  We present the physical properties of the eclipsing binary V2281 Cyg, which
shows a light-time effect due to a supposed tertiary component from its eclipse
timing variation according to the $Kepler$ observations. The high-resolution
spectra and $BVR$ photometric data of the system were obtained at Bohyunsan
Optical Astronomy Observatory and Mount Lemmon Optical Astronomy Observatory,
respectively. To determine the fundamental parameters of the eclipsing pair and
its circumbinary object, we simultaneously analyzed the radial velocities,
light curves, and eclipse times including the $Kepler$ data. The masses and
radii for the primary and secondary stars were determined with accuracy levels
of approximately 2\% and 1\%, respectively, as follows: $M_{1} = 1.61 \pm 0.04$
M$_\odot$ and $M_{2} = 1.60 \pm 0.04$ M$_\odot$, $R_{1} = 1.94 \pm 0.02$
R$_\odot$ and $R_{2} = 1.93 \pm 0.02$ R$_\odot$. If its orbit is coplanar with
the eclipsing binary, the period and semimajor axis of the third body were
calculated to be $P_{3b}=4.1$ years and $a_{3b}=4.06$ au, respectively, and its
mass is $M_{3b}=0.75$ M$_\odot$. The evolutionary state of the system was
investigated by comparing the masses and radii with theoretical models. The
results demonstrate that V2281 Cyg is a detached eclipsing binary, which
consists of twin main-sequence stars with an age of 1.5 Gyr.
