{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:T35WXRAO5GOKW5KBWM6UERBZM3","short_pith_number":"pith:T35WXRAO","schema_version":"1.0","canonical_sha256":"9efb6bc40ee99cab7541b33d42443966d4ff60afbf1802ff4cae0f18f8ab3027","source":{"kind":"arxiv","id":"2402.17741","version":2},"attestation_state":"computed","paper":{"title":"Testing the isotropy of cosmic acceleration with Pantheon+ and SH0ES: A cosmographic analysis","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Carlos A. P. Bengaly, C\\'assio Pigozzo, Jailson S. Alcaniz","submitted_at":"2024-02-27T18:19:32Z","abstract_excerpt":"We use a recent Pantheon+SH0ES compilation of Type Ia Supernova distance measurements at low-redshift, i.e., $0.01 \\leq z \\leq 0.10$, in order to investigate the directional dependency of the deceleration parameter ($q_0$) in different patches ($60^{\\circ}$ size) across the sky, as a probe of the statistical isotropy of the Universe. We adopt a cosmographic approach to compute the cosmological distances, fixing $H_0$ and $M_B$ to reference values provided by the collaboration. By looking at 500 different patches randomly taken across the sky, we find a maximum $\\sim 3\\sigma$ CL anisotropy leve"},"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":"2402.17741","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2024-02-27T18:19:32Z","cross_cats_sorted":["astro-ph.HE","gr-qc"],"title_canon_sha256":"3956797a4ac03d0e2def3c1de657b1f8144c581a8f4f85db398017c604778dc5","abstract_canon_sha256":"ee422a4c710b7cdce6d113a400e005df88503bc3310de02e9e11f342204c3a73"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T08:37:04.974391Z","signature_b64":"chLDpGbkgR8vAvkmpSc/PRw1O3oL8a8CbWoSQIFO8M+99TKTsutKdra2T0N4JOF6nuIKHTyFLY8D3iohvpRSDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9efb6bc40ee99cab7541b33d42443966d4ff60afbf1802ff4cae0f18f8ab3027","last_reissued_at":"2026-07-05T08:37:04.973914Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T08:37:04.973914Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Testing the isotropy of cosmic acceleration with Pantheon+ and SH0ES: A cosmographic analysis","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Carlos A. P. Bengaly, C\\'assio Pigozzo, Jailson S. Alcaniz","submitted_at":"2024-02-27T18:19:32Z","abstract_excerpt":"We use a recent Pantheon+SH0ES compilation of Type Ia Supernova distance measurements at low-redshift, i.e., $0.01 \\leq z \\leq 0.10$, in order to investigate the directional dependency of the deceleration parameter ($q_0$) in different patches ($60^{\\circ}$ size) across the sky, as a probe of the statistical isotropy of the Universe. We adopt a cosmographic approach to compute the cosmological distances, fixing $H_0$ and $M_B$ to reference values provided by the collaboration. By looking at 500 different patches randomly taken across the sky, we find a maximum $\\sim 3\\sigma$ CL anisotropy leve"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2402.17741","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/2402.17741/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":"2402.17741","created_at":"2026-07-05T08:37:04.973973+00:00"},{"alias_kind":"arxiv_version","alias_value":"2402.17741v2","created_at":"2026-07-05T08:37:04.973973+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2402.17741","created_at":"2026-07-05T08:37:04.973973+00:00"},{"alias_kind":"pith_short_12","alias_value":"T35WXRAO5GOK","created_at":"2026-07-05T08:37:04.973973+00:00"},{"alias_kind":"pith_short_16","alias_value":"T35WXRAO5GOKW5KB","created_at":"2026-07-05T08:37:04.973973+00:00"},{"alias_kind":"pith_short_8","alias_value":"T35WXRAO","created_at":"2026-07-05T08:37:04.973973+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2602.11093","citing_title":"New constraints on cosmic anisotropy from galaxy clusters using an improved dipole fitting method","ref_index":147,"is_internal_anchor":false},{"citing_arxiv_id":"2604.04408","citing_title":"Probing cosmic anisotropy with galaxy clusters and supernovae","ref_index":99,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/T35WXRAO5GOKW5KBWM6UERBZM3","json":"https://pith.science/pith/T35WXRAO5GOKW5KBWM6UERBZM3.json","graph_json":"https://pith.science/api/pith-number/T35WXRAO5GOKW5KBWM6UERBZM3/graph.json","events_json":"https://pith.science/api/pith-number/T35WXRAO5GOKW5KBWM6UERBZM3/events.json","paper":"https://pith.science/paper/T35WXRAO"},"agent_actions":{"view_html":"https://pith.science/pith/T35WXRAO5GOKW5KBWM6UERBZM3","download_json":"https://pith.science/pith/T35WXRAO5GOKW5KBWM6UERBZM3.json","view_paper":"https://pith.science/paper/T35WXRAO","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2402.17741&json=true","fetch_graph":"https://pith.science/api/pith-number/T35WXRAO5GOKW5KBWM6UERBZM3/graph.json","fetch_events":"https://pith.science/api/pith-number/T35WXRAO5GOKW5KBWM6UERBZM3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/T35WXRAO5GOKW5KBWM6UERBZM3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/T35WXRAO5GOKW5KBWM6UERBZM3/action/storage_attestation","attest_author":"https://pith.science/pith/T35WXRAO5GOKW5KBWM6UERBZM3/action/author_attestation","sign_citation":"https://pith.science/pith/T35WXRAO5GOKW5KBWM6UERBZM3/action/citation_signature","submit_replication":"https://pith.science/pith/T35WXRAO5GOKW5KBWM6UERBZM3/action/replication_record"}},"created_at":"2026-07-05T08:37:04.973973+00:00","updated_at":"2026-07-05T08:37:04.973973+00:00"}