{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:YDPOZVRATX7LXSRSZQAERYEHAQ","short_pith_number":"pith:YDPOZVRA","schema_version":"1.0","canonical_sha256":"c0deecd6209dfebbca32cc0048e08704304073dee1e9ad62ecf6a9cedbe72d1f","source":{"kind":"arxiv","id":"1906.02058","version":3},"attestation_state":"computed","paper":{"title":"Constraining the properties of HD 206893 B. A combination of radial velocity, direct imaging, and astrometry data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.EP","authors_text":"A. Boccaletti, A. Cheetham, A. Grandjean, A.-L. Maire, A.-M. Lagrange, A. Zurlo, B. A. Biller, C. Babusiaux, C. Lazzoni, C. Perrot, D. Mesa, D. Rouan, H. Beust, J. Hagelberg, J. H. Girard, J. Lannier, J.-L. Baudino, J. Milli, L. Rodet, M. Bonavita, M. Bonnefoy, M. Janson, N. Meunier, N. Zicher, P. Delorme, P. Rubini, R. Ligi, S. Aigrain","submitted_at":"2019-06-05T14:54:57Z","abstract_excerpt":"High contrast imaging enables the determination of orbital parameters for substellar companions (planets, brown dwarfs) from the observed relative astrometry and the estimation of model and age-dependent masses from their observed magnitudes or spectra. Combining astrometric positions with radial velocity gives direct constraints on the orbit and on the dynamical masses of companions. A brown dwarf was discovered with the VLT/SPHERE instrument in 2017, which orbits at $\\sim$ 11 au around HD 206893. Its mass was estimated between 12 and 50 $M_{Jup}$ from evolutionary models and its photometry. "},"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":"1906.02058","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.EP","submitted_at":"2019-06-05T14:54:57Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"bef52a0e05d8f07a6c834643b98bc52788997183cd73b11611853d0c91c8a7af","abstract_canon_sha256":"8810461b979b4cea772fcc81c3814caa334f42b54a693e428fbf166ad3725d11"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:39:39.403490Z","signature_b64":"rUeTNDTQq+15CbjFAg0pwIXiWQosAFeIxeGxb1Hlo7tUHr8qg2SKzP+MJBKpLlERIDb7nxB8Y4IlISDEmQQnBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c0deecd6209dfebbca32cc0048e08704304073dee1e9ad62ecf6a9cedbe72d1f","last_reissued_at":"2026-05-17T23:39:39.402866Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:39:39.402866Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Constraining the properties of HD 206893 B. A combination of radial velocity, direct imaging, and astrometry data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.EP","authors_text":"A. Boccaletti, A. Cheetham, A. Grandjean, A.-L. Maire, A.-M. Lagrange, A. Zurlo, B. A. Biller, C. Babusiaux, C. Lazzoni, C. Perrot, D. Mesa, D. Rouan, H. Beust, J. Hagelberg, J. H. Girard, J. Lannier, J.-L. Baudino, J. Milli, L. Rodet, M. Bonavita, M. Bonnefoy, M. Janson, N. Meunier, N. Zicher, P. Delorme, P. Rubini, R. Ligi, S. Aigrain","submitted_at":"2019-06-05T14:54:57Z","abstract_excerpt":"High contrast imaging enables the determination of orbital parameters for substellar companions (planets, brown dwarfs) from the observed relative astrometry and the estimation of model and age-dependent masses from their observed magnitudes or spectra. Combining astrometric positions with radial velocity gives direct constraints on the orbit and on the dynamical masses of companions. A brown dwarf was discovered with the VLT/SPHERE instrument in 2017, which orbits at $\\sim$ 11 au around HD 206893. Its mass was estimated between 12 and 50 $M_{Jup}$ from evolutionary models and its photometry. "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1906.02058","kind":"arxiv","version":3},"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":"1906.02058","created_at":"2026-05-17T23:39:39.402964+00:00"},{"alias_kind":"arxiv_version","alias_value":"1906.02058v3","created_at":"2026-05-17T23:39:39.402964+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1906.02058","created_at":"2026-05-17T23:39:39.402964+00:00"},{"alias_kind":"pith_short_12","alias_value":"YDPOZVRATX7L","created_at":"2026-05-18T12:33:33.725879+00:00"},{"alias_kind":"pith_short_16","alias_value":"YDPOZVRATX7LXSRS","created_at":"2026-05-18T12:33:33.725879+00:00"},{"alias_kind":"pith_short_8","alias_value":"YDPOZVRA","created_at":"2026-05-18T12:33:33.725879+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/YDPOZVRATX7LXSRSZQAERYEHAQ","json":"https://pith.science/pith/YDPOZVRATX7LXSRSZQAERYEHAQ.json","graph_json":"https://pith.science/api/pith-number/YDPOZVRATX7LXSRSZQAERYEHAQ/graph.json","events_json":"https://pith.science/api/pith-number/YDPOZVRATX7LXSRSZQAERYEHAQ/events.json","paper":"https://pith.science/paper/YDPOZVRA"},"agent_actions":{"view_html":"https://pith.science/pith/YDPOZVRATX7LXSRSZQAERYEHAQ","download_json":"https://pith.science/pith/YDPOZVRATX7LXSRSZQAERYEHAQ.json","view_paper":"https://pith.science/paper/YDPOZVRA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1906.02058&json=true","fetch_graph":"https://pith.science/api/pith-number/YDPOZVRATX7LXSRSZQAERYEHAQ/graph.json","fetch_events":"https://pith.science/api/pith-number/YDPOZVRATX7LXSRSZQAERYEHAQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YDPOZVRATX7LXSRSZQAERYEHAQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YDPOZVRATX7LXSRSZQAERYEHAQ/action/storage_attestation","attest_author":"https://pith.science/pith/YDPOZVRATX7LXSRSZQAERYEHAQ/action/author_attestation","sign_citation":"https://pith.science/pith/YDPOZVRATX7LXSRSZQAERYEHAQ/action/citation_signature","submit_replication":"https://pith.science/pith/YDPOZVRATX7LXSRSZQAERYEHAQ/action/replication_record"}},"created_at":"2026-05-17T23:39:39.402964+00:00","updated_at":"2026-05-17T23:39:39.402964+00:00"}