  In this paper, we present TESS photometry and high-resolution spectra of the
short-period Algol EW Boo. We obtained double-lined radial velocities (RVs)
from the time-series spectra and measured the effective temperature of the
primary star as $T_{\rm{eff,1}}$ = 8560 $\pm$ 118 K. For the orbital period
study, we collected all times of minima available for over the last 30 years.
It was found that the eclipse timing variation of the system could be
represented by a periodic oscillation of 17.6 $\pm$ 0.3 years with a
semi-amplitude of 0.0041 $\pm$ 0.0001 d. The orbital and physical parameters
were derived by simultaneously analyzing the TESS light and RV curves using the
Wilson-Devinney (WD) binary star modeling code. The component masses and radii
were showed over 3% precision: $M_{1}$ = 2.67 $\pm $ 0.08 M$_{\odot}$, $M_{2}$
= 0.43 $\pm $ 0.01 M$_{\odot}$, $R_{1}$ = 2.01 $\pm $ 0.02 R$_{\odot}$, and
$R_{2}$ = 1.35 $\pm $ 0.01 R$_{\odot}$. Furthermore, multiple frequency
analyses were performed for the light-curve residuals from the WD model. As a
result, we detected 17 pressure-mode pulsations in the region of 40.15 - 52.37
d$^{-1}$. The absolute dimensions and pulsation characteristics showed that the
$\delta$ Sct pulsator was the more massive and hotter primary star of the EW
Boo.
