{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:TVRBNFBVXWMTMOTQDV7G2RPVBR","short_pith_number":"pith:TVRBNFBV","schema_version":"1.0","canonical_sha256":"9d62169435bd99363a701d7e6d45f50c4b58cbec674b181cd9b8e3067e198b2f","source":{"kind":"arxiv","id":"1802.03234","version":1},"attestation_state":"computed","paper":{"title":"A revised distance to IRAS 16293$-$2422 from VLBA astrometry of associated water masers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"A. Hern\\'andez-G\\'omez, A. J. Mioduszewski, A. Sanna, E. Caux, G. N. Ortiz-Le\\'on, K. M. Menten, L. Loinard, M. Claussen, S. A. Dzib","submitted_at":"2018-02-09T12:45:25Z","abstract_excerpt":"IRAS 16293-2422 is a very well studied young stellar system seen in projection towards the L1689N cloud in the Ophiuchus complex. However, its distance is still uncertain with a range of values from 120 pc to 180 pc. Our goal is to measure the trigonometric parallax of this young star by means of H$_2$O maser emission. We use archival data from 15 epochs of VLBA observations of the 22.2 GHz water maser line. By modeling the displacement on the sky of the H$_2$O maser spots, we derived a trigonometric parallax of $7.1\\pm1.3$ mas, corresponding to a distance of $141_{-21}^{+30}$ pc. This new dis"},"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":"1802.03234","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2018-02-09T12:45:25Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"708e303d24a512a605ca49dcd99f14d66da7d2b998a23743ea2d9d4046d07594","abstract_canon_sha256":"5f6aaa601ebc3355ea7e24706e874f309784910de2407d7a2143cfbf3a001555"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:13:27.942134Z","signature_b64":"K3KEeUhmxGDdfVbMjBcX0meJXNA95015xKjBuKSLjBsWu9Y4KunXdByTqJStAVARM6lRSsJUNZqY6b1NsUlWDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9d62169435bd99363a701d7e6d45f50c4b58cbec674b181cd9b8e3067e198b2f","last_reissued_at":"2026-05-18T00:13:27.941635Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:13:27.941635Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A revised distance to IRAS 16293$-$2422 from VLBA astrometry of associated water masers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.SR","authors_text":"A. Hern\\'andez-G\\'omez, A. J. Mioduszewski, A. Sanna, E. Caux, G. N. Ortiz-Le\\'on, K. M. Menten, L. Loinard, M. Claussen, S. A. Dzib","submitted_at":"2018-02-09T12:45:25Z","abstract_excerpt":"IRAS 16293-2422 is a very well studied young stellar system seen in projection towards the L1689N cloud in the Ophiuchus complex. However, its distance is still uncertain with a range of values from 120 pc to 180 pc. Our goal is to measure the trigonometric parallax of this young star by means of H$_2$O maser emission. We use archival data from 15 epochs of VLBA observations of the 22.2 GHz water maser line. By modeling the displacement on the sky of the H$_2$O maser spots, we derived a trigonometric parallax of $7.1\\pm1.3$ mas, corresponding to a distance of $141_{-21}^{+30}$ pc. This new dis"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1802.03234","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":"1802.03234","created_at":"2026-05-18T00:13:27.941701+00:00"},{"alias_kind":"arxiv_version","alias_value":"1802.03234v1","created_at":"2026-05-18T00:13:27.941701+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1802.03234","created_at":"2026-05-18T00:13:27.941701+00:00"},{"alias_kind":"pith_short_12","alias_value":"TVRBNFBVXWMT","created_at":"2026-05-18T12:32:56.356000+00:00"},{"alias_kind":"pith_short_16","alias_value":"TVRBNFBVXWMTMOTQ","created_at":"2026-05-18T12:32:56.356000+00:00"},{"alias_kind":"pith_short_8","alias_value":"TVRBNFBV","created_at":"2026-05-18T12:32:56.356000+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.00212","citing_title":"Subarcsecond Multi-line Observations of NH$_3$ with VLA toward the Class 0 Source IRAS 16293-2422","ref_index":28,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/TVRBNFBVXWMTMOTQDV7G2RPVBR","json":"https://pith.science/pith/TVRBNFBVXWMTMOTQDV7G2RPVBR.json","graph_json":"https://pith.science/api/pith-number/TVRBNFBVXWMTMOTQDV7G2RPVBR/graph.json","events_json":"https://pith.science/api/pith-number/TVRBNFBVXWMTMOTQDV7G2RPVBR/events.json","paper":"https://pith.science/paper/TVRBNFBV"},"agent_actions":{"view_html":"https://pith.science/pith/TVRBNFBVXWMTMOTQDV7G2RPVBR","download_json":"https://pith.science/pith/TVRBNFBVXWMTMOTQDV7G2RPVBR.json","view_paper":"https://pith.science/paper/TVRBNFBV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1802.03234&json=true","fetch_graph":"https://pith.science/api/pith-number/TVRBNFBVXWMTMOTQDV7G2RPVBR/graph.json","fetch_events":"https://pith.science/api/pith-number/TVRBNFBVXWMTMOTQDV7G2RPVBR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/TVRBNFBVXWMTMOTQDV7G2RPVBR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/TVRBNFBVXWMTMOTQDV7G2RPVBR/action/storage_attestation","attest_author":"https://pith.science/pith/TVRBNFBVXWMTMOTQDV7G2RPVBR/action/author_attestation","sign_citation":"https://pith.science/pith/TVRBNFBVXWMTMOTQDV7G2RPVBR/action/citation_signature","submit_replication":"https://pith.science/pith/TVRBNFBVXWMTMOTQDV7G2RPVBR/action/replication_record"}},"created_at":"2026-05-18T00:13:27.941701+00:00","updated_at":"2026-05-18T00:13:27.941701+00:00"}