In Bocchino, Maggio & Sciortino (1996) we show that a PSPC
spectrum must have a few thousand
counts in order to avoid secondary minima problems in the 
space when fitted with our STNEI emission model. This effect is mainly
due to the moderate PSPC spectral resolution. Since 98% of the
spatial bins used for CIE spectral analysis in Paper I
contained less than 5000 counts, a spatial rebinning of the data was
necessary in order to use our STNEI 1T model. The new grid we have
adopted (Figure 2a) contains 48 non empty bins (versus the
273 bins of Paper I) with angular size of 
and
an approximate real size of 
pc (cf. and
pc in Paper I). It contains only 12 bins (25% of the
total) with less than
5000 counts (6 with less than 3000 counts) and it is a good
compromise between spatial resolution and statistics.
The spatial bin layout has been tailored to study the radial profile of the plasma thermodynamical parameters derived from the fits (see Figure 2a). In fact, each spatial bin is the intersection of an annulus at a given distance from the Vela pulsar and a circular sector with its vertex on the pulsar. For a large scale view of the Vela SNR and the position of our pointed observation, see Figure 1b (Plate 11), in Paper I. In Table 1 the number of counts in each bins is reported, as well as the distance of the chosen annuli and their position angle.