  Large-scale distributions of hot-gas temperature and Fe abundance in the
Perseus cluster have been studied with multi-pointing observations by the GIS
instrument on ASCA. Within a radius of 20' from the cluster center, the energy
spectra requires two temperature components, in which the cool component
indicates kT ~ 2 keV and the hot-component temperature shows a significant
decline from about 8 keV to 6 keV toward the center. In the outer region of the
cluster, the temperature shows a fluctuation with an amplitude of about 2 keV
and suggest that a western region at ~16' from the cluster center is relatively
hotter. As for the Fe abundance, a significant decline with radius is detected
from 0.44 solar at the center to ~0.1 solar at a 50' offset region. If observed
Fe-K line intensity within 4' from the center is suppressed by a factor of 2
due to the resonance scattering effect, the corrected Fe mass density follows
the galaxy distribution. Finally, our results do not support the large-scale
velocity gradients previously reported from the same GIS data.
