  Recent catalog of Faraday rotation measures (RM) of extragalactic sources
together with the synchrotron polarization data from WMAP and Planck provide us
with the wealth of information on magnetic fields of the Galaxy. However, the
integral character of these observables together with our position inside the
Galaxy makes the inference of the coherent Galactic magnetic field (GMF)
complicated and ambiguous. We combine several phenomenological components of
the GMF -- the spiral arms, the toroidal halo, the X-shaped field and the field
of the Local Bubble -- to construct a new model of the regular GMF outside of
the thin disk. To have control over the relative contributions of the RM and
polarization data to the fit we pay special attention to the estimation of
errors in data bins. To this end we develop a systematic method which is
uniformly applicable to different data sets. This method takes into account
individual measurement errors, the variance in the bin as well as fluctuations
in the data at angular scales larger than the bin size. This leads to decrease
of the errors and, as a result, to better sensitivity of the data to the model
content. We cross checked the stability of our method with the new LOFAR data.
We found that the four components listed above are sufficient to fit both the
RM and polarization data over the whole sky with only a small fraction masked
out. Moreover, we have achieved several important improvements compared to
previous approaches. Due to account of our location inside of the Local Bubble
our model does not require introduction of striated fields. For the first time
we showed that the Fan Region can be modeled as a Galactic-scale feature. The
pitch angle of the magnetic field in our fit converged to the value around 20
degrees. Interestingly, with value is very close to the direction of arms
inferred recently from Gaia data on upper main sequence stars.
