The pulse height of the signal from the analyzer can be used to
differentiate the good 
, which will deposit a lot of
energy,
from 
, cosmic rays, or other events
which deposit relatively little energy. Figure 
shows the
distribution of the energy deposited in the analyzer planes which is
essentially the pulse height signal from those planes.
Figure: Raw histogram of the pulse height distribution of hits in the
analyzer planes of the polarimeter. The pulse height is proportional to
the energy deposited in those planes.
A plot of the polar scattering angle, 
, versus the analyzer pulse
height more clearly separates the 
events from all others.
Figure shows this plot.
Figure: Polar scattering angle, 
, versus the analyzer pulse
height. The branch labelled (A) are primarily the 
events
while those in the box marked (B) are 
events,
cosmic ray events, and others that deposit very little energy.
The 
events show a higher energy deposition in the
analyzer, particularly for greater scattering angles. Most of the rest of
the events have a very small pulse height regardless of the scattering
angle. A cut on the data of the type defined by the box (A) in figure
was investigated, but it was found that such a 2-d cut does
not provide any better a FOM than did cuts on individual pulse height and
spectra.