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We present the analysis of an XMM observation of the Seyfert galaxy NGC 2992.The source was found in its highest level of X-ray activity yet detected, afactor $\sim 23.5$ higher in 2--10 keV flux than the historical minimum. NGC2992 is known to exhibit X-ray flaring activity on timescales of days to weeks,and the XMM data provide at least factor of $\sim 3$ better spectral resolutionin the Fe K band than any previously measured flaring X-ray state. We find thatthere is a broad feature in the \sim 5-7 keV band which could be interpreted asa relativistic Fe K$\alpha$ emission line. Its flux appears to have increasedin tandem with the 2--10 keV continuum when compared to a previous Suzakuobservation when the continuum was a factor of $\sim 8$ lower than that duringthe XMM observation. The XMM data are consistent with the general picture thatincreased X-ray activity and corresponding changes in the Fe K$\alpha$ lineemission occur in the innermost regions of the putative accretion disk. Thisbehavior contrasts with the behavior of other AGN in which the Fe K$\alpha$line does not respond to variability in the X-ray.

NGC 2992 in an X-ray high state observed by XMM: Response of the Relativistic Fe K$\alpha$ Line to the Continuum