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[ABRIDGED] The knowledge of the regular component of the Galactic magneticfield gives important information about the structure and dynamics of the MilkyWay, as well as constitutes a basic tool to determine cosmic rays trajectories.It can also provide clear windows where primordial magnetic fields could bedetected. We want to obtain the regular (large scale) pattern of the magneticfield distribution of the Milky Way that better fits the polarized synchrotronemission as seen by the 5-year WMAP data at 22 GHz. We have done a systematicstudy of a number of Galactic magnetic field models: axisymmetric, bisymmetric,logarithmic spiral arms, concentric circular rings with reversals andbi-toroidal. We have explored the parameter space defining each of these modelsusing a grid-based approach. In total, more than one million models arecomputed. The model selection is done using a Bayesian approach. For eachmodel, the posterior distributions are obtained and marginalised over theunwanted parameters to obtain the marginal 1-D probability distributionfunctions. In general, axisymmetric models provide a better description of thehalo component, although attending to their goodness-of-fit, the rest of themodels cannot be rejected. In the case of disk component, the analysis is notvery sensitive for obtaining the disk large scale structure, because of theeffective available area (less than 8% of the whole map and less than 40% ofthe disk). Nevertheless, within a given family of models, the best-fitparameters are compatible with those found in the literature. The family ofmodels that better describes the polarized synchrotron halo emission is theaxisymmetric one, with magnetic spiral arms with a pitch angle of ~24 degrees,and a strong vertical field of 1 microG at z ~ 1 kpc. When a radial variationis fitted, models require fast variations.

Constraining the regular Galactic Magnetic Field with the 5-year WMAP polarization measurements at 22 GHz