{"paper":{"title":"Discovery of Carbon Radio Recombination Lines in absorption towards Cygnus~A","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. Corstanje, A.G.G.M. Tielens, A.G. Polatidis, A. Horneffer, A. Karastergiou, A.M.M. Scaife, A. Schoenmakers, A. Shulevski, A. van der Horst, A.Zensus, B. Ciardi, B.W. Stappers, C. Ferrari, C. Sobey, C. Tasse, C. Toribio, C. Vocks, C. Vogt, D.D. Mulcahy, D. Engels, D. Schwarz, E. de Geus, E. Juette, E. Orru, F. Batejat, F. Breitling, F. De Gasperin, F. Salgado, G. Bernardi, G. Heald, G.J. White, G. Kuper, G. Macario, G. Mann, H. Falcke, H.J.A. Rottgering, H. Munk, H. Paas, H.R. Butcher, I.M. Avruch, I. van Bemmel, J. Anderson, J. Broderick, J.B.R. Oonk, J.C.A. Miller-Jones, J.D. Mol, J.E. Conway, J. Eisloeffel, J. Griessmeier, J. Kohler, J.P. Hamaker, J.P. McKean, J. Sluman, J. Swinbank, J. van Enst, J. van Leeuwen, J.W.T. Hessels, L.K. Morabito, M.A. Garrett, M. Brentjens, M. Brueggen, M. de Vos, M.E. Bell, M. Hoeft, M. Iacobelli, M.J. Bentum, M.J. Norden, M. Kramer, M. Kuniyoshi, M. Mevius, M. Pandey-Pommier, M. Steinmetz, M. Tagger, M.W. Wise, N.J. Jackson, O. Smirnov, O. Wucknitz, P. Best, P. Maat, P. Zarka, R.A. Fallows, R.A.M.J. Wijers, R. Beck, R. Fender, R.J. van Weeren, R. Pizzo, R. van Nieuwpoort, R. Vermeulen, S. Duscha, S. Markoff, S. ter Veen, S. Thoudam, S. Yatawatta, T.E. Hassall, V.I. Kondratiev, V. N. Pandey, W. Frieswijk, W. Klijn, W. Reich, Y. Tang","submitted_at":"2014-01-13T15:39:43Z","abstract_excerpt":"We present the first detection of carbon radio recombination line absorption along the line of sight to Cygnus A. The observations were carried out with the LOw Frequency ARray in the 33 to 57 MHz range. These low frequency radio observations provide us with a new line of sight to study the diffuse, neutral gas in our Galaxy. To our knowledge this is the first time that foreground Milky Way recombination line absorption has been observed against a bright extragalactic background source.\n  By stacking 48 carbon $\\alpha$ lines in the observed frequency range we detect carbon absorption with a si"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1401.2876","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"}