{"paper":{"title":"Low-frequency Faraday rotation measures towards pulsars using LOFAR: probing the 3-D Galactic halo magnetic field","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.GA","authors_text":"(10) SKA Organisation, 11), (11) Astro Space Centre Lebedev Physical Institute, 12), (12) Max Planck Institute for Radio Astronomy, 13, (13) Department of Physics McGill University, 14), (14) McGill Space Institute, (15) INAF - Osservatorio Astronomico di Cagliari, (16) Jodrell Bank Centre for Astrophysics, (17) Fakult\\\"at f\\\"ur Physik Universit\\\"at Bielefeld, (18) Department of Astrophysics/IMAPP Radboud University Nijmegen, (19) INAF - Istituto di Radioastronomia, 2, (20) Max Planck Institut f\\\"ur Astrophysik, (21) Dunlap Institute for Astronomy, (2) CSIRO Astronomy, 3, 3), (3) ASTRON Netherlands Institute for Radio Astronomy (4) Anton Pannekoek Institute for Astronomy, 4), (5) LPC2E - Universit\\'e d'Orl\\'eans / CNRS, 6), (6) Station de Radioastronomie de Nan\\c{c}ay, (7) Oxford Astrophysics, 8, (8) Department of Physics \\& Astronomy University of the Western Cape, 9), (9) Department of Physics, A. Karastergiou (7, A. Noutsos (12), Astrophysics), A. V. Bilous (4), B. W. Stappers (16), C. M. Tan (16), C. Sobey (1, C. Van Eck (21) ((1) International Centre for Radio Astronomy Research - Curtin University, D. Michilli (4, E. Carretti (19), E. F. Keane (10), E. J. Polzin (16), Electronics Rhodes University, G. Heald (2), J-M. Grie{\\ss}meier (5, J. P. W. Verbiest (17, J. van Leeuwen (3), J. W. T. Hessels (3, M. Haverkorn (18), M. Iacobelli (3), M. I. R. Alves (18), M. Kramer (12), M. Pilia (15), P. Weltevrede (16), Space Science, T. En{\\ss}lin (20), V. I. Kondratiev (3, W. Reich (12)","submitted_at":"2019-01-23T06:17:04Z","abstract_excerpt":"We determined Faraday rotation measures (RMs) towards 137 pulsars in the northern sky, using Low-Frequency Array (LOFAR) observations at 110-190 MHz. This low-frequency RM catalogue, the largest to date, improves the precision of existing RM measurements on average by a factor of 20 - due to the low frequency and wide bandwidth of the data, aided by the RM synthesis method. We report RMs towards 25 pulsars for the first time. The RMs were corrected for ionospheric Faraday rotation to increase the accuracy of our catalogue to approximately 0.1 rad m$^{\\rm -2}$. The ionospheric RM correction is "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1901.07738","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}