We present the physical properties of EPIC 245932119 ( K _ { p } = + 9.82 ) exhibiting both eclipses and pulsations from the K 2 photometry .
The binary modeling indicates that the eclipsing system is in detached or semi-detached configurations with a mass ratio of 0.283 or 0.245 , respectively , and that its light-curve parameters are almost unaffected by pulsations .
Multiple frequency analyses were performed for the light residuals in the outside-primary eclipsing phase after subtracting the binarity effects from the observed data .
We detected 35 frequencies with signal to noise amplitude ratios larger than 4.0 in two regions of 0.62 - 6.28 day ^ { -1 } and 19.36 - 24.07 day ^ { -1 } .
Among these , it is possible that some high signals close to the Nyquist limit f _ { Ny } may be reflections of real pulsation frequencies ( 2 f _ { Ny } - f _ { i } ) .
All frequencies ( f _ { 8 } , f _ { 9 } , f _ { 14 } , f _ { 18 } , f _ { 24 } , f _ { 32 } ) in the lower frequency region are orbital harmonics , and three high frequencies ( f _ { 19 } , f _ { 20 } , f _ { 22 } ) appear to be sidelobes split from the main frequency of f _ { 1 } = 22.77503 day ^ { -1 } .
Most of them are thought to be alias effects caused by the orbital frequency .
For the 26 other frequencies , the pulsation periods and pulsation constants are in the ranges of 0.041 - 0.052 days and 0.013 - 0.016 days , respectively .
These values and the position in the Hertzsprung-Russell diagram reveal that the primary component is a \delta Sct pulsator .
The observational properties of EPIC 245932119 are in good agreement with those for eclipsing binaries with \delta Sct-type pulsating components .