{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2005:6DNO4PT2YDFIAZT4TRBZPEG3CV","short_pith_number":"pith:6DNO4PT2","schema_version":"1.0","canonical_sha256":"f0daee3e7ac0ca80667c9c439790db155a0805f11644eb4dd7910e5b16c5664d","source":{"kind":"arxiv","id":"astro-ph/0512051","version":1},"attestation_state":"computed","paper":{"title":"Template Rotation Curves for Disk Galaxies","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Barbara Catinella, Martha P. Haynes, Riccardo Giovanelli","submitted_at":"2005-12-02T00:49:30Z","abstract_excerpt":"A homogeneous sample of ~2200 low redshift disk galaxies with both high sensitivity long-slit optical spectroscopy and detailed I-band photometry is used to construct average, or template, rotation curves in separate luminosity classes, spanning 6 magnitudes in I-band luminosity. The template rotation curves are expressed as functions both of exponential disk scale lengths r_d and of optical radii Ropt, and extend out to 4.5-6.5 r_d, depending on the luminosity bin. The two parameterizations yield slightly different results beyond Ropt because galaxies whose Halpha emission can be traced to la"},"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/0512051","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2005-12-02T00:49:30Z","cross_cats_sorted":[],"title_canon_sha256":"5e05a5e65bacf061001519781827c319a9df9c86104d88fd24d83f2abfca4d06","abstract_canon_sha256":"f90132ec51e99f592bf08e11b415a2ba3bef87bd6146f5d3e0b719b379313388"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:14:40.703088Z","signature_b64":"pkNmdzKFxPs9nwW5Gk80OUoHeA+vYvAflPX59NSTu9RwBpimcAqpxYDA+HrtcNJU9V6K/Pz5F2vdxPUEIdi6CA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f0daee3e7ac0ca80667c9c439790db155a0805f11644eb4dd7910e5b16c5664d","last_reissued_at":"2026-07-04T17:14:40.702685Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:14:40.702685Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Template Rotation Curves for Disk Galaxies","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Barbara Catinella, Martha P. Haynes, Riccardo Giovanelli","submitted_at":"2005-12-02T00:49:30Z","abstract_excerpt":"A homogeneous sample of ~2200 low redshift disk galaxies with both high sensitivity long-slit optical spectroscopy and detailed I-band photometry is used to construct average, or template, rotation curves in separate luminosity classes, spanning 6 magnitudes in I-band luminosity. The template rotation curves are expressed as functions both of exponential disk scale lengths r_d and of optical radii Ropt, and extend out to 4.5-6.5 r_d, depending on the luminosity bin. The two parameterizations yield slightly different results beyond Ropt because galaxies whose Halpha emission can be traced to la"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0512051","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/0512051/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/0512051","created_at":"2026-07-04T17:14:40.702742+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0512051v1","created_at":"2026-07-04T17:14:40.702742+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0512051","created_at":"2026-07-04T17:14:40.702742+00:00"},{"alias_kind":"pith_short_12","alias_value":"6DNO4PT2YDFI","created_at":"2026-07-04T17:14:40.702742+00:00"},{"alias_kind":"pith_short_16","alias_value":"6DNO4PT2YDFIAZT4","created_at":"2026-07-04T17:14:40.702742+00:00"},{"alias_kind":"pith_short_8","alias_value":"6DNO4PT2","created_at":"2026-07-04T17:14:40.702742+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.27853","citing_title":"MSA-3D: Rotation Curves and Dark Matter Fractions at z~0.5-1.7 with JWST/NIRSpec","ref_index":83,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/6DNO4PT2YDFIAZT4TRBZPEG3CV","json":"https://pith.science/pith/6DNO4PT2YDFIAZT4TRBZPEG3CV.json","graph_json":"https://pith.science/api/pith-number/6DNO4PT2YDFIAZT4TRBZPEG3CV/graph.json","events_json":"https://pith.science/api/pith-number/6DNO4PT2YDFIAZT4TRBZPEG3CV/events.json","paper":"https://pith.science/paper/6DNO4PT2"},"agent_actions":{"view_html":"https://pith.science/pith/6DNO4PT2YDFIAZT4TRBZPEG3CV","download_json":"https://pith.science/pith/6DNO4PT2YDFIAZT4TRBZPEG3CV.json","view_paper":"https://pith.science/paper/6DNO4PT2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0512051&json=true","fetch_graph":"https://pith.science/api/pith-number/6DNO4PT2YDFIAZT4TRBZPEG3CV/graph.json","fetch_events":"https://pith.science/api/pith-number/6DNO4PT2YDFIAZT4TRBZPEG3CV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/6DNO4PT2YDFIAZT4TRBZPEG3CV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/6DNO4PT2YDFIAZT4TRBZPEG3CV/action/storage_attestation","attest_author":"https://pith.science/pith/6DNO4PT2YDFIAZT4TRBZPEG3CV/action/author_attestation","sign_citation":"https://pith.science/pith/6DNO4PT2YDFIAZT4TRBZPEG3CV/action/citation_signature","submit_replication":"https://pith.science/pith/6DNO4PT2YDFIAZT4TRBZPEG3CV/action/replication_record"}},"created_at":"2026-07-04T17:14:40.702742+00:00","updated_at":"2026-07-04T17:14:40.702742+00:00"}