{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2001:GBWOTFBJCJLV6NEV7JHCKWNK6D","short_pith_number":"pith:GBWOTFBJ","schema_version":"1.0","canonical_sha256":"306ce9942912575f3495fa4e2559aaf0c94e7b3ba7b0a3cd4425ec7dcdd6b9c1","source":{"kind":"arxiv","id":"astro-ph/0108249","version":1},"attestation_state":"computed","paper":{"title":"Optical spectroscopy of isolated planetary mass objects in the sigma Orionis cluster","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"2), 5), C.A.L. Bailer-Jones (2). ((1) Universidad Aut\\'onoma de Madrid, CSIC, D. Barrado-y-Navascu\\'es (1, E.L. Mart\\'in (6), Hawaii, Heidelberg. Germany (3) California Institute of Technology, Madrid, M.R. Zapatero-Osorio (3), Pasadena, R. Mundt (2), R. Rebolo (4, Spain. (2) Max-Planck-Institut f\\\"ur Astronomie, Spain (5) Consejo Superior de Investigaciones Cient\\'ificas, Spain (6) Institute of Astronomy. University of Hawaii, Tenerife, USA), USA (4) Instituto de Astrof\\'isica de Canarias, V.J.S. B\\'ejar (4)","submitted_at":"2001-08-15T01:37:09Z","abstract_excerpt":"We have obtained low resolution optical spectra of 15 isolated planetary mass objects (IPMOs) in the sigma Orionis cluster, and derived spectral types by comparison with nearby M and L dwarfs. The spectral types are in the range late M - mid L, in agreement with our expectations based on colors and magnitudes for bona fide members. Therefore, most of these objects have masses below the deuterium burning limit. About 2/3 show H(alpha) in emission at our spectral resolution. From our spectroscopic and photometric data, we infer that three IPMOs in this sample may be binaries with components of s"},"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/0108249","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2001-08-15T01:37:09Z","cross_cats_sorted":[],"title_canon_sha256":"28046a05c391a19a947ceaafa91629c301372f9e38b3f0121538acd6cb5e72ae","abstract_canon_sha256":"e6e23e98856c4e634ac2160eba79054612e008c6e34f10776fbded4585954c29"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:09:10.875892Z","signature_b64":"a/vOE+/1EVJNUrR+j6IRMDKpErbVHlz7yp5KomESV6VfGhfhWq5pc04DMRKADPhtF6U/Evxygu/LTGa/IettCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"306ce9942912575f3495fa4e2559aaf0c94e7b3ba7b0a3cd4425ec7dcdd6b9c1","last_reissued_at":"2026-05-18T01:09:10.875239Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:09:10.875239Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Optical spectroscopy of isolated planetary mass objects in the sigma Orionis cluster","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"2), 5), C.A.L. Bailer-Jones (2). ((1) Universidad Aut\\'onoma de Madrid, CSIC, D. Barrado-y-Navascu\\'es (1, E.L. Mart\\'in (6), Hawaii, Heidelberg. Germany (3) California Institute of Technology, Madrid, M.R. Zapatero-Osorio (3), Pasadena, R. Mundt (2), R. Rebolo (4, Spain. (2) Max-Planck-Institut f\\\"ur Astronomie, Spain (5) Consejo Superior de Investigaciones Cient\\'ificas, Spain (6) Institute of Astronomy. University of Hawaii, Tenerife, USA), USA (4) Instituto de Astrof\\'isica de Canarias, V.J.S. B\\'ejar (4)","submitted_at":"2001-08-15T01:37:09Z","abstract_excerpt":"We have obtained low resolution optical spectra of 15 isolated planetary mass objects (IPMOs) in the sigma Orionis cluster, and derived spectral types by comparison with nearby M and L dwarfs. The spectral types are in the range late M - mid L, in agreement with our expectations based on colors and magnitudes for bona fide members. Therefore, most of these objects have masses below the deuterium burning limit. About 2/3 show H(alpha) in emission at our spectral resolution. From our spectroscopic and photometric data, we infer that three IPMOs in this sample may be binaries with components of s"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0108249","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":"astro-ph/0108249","created_at":"2026-05-18T01:09:10.875334+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0108249v1","created_at":"2026-05-18T01:09:10.875334+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0108249","created_at":"2026-05-18T01:09:10.875334+00:00"},{"alias_kind":"pith_short_12","alias_value":"GBWOTFBJCJLV","created_at":"2026-05-18T12:25:50.254431+00:00"},{"alias_kind":"pith_short_16","alias_value":"GBWOTFBJCJLV6NEV","created_at":"2026-05-18T12:25:50.254431+00:00"},{"alias_kind":"pith_short_8","alias_value":"GBWOTFBJ","created_at":"2026-05-18T12:25:50.254431+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/GBWOTFBJCJLV6NEV7JHCKWNK6D","json":"https://pith.science/pith/GBWOTFBJCJLV6NEV7JHCKWNK6D.json","graph_json":"https://pith.science/api/pith-number/GBWOTFBJCJLV6NEV7JHCKWNK6D/graph.json","events_json":"https://pith.science/api/pith-number/GBWOTFBJCJLV6NEV7JHCKWNK6D/events.json","paper":"https://pith.science/paper/GBWOTFBJ"},"agent_actions":{"view_html":"https://pith.science/pith/GBWOTFBJCJLV6NEV7JHCKWNK6D","download_json":"https://pith.science/pith/GBWOTFBJCJLV6NEV7JHCKWNK6D.json","view_paper":"https://pith.science/paper/GBWOTFBJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0108249&json=true","fetch_graph":"https://pith.science/api/pith-number/GBWOTFBJCJLV6NEV7JHCKWNK6D/graph.json","fetch_events":"https://pith.science/api/pith-number/GBWOTFBJCJLV6NEV7JHCKWNK6D/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/GBWOTFBJCJLV6NEV7JHCKWNK6D/action/timestamp_anchor","attest_storage":"https://pith.science/pith/GBWOTFBJCJLV6NEV7JHCKWNK6D/action/storage_attestation","attest_author":"https://pith.science/pith/GBWOTFBJCJLV6NEV7JHCKWNK6D/action/author_attestation","sign_citation":"https://pith.science/pith/GBWOTFBJCJLV6NEV7JHCKWNK6D/action/citation_signature","submit_replication":"https://pith.science/pith/GBWOTFBJCJLV6NEV7JHCKWNK6D/action/replication_record"}},"created_at":"2026-05-18T01:09:10.875334+00:00","updated_at":"2026-05-18T01:09:10.875334+00:00"}