and an extra soft component that contributes to the emission below $5 \keV$. Near apastron the hot component has a temperature of $kT=3.3 \keV$, while the extra soft component has a temperature of $kT = 1.1 \keV$. In KS08 we have studied only the hot component because we know this region comes from the strongly shocked (perpendicular shock) secondary wind before it suffers any adiabatic cooling. Therefore, we can safely estimate its location to be close to the stagnation point of the colliding winds (apex), but somewhat closer to the secondary. The source and location of the $kT \sim 1 \keV$ gas, on the other hand, is less secure, but it probably resides in an extended region. The very important thing we do learn from H07 analysis of the X-ray emission by the $kT \sim 1 \keV$ gas is that the contribution of absorbing gas around the winds interaction region to the column density is $N_{H-e} \la 5 \times 10^{22} \cm^{-2}$. This implies that any column density of $N_H >  5 \times 10^{22} \cm^{-2}$ must come from material close to the binary system, at most $\sim 100 \AU$.

P09 tried to fit the RXTE light curve of the emission in 