{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:SYYNQ3TDZR7KOSLL2RTTTATLXE","short_pith_number":"pith:SYYNQ3TD","schema_version":"1.0","canonical_sha256":"9630d86e63cc7ea7496bd46739826bb92a52c961de43092c1b2333891944367b","source":{"kind":"arxiv","id":"1110.2178","version":1},"attestation_state":"computed","paper":{"title":"The Optical Gravitational Lensing Experiment. High Proper Motion Stars in the OGLE-III Data for Magellanic Clouds Fields","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"2), (2) Universidad de Concepcion, 3), (3) Institute of Astronomy, A. Udalski (1), Cambridge, Chile, Concepcion, Departamento de Fisica, G. Pietrzynski (1, I. Soszynski (1), K. Ulaczyk (1) ((1) Warsaw University Observatory, L. Wyrzykowski (1, M. K. Szymanski (1), M. Kubiak (1), Poland, R. Poleski (1), UK), University of Cambridge, Warszawa","submitted_at":"2011-10-10T20:00:03Z","abstract_excerpt":"We present the results of a search for High Proper Motion (HPM) stars, i.e. the ones with \\mu > 100 mas/yr, in the direction to the Magellanic Clouds. This sky area was not examined in detail as the high stellar density hampers efforts in performing high-quality astrometry.\n  Altogether 549 HPM stars were found with median uncertainties of proper motions per coordinate equal to 0.5 mas/yr. The fastest HPM star has the proper motion of 722.19 +/- 0.74 mas/yr. For the majority of objects (70%) parallaxes were also measured. The highest value found is \\pi = 91.3 +/-1.6 mas. The parallaxes were us"},"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":"1110.2178","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2011-10-10T20:00:03Z","cross_cats_sorted":[],"title_canon_sha256":"b7d6606ecaf680425bc94f884739ac0db98d5b0efceff04ea90dc9102788e07f","abstract_canon_sha256":"9e4d596285da093d90108318e5a236a18b9970455fb3eba6960d8dd3ad4c0b30"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:11:17.455530Z","signature_b64":"GmOQL8Ui0QEDzsaRBAxw4cXb0TLaJmLIAwRlrQHlIRW5mgV1psJGXjXLQUkvqaIz3eWQnZ2BRATMNUWo2TitBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9630d86e63cc7ea7496bd46739826bb92a52c961de43092c1b2333891944367b","last_reissued_at":"2026-05-18T04:11:17.454670Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:11:17.454670Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Optical Gravitational Lensing Experiment. High Proper Motion Stars in the OGLE-III Data for Magellanic Clouds Fields","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"2), (2) Universidad de Concepcion, 3), (3) Institute of Astronomy, A. Udalski (1), Cambridge, Chile, Concepcion, Departamento de Fisica, G. Pietrzynski (1, I. Soszynski (1), K. Ulaczyk (1) ((1) Warsaw University Observatory, L. Wyrzykowski (1, M. K. Szymanski (1), M. Kubiak (1), Poland, R. Poleski (1), UK), University of Cambridge, Warszawa","submitted_at":"2011-10-10T20:00:03Z","abstract_excerpt":"We present the results of a search for High Proper Motion (HPM) stars, i.e. the ones with \\mu > 100 mas/yr, in the direction to the Magellanic Clouds. This sky area was not examined in detail as the high stellar density hampers efforts in performing high-quality astrometry.\n  Altogether 549 HPM stars were found with median uncertainties of proper motions per coordinate equal to 0.5 mas/yr. The fastest HPM star has the proper motion of 722.19 +/- 0.74 mas/yr. For the majority of objects (70%) parallaxes were also measured. The highest value found is \\pi = 91.3 +/-1.6 mas. The parallaxes were us"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1110.2178","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":"1110.2178","created_at":"2026-05-18T04:11:17.454815+00:00"},{"alias_kind":"arxiv_version","alias_value":"1110.2178v1","created_at":"2026-05-18T04:11:17.454815+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1110.2178","created_at":"2026-05-18T04:11:17.454815+00:00"},{"alias_kind":"pith_short_12","alias_value":"SYYNQ3TDZR7K","created_at":"2026-05-18T12:26:41.206345+00:00"},{"alias_kind":"pith_short_16","alias_value":"SYYNQ3TDZR7KOSLL","created_at":"2026-05-18T12:26:41.206345+00:00"},{"alias_kind":"pith_short_8","alias_value":"SYYNQ3TD","created_at":"2026-05-18T12:26:41.206345+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/SYYNQ3TDZR7KOSLL2RTTTATLXE","json":"https://pith.science/pith/SYYNQ3TDZR7KOSLL2RTTTATLXE.json","graph_json":"https://pith.science/api/pith-number/SYYNQ3TDZR7KOSLL2RTTTATLXE/graph.json","events_json":"https://pith.science/api/pith-number/SYYNQ3TDZR7KOSLL2RTTTATLXE/events.json","paper":"https://pith.science/paper/SYYNQ3TD"},"agent_actions":{"view_html":"https://pith.science/pith/SYYNQ3TDZR7KOSLL2RTTTATLXE","download_json":"https://pith.science/pith/SYYNQ3TDZR7KOSLL2RTTTATLXE.json","view_paper":"https://pith.science/paper/SYYNQ3TD","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1110.2178&json=true","fetch_graph":"https://pith.science/api/pith-number/SYYNQ3TDZR7KOSLL2RTTTATLXE/graph.json","fetch_events":"https://pith.science/api/pith-number/SYYNQ3TDZR7KOSLL2RTTTATLXE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SYYNQ3TDZR7KOSLL2RTTTATLXE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SYYNQ3TDZR7KOSLL2RTTTATLXE/action/storage_attestation","attest_author":"https://pith.science/pith/SYYNQ3TDZR7KOSLL2RTTTATLXE/action/author_attestation","sign_citation":"https://pith.science/pith/SYYNQ3TDZR7KOSLL2RTTTATLXE/action/citation_signature","submit_replication":"https://pith.science/pith/SYYNQ3TDZR7KOSLL2RTTTATLXE/action/replication_record"}},"created_at":"2026-05-18T04:11:17.454815+00:00","updated_at":"2026-05-18T04:11:17.454815+00:00"}