{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2004:MCZLMNE3QGINPA3FTW6D4CTIDH","short_pith_number":"pith:MCZLMNE3","schema_version":"1.0","canonical_sha256":"60b2b6349b8190d783659dbc3e0a6819cb3e694acc0fb40401cdb8a383f65174","source":{"kind":"arxiv","id":"astro-ph/0411403","version":1},"attestation_state":"computed","paper":{"title":"HST and FUSE Spectroscopy of Hot Hydrogen-Rich Central Stars of Planetary Nebulae","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A.I.D. Hoffmann, I. Traulsen, J.W. Kruk, K. Werner, S. Dreizler, T. Rauch","submitted_at":"2004-11-15T14:19:00Z","abstract_excerpt":"High-resolution UV spectra, obtained with HST and FUSE, enable us to analyse hot hydrogen-rich central stars in detail. Up to now, optical hydrogen and helium lines have been used to derive temperature and surface gravity. Those lines, however, are rather insensitive; in particular, neutral helium lines have completely vanished in the hottest central stars. Therefore, we have concentrated on ionization balances of metals, which have a rich line spectrum in the UV, to establish a new temperature scale for our sample. Furthermore, we have determined abundances of light metals, which had been poo"},"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":"astro-ph/0411403","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2004-11-15T14:19:00Z","cross_cats_sorted":[],"title_canon_sha256":"4cd45405dd76223269125abb4abd37897d6bba9b2edd6a013a14ccca5cb9d3ce","abstract_canon_sha256":"f26cf703ba05e5870e173b7bc97ea9dbd10907e2a0f9dcaf25784893faddaca5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T14:13:53.683173Z","signature_b64":"cwT0hfwyW+V5D36TRLIqlQJVPG+jDR7vQhU/l/PYPeUzeXQzJquGKcHe7UsYRAyoDhCQ89v7phzFfTPSOmUhCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"60b2b6349b8190d783659dbc3e0a6819cb3e694acc0fb40401cdb8a383f65174","last_reissued_at":"2026-07-04T14:13:53.682784Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T14:13:53.682784Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"HST and FUSE Spectroscopy of Hot Hydrogen-Rich Central Stars of Planetary Nebulae","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A.I.D. Hoffmann, I. Traulsen, J.W. Kruk, K. Werner, S. Dreizler, T. Rauch","submitted_at":"2004-11-15T14:19:00Z","abstract_excerpt":"High-resolution UV spectra, obtained with HST and FUSE, enable us to analyse hot hydrogen-rich central stars in detail. Up to now, optical hydrogen and helium lines have been used to derive temperature and surface gravity. Those lines, however, are rather insensitive; in particular, neutral helium lines have completely vanished in the hottest central stars. Therefore, we have concentrated on ionization balances of metals, which have a rich line spectrum in the UV, to establish a new temperature scale for our sample. Furthermore, we have determined abundances of light metals, which had been poo"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0411403","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/0411403/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":"astro-ph/0411403","created_at":"2026-07-04T14:13:53.682849+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0411403v1","created_at":"2026-07-04T14:13:53.682849+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0411403","created_at":"2026-07-04T14:13:53.682849+00:00"},{"alias_kind":"pith_short_12","alias_value":"MCZLMNE3QGIN","created_at":"2026-07-04T14:13:53.682849+00:00"},{"alias_kind":"pith_short_16","alias_value":"MCZLMNE3QGINPA3F","created_at":"2026-07-04T14:13:53.682849+00:00"},{"alias_kind":"pith_short_8","alias_value":"MCZLMNE3","created_at":"2026-07-04T14:13:53.682849+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.11394","citing_title":"SDSS-V LVM: Revealing the Physical and Chemical Structure of the Helix Nebula","ref_index":98,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MCZLMNE3QGINPA3FTW6D4CTIDH","json":"https://pith.science/pith/MCZLMNE3QGINPA3FTW6D4CTIDH.json","graph_json":"https://pith.science/api/pith-number/MCZLMNE3QGINPA3FTW6D4CTIDH/graph.json","events_json":"https://pith.science/api/pith-number/MCZLMNE3QGINPA3FTW6D4CTIDH/events.json","paper":"https://pith.science/paper/MCZLMNE3"},"agent_actions":{"view_html":"https://pith.science/pith/MCZLMNE3QGINPA3FTW6D4CTIDH","download_json":"https://pith.science/pith/MCZLMNE3QGINPA3FTW6D4CTIDH.json","view_paper":"https://pith.science/paper/MCZLMNE3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0411403&json=true","fetch_graph":"https://pith.science/api/pith-number/MCZLMNE3QGINPA3FTW6D4CTIDH/graph.json","fetch_events":"https://pith.science/api/pith-number/MCZLMNE3QGINPA3FTW6D4CTIDH/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MCZLMNE3QGINPA3FTW6D4CTIDH/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MCZLMNE3QGINPA3FTW6D4CTIDH/action/storage_attestation","attest_author":"https://pith.science/pith/MCZLMNE3QGINPA3FTW6D4CTIDH/action/author_attestation","sign_citation":"https://pith.science/pith/MCZLMNE3QGINPA3FTW6D4CTIDH/action/citation_signature","submit_replication":"https://pith.science/pith/MCZLMNE3QGINPA3FTW6D4CTIDH/action/replication_record"}},"created_at":"2026-07-04T14:13:53.682849+00:00","updated_at":"2026-07-04T14:13:53.682849+00:00"}