{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:V35PDP3XT6IXLG6MRDG3SV7BG3","short_pith_number":"pith:V35PDP3X","schema_version":"1.0","canonical_sha256":"aefaf1bf779f91759bcc88cdb957e136c80800aef0a95f5af4d17a4ede268d3f","source":{"kind":"arxiv","id":"1505.01739","version":1},"attestation_state":"computed","paper":{"title":"An infrared diagnostic for magnetism in hot stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"C. A. H. Condori, C. Neiner, J. C. N. Campagnolo, J. H. Grunhut, M. Borges Fernandes, M. E. Oksala, M. Kraus, T. B. Souza","submitted_at":"2015-05-07T15:21:32Z","abstract_excerpt":"Magnetospheric observational proxies are used for indirect detection of magnetic fields in hot stars in the X-ray, UV, optical, and radio wavelength ranges. To determine the viability of infrared (IR) hydrogen recombination lines as a magnetic diagnostic for these stars, we have obtained low-resolution (R~1200), near-IR spectra of the known magnetic B2V stars HR 5907 and HR 7355, taken with the Ohio State Infrared Imager/Spectrometer (OSIRIS) attached to the 4.1m Southern Astrophysical Research (SOAR) Telescope. Both stars show definite variable emission features in IR hydrogen lines of the Br"},"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":"1505.01739","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2015-05-07T15:21:32Z","cross_cats_sorted":[],"title_canon_sha256":"e7a298c00bef7917edecb3fca95303c26cfa80c4bfe770eba17e48a0538734b0","abstract_canon_sha256":"fe056f763e946cd40fb1b58dc59e2979d02f2db33649a0f9d9ca963db200e310"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:46:14.664118Z","signature_b64":"F8Ezuhu41o+nloDiLG4E5P+oTrrG7wXZb+5NyPmzqzuBhRe5VApG5uppQqxErjtLkb0uRMWyFjCV0pUNalUCBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"aefaf1bf779f91759bcc88cdb957e136c80800aef0a95f5af4d17a4ede268d3f","last_reissued_at":"2026-05-18T01:46:14.663439Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:46:14.663439Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"An infrared diagnostic for magnetism in hot stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"C. A. H. Condori, C. Neiner, J. C. N. Campagnolo, J. H. Grunhut, M. Borges Fernandes, M. E. Oksala, M. Kraus, T. B. Souza","submitted_at":"2015-05-07T15:21:32Z","abstract_excerpt":"Magnetospheric observational proxies are used for indirect detection of magnetic fields in hot stars in the X-ray, UV, optical, and radio wavelength ranges. To determine the viability of infrared (IR) hydrogen recombination lines as a magnetic diagnostic for these stars, we have obtained low-resolution (R~1200), near-IR spectra of the known magnetic B2V stars HR 5907 and HR 7355, taken with the Ohio State Infrared Imager/Spectrometer (OSIRIS) attached to the 4.1m Southern Astrophysical Research (SOAR) Telescope. Both stars show definite variable emission features in IR hydrogen lines of the Br"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1505.01739","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":""},"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":"1505.01739","created_at":"2026-05-18T01:46:14.663547+00:00"},{"alias_kind":"arxiv_version","alias_value":"1505.01739v1","created_at":"2026-05-18T01:46:14.663547+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1505.01739","created_at":"2026-05-18T01:46:14.663547+00:00"},{"alias_kind":"pith_short_12","alias_value":"V35PDP3XT6IX","created_at":"2026-05-18T12:29:44.643036+00:00"},{"alias_kind":"pith_short_16","alias_value":"V35PDP3XT6IXLG6M","created_at":"2026-05-18T12:29:44.643036+00:00"},{"alias_kind":"pith_short_8","alias_value":"V35PDP3X","created_at":"2026-05-18T12:29:44.643036+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.23768","citing_title":"GMRT Survey of Radio Emission from Magnetic Massive Stars -- I: Emission from Single Stars at sub-GHz Frequencies","ref_index":246,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/V35PDP3XT6IXLG6MRDG3SV7BG3","json":"https://pith.science/pith/V35PDP3XT6IXLG6MRDG3SV7BG3.json","graph_json":"https://pith.science/api/pith-number/V35PDP3XT6IXLG6MRDG3SV7BG3/graph.json","events_json":"https://pith.science/api/pith-number/V35PDP3XT6IXLG6MRDG3SV7BG3/events.json","paper":"https://pith.science/paper/V35PDP3X"},"agent_actions":{"view_html":"https://pith.science/pith/V35PDP3XT6IXLG6MRDG3SV7BG3","download_json":"https://pith.science/pith/V35PDP3XT6IXLG6MRDG3SV7BG3.json","view_paper":"https://pith.science/paper/V35PDP3X","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1505.01739&json=true","fetch_graph":"https://pith.science/api/pith-number/V35PDP3XT6IXLG6MRDG3SV7BG3/graph.json","fetch_events":"https://pith.science/api/pith-number/V35PDP3XT6IXLG6MRDG3SV7BG3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/V35PDP3XT6IXLG6MRDG3SV7BG3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/V35PDP3XT6IXLG6MRDG3SV7BG3/action/storage_attestation","attest_author":"https://pith.science/pith/V35PDP3XT6IXLG6MRDG3SV7BG3/action/author_attestation","sign_citation":"https://pith.science/pith/V35PDP3XT6IXLG6MRDG3SV7BG3/action/citation_signature","submit_replication":"https://pith.science/pith/V35PDP3XT6IXLG6MRDG3SV7BG3/action/replication_record"}},"created_at":"2026-05-18T01:46:14.663547+00:00","updated_at":"2026-05-18T01:46:14.663547+00:00"}