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To determine the properties of the Faraday screen and the magnetic field nearthe central region of the Galaxy, we measured the Faraday rotation measure (RM)towards 60 background extragalactic source components through the -6 deg < l <6deg, -2 deg < b < 2 deg region of the Galaxy using the 4.8 and 8.5 GHz bands ofthe ATCA and VLA. Here we use the measured RMs to estimate the systematic andthe random components of the magnetic fields. The measured RMs are found to bemostly positive for the sample sources in the region. This is consistent witheither a large scale bisymmetric spiral magnetic fields in the Galaxy or withfields oriented along the central bar of the Galaxy. The outer scale of the RMfluctuation is found to be about 40 pc, which is much larger than the observedRM size scales towards the non-thermal filaments (NTFs). The RM structurefunction is well-fitted with a power law index of 0.7 +/- 0.1 at length scalesof 0.3 to 100 pc. If Gaussian random processes in the ISM are valid, the powerlaw index is consistent with a two dimensional Kolmogorov turbulence. If thereis indeed a strong magnetic field within 1 degree (radius 150 pc) from the GC,the strength of the random field in the region is estimated to be 20microGauss. Given the highly turbulent magnetoionic ISM in this region, thestrength of the systematic component of the magnetic fields would most likelybe close to that of the random component. This suggests that the earlierestimated milliGauss magnetic field near the NTFs is localised and does notpervade the central 300 pc of the Galaxy.

Magnetic field near the central region of the Galaxy: Rotation measure of extragalactic sources