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In this paper, we present TESS photometry and high-resolution spectra of theshort-period Algol EW Boo. We obtained double-lined radial velocities (RVs)from the time-series spectra and measured the effective temperature of theprimary star as $T_{\rm{eff,1}}$ = 8560 $\pm$ 118 K. For the orbital periodstudy, 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 berepresented by a periodic oscillation of 17.6 $\pm$ 0.3 years with asemi-amplitude of 0.0041 $\pm$ 0.0001 d. The orbital and physical parameterswere derived by simultaneously analyzing the TESS light and RV curves using theWilson-Devinney (WD) binary star modeling code. The component masses and radiiwere 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 frequencyanalyses were performed for the light-curve residuals from the WD model. As aresult, we detected 17 pressure-mode pulsations in the region of 40.15 - 52.37d$^{-1}$. The absolute dimensions and pulsation characteristics showed that the$\delta$ Sct pulsator was the more massive and hotter primary star of the EWBoo.

A Photometric and Spectroscopic Study of the Short-Period Algol EW Bo\"{o}tis with a $\delta$ Sct Pulsator