{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:PCFQHNSFZLHUBRBT7NQWS2GJ2A","short_pith_number":"pith:PCFQHNSF","schema_version":"1.0","canonical_sha256":"788b03b645cacf40c433fb616968c9d0150a3972f8b978a6837e011eed82c8aa","source":{"kind":"arxiv","id":"2006.00965","version":2},"attestation_state":"computed","paper":{"title":"$\\textit{Gaia}$ white dwarfs within 40 pc I: spectroscopic observations of new candidates","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Nitta, A. Rebassa-Mansergas, B. T. G\\\"ansicke, C. J. Manser, D. de Martino, D. Koester, E. Cukanovaite, I. Pelisoli, J. Farihi, J. J. Hermes, J.-J. Ren, J. McCleery, M. A. Hollands, M. J. Hoskin, M. R. Schreiber, N. Giammichele, N. P. Gentile Fusillo, O. Toloza, P.-E. Tremblay, P. Izquierdo, R. Raddi, R. Silvotti, S. Charpinet, S. G. Parsons, S. J. Kleinman, S. Jordan, S. O. Kepler, S. Toonen, S. Torres, T. Cunningham, T. R. Marsh, V. Van Grootel, W. R. Brown","submitted_at":"2020-06-01T14:22:10Z","abstract_excerpt":"We present a spectroscopic survey of 230 white dwarf candidates within 40 pc of the Sun from the William Herschel Telescope and Gran Telescopio Canarias. All candidates were selected from $\\textit{Gaia}$ Data Release 2 (DR2) and in almost all cases had no prior spectroscopic classifications. We find a total of 191 confirmed white dwarfs and 39 main-sequence star contaminants. The majority of stellar remnants in the sample are relatively cool ($\\langle T_{\\rm eff} \\rangle$ = 6200 K), showing either hydrogen Balmer lines or a featureless spectrum, corresponding to 89 DA and 76 DC white dwarfs, r"},"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":"2006.00965","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2020-06-01T14:22:10Z","cross_cats_sorted":[],"title_canon_sha256":"23fcce5f101f569cd8bc02532cb5f05de1872d99388bbcc69f3e7b33ac0cdbcb","abstract_canon_sha256":"35041db3d5527e1dfa353030b4ca43b917075c0648d02c664bb6fcb25dfed174"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:16:54.418647Z","signature_b64":"ntcPjjj0d6AxsGXSNailBBplOQ7o1evwpFdPCSsx3Xxdh61jtRrK7fnhhA/CUOd44b6vT/jn6nDrerMUZTYcCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"788b03b645cacf40c433fb616968c9d0150a3972f8b978a6837e011eed82c8aa","last_reissued_at":"2026-07-05T01:16:54.418129Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:16:54.418129Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"$\\textit{Gaia}$ white dwarfs within 40 pc I: spectroscopic observations of new candidates","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Nitta, A. Rebassa-Mansergas, B. T. G\\\"ansicke, C. J. Manser, D. de Martino, D. Koester, E. Cukanovaite, I. Pelisoli, J. Farihi, J. J. Hermes, J.-J. Ren, J. McCleery, M. A. Hollands, M. J. Hoskin, M. R. Schreiber, N. Giammichele, N. P. Gentile Fusillo, O. Toloza, P.-E. Tremblay, P. Izquierdo, R. Raddi, R. Silvotti, S. Charpinet, S. G. Parsons, S. J. Kleinman, S. Jordan, S. O. Kepler, S. Toonen, S. Torres, T. Cunningham, T. R. Marsh, V. Van Grootel, W. R. Brown","submitted_at":"2020-06-01T14:22:10Z","abstract_excerpt":"We present a spectroscopic survey of 230 white dwarf candidates within 40 pc of the Sun from the William Herschel Telescope and Gran Telescopio Canarias. All candidates were selected from $\\textit{Gaia}$ Data Release 2 (DR2) and in almost all cases had no prior spectroscopic classifications. We find a total of 191 confirmed white dwarfs and 39 main-sequence star contaminants. The majority of stellar remnants in the sample are relatively cool ($\\langle T_{\\rm eff} \\rangle$ = 6200 K), showing either hydrogen Balmer lines or a featureless spectrum, corresponding to 89 DA and 76 DC white dwarfs, r"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2006.00965","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2006.00965/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"2006.00965","created_at":"2026-07-05T01:16:54.418188+00:00"},{"alias_kind":"arxiv_version","alias_value":"2006.00965v2","created_at":"2026-07-05T01:16:54.418188+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2006.00965","created_at":"2026-07-05T01:16:54.418188+00:00"},{"alias_kind":"pith_short_12","alias_value":"PCFQHNSFZLHU","created_at":"2026-07-05T01:16:54.418188+00:00"},{"alias_kind":"pith_short_16","alias_value":"PCFQHNSFZLHUBRBT","created_at":"2026-07-05T01:16:54.418188+00:00"},{"alias_kind":"pith_short_8","alias_value":"PCFQHNSF","created_at":"2026-07-05T01:16:54.418188+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/PCFQHNSFZLHUBRBT7NQWS2GJ2A","json":"https://pith.science/pith/PCFQHNSFZLHUBRBT7NQWS2GJ2A.json","graph_json":"https://pith.science/api/pith-number/PCFQHNSFZLHUBRBT7NQWS2GJ2A/graph.json","events_json":"https://pith.science/api/pith-number/PCFQHNSFZLHUBRBT7NQWS2GJ2A/events.json","paper":"https://pith.science/paper/PCFQHNSF"},"agent_actions":{"view_html":"https://pith.science/pith/PCFQHNSFZLHUBRBT7NQWS2GJ2A","download_json":"https://pith.science/pith/PCFQHNSFZLHUBRBT7NQWS2GJ2A.json","view_paper":"https://pith.science/paper/PCFQHNSF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2006.00965&json=true","fetch_graph":"https://pith.science/api/pith-number/PCFQHNSFZLHUBRBT7NQWS2GJ2A/graph.json","fetch_events":"https://pith.science/api/pith-number/PCFQHNSFZLHUBRBT7NQWS2GJ2A/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PCFQHNSFZLHUBRBT7NQWS2GJ2A/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PCFQHNSFZLHUBRBT7NQWS2GJ2A/action/storage_attestation","attest_author":"https://pith.science/pith/PCFQHNSFZLHUBRBT7NQWS2GJ2A/action/author_attestation","sign_citation":"https://pith.science/pith/PCFQHNSFZLHUBRBT7NQWS2GJ2A/action/citation_signature","submit_replication":"https://pith.science/pith/PCFQHNSFZLHUBRBT7NQWS2GJ2A/action/replication_record"}},"created_at":"2026-07-05T01:16:54.418188+00:00","updated_at":"2026-07-05T01:16:54.418188+00:00"}