top layer of PCU2 and modeling the inferred Galactic Ridge emission using our fits to the Sept. 1st data. Fitting with an absorbed powerlaw gives a good reduced chi-squared, but a residual near 6.5 keV suggests the addition of an iron line (this is in addition to the Galactic Ridge iron line seen in the Sept. data). Freezing $N_H$ to the cluster value, we obtain $\Gamma=1.78\pm0.03$, $L_X$(0.5-10 keV)$=2.4\pm0.1\times10^{36}$ , with an iron line at $6.6^{+0.6}_{-0.4}$ keV, of equivalent width $54\pm39$ eV (90% confidence). An F-test suggests this is reasonable, providing 3.6% probability of such a $\Delta \chi^2$ by chance. Other AMXPs have displayed evidence of Fe K lines (e.g. SAX J1808.4-3658, @Cackett09 [@Papitto09]; HETE J1900.1-2455, @Cackett10; Swift J1756.9-2508, @Patruno10), often showing relativistic broadening which our observations are unable to resolve.

Two /PCA observations were obtained during the early October outburst, both during the source’s decline. We identified pulsations in the first (Oct. 1st) observation, confirming that pulsations are common from this object [@Altamirano09]. The second (Oct. 3rd) occurred after NGC 6440 X-2 had dipped below the PCA’s sensitivity limit. We model the Galactic Ridge contribution to the Oct. 1st observation, using the Oct. 3rd observation, finding $\Gamma=1.78\pm0.15$, $L_X$(0.5-10)$=8.4^{+0.8}_{-0.5}\times10^{35}$ (see Table 