  The Galactic Centre (GC) has experienced a high degree of recent star-forming
activity, as evidenced by the large number of massive stars currently residing
there. The relative abundances of chemical elements in the GC may provide
insights into the origins of this activity. Here, we present high-resolution
$H$-band spectra of two Red Supergiants in the GC (IRS~7 and VR~5-7), and in
combination with spectral synthesis we derive abundances for Fe and C, as well
as other $\alpha$-elements Ca, Si, Mg Ti and O. We find that the C-depletion in
VR~5-7 is consistent with the predictions of evolutionary models of RSGs, while
the heavy depletion of C and O in IRS~7's atmosphere is indicative of deep
mixing, possibly due to fast initial rotation and/or enhanced mass-loss. Our
results indicate that the {\it current} surface Fe/H content of each star is
slightly above Solar. However, comparisons to evolutionary models indicate that
the {\it initial} Fe/H ratio was likely closer to Solar, and has been driven
higher by H-depletion at the stars' surface. Overall, we find $\alpha$/Fe
ratios for both stars which are consistent with the thin Galactic disk. These
results are consistent with other chemical studies of the GC, given the
precision to which abundances can currently be determined. We argue that the GC
abundances are consistent with a scenario in which the recent star-forming
activity in the GC was fuelled by either material travelling down the Bar from
the inner disk, or from the winds of stars in the inner Bulge -- with no need
to invoke top-heavy stellar Initial Mass Functions to explain anomalous
abundance ratios.
