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Magnetic fields have been observed in galaxy clusters with strengths of theorder of $\sim \mu$G. The non-thermal pressure exerted by magnetic fields alsocontributes to the total pressure in galaxy clusters and can in turn affect theestimates of the gas mass fraction, $f_{gas}$. In this paper, we haveconsidered a central magnetic field strength of $5\mu$G, motivated byobservations and simulations of galaxy clusters. The profile of the magneticfield has also been taken from the results obtained from simulations andobservations. The role of magnetic field has been taken into account ininferring the gas density distribution through the hydrostatic equilibriumcondition (HSE) by including the magnetic pressure. We have found that theresultant gas mass fraction is smaller with magnetic field as compared to thatwithout magnetic field. However, this decrease is dependent on the strength andthe profile of the magnetic field. We have also determined the total mass usingthe NFW profile to check for the dependency of $f_{gas}$ estimates on totalmass estimators. From our analysis, we conclude that for the magnetic fieldstrength that galaxy clusters seem to possess, the non-thermal pressure frommagnetic fields has an impact of $\approx 1~\%$ on the gas mass fraction ofgalaxy clusters. However, with upcoming facilities like Square Kilometre Array(SKA), it can be further expected to improve with more precise observations ofthe magnetic field strength and profile in galaxy clusters, particularly in theinterior region.

Impact of magnetic field on the gas mass fraction of galaxy clusters