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Measurements of exoplanetary orbital obliquity angles for different classesof 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 wepresent 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 dataand our newly obtained CARMENES transit observations, we estimated thespin-orbit misalignment angle, \textlambda, to be$-42.0^{+11.3}_{-10.6}$\,$\deg$, which challenges Laplacian ideals of planetformation. Through the addition of these new radial velocity (RV) data pointsobtained with CARMENES, we also derived marginal improvements on other orbitaland bulk parameters for the planet, as compared to previously published values.We showed the robustness of the obliquity measurement through model comparisonwith an aligned orbit. Finally, we demonstrated the inability of the obtaineddata to probe any possible extended atmosphere of the planet, due to a lack ofprecision, and place the atmosphere in the context of a parameter detectionspace.

Moderately misaligned orbit of the warm sub-Saturn HD 332231 b