{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:SMUWDLQMTUMM5TEFVGW5TQKQ33","short_pith_number":"pith:SMUWDLQM","schema_version":"1.0","canonical_sha256":"932961ae0c9d18cecc85a9add9c150dec2d89e260efd2164c6d2d444b8eee1ea","source":{"kind":"arxiv","id":"1901.04896","version":1},"attestation_state":"computed","paper":{"title":"An Asymmetric Keplerian Disk Surrounding the O-type Protostar IRAS16547$-$4247","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"Aina Palau (UNAM), Andres Guzman (NAOJ), Guido Garay (UC), Luis A. Zapata (UNAM), Luis F. Rodriguez (UNAM), Manuel Fernandez-Lopez (IAR), Robert Estalella (UB)","submitted_at":"2019-01-15T16:05:55Z","abstract_excerpt":"During the last decades, a great interest has emerged to know if even the most massive stars in our galaxy (namely the spectral O-type stars) are formed in a similar manner as the low- and intermediate-mass stars, that is, through the presence of accreting disks and powerful outflows. Here, using sensitive observations of the Atacama Large Millimeter/Submillimeter Array (ALMA), we report a resolved Keplerian disk (with fifteen synthesized beams across its major axis) surrounding the deeply embedded O-type protostar IRAS16547$-$4247. The disk shows some asymmetries that could arise because of t"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"1901.04896","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2019-01-15T16:05:55Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"9039e56fd315f474e2f0bee012136815adf903b1ef9a3f2bce652ae075d86b30","abstract_canon_sha256":"2a8ba819c94730e891167e7d0892fcd5c1b3f05d0a7f7a25572dfaae15d062e2"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:52:38.582937Z","signature_b64":"aOx7FMcsyx5ieusIEniVslS4iiP6/ST/j8fzx351eRZDTSfFGm8nVSC8B3gohPMyn9vf+2rMFijT78/t9tvIBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"932961ae0c9d18cecc85a9add9c150dec2d89e260efd2164c6d2d444b8eee1ea","last_reissued_at":"2026-05-17T23:52:38.582168Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:52:38.582168Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"An Asymmetric Keplerian Disk Surrounding the O-type Protostar IRAS16547$-$4247","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"Aina Palau (UNAM), Andres Guzman (NAOJ), Guido Garay (UC), Luis A. Zapata (UNAM), Luis F. Rodriguez (UNAM), Manuel Fernandez-Lopez (IAR), Robert Estalella (UB)","submitted_at":"2019-01-15T16:05:55Z","abstract_excerpt":"During the last decades, a great interest has emerged to know if even the most massive stars in our galaxy (namely the spectral O-type stars) are formed in a similar manner as the low- and intermediate-mass stars, that is, through the presence of accreting disks and powerful outflows. Here, using sensitive observations of the Atacama Large Millimeter/Submillimeter Array (ALMA), we report a resolved Keplerian disk (with fifteen synthesized beams across its major axis) surrounding the deeply embedded O-type protostar IRAS16547$-$4247. The disk shows some asymmetries that could arise because of t"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1901.04896","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":"1901.04896","created_at":"2026-05-17T23:52:38.582283+00:00"},{"alias_kind":"arxiv_version","alias_value":"1901.04896v1","created_at":"2026-05-17T23:52:38.582283+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1901.04896","created_at":"2026-05-17T23:52:38.582283+00:00"},{"alias_kind":"pith_short_12","alias_value":"SMUWDLQMTUMM","created_at":"2026-05-18T12:33:27.125529+00:00"},{"alias_kind":"pith_short_16","alias_value":"SMUWDLQMTUMM5TEF","created_at":"2026-05-18T12:33:27.125529+00:00"},{"alias_kind":"pith_short_8","alias_value":"SMUWDLQM","created_at":"2026-05-18T12:33:27.125529+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.12595","citing_title":"Global and Local Infall in the ASHES Sample (GLASHES). II. Asymmetric Line Profiles around Dense Cores in 70 $\\mu$m Dark Massive Clumps","ref_index":249,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/SMUWDLQMTUMM5TEFVGW5TQKQ33","json":"https://pith.science/pith/SMUWDLQMTUMM5TEFVGW5TQKQ33.json","graph_json":"https://pith.science/api/pith-number/SMUWDLQMTUMM5TEFVGW5TQKQ33/graph.json","events_json":"https://pith.science/api/pith-number/SMUWDLQMTUMM5TEFVGW5TQKQ33/events.json","paper":"https://pith.science/paper/SMUWDLQM"},"agent_actions":{"view_html":"https://pith.science/pith/SMUWDLQMTUMM5TEFVGW5TQKQ33","download_json":"https://pith.science/pith/SMUWDLQMTUMM5TEFVGW5TQKQ33.json","view_paper":"https://pith.science/paper/SMUWDLQM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1901.04896&json=true","fetch_graph":"https://pith.science/api/pith-number/SMUWDLQMTUMM5TEFVGW5TQKQ33/graph.json","fetch_events":"https://pith.science/api/pith-number/SMUWDLQMTUMM5TEFVGW5TQKQ33/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SMUWDLQMTUMM5TEFVGW5TQKQ33/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SMUWDLQMTUMM5TEFVGW5TQKQ33/action/storage_attestation","attest_author":"https://pith.science/pith/SMUWDLQMTUMM5TEFVGW5TQKQ33/action/author_attestation","sign_citation":"https://pith.science/pith/SMUWDLQMTUMM5TEFVGW5TQKQ33/action/citation_signature","submit_replication":"https://pith.science/pith/SMUWDLQMTUMM5TEFVGW5TQKQ33/action/replication_record"}},"created_at":"2026-05-17T23:52:38.582283+00:00","updated_at":"2026-05-17T23:52:38.582283+00:00"}