{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:BMSS2PDBOVD3XJE2VNPEZHESVT","short_pith_number":"pith:BMSS2PDB","schema_version":"1.0","canonical_sha256":"0b252d3c617547bba49aab5e4c9c92acffdb2f812fcb27138d1386e1af177725","source":{"kind":"arxiv","id":"1109.1220","version":1},"attestation_state":"computed","paper":{"title":"The nature of the embedded intermediate-mass T Tauri star DK Cha","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["physics.space-ph"],"primary_cat":"astro-ph.SR","authors_text":"2, (2) INAF-Osservatorio Astronomico di Roma, 3), (3) Max-Planck-Institut f\\\"ur Radioastronomie, (4) Th\\\"uringer Landessternwarte Tautenburg), Alessio Caratti o Garatti (1), Brunella Nisini (2), Dario Lorenzetti (2), Jochen Eisl\\\"offel (4), Rebeca Garcia Lopez (1, Simone Antoniucci (2), Teresa Giannini (2), Tom Ray (1) ((1) Dublin Institute for Advanced Studies","submitted_at":"2011-09-06T16:13:04Z","abstract_excerpt":"Most of our knowledge about star formation is based on studies of low-mass stars, whereas very little is known about the properties of the circumstellar material around young and embedded intermidiate-mass T Tauri stars (IMTTSs). We present an analysis of the excitation and accretion properties of the young IMTTS DK Cha. The nearly face-on configuration of this source allows us to have direct access to the star-disk system through the excavated envelope and outflow cavity. Based on LR optical and IR spectroscopy obtained with SofI/EFOSC2 on the NTT we derive the spectrum of DK Cha from ~0.6 to"},"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":"1109.1220","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2011-09-06T16:13:04Z","cross_cats_sorted":["physics.space-ph"],"title_canon_sha256":"31ffa0092043ff5508e495c955cf94e1a371ddd90538ea67a61700bfcb50abc7","abstract_canon_sha256":"c26db3a0ab049787139aa9f4ab73df86053d8b68ef973a52573bf71943beac88"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:00:38.907012Z","signature_b64":"UI/CLOhJH1kpls/bUohVABCjsqoDbmkpJt8K2jcr7yXnvOhnKF4+80kKMIhyIkYvHP6TKDZ2stXOWZtbOdwcBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0b252d3c617547bba49aab5e4c9c92acffdb2f812fcb27138d1386e1af177725","last_reissued_at":"2026-05-18T02:00:38.906413Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:00:38.906413Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The nature of the embedded intermediate-mass T Tauri star DK Cha","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["physics.space-ph"],"primary_cat":"astro-ph.SR","authors_text":"2, (2) INAF-Osservatorio Astronomico di Roma, 3), (3) Max-Planck-Institut f\\\"ur Radioastronomie, (4) Th\\\"uringer Landessternwarte Tautenburg), Alessio Caratti o Garatti (1), Brunella Nisini (2), Dario Lorenzetti (2), Jochen Eisl\\\"offel (4), Rebeca Garcia Lopez (1, Simone Antoniucci (2), Teresa Giannini (2), Tom Ray (1) ((1) Dublin Institute for Advanced Studies","submitted_at":"2011-09-06T16:13:04Z","abstract_excerpt":"Most of our knowledge about star formation is based on studies of low-mass stars, whereas very little is known about the properties of the circumstellar material around young and embedded intermidiate-mass T Tauri stars (IMTTSs). We present an analysis of the excitation and accretion properties of the young IMTTS DK Cha. The nearly face-on configuration of this source allows us to have direct access to the star-disk system through the excavated envelope and outflow cavity. Based on LR optical and IR spectroscopy obtained with SofI/EFOSC2 on the NTT we derive the spectrum of DK Cha from ~0.6 to"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1109.1220","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":"1109.1220","created_at":"2026-05-18T02:00:38.906495+00:00"},{"alias_kind":"arxiv_version","alias_value":"1109.1220v1","created_at":"2026-05-18T02:00:38.906495+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1109.1220","created_at":"2026-05-18T02:00:38.906495+00:00"},{"alias_kind":"pith_short_12","alias_value":"BMSS2PDBOVD3","created_at":"2026-05-18T12:26:24.575870+00:00"},{"alias_kind":"pith_short_16","alias_value":"BMSS2PDBOVD3XJE2","created_at":"2026-05-18T12:26:24.575870+00:00"},{"alias_kind":"pith_short_8","alias_value":"BMSS2PDB","created_at":"2026-05-18T12:26:24.575870+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/BMSS2PDBOVD3XJE2VNPEZHESVT","json":"https://pith.science/pith/BMSS2PDBOVD3XJE2VNPEZHESVT.json","graph_json":"https://pith.science/api/pith-number/BMSS2PDBOVD3XJE2VNPEZHESVT/graph.json","events_json":"https://pith.science/api/pith-number/BMSS2PDBOVD3XJE2VNPEZHESVT/events.json","paper":"https://pith.science/paper/BMSS2PDB"},"agent_actions":{"view_html":"https://pith.science/pith/BMSS2PDBOVD3XJE2VNPEZHESVT","download_json":"https://pith.science/pith/BMSS2PDBOVD3XJE2VNPEZHESVT.json","view_paper":"https://pith.science/paper/BMSS2PDB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1109.1220&json=true","fetch_graph":"https://pith.science/api/pith-number/BMSS2PDBOVD3XJE2VNPEZHESVT/graph.json","fetch_events":"https://pith.science/api/pith-number/BMSS2PDBOVD3XJE2VNPEZHESVT/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/BMSS2PDBOVD3XJE2VNPEZHESVT/action/timestamp_anchor","attest_storage":"https://pith.science/pith/BMSS2PDBOVD3XJE2VNPEZHESVT/action/storage_attestation","attest_author":"https://pith.science/pith/BMSS2PDBOVD3XJE2VNPEZHESVT/action/author_attestation","sign_citation":"https://pith.science/pith/BMSS2PDBOVD3XJE2VNPEZHESVT/action/citation_signature","submit_replication":"https://pith.science/pith/BMSS2PDBOVD3XJE2VNPEZHESVT/action/replication_record"}},"created_at":"2026-05-18T02:00:38.906495+00:00","updated_at":"2026-05-18T02:00:38.906495+00:00"}