SFRs ($\lesssim$ few
M$_\odot$yr$^{-1}$). Our results point out that galaxies with small SFRs and
large diffuse X-ray luminosities are excellent candidates for detection of the
elusive CGM.
