{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2003:W2DXO5IYI6Q3CEYE3EKBBQDYP4","short_pith_number":"pith:W2DXO5IY","schema_version":"1.0","canonical_sha256":"b68777751847a1b11304d91410c0787f18c3c7bcfe4f4018336d21f05d6dc459","source":{"kind":"arxiv","id":"astro-ph/0303565","version":1},"attestation_state":"computed","paper":{"title":"Evidence for a T Tauri Phase in Young Brown Dwarfs","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Gibor Basri, Ray Jayawardhana, Subhanjoy Mohanty","submitted_at":"2003-03-25T21:04:08Z","abstract_excerpt":"As part of a multi-faceted program to investigate the origin and early evolution of sub-stellar objects, we present high-resolution Keck optical spectra of 14 very low mass sources in the IC 348 young cluster and the Taurus star-forming cloud. All of our targets, which span a range of spectral types from M5 to M8, exhibit moderate to very strong H$\\alpha$ emission. In half of the IC 348 objects, the H$\\alpha$ profiles are broad and asymmetric, indicative of on-going accretion. Of these, IC348-355 (M8) is the lowest mass object to date to show accretion-like H$\\alpha$. Three of our ~M6 IC 348 t"},"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/0303565","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2003-03-25T21:04:08Z","cross_cats_sorted":[],"title_canon_sha256":"08ef36bfe9b077675b2df200743c1cc632b819b00cea74d9a806daa7cf48a5cd","abstract_canon_sha256":"e0c68a672b9069a68066dff8bcebcd2cb96a2b2a81378d5af5b0eede1c729876"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:36:44.396738Z","signature_b64":"TmkqevgSzukxRBOmajMZ7Cfg1IbsnRJWvh0Tt/a+juCbnj2+xLkzrfTciKIK869Db0I2lHWZdfpC3R1rN8DpBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b68777751847a1b11304d91410c0787f18c3c7bcfe4f4018336d21f05d6dc459","last_reissued_at":"2026-07-04T16:36:44.396304Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:36:44.396304Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Evidence for a T Tauri Phase in Young Brown Dwarfs","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Gibor Basri, Ray Jayawardhana, Subhanjoy Mohanty","submitted_at":"2003-03-25T21:04:08Z","abstract_excerpt":"As part of a multi-faceted program to investigate the origin and early evolution of sub-stellar objects, we present high-resolution Keck optical spectra of 14 very low mass sources in the IC 348 young cluster and the Taurus star-forming cloud. All of our targets, which span a range of spectral types from M5 to M8, exhibit moderate to very strong H$\\alpha$ emission. In half of the IC 348 objects, the H$\\alpha$ profiles are broad and asymmetric, indicative of on-going accretion. Of these, IC348-355 (M8) is the lowest mass object to date to show accretion-like H$\\alpha$. Three of our ~M6 IC 348 t"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0303565","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/astro-ph/0303565/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":"astro-ph/0303565","created_at":"2026-07-04T16:36:44.396383+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0303565v1","created_at":"2026-07-04T16:36:44.396383+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0303565","created_at":"2026-07-04T16:36:44.396383+00:00"},{"alias_kind":"pith_short_12","alias_value":"W2DXO5IYI6Q3","created_at":"2026-07-04T16:36:44.396383+00:00"},{"alias_kind":"pith_short_16","alias_value":"W2DXO5IYI6Q3CEYE","created_at":"2026-07-04T16:36:44.396383+00:00"},{"alias_kind":"pith_short_8","alias_value":"W2DXO5IY","created_at":"2026-07-04T16:36:44.396383+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2507.08592","citing_title":"XMM-Newton follow-up of two eROSITA X-ray binary candidates","ref_index":83,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/W2DXO5IYI6Q3CEYE3EKBBQDYP4","json":"https://pith.science/pith/W2DXO5IYI6Q3CEYE3EKBBQDYP4.json","graph_json":"https://pith.science/api/pith-number/W2DXO5IYI6Q3CEYE3EKBBQDYP4/graph.json","events_json":"https://pith.science/api/pith-number/W2DXO5IYI6Q3CEYE3EKBBQDYP4/events.json","paper":"https://pith.science/paper/W2DXO5IY"},"agent_actions":{"view_html":"https://pith.science/pith/W2DXO5IYI6Q3CEYE3EKBBQDYP4","download_json":"https://pith.science/pith/W2DXO5IYI6Q3CEYE3EKBBQDYP4.json","view_paper":"https://pith.science/paper/W2DXO5IY","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0303565&json=true","fetch_graph":"https://pith.science/api/pith-number/W2DXO5IYI6Q3CEYE3EKBBQDYP4/graph.json","fetch_events":"https://pith.science/api/pith-number/W2DXO5IYI6Q3CEYE3EKBBQDYP4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/W2DXO5IYI6Q3CEYE3EKBBQDYP4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/W2DXO5IYI6Q3CEYE3EKBBQDYP4/action/storage_attestation","attest_author":"https://pith.science/pith/W2DXO5IYI6Q3CEYE3EKBBQDYP4/action/author_attestation","sign_citation":"https://pith.science/pith/W2DXO5IYI6Q3CEYE3EKBBQDYP4/action/citation_signature","submit_replication":"https://pith.science/pith/W2DXO5IYI6Q3CEYE3EKBBQDYP4/action/replication_record"}},"created_at":"2026-07-04T16:36:44.396383+00:00","updated_at":"2026-07-04T16:36:44.396383+00:00"}