J/A+A/654/A5ivo://CDS.VizieR/J/A+A/654/A5doi:10.26093/cds/vizier/bc-me/lfCDSTuric L.Jelic V.Jaspers R.Haverkorn M.Bracco A.Erceg A.Ceraj L.,van Eck C.Zaroubi S.2026-07-01T14:00:17Z2021-10-01T08:13:08ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmilky-way-galaxypolarimetryradio-continuum-emissionFaraday 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 -10rad/m^2^ and +15rad/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 (~20{deg}). In one field, two groups of stars at distances below and above 200pc, 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.2021A&A...654A...5Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/654/A5CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/654/A5https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/654/A5http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/654/A5https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/654/A5https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/654/A5http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/654/A5GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/654/A5/list (List of fits datacubes)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/654/A5/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/654/A5/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/654/A5/list?GETtext/xml+votable180.050000true111.6708348.195830.0055555555555555566/5090 6462 6937https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/654/A5?format=asciiRadiodefaultJ/A+A/654/A5/listList of fits datacubesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right ascension of image centre (J2000)degpos.eq.ra;meta.mainDEJ2000Declination of image centre (J2000)degpos.eq.dec;meta.mainNxNumber of pixels in along X-axismeta.numberintNyNumber of pixels in along Y-axismeta.numberintNzNumber of pixels in Faraday depthmeta.numberintsizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of the fits file in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the fits filemeta.title;meta.fitschar