  Measurements of exoplanetary orbital obliquity angles for different classes
of planets are an essential tool in testing various planet formation theories.
Measurements for those transiting planets on relatively large orbital periods
($P$\,$>$\,10\,d) present a rather difficult observational challenge. Here we
present the obliquity measurement for the warm sub-Saturn planet HD\,332231\,b,
which was discovered through Transiting Exoplanet Survey Satellite (TESS)
photometry of sectors 14 and 15, on a relatively large orbital period
(18.7\,d). Through a joint analysis of previously obtained spectroscopic data
and our newly obtained CARMENES transit observations, we estimated the
spin-orbit misalignment angle, \textlambda, to be
$-42.0^{+11.3}_{-10.6}$\,$\deg$, which challenges Laplacian ideals of planet
formation. Through the addition of these new radial velocity (RV) data points
obtained with CARMENES, we also derived marginal improvements on other orbital
and bulk parameters for the planet, as compared to previously published values.
We showed the robustness of the obliquity measurement through model comparison
with an aligned orbit. Finally, we demonstrated the inability of the obtained
data to probe any possible extended atmosphere of the planet, due to a lack of
precision, and place the atmosphere in the context of a parameter detection
space.
