{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:4A32LKG2RBPQZCPSPYGGEVYNJT","short_pith_number":"pith:4A32LKG2","schema_version":"1.0","canonical_sha256":"e037a5a8da885f0c89f27e0c62570d4ce293b029f49dab71f9df41ca54deaf82","source":{"kind":"arxiv","id":"1804.09376","version":2},"attestation_state":"computed","paper":{"title":"Gaia Data Release 2: using Gaia parallaxes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.IM","authors_text":"A. Castro-Ginard, A.G.A. Brown, C.A.L. Bailer-Jones, C. Babusiaux, F. Arenou, H.E. Delgado, J. de Bruijne, L.M. Sarro, T. Prusti, X. Luri","submitted_at":"2018-04-25T06:25:26Z","abstract_excerpt":"The second Gaia data release (GDR2) provides precise five-parameter astrometric data (positions, proper motions and parallaxes) for an unprecedented amount of sources (more than $1.3$ billion, mostly stars). The use of this wealth of astrometric data comes with a specific challenge: how does one properly infer from these data the astrophysical parameters of interest?\n  The main - but not only - focus of this paper is the issue of the estimation of distances from parallaxes, possibly combined with other information. We start with a critical review of the methods traditionally used to obtain 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":"1804.09376","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.IM","submitted_at":"2018-04-25T06:25:26Z","cross_cats_sorted":[],"title_canon_sha256":"efd611a21b6dcd979d03026c4be90e685dab5de7ea01cd4e08d745325b30d142","abstract_canon_sha256":"a32709a7e677e0c5fd709e1137081402c6c2aad3b50e0d3544c6888fa57baafe"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:08:07.360833Z","signature_b64":"fiZutTF6lanAhMulYAAbCiqbTPyYfjlCeEDlHp7rwkkh4IXi+eC3aIuYj/HP1U7GznHoilHcdFS5mVL8jFVpDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e037a5a8da885f0c89f27e0c62570d4ce293b029f49dab71f9df41ca54deaf82","last_reissued_at":"2026-05-18T00:08:07.360383Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:08:07.360383Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Gaia Data Release 2: using Gaia parallaxes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.IM","authors_text":"A. Castro-Ginard, A.G.A. Brown, C.A.L. Bailer-Jones, C. Babusiaux, F. Arenou, H.E. Delgado, J. de Bruijne, L.M. Sarro, T. Prusti, X. Luri","submitted_at":"2018-04-25T06:25:26Z","abstract_excerpt":"The second Gaia data release (GDR2) provides precise five-parameter astrometric data (positions, proper motions and parallaxes) for an unprecedented amount of sources (more than $1.3$ billion, mostly stars). The use of this wealth of astrometric data comes with a specific challenge: how does one properly infer from these data the astrophysical parameters of interest?\n  The main - but not only - focus of this paper is the issue of the estimation of distances from parallaxes, possibly combined with other information. We start with a critical review of the methods traditionally used to obtain dis"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1804.09376","kind":"arxiv","version":2},"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":"1804.09376","created_at":"2026-05-18T00:08:07.360453+00:00"},{"alias_kind":"arxiv_version","alias_value":"1804.09376v2","created_at":"2026-05-18T00:08:07.360453+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1804.09376","created_at":"2026-05-18T00:08:07.360453+00:00"},{"alias_kind":"pith_short_12","alias_value":"4A32LKG2RBPQ","created_at":"2026-05-18T12:32:05.422762+00:00"},{"alias_kind":"pith_short_16","alias_value":"4A32LKG2RBPQZCPS","created_at":"2026-05-18T12:32:05.422762+00:00"},{"alias_kind":"pith_short_8","alias_value":"4A32LKG2","created_at":"2026-05-18T12:32:05.422762+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"1906.09040","citing_title":"Astronomical distance scales in the Gaia era","ref_index":29,"is_internal_anchor":true},{"citing_arxiv_id":"1906.09500","citing_title":"Solving the distance discrepancy for the open cluster NGC 2453. The planetary nebula NGC 2452 is not a cluster member","ref_index":27,"is_internal_anchor":true},{"citing_arxiv_id":"2605.23209","citing_title":"TESS Observations of Stochastic Low-frequency Variability in Extreme Helium Stars","ref_index":247,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4A32LKG2RBPQZCPSPYGGEVYNJT","json":"https://pith.science/pith/4A32LKG2RBPQZCPSPYGGEVYNJT.json","graph_json":"https://pith.science/api/pith-number/4A32LKG2RBPQZCPSPYGGEVYNJT/graph.json","events_json":"https://pith.science/api/pith-number/4A32LKG2RBPQZCPSPYGGEVYNJT/events.json","paper":"https://pith.science/paper/4A32LKG2"},"agent_actions":{"view_html":"https://pith.science/pith/4A32LKG2RBPQZCPSPYGGEVYNJT","download_json":"https://pith.science/pith/4A32LKG2RBPQZCPSPYGGEVYNJT.json","view_paper":"https://pith.science/paper/4A32LKG2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1804.09376&json=true","fetch_graph":"https://pith.science/api/pith-number/4A32LKG2RBPQZCPSPYGGEVYNJT/graph.json","fetch_events":"https://pith.science/api/pith-number/4A32LKG2RBPQZCPSPYGGEVYNJT/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4A32LKG2RBPQZCPSPYGGEVYNJT/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4A32LKG2RBPQZCPSPYGGEVYNJT/action/storage_attestation","attest_author":"https://pith.science/pith/4A32LKG2RBPQZCPSPYGGEVYNJT/action/author_attestation","sign_citation":"https://pith.science/pith/4A32LKG2RBPQZCPSPYGGEVYNJT/action/citation_signature","submit_replication":"https://pith.science/pith/4A32LKG2RBPQZCPSPYGGEVYNJT/action/replication_record"}},"created_at":"2026-05-18T00:08:07.360453+00:00","updated_at":"2026-05-18T00:08:07.360453+00:00"}