{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:C2FOSA35RAH7N5ML2QJDLW75U7","short_pith_number":"pith:C2FOSA35","schema_version":"1.0","canonical_sha256":"168ae9037d880ff6f58bd41235dbfda7d5a19c7597bf2ff3f30b1ccb6c446541","source":{"kind":"arxiv","id":"2511.03394","version":2},"attestation_state":"computed","paper":{"title":"The subtle statistics of the distance ladder: On the distance prior and selection effects","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"Harry Desmond, Indranil Banik, Jos\\'e Antonio N\\'ajera, Richard Stiskalek","submitted_at":"2025-11-05T11:55:20Z","abstract_excerpt":"Statistical methodology is rarely considered significant in distance-ladder studies or a potential contributor to the Hubble tension. We suggest it should be, highlighting two appreciable issues. First, astronomical distances are inferred latent parameters, requiring a prior. We show that the (often implicit) uniform priors on distance moduli common to Bayesian distance-ladder analyses bias distances low due to objects being uniformly distributed in volume, which biases the Hubble constant high. Frequentist $\\chi^2$ methods are unbiased for volume- or redshift-limited samples only if the redsh"},"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":"2511.03394","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2025-11-05T11:55:20Z","cross_cats_sorted":["astro-ph.GA"],"title_canon_sha256":"ca063b956ad108149ed92010c90d0c15c29b489e50ad4fd80cb10171454ce712","abstract_canon_sha256":"8e086e6429fbf522c0141546d0282eb815144a8168fb87ebbbf322818c81db81"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-08T14:18:56.838198Z","signature_b64":"taGsMHxPgIxwYHCdqX9OHsPheBEe3TddB1ntRKOnd8l92E52zajj2EYGvVyWGk03c8HrqZhYuKLviXfThEJaAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"168ae9037d880ff6f58bd41235dbfda7d5a19c7597bf2ff3f30b1ccb6c446541","last_reissued_at":"2026-07-08T14:18:56.837699Z","signature_status":"signed_v1","first_computed_at":"2026-07-08T14:18:56.837699Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The subtle statistics of the distance ladder: On the distance prior and selection effects","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA"],"primary_cat":"astro-ph.CO","authors_text":"Harry Desmond, Indranil Banik, Jos\\'e Antonio N\\'ajera, Richard Stiskalek","submitted_at":"2025-11-05T11:55:20Z","abstract_excerpt":"Statistical methodology is rarely considered significant in distance-ladder studies or a potential contributor to the Hubble tension. We suggest it should be, highlighting two appreciable issues. First, astronomical distances are inferred latent parameters, requiring a prior. We show that the (often implicit) uniform priors on distance moduli common to Bayesian distance-ladder analyses bias distances low due to objects being uniformly distributed in volume, which biases the Hubble constant high. Frequentist $\\chi^2$ methods are unbiased for volume- or redshift-limited samples only if the redsh"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2511.03394","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/2511.03394/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":"2511.03394","created_at":"2026-07-08T14:18:56.837763+00:00"},{"alias_kind":"arxiv_version","alias_value":"2511.03394v2","created_at":"2026-07-08T14:18:56.837763+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2511.03394","created_at":"2026-07-08T14:18:56.837763+00:00"},{"alias_kind":"pith_short_12","alias_value":"C2FOSA35RAH7","created_at":"2026-07-08T14:18:56.837763+00:00"},{"alias_kind":"pith_short_16","alias_value":"C2FOSA35RAH7N5ML","created_at":"2026-07-08T14:18:56.837763+00:00"},{"alias_kind":"pith_short_8","alias_value":"C2FOSA35","created_at":"2026-07-08T14:18:56.837763+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2606.02712","citing_title":"Constraints on the gravitational potential from DESI DR2 BAO and its implications for the local void scenario","ref_index":193,"is_internal_anchor":true},{"citing_arxiv_id":"2606.12980","citing_title":"A Review on Resolving the Hubble Tension via Late-Universe Physics","ref_index":167,"is_internal_anchor":true},{"citing_arxiv_id":"2606.17142","citing_title":"Hawai`i Supernova Flows: Bulk Flow Measurements using SNe Ia in the Optical and NIR","ref_index":18,"is_internal_anchor":true},{"citing_arxiv_id":"2606.27195","citing_title":"HALO II: Constraining Hubble constant $H_{0}$ through continuum delay fitting of Fairall 9","ref_index":30,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/C2FOSA35RAH7N5ML2QJDLW75U7","json":"https://pith.science/pith/C2FOSA35RAH7N5ML2QJDLW75U7.json","graph_json":"https://pith.science/api/pith-number/C2FOSA35RAH7N5ML2QJDLW75U7/graph.json","events_json":"https://pith.science/api/pith-number/C2FOSA35RAH7N5ML2QJDLW75U7/events.json","paper":"https://pith.science/paper/C2FOSA35"},"agent_actions":{"view_html":"https://pith.science/pith/C2FOSA35RAH7N5ML2QJDLW75U7","download_json":"https://pith.science/pith/C2FOSA35RAH7N5ML2QJDLW75U7.json","view_paper":"https://pith.science/paper/C2FOSA35","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2511.03394&json=true","fetch_graph":"https://pith.science/api/pith-number/C2FOSA35RAH7N5ML2QJDLW75U7/graph.json","fetch_events":"https://pith.science/api/pith-number/C2FOSA35RAH7N5ML2QJDLW75U7/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/C2FOSA35RAH7N5ML2QJDLW75U7/action/timestamp_anchor","attest_storage":"https://pith.science/pith/C2FOSA35RAH7N5ML2QJDLW75U7/action/storage_attestation","attest_author":"https://pith.science/pith/C2FOSA35RAH7N5ML2QJDLW75U7/action/author_attestation","sign_citation":"https://pith.science/pith/C2FOSA35RAH7N5ML2QJDLW75U7/action/citation_signature","submit_replication":"https://pith.science/pith/C2FOSA35RAH7N5ML2QJDLW75U7/action/replication_record"}},"created_at":"2026-07-08T14:18:56.837763+00:00","updated_at":"2026-07-08T14:18:56.837763+00:00"}