  The Hairy Kerr black hole is a novel black hole solution that depicts a
rotating space-time encompassed by an axisymmetric fluid. It has significant
observational importance and is an excellent candidate for an astrophysical
black hole. Our study investigates the impact of the hairy charge on the
quasi-periodic oscillations (QPOs) of X-ray binaries in the Hairy Kerr black
hole (HKBH) space-time. The relativistic precession model is employed to
compute the three principal frequencies of the accretion disk encircling the
HKBH. We compare our outcomes with the observations of five X-ray binaries and
employ a Markov chain Monte Carlo (MCMC) simulation for restricting the hairy
charge parameters. There is no substantial evidence for the existence of hairy
charge in the HKBH space-time. Therefore, we are placing observational
constraints on the deformation parameters with $0<\alpha<0.07697$ and hairy
charge values ranging from $0.27182<l_0/M<2.0$.
