  Tidal dissipation in binary systems is the primary source for synchronization
and circularization of the objects in the system. The efficiency of the
dissipation of tidal energy inside stars or planets results in significant
changes in observed properties of the binary system and is often studied
empirically using a parameter, commonly known as the modified tidal quality
factor ($Q_\star'$). Though often assumed constant, in general that parameter
will depend on the particular tidal wave experiencing the dissipation and the
properties of the tidally distorted object. In this work we study the frequency
dependence of $Q_\star'$ for Sun-like stars. We parameterize $Q_\star'$ as a
saturating power-law in tidal frequency and obtain constraints using the
stellar rotation period of 70 eclipsing binaries observed by Kepler. We use
Bayesian analysis to account for the uncertainties in the observational data
required for tidal evolution. Our analysis shows that $Q_\star'$ is well
constrained for tidal periods > 15 days, with a value of $Q_\star' \sim 10^8$
for periods > 30 days and a slight suggested decrease at shorter periods. For
tidal periods < 15 days, $Q_\star'$ is no longer tightly constrained, allowing
for a broad range of possible values that overlaps with the constraints
obtained using tidal circularization in binaries, which point to much more
efficient dissipation: $Q_\star' \sim 10^6$.
