Multi-tracer analysis of straight depolarisation canals in the surroundings of the 3C 196 field

• Published in: arXiv.org 2021-09
• Main Authors: Turić, Luka, Jelić, Vibor, Jaspers, Rutger, Haverkorn, Marijke, Bracco, Andrea, Erceg, Ana, Ceraj, Lana, Cameron van Eck, Zaroubi, Saleem
• Format: Article
• Language: English
• Subjects: Canals; Complex systems; Depolarization; Dust; Emission analysis; Filaments; Hough transformation; Interstellar matter; LOFAR; Magnetic fields; Multiphase; Polarization; Stellar magnetic fields; Tomography
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2108.10679

Faraday tomography of a field centred on the extragalactic point source 3C 196 with the LOw Frequency ARray (LOFAR) revealed an intertwined structure of diffuse polarised emission with straight depolarisation canals and tracers of the magnetized and multi-phase interstellar medium (ISM), such as dust and line emission from atomic hydrogen (HI). This study aims at extending the multi-tracer analysis of LOFAR data to three additional fields in the surroundings of the 3C 196 field. For the first time, we study the three-dimensional structure of the LOFAR emission by determining the distance to the depolarisation canals. We use the Rolling Hough Transform to compare the orientation of the depolarisation canals with that of the filamentary structure seen in HI and, based on starlight and dust polarisation data, with that of the plane-of-the-sky magnetic field. Stellar parallaxes from \(Gaia\) complement the starlight polarisation with the corresponding distances. Faraday tomography of the three fields shows a rich network of diffuse polarised emission at Faraday depths between \(-10~{\rm rad~m^{-2}}\) and \(+15~{\rm rad~m^{-2}}\). A complex system of straight depolarisation canals resembles that of the 3C 196 field. The depolarisation canals align both with the HI filaments and with the magnetic field probed by dust. The observed alignment suggests that an ordered magnetic field organises the multiphase ISM over a large area (\(\sim\)20\(^{\circ}\)). In one field, two groups of stars at distances below and above 200 pc, respectively, show distinct magnetic-field orientations. These are both comparable with the orientations of the depolarisation canals in the same field. We conclude that the depolarisation canals likely trace the same change of the magnetic field as probed by the stars, which corresponds to the edge of the Local Bubble.