{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:2ZI3ZU7DDTMQMCRUNN53SXIB2X","short_pith_number":"pith:2ZI3ZU7D","schema_version":"1.0","canonical_sha256":"d651bcd3e31cd9060a346b7bb95d01d5d55bf5593bc6de366c7db408db34d14e","source":{"kind":"arxiv","id":"1901.01882","version":1},"attestation_state":"computed","paper":{"title":"Investigating High Mass X-ray Binaries at hard X-rays with INTEGRAL","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Adamantia Paizis (INAF-IASF Milano, Italy), Lara Sidoli","submitted_at":"2019-01-07T15:26:31Z","abstract_excerpt":"The INTEGRAL archive developed at INAF-IASF Milano with the available public observations from late 2002 to 2016 is investigated to extract the X-ray properties of 58 High Mass X-ray Binaries (HMXBs). This sample consists of sources hosting either a Be star (Be/XRBs) or an early-type supergiant companion (SgHMXBs), including the Supergiant Fast X-ray Transients (SFXTs). INTEGRAL light curves (sampled at 2 ks) are used to build their hard X-ray luminosity distributions, returning the source duty cycles, the range of variability of the X-ray luminosity and the time spent in each luminosity state"},"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":"1901.01882","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2019-01-07T15:26:31Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"a042e4df7859c5284f497d0376cb83143d1e22ebece1d4d2b599a81ea89180ce","abstract_canon_sha256":"e66d1df4d9e5593345cdb2de4f51e7195d96b425167ca01193fc8ca89357e67e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:42:14.338142Z","signature_b64":"bd8/aEQVJDTBQWXSVVLgypqj+B59kNvSL4hZ2r13wzAv4suYWxCeuNKmIyC/ZRoJy4HyZth302q0L4oRpxFSAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d651bcd3e31cd9060a346b7bb95d01d5d55bf5593bc6de366c7db408db34d14e","last_reissued_at":"2026-07-05T00:42:14.337725Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:42:14.337725Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Investigating High Mass X-ray Binaries at hard X-rays with INTEGRAL","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Adamantia Paizis (INAF-IASF Milano, Italy), Lara Sidoli","submitted_at":"2019-01-07T15:26:31Z","abstract_excerpt":"The INTEGRAL archive developed at INAF-IASF Milano with the available public observations from late 2002 to 2016 is investigated to extract the X-ray properties of 58 High Mass X-ray Binaries (HMXBs). This sample consists of sources hosting either a Be star (Be/XRBs) or an early-type supergiant companion (SgHMXBs), including the Supergiant Fast X-ray Transients (SFXTs). INTEGRAL light curves (sampled at 2 ks) are used to build their hard X-ray luminosity distributions, returning the source duty cycles, the range of variability of the X-ray luminosity and the time spent in each luminosity state"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1901.01882","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/1901.01882/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":"1901.01882","created_at":"2026-07-05T00:42:14.337783+00:00"},{"alias_kind":"arxiv_version","alias_value":"1901.01882v1","created_at":"2026-07-05T00:42:14.337783+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1901.01882","created_at":"2026-07-05T00:42:14.337783+00:00"},{"alias_kind":"pith_short_12","alias_value":"2ZI3ZU7DDTMQ","created_at":"2026-07-05T00:42:14.337783+00:00"},{"alias_kind":"pith_short_16","alias_value":"2ZI3ZU7DDTMQMCRU","created_at":"2026-07-05T00:42:14.337783+00:00"},{"alias_kind":"pith_short_8","alias_value":"2ZI3ZU7D","created_at":"2026-07-05T00:42:14.337783+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1908.03582","citing_title":"Probing clumpy wind accretion in IGR J18027-2016 with XMM-Newton","ref_index":216,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2ZI3ZU7DDTMQMCRUNN53SXIB2X","json":"https://pith.science/pith/2ZI3ZU7DDTMQMCRUNN53SXIB2X.json","graph_json":"https://pith.science/api/pith-number/2ZI3ZU7DDTMQMCRUNN53SXIB2X/graph.json","events_json":"https://pith.science/api/pith-number/2ZI3ZU7DDTMQMCRUNN53SXIB2X/events.json","paper":"https://pith.science/paper/2ZI3ZU7D"},"agent_actions":{"view_html":"https://pith.science/pith/2ZI3ZU7DDTMQMCRUNN53SXIB2X","download_json":"https://pith.science/pith/2ZI3ZU7DDTMQMCRUNN53SXIB2X.json","view_paper":"https://pith.science/paper/2ZI3ZU7D","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1901.01882&json=true","fetch_graph":"https://pith.science/api/pith-number/2ZI3ZU7DDTMQMCRUNN53SXIB2X/graph.json","fetch_events":"https://pith.science/api/pith-number/2ZI3ZU7DDTMQMCRUNN53SXIB2X/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2ZI3ZU7DDTMQMCRUNN53SXIB2X/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2ZI3ZU7DDTMQMCRUNN53SXIB2X/action/storage_attestation","attest_author":"https://pith.science/pith/2ZI3ZU7DDTMQMCRUNN53SXIB2X/action/author_attestation","sign_citation":"https://pith.science/pith/2ZI3ZU7DDTMQMCRUNN53SXIB2X/action/citation_signature","submit_replication":"https://pith.science/pith/2ZI3ZU7DDTMQMCRUNN53SXIB2X/action/replication_record"}},"created_at":"2026-07-05T00:42:14.337783+00:00","updated_at":"2026-07-05T00:42:14.337783+00:00"}