{"paper":{"title":"Studying Galactic interstellar turbulence through fluctuations in synchrotron emission: First LOFAR Galactic foreground detection","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Alexov, A. Asgekar, A. Bonafede, A. G. Polatidis, A. Horneffer, A. Karastergiou, A. Scaife, A. W. Gunst, A. Zensus, B. Ciardi, B. W. Stappers, C. Ferrari, C. Horellou, C. Sobey, C. Sotomayor-Beltran, C. Tasse, C. Toribio, C. Vocks, C. Vogt, D. D. Mulcahy, D. Engels, D. Schwarz, E. de Geus, E. Orr\\'u, F. Breitling, F. De Gasperin, G. Bernardi, G. Heald, G. Kuper, G. Macario, G. Mann, H. Falcke, H. Junklewitz, H. Munk, H. R. Butcher, H. R\\\"ottgering, I. M. Avruch, I. van Bemmel, J. Anderson, J. Broderick, J. E. Conway, J. Eisloffel, J. Griessmeier, J. Horandel, J. P. Hamaker, J. P. McKean, J. Sluman, J. van Leeuwen, J. W. T. Hessels, K. Chyzy, L. Birzan, L. V. E. Koopmans, M. A. Garrett, M. Bruggen, M. E. Bell, M. Haverkorn, M. Hoeft, M. Iacobelli, M. J. Bentum, M. Kramer, M. Kuniyoshi, M. Pandey-Pommier, M. R. Bell, M. Steinmetz, M. Tagger, M. W. Wise, O. Smirnov, O. Wucknitz, P. Best, P. Zarka, R. A. Fallows, R. Beck, R. F. Pizzo, R.-J. Dettmar, R. J. van Weeren, R. Paladino, R. Vermeulen, S. Duscha, S. Yatawatta, T.A. En{\\ss}lin, T. E. Hassall, V. I. Kondratiev, V. Jelic, W. Frieswijk, W. Jurusik, W. N. Brouw, W. Reich, Y. Tang","submitted_at":"2013-08-13T09:52:20Z","abstract_excerpt":"The characteristic outer scale of turbulence and the ratio of the random to ordered components of the magnetic field are key parameters to characterise magnetic turbulence in the interstellar gas, which affects the propagation of cosmic rays within the Galaxy. We provide new constraints to those two parameters. We use the LOw Frequency ARray (LOFAR) to image the diffuse continuum emission in the Fan region at (l,b) (137.0,+7.0) at 80\"x70\" resolution in the range [146,174] MHz. We detect multi-scale fluctuations in the Galactic synchrotron emission and compute their power spectrum. Applying the"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1308.2804","kind":"arxiv","version":2},"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"}