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We investigate the properties of the Galactic ISM by applying Faradaytomography to a radio polarization data set in the direction of the Galacticanti-centre. We address the problem of missing large-scale structure in ourdata, and show that this does not play an important role for the results wepresent. The main peak of the Faraday depth spectra in our data set is notmeasurably resolved for about 8% of the lines of sight. An unresolved peakindicates a separation between the regions with Faraday rotation andsynchrotron emission. However, cosmic rays pervade the ISM, and synchrotronemission would therefore also be produced where there is Faraday rotation. Wesuggest that the orientation of the magnetic field can separate the twoeffects. By modelling the thermal electron contribution to the Faraday depth,we map the strength of the magnetic field component along the line of sight.Polarized point sources in our data set have rotation measures that arecomparable to the Faraday depths of the diffuse emission in our data. OurFaraday depth maps show narrow canals of low polarized intensity. We concludethat depolarization over the telescope beam produces at least some of thesecanals. Finally, we investigate the properties of one conspicuous region inthis data set and argue that it is created by a decrease in line-of-sightdepolarization compared to its surroundings.

WSRT Faraday tomography of the Galactic ISM at \lambda ~ 0.86 m