  We conducted a follow-up study on the analysis of the LOw Frequency ARray
(LOFAR) Two-metre Sky Survey (LoTSS) mosaic in the high-latitude outer Galaxy
presented in the first paper of this series. Here, we focus on the search for
alignment between the magnetic field traced by dust, HI filaments, starlight
optical linear polarisation, and linear depolarised structures (depolarisation
canals) observed in low-frequency synchrotron polarisation. This alignment was
previously found in several smaller fields observed with LOFAR, offering
valuable insights into the nature of the interstellar medium and the 3D spatial
distribution of the diffuse ionised medium. We aim to determine whether the
alignment of the interstellar medium (ISM) phases observed through multiple
tracers is a common occurrence or an exception. Additionally, in areas where
depolarisation canals align with the magnetic field, we use starlight
polarisation to constrain the distance to the structures associated with the
observed canals. We employed the Rolling Hough Transform (RHT) and projected
Rayleigh statistics (PRS) to identify and quantify the alignment between the
different tracers. On the scale of the whole mosaic, we did not find any
evidence of a universal alignment among the three tracers. However, in one
particular area, the western region (Dec between $29^\circ$ and $70^\circ$ and
RA between $\mathrm{7^h44^m}$ and $\mathrm{9^h20^m}$), we do find a significant
alignment between the magnetic field, depolarisation canals, and HI filaments.
Based on this alignment, we used the starlight polarisation of stars with known
parallax distances to estimate that the minimum distance to the structures
observed by LOFAR in this region lies within the range of 200 to 240 pc. We
associate these structures with the edge of the Local Bubble.
