{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:XKNQ2RRO5ISQU3BTVBRBNTSA53","short_pith_number":"pith:XKNQ2RRO","schema_version":"1.0","canonical_sha256":"ba9b0d462eea250a6c33a86216ce40eef86374f437300497786494e2e2277e2b","source":{"kind":"arxiv","id":"2307.12251","version":1},"attestation_state":"computed","paper":{"title":"Velocity Dispersion $\\sigma_{\\rm aper}$ Aperture Corrections as a Function of Galaxy Properties from Integral-field Stellar Kinematics of 10,000 MaNGA Galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Kai Zhu, Michele Cappellari, Ran Li, Shengdong Lu, Shude Mao, Xiaoyue Cao","submitted_at":"2023-07-23T07:45:52Z","abstract_excerpt":"The second moment of the stellar velocity within the effective radius, denoted by $\\sigma_{\\rm e}^2$, is a crucial quantity in galaxy studies as it provides insight into galaxy properties and their mass distributions. However, large spectroscopic surveys typically do not measure $\\sigma_{\\rm e}$ directly, instead providing $\\sigma_{\\rm aper}$, the second moment of the stellar velocity within a fixed fiber aperture. In this paper, we derive an empirical aperture correction formula, given by $\\sigma_{\\rm aper}/\\sigma_{\\rm e}=(R_{\\rm aper}/R_{\\rm e})^{\\alpha}$, using spatially resolved stellar ki"},"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":"2307.12251","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2023-07-23T07:45:52Z","cross_cats_sorted":[],"title_canon_sha256":"592bf1a8ce53e1c4cd350cf750d9727e7c99d90f21bda479803abe896883e85a","abstract_canon_sha256":"b0661e30ee8666f1f3a7206091d1c4656c34cf843343acfe088b7a12f835595c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:33:51.547422Z","signature_b64":"4XkYWMUhppBBdxxm/T8aDPfZ9/tOAa2Tk2EW7W1wS8mg5IlH4gJ5nBwEFIC3xwAABdLa9O8VNlQ5WHjXxCg/Dg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ba9b0d462eea250a6c33a86216ce40eef86374f437300497786494e2e2277e2b","last_reissued_at":"2026-07-05T06:33:51.546985Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:33:51.546985Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Velocity Dispersion $\\sigma_{\\rm aper}$ Aperture Corrections as a Function of Galaxy Properties from Integral-field Stellar Kinematics of 10,000 MaNGA Galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Kai Zhu, Michele Cappellari, Ran Li, Shengdong Lu, Shude Mao, Xiaoyue Cao","submitted_at":"2023-07-23T07:45:52Z","abstract_excerpt":"The second moment of the stellar velocity within the effective radius, denoted by $\\sigma_{\\rm e}^2$, is a crucial quantity in galaxy studies as it provides insight into galaxy properties and their mass distributions. However, large spectroscopic surveys typically do not measure $\\sigma_{\\rm e}$ directly, instead providing $\\sigma_{\\rm aper}$, the second moment of the stellar velocity within a fixed fiber aperture. In this paper, we derive an empirical aperture correction formula, given by $\\sigma_{\\rm aper}/\\sigma_{\\rm e}=(R_{\\rm aper}/R_{\\rm e})^{\\alpha}$, using spatially resolved stellar ki"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2307.12251","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/2307.12251/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":"2307.12251","created_at":"2026-07-05T06:33:51.547048+00:00"},{"alias_kind":"arxiv_version","alias_value":"2307.12251v1","created_at":"2026-07-05T06:33:51.547048+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2307.12251","created_at":"2026-07-05T06:33:51.547048+00:00"},{"alias_kind":"pith_short_12","alias_value":"XKNQ2RRO5ISQ","created_at":"2026-07-05T06:33:51.547048+00:00"},{"alias_kind":"pith_short_16","alias_value":"XKNQ2RRO5ISQU3BT","created_at":"2026-07-05T06:33:51.547048+00:00"},{"alias_kind":"pith_short_8","alias_value":"XKNQ2RRO","created_at":"2026-07-05T06:33:51.547048+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2509.08041","citing_title":"Uncertainties in the supermassive black hole abundance and implications for the GW background","ref_index":49,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XKNQ2RRO5ISQU3BTVBRBNTSA53","json":"https://pith.science/pith/XKNQ2RRO5ISQU3BTVBRBNTSA53.json","graph_json":"https://pith.science/api/pith-number/XKNQ2RRO5ISQU3BTVBRBNTSA53/graph.json","events_json":"https://pith.science/api/pith-number/XKNQ2RRO5ISQU3BTVBRBNTSA53/events.json","paper":"https://pith.science/paper/XKNQ2RRO"},"agent_actions":{"view_html":"https://pith.science/pith/XKNQ2RRO5ISQU3BTVBRBNTSA53","download_json":"https://pith.science/pith/XKNQ2RRO5ISQU3BTVBRBNTSA53.json","view_paper":"https://pith.science/paper/XKNQ2RRO","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2307.12251&json=true","fetch_graph":"https://pith.science/api/pith-number/XKNQ2RRO5ISQU3BTVBRBNTSA53/graph.json","fetch_events":"https://pith.science/api/pith-number/XKNQ2RRO5ISQU3BTVBRBNTSA53/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XKNQ2RRO5ISQU3BTVBRBNTSA53/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XKNQ2RRO5ISQU3BTVBRBNTSA53/action/storage_attestation","attest_author":"https://pith.science/pith/XKNQ2RRO5ISQU3BTVBRBNTSA53/action/author_attestation","sign_citation":"https://pith.science/pith/XKNQ2RRO5ISQU3BTVBRBNTSA53/action/citation_signature","submit_replication":"https://pith.science/pith/XKNQ2RRO5ISQU3BTVBRBNTSA53/action/replication_record"}},"created_at":"2026-07-05T06:33:51.547048+00:00","updated_at":"2026-07-05T06:33:51.547048+00:00"}