  In this review, I will first introduce possible methods to probe the
large-scale magnetic fields in our Galaxy and discuss their limitations. The
magnetic fields in the Galactic halo, mainly revealed by the sky distribution
of rotation measures of extragalactic radio sources, probably have a global
structure of a twisted dipole field. The large-scale field structure in the
Galactic disk has been most efficiently deduced from pulsar rotation measures
(RMs). There has been a lot of progress since the 1980s when the magnetic field
in the local area of our Galaxy was first traced by a very small sample of
local pulsars. Now we have pulsars distributed in about one third of the whole
Galactic disk of the interstellar medium, which shows that the large-scale
magnetic fields go along the spiral arms and that the field directions reverse
from arm to arm. The RMs of newly discovered pulsars in the very inner Galaxy
have been used to show the coherent magnetic field in the Norma arm. The
magnetic fields in the Galactic disk most probably have a bisymmetric spiral
structure.
