{"paper":{"title":"The Spectral Energy Distributions of Fermi Blazars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"A. Y. Zhou, C. Lin, G. Y. Luo, H. B. Xiao, J. H. Fan, J. H. Yang, T. X. Hua, Y.H. Yuan, Y. Liu, Z. Y. Pei","submitted_at":"2016-08-13T09:31:57Z","abstract_excerpt":"(Abridged) In this paper, multi-wavelength data are compiled for a sample of 1425 Fermi blazars to calculate their spectral energy distributions (SEDs). A parabolic function, $\\log(\\nu F_{\\nu}) = P_1(\\log\\nu - P_2)^2 + P_3,$ is used for SED fitting. Synchrotron peak frequency ($\\log \\nu_p$), spectral curvature ($P_1$), peak flux ($\\nu_{\\rm p}F_{\\rm \\nu_p}$), and integrated flux ($\\nu F_{\\nu}$) are successfully obtained for 1392 blazars (461 flat spectrum radio quasars-FSRQs, 620 BL Lacs-BLs and 311 blazars of uncertain type-BCUs, 999 sources have known redshifts). Monochromatic luminosity at r"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1608.03958","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"}