  We use line-of-sight velocity information on the filamentary emission-line
nebula of NGC 1275 to infer a dynamical model of the nebula's flow through the
surrounding intracluster gas. We detect outflowing gas and flow patterns that
match simulations of buoyantly rising bubbles from which we deduce that some of
the nebula filaments have been drawn out of NGC 1275. We find a radial gradient
of the ratio [NII]6584/H-alpha which may be due to a variation in metallicity,
interactions with the surrounding intracluster medium or a hardening of the
excitation mechanism. We find no preferred spatial correlation of stellar
clusters within the filaments and there is a notable lack of [OIII]5007
emission, therefore it is unlikely that the filaments are ionized by stellar
UV.
