{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:4OQVZ2HPURFYXR23RCNDREH374","short_pith_number":"pith:4OQVZ2HP","schema_version":"1.0","canonical_sha256":"e3a15ce8efa44b8bc75b889a3890fbff00215fe95d89208ade671877fc583f22","source":{"kind":"arxiv","id":"2401.05838","version":1},"attestation_state":"computed","paper":{"title":"NIR spectral classification of the companion in the gamma-ray binary HESS J1832-093 as an O6 V star","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Alessandro Papitto, Brian van Soelen, Emma de O\\~na Wilhelmi, Ignacio Negueruela, Marc Rib\\'o, Pol Bordas","submitted_at":"2024-01-11T11:19:29Z","abstract_excerpt":"HESS J1832-093 is a member of the rare class of gamma-ray binaries, as recently confirmed by the detection of orbitally modulated X-ray and gamma-ray emission with a period of ~86 d. The spectral type of the massive companion star has been difficult to retrieve as there is no optical counterpart, but the system is coincident with a near-infrared source. Previous results have shown that the infrared counterpart is consistent with an O or B type star, but a clear classification is still lacking. We observed the counterpart twice, in 2019 and 2021, with the X-Shooter spectrograph operating on the"},"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":"2401.05838","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2024-01-11T11:19:29Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"8c7de3d4377b0bd2bae3bbf6aa496f93ecd3c0810020d582342a207c0dfb5924","abstract_canon_sha256":"544c6375cc85a69f10dd93ce0c912905ab1264e630cd58becdc804ee52d7fd33"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T07:32:36.378226Z","signature_b64":"sYnFBN6I+MA7MXgF+Kwle3CdGbCXnnpulsYSs6n3Gw1ZHr6Fo9LgL98nTD/L6CXO4ft/og1SiIyeNdhbGoxdBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e3a15ce8efa44b8bc75b889a3890fbff00215fe95d89208ade671877fc583f22","last_reissued_at":"2026-07-05T07:32:36.377810Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T07:32:36.377810Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"NIR spectral classification of the companion in the gamma-ray binary HESS J1832-093 as an O6 V star","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Alessandro Papitto, Brian van Soelen, Emma de O\\~na Wilhelmi, Ignacio Negueruela, Marc Rib\\'o, Pol Bordas","submitted_at":"2024-01-11T11:19:29Z","abstract_excerpt":"HESS J1832-093 is a member of the rare class of gamma-ray binaries, as recently confirmed by the detection of orbitally modulated X-ray and gamma-ray emission with a period of ~86 d. The spectral type of the massive companion star has been difficult to retrieve as there is no optical counterpart, but the system is coincident with a near-infrared source. Previous results have shown that the infrared counterpart is consistent with an O or B type star, but a clear classification is still lacking. We observed the counterpart twice, in 2019 and 2021, with the X-Shooter spectrograph operating on the"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2401.05838","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/2401.05838/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":"2401.05838","created_at":"2026-07-05T07:32:36.377871+00:00"},{"alias_kind":"arxiv_version","alias_value":"2401.05838v1","created_at":"2026-07-05T07:32:36.377871+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2401.05838","created_at":"2026-07-05T07:32:36.377871+00:00"},{"alias_kind":"pith_short_12","alias_value":"4OQVZ2HPURFY","created_at":"2026-07-05T07:32:36.377871+00:00"},{"alias_kind":"pith_short_16","alias_value":"4OQVZ2HPURFYXR23","created_at":"2026-07-05T07:32:36.377871+00:00"},{"alias_kind":"pith_short_8","alias_value":"4OQVZ2HP","created_at":"2026-07-05T07:32:36.377871+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2411.16606","citing_title":"Detection of X-ray Emission from a Bright Long-Period Radio Transient","ref_index":89,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4OQVZ2HPURFYXR23RCNDREH374","json":"https://pith.science/pith/4OQVZ2HPURFYXR23RCNDREH374.json","graph_json":"https://pith.science/api/pith-number/4OQVZ2HPURFYXR23RCNDREH374/graph.json","events_json":"https://pith.science/api/pith-number/4OQVZ2HPURFYXR23RCNDREH374/events.json","paper":"https://pith.science/paper/4OQVZ2HP"},"agent_actions":{"view_html":"https://pith.science/pith/4OQVZ2HPURFYXR23RCNDREH374","download_json":"https://pith.science/pith/4OQVZ2HPURFYXR23RCNDREH374.json","view_paper":"https://pith.science/paper/4OQVZ2HP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2401.05838&json=true","fetch_graph":"https://pith.science/api/pith-number/4OQVZ2HPURFYXR23RCNDREH374/graph.json","fetch_events":"https://pith.science/api/pith-number/4OQVZ2HPURFYXR23RCNDREH374/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4OQVZ2HPURFYXR23RCNDREH374/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4OQVZ2HPURFYXR23RCNDREH374/action/storage_attestation","attest_author":"https://pith.science/pith/4OQVZ2HPURFYXR23RCNDREH374/action/author_attestation","sign_citation":"https://pith.science/pith/4OQVZ2HPURFYXR23RCNDREH374/action/citation_signature","submit_replication":"https://pith.science/pith/4OQVZ2HPURFYXR23RCNDREH374/action/replication_record"}},"created_at":"2026-07-05T07:32:36.377871+00:00","updated_at":"2026-07-05T07:32:36.377871+00:00"}