  For the upcoming PLAnetary Transits and Oscillation of stars (PLATO)
satellite mission, a large number of target stars are required to yield a
statistically significant number of planet transits. Locating the centres of
the long duration observational phase (LOP) fields closer to the Galactic plane
will increase the target star numbers but also the astrophysical false
positives (FPs) from blended eclipsing binary systems. We utilise the Binary
Stellar Evolution and Population Synthesis (BiSEPS) code, to create a complete
synthetic stellar and planetary population for the proposed southern LOP field
(LOPS0), as well as for a representative portion of the northern LOP field
(LOPNsub). For LOPS0 we find an overall low FP rate for planets smaller than
Neptunes. The FP rate generally shows little variation with Galactic longitude
(l), and a modest increase with decreasing Galactic latitude (|b|). The
location of the LOPS field centre within the current allowed region is not
strongly constrained by FPs. Analysis of LOPNsub suggests a markedly increased
number of FPs across the full range of planet radii at low |b| resulting in
approximately twice the percent FP rate in the LOPNsub compared to the
corresponding southern field segment in the planet radius range -0.2 <
log(R/Rsun) <= 0.4. However, only a few percent of fully eclipsing FPs in LOPS0
in this radius range have periods
