Context :

Aims : Given that in most cases just thermal pressure is taken into account in the hydrostatic equilibrium equation to estimate galaxy cluster mass , the main purpose of this paper is to consider the contribution of all three non-thermal components to total mass measurements .
The non-thermal pressure is composed by cosmic rays , turbulence and magnetic pressures .

Methods : To estimate the thermal pressure we used public XMM- Newton archival data of five Abell clusters to derive temperature and density profiles .
To describe the magnetic pressure , we assume a radial distribution for the magnetic field , B ( r ) \propto \rho _ { g } ^ { \alpha } , to seek generality we assume \alpha within the range of 0.5 to 0.9 , as indicated by observations and numerical simulations .
Turbulent motions and bulk velocities add a turbulent pressure , which is considered using an estimate from numerical simulations .
For this component , we assume an isotropic pressure , P _ { turb } = \frac { 1 } { 3 } \rho _ { g } ( \sigma _ { r } ^ { 2 } + \sigma _ { t } ^ { 2 } ) .
We also consider the contribution of cosmic ray pressure , P _ { cr } \propto r ^ { -0.5 } .
Thus , besides the gas ( thermal ) pressure , we include these three non-thermal components in the magnetohydrostatic equilibrium equation and compare the total mass estimates with the values obtained without them .

Results : A consistent description for the non-thermal component could yield a variation in mass estimates that extends from 10 % to \sim 30 % .
We verified that in the inner parts of cool core clusters the cosmic ray component is comparable to the magnetic pressure , while in non-cool core clusters the cosmic ray component is dominant .
For cool core clusters the magnetic pressure is the dominant component , contributing more than 50 % of the total mass variation due to non-thermal pressure components .
However , for non-cool core clusters , the major influence comes from the cosmic ray pressure that accounts for more than 80 % of the total mass variation due to non-thermal pressure effects .
For our sample , the maximum influence of the turbulent component to the total mass variation can be almost 20 % .
Although all of the assumptions agree with previous works , it is important to notice that our results rely on the specific parametrization adopted in this work .
We show that this analysis can be regarded as a starting point for a more detailed and refined exploration of the influence of non-thermal pressure in the intra-cluster medium ( ICM ) .

Conclusions :