{"paper":{"title":"The far-infrared/radio correlation as probed by Herschel","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A., A. Amblard, A. Blain, A. Bongiovanni, A. Boselli, A. Cava, A. Cimatti, A. Conley, A. Cooray, A. Franceschini, A. J. Smith, A. M. J. Mortier, A. Omont, A. Papageorgiou, A. Poglitsch, A. Saintonge, B. Altieri, B. Maffei, B. Magnelli, B. O'Halloran, B. Schulz, C. D. Dowell, C. Gruppioni, C. K. Xu, C. P. Pearson, D. Burgarella, D. Elbaz, D. Farrah, D. L. Clements, D. L. Shupe, D. Lutz, Douglas Scott, D. Rigopoulou, D. Rizzo, E. Daddi, Edinburgh), E. Dwek, E. Hatziminaoglou, E. Ibar, E. Sturm, F. N. Owen, F. Pozzi, G. E. Morrison, G. Lagache, G. Magdis, G. Mainetti, G. Raymond, G. Rodighiero, G. Wright, H. Aussel, H. Dominguez, H. T. Nguyen, IfA, I. G. Roseboom, I. Valtchanov, J. A. Stevens, J. Bock, J. Cepa, J. Glenn, J. I. Rawlings, J. Vieira, K. E. Tugwell, K. Isaak, L. Conversi, L. Levenson, L. Marchetti, L. Riguccini, L. Shao, L. Tacconi, L. Vigroux, L. Wang, M. Cirasuolo, M. Fox, M. Griffin, M. Halpern, M. J. Page, M. Pohlen, M. Rowan-Robinson, M. Sanchez Portal, M. Symeonidis, M. Trichas, M. Vaccari, M. Zemcov, N. Castro, N. Lu, N. Seymour, P. Andreani, P. Chanial, P. Panuzzo, P. Popesso, P. Santini, R. Auld, R. Genzel, R. J. Ivison (UK ATC, R. Maiolino, R. Nordon, R. Ward, S. Berta, S. Eales, S. J. Oliver, S. Madden, T. Babbedge, V. Arumugam, V. Buat, W. Gear","submitted_at":"2010-05-06T20:00:20Z","abstract_excerpt":"We set out to determine the ratio, q(IR), of rest-frame 8-1000um flux, S(IR), to monochromatic radio flux, S(1.4GHz), for galaxies selected at far-IR and radio wavelengths, to search for signs that the ratio evolves with redshift, luminosity or dust temperature, and to identify any far-IR-bright outliers - useful laboratories for exploring why the far-IR/radio correlation is generally so tight when the prevailing theory suggests variations are almost inevitable. We use flux-limited 250-um and 1.4-GHz samples, obtained in GOODS-N using Herschel (HerMES; PEP) and the VLA. We determine bolometric"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1005.1072","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"}