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This study aims to characterize linear polarization structures in LOFARobservations of the interstellar medium (ISM) in the 3C196 field, one of theprimary fields of the LOFAR-Epoch of Reionization key science project. We haveused the high band antennas (HBA) of LOFAR to image this region and RotationMeasure (RM) synthesis to unravel the distribution of polarized structures inFaraday depth. The brightness temperature of the detected Galactic emission is$5-15~{\rm K}$ in polarized intensity and covers the range from -3 to +8 ${\rmrad~m^{-2}}$ in Faraday depth. The most interesting morphological feature is astrikingly straight filament at a Faraday depth of $+0.5~{\rm rad~m^{-2}}$running from north to south, right through the centre of the field and parallelto the Galactic plane. There is also an interesting system of lineardepolarization canals conspicuous in an image showing the peaks of Faradayspectra. We used the Westerbork Synthesis Radio Telescope (WSRT) at 350 MHz toimage the same region. For the first time, we see some common morphology in theRM cubes made at 150 and 350~{\rm MHz}. There is no indication of diffuseemission in total intensity in the interferometric data, in line with resultsat higher frequencies and previous LOFAR observations. Based on our results, wedetermined physical parameters of the ISM and proposed a simple model that mayexplain the observed distribution of the intervening magneto-ionic medium. Themean line-of-sight magnetic field component, $B_\parallel$, is determined to be$0.3\pm0.1~{\rm \mu G}$ and its spatial variation across the 3C196 field is$0.1~{\rm \mu G}$. The filamentary structure is probably an ionized filament inthe ISM, located somewhere within the Local Bubble. This filamentary structureshows an excess in thermal electron density ($n_e B_\parallel>6.2~{\rmcm^{-3}\mu G}$) compared to its surroundings.

Linear polarization structures in LOFAR observations of the interstellar medium in the 3C196 field