  EL CVn-type eclipsing binaries are composed of a massive A-type main-sequence
primary star and a hotter B-type secondary star. This paper presents the
time-series photometric and asteroseismic results of the EL CVn-type star
1SWASP J024743.37-251549.2. Well-defined eclipsing light curves were
constructed by using the novel high-cadence $BV$ data and archival {\it TESS}
data, and the physical parameters of each binary component were derived by
modeling the light curves. Multiple frequency analysis was performed to
investigate the pulsation properties of the binary components. A reliable
signal could not be detected in the high-frequency region of 100--300
day$^{-1}$, unlike in the previous discovery of three frequencies around 200
day$^{-1}$. This indicates that the pulsation amplitudes of the pre-helium
white dwarf secondary component decreased considerably. By contrast, 12
frequencies were detected in the range of 33 to 53 day$^{-1}$. Most of them
were classified as $\delta$ Sct-type pulsations originating from the primary
star. Theoretical frequencies for the seismic analysis were obtained by adding
the non-rotating model frequencies from the GYRE and their rotational shifts
from the complete calculation approach. Grid-based fitting was conducted for
various stellar properties. The theoretical frequencies and stellar parameters
of the best solution concurred well with the observations. The rotation rate
was constrained to 1.50 $\pm$ 0.02 day$^{-1}$, indicating the synchronized
rotation of the primary star. The results imply that the complete approach
based on the polytropic model is applicable to the seismic analysis of
fast-rotating $\delta$ Sct stars.
