{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2002:YORC4BNJOQ7WQVYPTG7TPJXICO","short_pith_number":"pith:YORC4BNJ","schema_version":"1.0","canonical_sha256":"c3a22e05a9743f68570f99bf37a6e81385434232cfb8e1303f90e290b4e34f0d","source":{"kind":"arxiv","id":"astro-ph/0207506","version":1},"attestation_state":"computed","paper":{"title":"The TeV spectrum of H1426+428","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Falcone, A.M. Hillas, B. Power-Mooney, C. Duke, D.A. Carter-Lewis, D. Horan, D.J. Fegan, D. Kieda, D. M\\\"uller, D. Petry, F. Krennrich, G.H. Sembroski, G. Walker, H.J. Rose, I. de la Calle Perez, I.H. Bond, J.A. Gaidos, J. Hall, J.H. Buckley, J. Holder, J. Kildea, J. Knapp, J.P. Finley, J. Quinn, K. Gibbs, K. Kosack, M. Jordan, M. Kertzman, M. Page, M. Schroedter, N. Stanton, N.W. Reay, P. Moriarty, P.T. Reynolds, R. Ong, R. Pallassini, R. Sidwell, S. Gammell, S.J. Fegan, S. LeBohec, S.M. Bradbury, S.P. Swordy, S.P. Wakely, T.A. Hall, T.C. Weekes, T.N. Nagai, V.V. Vassiliev, W. Cui","submitted_at":"2002-07-23T16:16:59Z","abstract_excerpt":"The BL Lac object H1426+428 was recently detected as a high energy gamma-ray source by the VERITAS collaboration (Horan et al. 2002). We have reanalyzed the 2001 portion of the data used in the detection in order to examine the spectrum of H1426+428 above 250 GeV. We find that the time-averaged spectrum agrees with a power law of the shape dF/dE = 10^(-7.31 +- 0.15(stat) +- 0.16(syst)) x E^(-3.50 +- 0.35(stat) +- 0.05(syst)) m^(-2)s^(-1)TeV^(-1) The statistical evidence from our data for emission above 2.5 TeV is 2.6 sigma. With 95% c.l., the integral flux of H1426+428 above 2.5 TeV is larger "},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"astro-ph/0207506","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2002-07-23T16:16:59Z","cross_cats_sorted":[],"title_canon_sha256":"7d31da63271671a9a4f4173ff94d29d636beff5722b6c973afd3a1cf9447f4f7","abstract_canon_sha256":"380321e2ba758b2432a3588fb62ced1b12a06a3a2d150ecd65091c533d396f57"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:18:00.467500Z","signature_b64":"PCh+iqMfUi8XzibJNnqiC7sm4QOMCa+p/0kFsnCInZskGaVAxBtgbJVTblKBwDVEyTQF/qy6UR1qYgHOL460BA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c3a22e05a9743f68570f99bf37a6e81385434232cfb8e1303f90e290b4e34f0d","last_reissued_at":"2026-07-04T15:18:00.466970Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:18:00.466970Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The TeV spectrum of H1426+428","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Falcone, A.M. Hillas, B. Power-Mooney, C. Duke, D.A. Carter-Lewis, D. Horan, D.J. Fegan, D. Kieda, D. M\\\"uller, D. Petry, F. Krennrich, G.H. Sembroski, G. Walker, H.J. Rose, I. de la Calle Perez, I.H. Bond, J.A. Gaidos, J. Hall, J.H. Buckley, J. Holder, J. Kildea, J. Knapp, J.P. Finley, J. Quinn, K. Gibbs, K. Kosack, M. Jordan, M. Kertzman, M. Page, M. Schroedter, N. Stanton, N.W. Reay, P. Moriarty, P.T. Reynolds, R. Ong, R. Pallassini, R. Sidwell, S. Gammell, S.J. Fegan, S. LeBohec, S.M. Bradbury, S.P. Swordy, S.P. Wakely, T.A. Hall, T.C. Weekes, T.N. Nagai, V.V. Vassiliev, W. Cui","submitted_at":"2002-07-23T16:16:59Z","abstract_excerpt":"The BL Lac object H1426+428 was recently detected as a high energy gamma-ray source by the VERITAS collaboration (Horan et al. 2002). We have reanalyzed the 2001 portion of the data used in the detection in order to examine the spectrum of H1426+428 above 250 GeV. We find that the time-averaged spectrum agrees with a power law of the shape dF/dE = 10^(-7.31 +- 0.15(stat) +- 0.16(syst)) x E^(-3.50 +- 0.35(stat) +- 0.05(syst)) m^(-2)s^(-1)TeV^(-1) The statistical evidence from our data for emission above 2.5 TeV is 2.6 sigma. 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