{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2004:QPJR27JWW6764MFDX2HZYJMHXC","short_pith_number":"pith:QPJR27JW","schema_version":"1.0","canonical_sha256":"83d31d7d36b7bfee30a3be8f9c2587b888bdc40e6e01b372dc7cd9aac65596ad","source":{"kind":"arxiv","id":"astro-ph/0408453","version":2},"attestation_state":"computed","paper":{"title":"High Energy Observations of XRF 030723: Evidence for an Off-axis Gamma-Ray Burst?","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Dullighan, A. Levine, A. Yoshida, C. Barraud, C. Graziani, D. Q. Lamb, E. E. Fenimore, E. Morgan, F. Martel, G. B. Crew, G. Pizzichini, G. Prigozhin, G. Ricker, J. Braga, J. Doty, J-F. Olive, J. G. Jernigan, J-L. Atteia, J-P. Dezalay, J. Villasenor, K. Hurley, K. Torii, M. Boer, M. Galassi, M. Matsuoka, M. Suzuki, N. Kawai, N. R. Butler, P. Ford, R. Manchanda, R. Vanderspek, S. E. Woosley, T. Cline, T. Q. Donaghy, T. Sakamoto, T. Tamagawa, Y. Shirasaki","submitted_at":"2004-08-24T19:16:24Z","abstract_excerpt":"We report High Energy Transient Explorer 2 (HETE-2) Wide Field X-ray Monitor/French Gamma Telescope observations of XRF030723 along with observations of the XRF afterglow made using the 6.5m Magellan Clay telescope and the Chandra X-ray Observatory. The observed peak energy E_pk_obs of the nu F_nu burst spectrum is found to lie within (or below) the WXM 2-25 keV passband at 98.5% confidence, and no counts are detected above 30 keV. Our best fit value is E_pk_obs=8.4+3.5/-3.4 keV. The ratio of X-ray to Gamma-ray flux for the burst follows a correlation found for GRBs observed with HETE-2, and t"},"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/0408453","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2004-08-24T19:16:24Z","cross_cats_sorted":[],"title_canon_sha256":"3ca4f2182fcc282fe6e4ba77f9d59af5de558263e1afb14db8fa7e2aa3306d1b","abstract_canon_sha256":"3a976013e34cfbc44a7cb8bc4a9b53f884a5e912f254415a6556bf2f9a2d96ad"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:44:32.961475Z","signature_b64":"hyE2PgcUBdVhYBM/28rPzGVfhC17TO7RU3ALOGG9KIUDycTOmBbykgyzrtDJch53kGzjLUsfsv19S595KtyfAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"83d31d7d36b7bfee30a3be8f9c2587b888bdc40e6e01b372dc7cd9aac65596ad","last_reissued_at":"2026-07-04T16:44:32.961051Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:44:32.961051Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"High Energy Observations of XRF 030723: Evidence for an Off-axis Gamma-Ray Burst?","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Dullighan, A. Levine, A. Yoshida, C. Barraud, C. Graziani, D. Q. Lamb, E. E. Fenimore, E. Morgan, F. Martel, G. B. Crew, G. Pizzichini, G. Prigozhin, G. Ricker, J. Braga, J. Doty, J-F. Olive, J. G. Jernigan, J-L. Atteia, J-P. Dezalay, J. Villasenor, K. Hurley, K. Torii, M. Boer, M. Galassi, M. Matsuoka, M. Suzuki, N. Kawai, N. R. Butler, P. Ford, R. Manchanda, R. Vanderspek, S. E. Woosley, T. Cline, T. Q. Donaghy, T. Sakamoto, T. Tamagawa, Y. Shirasaki","submitted_at":"2004-08-24T19:16:24Z","abstract_excerpt":"We report High Energy Transient Explorer 2 (HETE-2) Wide Field X-ray Monitor/French Gamma Telescope observations of XRF030723 along with observations of the XRF afterglow made using the 6.5m Magellan Clay telescope and the Chandra X-ray Observatory. The observed peak energy E_pk_obs of the nu F_nu burst spectrum is found to lie within (or below) the WXM 2-25 keV passband at 98.5% confidence, and no counts are detected above 30 keV. Our best fit value is E_pk_obs=8.4+3.5/-3.4 keV. The ratio of X-ray to Gamma-ray flux for the burst follows a correlation found for GRBs observed with HETE-2, and t"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0408453","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/0408453/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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"},"aliases":[{"alias_kind":"arxiv","alias_value":"astro-ph/0408453","created_at":"2026-07-04T16:44:32.961112+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0408453v2","created_at":"2026-07-04T16:44:32.961112+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0408453","created_at":"2026-07-04T16:44:32.961112+00:00"},{"alias_kind":"pith_short_12","alias_value":"QPJR27JWW676","created_at":"2026-07-04T16:44:32.961112+00:00"},{"alias_kind":"pith_short_16","alias_value":"QPJR27JWW6764MFD","created_at":"2026-07-04T16:44:32.961112+00:00"},{"alias_kind":"pith_short_8","alias_value":"QPJR27JW","created_at":"2026-07-04T16:44:32.961112+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QPJR27JWW6764MFDX2HZYJMHXC","json":"https://pith.science/pith/QPJR27JWW6764MFDX2HZYJMHXC.json","graph_json":"https://pith.science/api/pith-number/QPJR27JWW6764MFDX2HZYJMHXC/graph.json","events_json":"https://pith.science/api/pith-number/QPJR27JWW6764MFDX2HZYJMHXC/events.json","paper":"https://pith.science/paper/QPJR27JW"},"agent_actions":{"view_html":"https://pith.science/pith/QPJR27JWW6764MFDX2HZYJMHXC","download_json":"https://pith.science/pith/QPJR27JWW6764MFDX2HZYJMHXC.json","view_paper":"https://pith.science/paper/QPJR27JW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0408453&json=true","fetch_graph":"https://pith.science/api/pith-number/QPJR27JWW6764MFDX2HZYJMHXC/graph.json","fetch_events":"https://pith.science/api/pith-number/QPJR27JWW6764MFDX2HZYJMHXC/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QPJR27JWW6764MFDX2HZYJMHXC/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QPJR27JWW6764MFDX2HZYJMHXC/action/storage_attestation","attest_author":"https://pith.science/pith/QPJR27JWW6764MFDX2HZYJMHXC/action/author_attestation","sign_citation":"https://pith.science/pith/QPJR27JWW6764MFDX2HZYJMHXC/action/citation_signature","submit_replication":"https://pith.science/pith/QPJR27JWW6764MFDX2HZYJMHXC/action/replication_record"}},"created_at":"2026-07-04T16:44:32.961112+00:00","updated_at":"2026-07-04T16:44:32.961112+00:00"}