{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:KTYE6APEVSHSQSSY6MPL7Y22S4","short_pith_number":"pith:KTYE6APE","schema_version":"1.0","canonical_sha256":"54f04f01e4ac8f284a58f31ebfe35a9738771c4459bd24d6bb27ef5e1200aa20","source":{"kind":"arxiv","id":"2104.14481","version":3},"attestation_state":"computed","paper":{"title":"Hints for a gravitational constant transition in Tully-Fisher data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","gr-qc","hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"George Alestas, Ioannis Antoniou, Leandros Perivolaropoulos","submitted_at":"2021-04-29T16:45:21Z","abstract_excerpt":"We use an up to date compilation of Tully-Fisher data to search for transitions in the evolution of the Tully-Fisher relation. Using an up to date data compilation, we find hints at $\\approx 3\\sigma$ level for a transition at critical distances $D_c \\simeq 9 Mpc$ and $D_c \\simeq 17 Mpc$. We split the full sample in two subsamples according to the measured galaxy distance with respect to a splitting distance $D_c$ and identify the likelihood of the best fit slope and intercept of one sample with respect to the best fit corresponding values of the other sample. For $D_c \\simeq 9 Mpc$ and $D_c \\s"},"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":"2104.14481","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2021-04-29T16:45:21Z","cross_cats_sorted":["astro-ph.GA","gr-qc","hep-ph","hep-th"],"title_canon_sha256":"ddec7a96425c3548d115217fdea4b64bd0516d7f2e59efdd2a20ec6285125557","abstract_canon_sha256":"2f941eaf9263900bdcfc458897244cf016a01235cd24b9523d6ed588ac6d8fb4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:20:35.781686Z","signature_b64":"8x5jPwbI+O80XXXdlW5mL5vt6sLVbM6b35bCT3coLPg5cea43vNdNBAEQbqs6U1PwmGI+JgY1pyyOc00FEBsBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"54f04f01e4ac8f284a58f31ebfe35a9738771c4459bd24d6bb27ef5e1200aa20","last_reissued_at":"2026-07-05T03:20:35.781208Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:20:35.781208Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Hints for a gravitational constant transition in Tully-Fisher data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","gr-qc","hep-ph","hep-th"],"primary_cat":"astro-ph.CO","authors_text":"George Alestas, Ioannis Antoniou, Leandros Perivolaropoulos","submitted_at":"2021-04-29T16:45:21Z","abstract_excerpt":"We use an up to date compilation of Tully-Fisher data to search for transitions in the evolution of the Tully-Fisher relation. Using an up to date data compilation, we find hints at $\\approx 3\\sigma$ level for a transition at critical distances $D_c \\simeq 9 Mpc$ and $D_c \\simeq 17 Mpc$. We split the full sample in two subsamples according to the measured galaxy distance with respect to a splitting distance $D_c$ and identify the likelihood of the best fit slope and intercept of one sample with respect to the best fit corresponding values of the other sample. For $D_c \\simeq 9 Mpc$ and $D_c \\s"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2104.14481","kind":"arxiv","version":3},"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/2104.14481/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":"2104.14481","created_at":"2026-07-05T03:20:35.781264+00:00"},{"alias_kind":"arxiv_version","alias_value":"2104.14481v3","created_at":"2026-07-05T03:20:35.781264+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2104.14481","created_at":"2026-07-05T03:20:35.781264+00:00"},{"alias_kind":"pith_short_12","alias_value":"KTYE6APEVSHS","created_at":"2026-07-05T03:20:35.781264+00:00"},{"alias_kind":"pith_short_16","alias_value":"KTYE6APEVSHSQSSY","created_at":"2026-07-05T03:20:35.781264+00:00"},{"alias_kind":"pith_short_8","alias_value":"KTYE6APE","created_at":"2026-07-05T03:20:35.781264+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.12587","citing_title":"Impact of the SNe Ia Magnitude Transition at 20 Mpc on Cosmological Parameter Estimation","ref_index":52,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KTYE6APEVSHSQSSY6MPL7Y22S4","json":"https://pith.science/pith/KTYE6APEVSHSQSSY6MPL7Y22S4.json","graph_json":"https://pith.science/api/pith-number/KTYE6APEVSHSQSSY6MPL7Y22S4/graph.json","events_json":"https://pith.science/api/pith-number/KTYE6APEVSHSQSSY6MPL7Y22S4/events.json","paper":"https://pith.science/paper/KTYE6APE"},"agent_actions":{"view_html":"https://pith.science/pith/KTYE6APEVSHSQSSY6MPL7Y22S4","download_json":"https://pith.science/pith/KTYE6APEVSHSQSSY6MPL7Y22S4.json","view_paper":"https://pith.science/paper/KTYE6APE","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2104.14481&json=true","fetch_graph":"https://pith.science/api/pith-number/KTYE6APEVSHSQSSY6MPL7Y22S4/graph.json","fetch_events":"https://pith.science/api/pith-number/KTYE6APEVSHSQSSY6MPL7Y22S4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KTYE6APEVSHSQSSY6MPL7Y22S4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KTYE6APEVSHSQSSY6MPL7Y22S4/action/storage_attestation","attest_author":"https://pith.science/pith/KTYE6APEVSHSQSSY6MPL7Y22S4/action/author_attestation","sign_citation":"https://pith.science/pith/KTYE6APEVSHSQSSY6MPL7Y22S4/action/citation_signature","submit_replication":"https://pith.science/pith/KTYE6APEVSHSQSSY6MPL7Y22S4/action/replication_record"}},"created_at":"2026-07-05T03:20:35.781264+00:00","updated_at":"2026-07-05T03:20:35.781264+00:00"}