  It is known from archival TESS data that the semi-detached Algol system XZ
UMa is one of the candidate binary stars exhibiting short-period oscillations.
We secured new high-resolution spectroscopic observations for the program
target to better understand its binary and pulsation properties. From the
echelle spectra, the radial velocities (RVs) of the eclipsing pair were
derived, and the atmosphere parameters of the primary component were measured
to be $v_{\rm A}\sin$$i = 80\pm7$ km s$^{-1}$, $T_{\rm eff,A}$ = $7940\pm120$
K, and [M/H] = $-0.15\pm0.20$. The combined solution of our double-lined RVs
and the TESS data provides robust physical parameters for XZ UMa with mass and
radius measurement precision of better than 2 \%. The outside-eclipse residuals
from a mean light curve in the 0.002 phase bin were used for multifrequency
analyses, and we extracted 32 significant frequencies (22 in $<$ 5.0 day$^{-1}$
and 10 in 39$-$52 day$^{-1}$). The low frequencies may be mostly aliasing
sidelobes, while six of the high frequencies may be pulsation signals arising
from the detached primary located inside the $\delta$ Sct domain. Their
periods, pulsation constants, and pulsational-orbital-period ratios indicate
that the mass-accretion primary star is a $\delta$ Sct pulsator and, hence, XZ
UMa is an oscillating eclipsing Algol.
