{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:7EQTDER2YALOB2QRWR6KWRYJXI","short_pith_number":"pith:7EQTDER2","schema_version":"1.0","canonical_sha256":"f92131923ac016e0ea11b47cab4709ba3d376df810f5940676488992cf801fa5","source":{"kind":"arxiv","id":"2101.08131","version":1},"attestation_state":"computed","paper":{"title":"Pulse energy distribution for RRAT J0139+33 according to observations at the frequency 111 MHz","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"E.A. Brylyakova, S.A. Tyul'bashev","submitted_at":"2021-01-19T13:55:14Z","abstract_excerpt":"Using five year monitoring observations, we did a blind search for pulses for rotating radio transient (RRAT) J0139+33 and PSR B0320+39. At the interval \\pm 1.5m of the time corresponding to the source passing through the meridian, we detected 39377 individual pulses for the pulsar B0320+39 and 1013 pulses for RRAT J0139+33. The share of registered pulses from the total number of observed periods for the pulsar B0320+39 is 74%, and for the transient J0139+33 it is 0.42%. Signal-to-noise ratio (S/N) for the strongest registered pulses is approximately equal to: S/N = 262 (for B0320+39) and S/N "},"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":"2101.08131","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2021-01-19T13:55:14Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"a910c9e139598d1022a3361f3848caefa4a8f85367bbfc87cf32838b32731b15","abstract_canon_sha256":"dddd1e369b64b601947d842dca713d7100e82406eb720a3b458a5e6310c31e92"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T02:29:42.583356Z","signature_b64":"iUekEopEMYgci/46tUB866yIUvtoEOC++7N1saL9cgyqO+rp4Q5aFWPDTxarIq0VNpzHrVtG/FhVid0NIPquDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f92131923ac016e0ea11b47cab4709ba3d376df810f5940676488992cf801fa5","last_reissued_at":"2026-07-05T02:29:42.582832Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T02:29:42.582832Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Pulse energy distribution for RRAT J0139+33 according to observations at the frequency 111 MHz","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"E.A. Brylyakova, S.A. Tyul'bashev","submitted_at":"2021-01-19T13:55:14Z","abstract_excerpt":"Using five year monitoring observations, we did a blind search for pulses for rotating radio transient (RRAT) J0139+33 and PSR B0320+39. At the interval \\pm 1.5m of the time corresponding to the source passing through the meridian, we detected 39377 individual pulses for the pulsar B0320+39 and 1013 pulses for RRAT J0139+33. The share of registered pulses from the total number of observed periods for the pulsar B0320+39 is 74%, and for the transient J0139+33 it is 0.42%. Signal-to-noise ratio (S/N) for the strongest registered pulses is approximately equal to: S/N = 262 (for B0320+39) and S/N "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2101.08131","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2101.08131/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":"2101.08131","created_at":"2026-07-05T02:29:42.582893+00:00"},{"alias_kind":"arxiv_version","alias_value":"2101.08131v1","created_at":"2026-07-05T02:29:42.582893+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2101.08131","created_at":"2026-07-05T02:29:42.582893+00:00"},{"alias_kind":"pith_short_12","alias_value":"7EQTDER2YALO","created_at":"2026-07-05T02:29:42.582893+00:00"},{"alias_kind":"pith_short_16","alias_value":"7EQTDER2YALOB2QR","created_at":"2026-07-05T02:29:42.582893+00:00"},{"alias_kind":"pith_short_8","alias_value":"7EQTDER2","created_at":"2026-07-05T02:29:42.582893+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2509.03001","citing_title":"Low-frequency observations of low-mass binary systems with neutron star candidates","ref_index":9,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/7EQTDER2YALOB2QRWR6KWRYJXI","json":"https://pith.science/pith/7EQTDER2YALOB2QRWR6KWRYJXI.json","graph_json":"https://pith.science/api/pith-number/7EQTDER2YALOB2QRWR6KWRYJXI/graph.json","events_json":"https://pith.science/api/pith-number/7EQTDER2YALOB2QRWR6KWRYJXI/events.json","paper":"https://pith.science/paper/7EQTDER2"},"agent_actions":{"view_html":"https://pith.science/pith/7EQTDER2YALOB2QRWR6KWRYJXI","download_json":"https://pith.science/pith/7EQTDER2YALOB2QRWR6KWRYJXI.json","view_paper":"https://pith.science/paper/7EQTDER2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2101.08131&json=true","fetch_graph":"https://pith.science/api/pith-number/7EQTDER2YALOB2QRWR6KWRYJXI/graph.json","fetch_events":"https://pith.science/api/pith-number/7EQTDER2YALOB2QRWR6KWRYJXI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7EQTDER2YALOB2QRWR6KWRYJXI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7EQTDER2YALOB2QRWR6KWRYJXI/action/storage_attestation","attest_author":"https://pith.science/pith/7EQTDER2YALOB2QRWR6KWRYJXI/action/author_attestation","sign_citation":"https://pith.science/pith/7EQTDER2YALOB2QRWR6KWRYJXI/action/citation_signature","submit_replication":"https://pith.science/pith/7EQTDER2YALOB2QRWR6KWRYJXI/action/replication_record"}},"created_at":"2026-07-05T02:29:42.582893+00:00","updated_at":"2026-07-05T02:29:42.582893+00:00"}