  We have measured the mean peculiar motions of 103 early-type galaxies in 7
clusters in the Perseus-Pisces (PP) ridge or PP background, and a further 249
such galaxies in 9 calibrating clusters from the literature, using the inverse
Fundamental Plane relation. This relation is found to have a distance error of
20% per galaxy. None of the 6 clusters in the PP ridge has a significant motion
with respect to the CMB frame, but the PP background cluster J8 shows marginal
evidence of `backside infall' into the PP supercluster. The full 16 cluster
sample has a mean CMB-frame bulk motion of 420 +/- 280 km/s, towards l=262,
b=-25. This result is consistent both with no bulk motion in the CMB frame and
with the ~350 km/s bulk motion found by Courteau et al. It is inconsistent at
the 98% confidence level with the ~700 km/s bulk flow found by Lauer & Postman
(LP). The PP ridge clusters are found to have a small and statistically
insignificant mean radial motion with respect to the CMB frame: -60 +/- 220
km/s. A comparison between our cluster peculiar velocities and the predicted
peculiar velocities from the IRAS 1.2 Jy density field, smoothed on a 500 km/s
scale, yields beta_I = Omega^0.6/b_I = 0.95 +/- 0.48, consistent with previous
results. We find agreement between our peculiar motions and published
Tully-Fisher results for the same clusters. The disagreement between the 11
clusters common to our sample and that of LP, based on BCGs, is statistically
significant at the >~ 99.7% confidence level indicating that the errors of one
or both of these data sets are underestimated. When the BCG distances corrected
for the X-ray luminosity of the host cluster are used, the disagreement is
reduced to the ~94% confidence level. (Abridged)
