  We present the first Doppler images of the prototypical active binary star RS
CVn, derived from high-resolution spectra observed in 2004, 2016 and 2017,
using three different telescopes and observing sites. We apply the
least-squares deconvolution technique to all observed spectra to obtain high
signal-to-noise line profiles, which are used to derive the surface images of
the active K-type component. Our images show a complex spot pattern on the K
star, distributed widely in longitude. All starspots revealed by our Doppler
images are located below a latitude of about 70$^{\circ}$. In accordance with
previous light-curve modeling studies, we find no indication of a polar spot on
the K star. Using Doppler images derived from two consecutive rotational
cycles, we estimate a surface differential rotation rate of $\Delta\Omega =
-0.039 \pm 0.003 ~rad~d^{-1}$ and $\alpha = \Delta\Omega/\Omega_{eq} = -0.030
\pm 0.002$ for the K star. Given the limited phase coverage during those two
rotations, the uncertainty of our differential rotation estimate is presumably
higher.
