  Ultra-hot Jupiters (UHJs) orbiting pulsating A/F stars represent an important
subset of the exoplanetary demographic, as they are excellent candidates for
the study of exoplanetary atmospheres, as well as being astrophysical
laboratories for the investigation of planet-to-star interactions. We analyse
the \texttt{TESS} (Transiting Exoplanet Survey Satellite) light curve of the
WASP-167 system, consisting of an F1V star and a substellar companion on a
$\sim 2.02$ day orbit. We model the combination of the ellipsoidal variability
and the Doppler beaming to measure the mass of WASP-167b, and the reflection
effect to obtain constraints on the geometric albedo, while placing a special
emphasis on noise separation. We implement a basic model to determine the
dayside ($T_{\rm Day}$), nightside ($T_{\rm Night}$) and intrinsic ($T_{\rm
Internal}$) temperatures of WASP-167b and put a constraint on its Bond albedo.
We confirm the transit parameters of the planet seen in the literature. We find
that a resonant $\sim 2P^{-1}$ stellar signal (which may originate from
planet-to-star interactions) interferes with the phase curve analysis. After
considerate treatment of this signal, we find $M_p = 0.34 \pm 0.22$~$M_J$. We
measure a dayside temperature of $2790 \pm 100$ K, classifying WASP-167b as an
UHJ. We find a $2\sigma$ upper limit of $0.51$ on its Bond albedo, and
determine the geometric albedo at $0.34 \pm 0.11$ ($1 \sigma$ uncertainty).
With an occultation depth of $106.8 \pm 27.3$ ppm in the \texttt{TESS}
passband, the UHJ WASP-167b will be an excellent target for atmospheric
studies, especially those at thermal wavelength ranges, where the stellar
pulsations are expected to be be less influential.
