  Magnetic fields have been observed in galaxy clusters with strengths of the
order of $\sim \mu$G. The non-thermal pressure exerted by magnetic fields also
contributes to the total pressure in galaxy clusters and can in turn affect the
estimates of the gas mass fraction, $f_{gas}$. In this paper, we have
considered a central magnetic field strength of $5\mu$G, motivated by
observations and simulations of galaxy clusters. The profile of the magnetic
field has also been taken from the results obtained from simulations and
observations. The role of magnetic field has been taken into account in
inferring the gas density distribution through the hydrostatic equilibrium
condition (HSE) by including the magnetic pressure. We have found that the
resultant gas mass fraction is smaller with magnetic field as compared to that
without magnetic field. However, this decrease is dependent on the strength and
the profile of the magnetic field. We have also determined the total mass using
the NFW profile to check for the dependency of $f_{gas}$ estimates on total
mass estimators. From our analysis, we conclude that for the magnetic field
strength that galaxy clusters seem to possess, the non-thermal pressure from
magnetic fields has an impact of $\approx 1~\%$ on the gas mass fraction of
galaxy clusters. However, with upcoming facilities like Square Kilometre Array
(SKA), it can be further expected to improve with more precise observations of
the magnetic field strength and profile in galaxy clusters, particularly in the
interior region.
