  Hot Jupiters present a unique opportunity for measuring how planet formation
history shapes present-day atmospheric composition. However, due to the myriad
pathways influencing composition, a well-constructed sample of planets is
needed to determine whether formation history can be accurately traced back
from atmospheric composition. To this end, the BOWIE-ALIGN survey will compare
the compositions of 8 hot Jupiters around F stars, 4 with orbits aligned with
the stellar rotation axis and 4 misaligned. Using the alignment as an indicator
for planets that underwent disc migration or high-eccentricity migration, one
can determine whether migration history produces notable differences in
composition between the two samples of planets. This paper describes the planet
formation model that motivates our observing programme. Our model traces the
accretion of chemical components from the gas and dust in the disc over a broad
parameter space to create a full, unbiased model sample from which we can
estimate the range of final atmospheric compositions. For high metallicity
atmospheres (O/H > 10 times solar), the C/O ratios of aligned and misaligned
planets diverge, with aligned planets having lower C/O (< 0.25) due to the
accretion of oxygen-rich silicates from the inner disc. However, silicates may
rain out instead of releasing their oxygen into the atmosphere. This would
significantly increase the C/O of aligned planets (C/O > 0.6), inverting the
trend between the aligned and misaligned planets. Nevertheless, by comparing
statistically significant samples of aligned and misaligned planets, we expect
atmospheric composition to constrain how planets form.
