  We have determined elemental abundance ratios in the core of the Perseus
cluster for several elements. These ratios indicate a central dominance of SN
Ia ejecta similar to that found for A496, A2199 and A3571 (Dupke & White 2000).
Simultaneous analysis of ASCA spectra from SIS1, GIS 2&3 shows that the ratio
of Ni to Fe abundances is ~ (3.4 +- 1.1) times Solar within the central 4'.
This ratio is consistent with (and more precise than) that observed in other
clusters whose central regions are dominated by SN Ia ejecta. Such a large Ni
over-abundance is predicted by "Convective Deflagration" explosion models for
SN Ia such as "W7" but is inconsistent with delayed detonation models. We note
that with current instrumentation the NiK(alpha) line is confused with
FeK(beta) and that the Ni over-abundance we observe has been interpreted by
others as an anomalously large ratio of FeK(beta) to FeK(alpha) caused by
resonant scattering in the FeK(alpha) line. We argue that a central enhancement
of SN Ia ejecta and hence a high ratio of Ni to Fe is naturally explained by
scenarios that include the generation of chemical gradients by suppressed SN Ia
winds or ram-pressure stripping of cluster galaxies. It is not necessary to
suppose that the intracluster gas is optically thick to resonant scattering of
the FeK(alpha) line.
